Untitled - ESO
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<strong>ESO</strong><br />
European Organisation<br />
for Astronomical<br />
Research in the<br />
Southern Hemisphere<br />
Annual Report 2006<br />
presented to the Council by the<br />
Director General<br />
Dr. Catherine Cesarsky
About <strong>ESO</strong><br />
<strong>ESO</strong> is the foremost intergovernmental<br />
European Science and Technology organisation<br />
in the field of ground-based<br />
astrophysics. It is supported by 1 countries:<br />
Belgium, Denmark, France, Finland,<br />
Germany, Italy, the Netherlands, Portugal,<br />
Spain, Sweden, Switzerland and the<br />
United Kingdom. The Czech Republic is<br />
currently in the process of joining <strong>ESO</strong><br />
(Status as of 31.1 . 006). Further<br />
countries have expressed interest in<br />
membership.<br />
Created in 196 , <strong>ESO</strong> provides state-ofthe-art<br />
research facilities to European<br />
astronomers and astrophysicists. In pursuit<br />
of this task, <strong>ESO</strong>’s activities cover<br />
a wide spectrum including the design<br />
and construction of world-class groundbased<br />
observational facilities for the<br />
member-state scientists, large telescope<br />
projects, design of innovative scientific<br />
instruments, developing new and advanced<br />
technologies, furthering European<br />
cooperation and carrying out European<br />
educational programmes.<br />
<strong>ESO</strong> operates the La Silla Paranal Observatory<br />
at several sites in the Atacama Desert<br />
region of Chile. The first site is at<br />
La Silla, a 400 m high mountain 600 km<br />
north of Santiago de Chile. It is equipped<br />
with several optical telescopes with mirror<br />
diameters of up to 3.6 metres. The<br />
3.5-m New Technology Telescope (NTT)<br />
was the first in the world to have a computer-controlled<br />
main mirror.<br />
Whilst La Silla remains one of the scientifically<br />
most productive observing sites in<br />
the world, the 600 m high Paranal site<br />
with the Very Large Telescope array (VLT)<br />
is the flagship facility of European astronomy.<br />
Paranal is situated about 130 km<br />
south of Antofagasta in Chile, 1 km inland<br />
from the Pacific Coast in what is<br />
probably the driest area in the world. Scientific<br />
operations began in 1999 and have<br />
resulted in a high number of extremely<br />
successful research programmes. The<br />
VLT is a most unusual telescope, based<br />
on the latest technology. It is not just<br />
one, but an array of four telescopes, each<br />
with a main mirror of 8. -m diameter.<br />
With one such telescope, images of celestial<br />
objects as faint as magnitude 30<br />
have been obtained in a one-hour exposure.<br />
This corresponds to seeing objects<br />
that are four billion times fainter than<br />
what can be seen with the naked eye.<br />
<strong>ESO</strong> Annual Report 006<br />
One of the most exciting features of the<br />
VLT is the possibility to use it as a giant<br />
optical interferometer (VLT Interferometer<br />
or VLTI). This is done by combining the<br />
light from several of the telescopes, including<br />
one or more of four 1.8-m moveable<br />
Auxiliary Telescopes. In the interferometric<br />
mode, one can reach the resolution on<br />
the sky that would be obtained with a<br />
telescope of the size of the separation<br />
between the most distant of the combined<br />
mirrors.<br />
Artist’s impression<br />
of a part of ALMA<br />
on Chajnantor.<br />
The . -m, the 3.5-m<br />
NTT and the 3.6-m<br />
telescopes at La Silla.<br />
In 006, over 1700 proposals were made<br />
for the use of <strong>ESO</strong> telescopes. They<br />
have resulted in a large number of peerreviewed<br />
publications. In 006, 630 refereed<br />
papers based on data from <strong>ESO</strong><br />
telescopes were published.<br />
<strong>ESO</strong> is also a major partner in the Atacama<br />
Large Millimeter/Submillimeter Array<br />
(ALMA), one of the largest ground-based<br />
astronomy projects of the next decade.
ALMA will be comprised of a main array<br />
of fifty 1 -m submillimetre quality antennas,<br />
with baselines of several kilometres.<br />
An additional compact array of four 1 -m<br />
and twelve 7-m antennas complements<br />
the main array. Construction of ALMA<br />
started in 003 and will be completed in<br />
01 ; it will become incrementally operational<br />
from 010 on. ALMA is located on<br />
the high-altitude Llano de Chajnantor<br />
(5 000 m elevation), east of the village of<br />
San Pedro de Atacama in Chile. The<br />
ALMA project is a partnership between<br />
Europe, Japan and North America in<br />
cooperation with the Republic of Chile.<br />
ALMA is funded in Europe by <strong>ESO</strong>, in<br />
Japan by the National Institutes of Natural<br />
Sciences in cooperation with the<br />
Academia Sinica in Taiwan and in North<br />
America by the U.S. National Science<br />
Foundation in cooperation with the National<br />
Research Council of Canada.<br />
ALMA construction and operations are<br />
led on behalf of Europe by <strong>ESO</strong>, on behalf<br />
of Japan by the National Astronomical<br />
Observatory of Japan and on be-<br />
half of North America by the National<br />
Radio Astronomy Observatory, which is<br />
managed by Associated Universities, Inc.<br />
The Chajnantor site is also home of the<br />
1 -m APEX submillimetre/millimetre-wavelength<br />
telescope, operated by <strong>ESO</strong> on<br />
behalf of the Onsala Space Observatory,<br />
the Max-Planck Institute for Radio Astronomy<br />
and <strong>ESO</strong> itself.<br />
<strong>ESO</strong> has built up considerable expertise<br />
in developing, integrating and operat-<br />
ing large astronomical telescopes at remote<br />
sites. Together with the ideas developed<br />
in the framework of the OWL<br />
Conceptual Study and the EC co-funded<br />
Extremely Large Telescope Design Study,<br />
this expertise forms the backbone of<br />
the effort to develop a next-generation<br />
extremely large ground-based optical/infrared<br />
telescope for Europe’s astronomers.<br />
For this project, currently known as<br />
the European Extremely Large Telescope<br />
(E-ELT), <strong>ESO</strong> has developed a basic reference<br />
design for a 4 -m telescope with<br />
a novel five-mirror optical concept. The<br />
current detailed design phase is scheduled<br />
to be completed by the end of 009.<br />
The <strong>ESO</strong> headquarters are located in<br />
Garching, near Munich, Germany. This is<br />
the scientific, technical and administrative<br />
centre of <strong>ESO</strong> where technical development<br />
programmes are carried out to provide<br />
the observatories with the most<br />
advanced instruments. It is also home for<br />
the Space Telescope – European Coordinating<br />
Facility (ST-ECF), operated jointly<br />
by <strong>ESO</strong> and the European Space Agency<br />
(ESA).<br />
Artist’s impression<br />
of the E-ELT.<br />
The VLT Array<br />
at Paranal.<br />
<strong>ESO</strong> Annual Report 006<br />
3
Contents<br />
Foreword 6<br />
Introduction 7<br />
Research Highlights 10<br />
La Silla Paranal Observatory 30<br />
Atacama Large Millimeter/Submillimeter Array 38<br />
The European Extremely Large Telescope 45<br />
Organisation and Personnel<br />
Organigramme 49<br />
List of Personnel 50<br />
Personnel Services 5<br />
Instrumentation 53<br />
Technical Developments 57<br />
Science Archive Operation 60<br />
The European Virtual Observatory 6<br />
ST-ECF 63<br />
Public Outreach 65<br />
<strong>ESO</strong> Press Releases 68<br />
Relations with Chile 70<br />
European Affairs 7<br />
Committees<br />
Council 76<br />
The Scientific Technical Committee 77<br />
Finance Committee 80<br />
The Users’ Committee 80<br />
The Observing Programmes Commitee 8<br />
Summary of Use of Telescopes by Discipline 84<br />
Publications 86<br />
Financial Statement 105<br />
Four Seasons at a Glance 106<br />
Glossary of Frequently Used Acronyms 110<br />
DVD 113<br />
<strong>ESO</strong> Annual Report 006<br />
5
6<br />
<strong>ESO</strong> Annual Report 006<br />
Foreword<br />
It would be evident even to the most casual<br />
observer that <strong>ESO</strong> is as vibrant and<br />
dynamic as ever with a strong track record<br />
of excellence and ambitious projects.<br />
Some of these projects are now operational<br />
facilities, some are under construction<br />
and others are in the design phase.<br />
The task of Council is to provide the overall<br />
strategy and a framework for the further<br />
evolution of the organisation and it is<br />
this forward-looking task that makes the<br />
work of Council members so rewarding.<br />
Arguably, the most important issue<br />
regarding the future that Council had to<br />
address in 006 was the decision to<br />
endorse the proposal to embark on the<br />
detailed design study for a European<br />
Extremely Large Telescope (E-ELT). The<br />
study, scheduled to last for three years,<br />
will lead to a proposal for construction for<br />
Council to consider in due course. Council<br />
was able to take this decision not<br />
least because of the impressive preparatory<br />
work by <strong>ESO</strong> and the various working<br />
groups with strong involvement by the<br />
scientific community across Europe. In<br />
taking this important step Council recognised<br />
that the E-ELT is crucial to the further<br />
development of European astronomy<br />
and its ability to retain a competitive edge<br />
on a global stage.<br />
Building the E-ELT is as big a challenge<br />
to all of us as any of the preceding projects<br />
in <strong>ESO</strong>’s already impressive project<br />
portfolio. We can succeed only if we<br />
manage to harness the necessary resources<br />
– financial, technological and<br />
human. It is therefore gratifying that more<br />
potential member countries continue to<br />
express interest in joining. I was delighted<br />
that the entry of Spain as the 1 th member<br />
state of <strong>ESO</strong> was becoming a reality<br />
at the end of the year, with just the final<br />
formalities pending. Spain plays an important<br />
role in European astronomy and<br />
its membership of <strong>ESO</strong> is a very welcome.<br />
At its December meeting Council<br />
also approved the entry of the Czech<br />
Republic, the first of the Central European<br />
countries to join.<br />
The expansion of <strong>ESO</strong>’s membership<br />
base is clearly important in the context of<br />
the E-ELT. It also strengthens <strong>ESO</strong> as<br />
the focal point for Europe’s astronomers<br />
and thus reinforces the significance of<br />
the organisation as an important actor in<br />
the European Research Area.<br />
<strong>ESO</strong>’s overall role in the European research<br />
landscape is an important question<br />
that warrants serious consideration.<br />
At the June meeting of Council, the<br />
Science Strategy Working Group presented<br />
several scenarios that are now<br />
subject to further debate.<br />
Entrusting the management of the organisation<br />
to the most competent leader<br />
is clearly most important to all of us. With<br />
the term of the current Director Gener-<br />
al coming to its end by September 007,<br />
Council set up a search committee for<br />
the next DG, leading to the selection<br />
of Prof. Tim de Zeeuw as successor to<br />
Dr. Catherine Cesarsky. With this decision,<br />
Council has provided the base<br />
for a smooth transition of the management<br />
of <strong>ESO</strong>.<br />
In conclusion I am pleased to note that by<br />
the end of the year, Council, working with<br />
the Executive, had acted to set <strong>ESO</strong> on<br />
a track towards a very exciting future and<br />
I wish to express my sincere thanks to<br />
all involved in this important endeavour.<br />
Richard Wade<br />
President of the <strong>ESO</strong> Council
Introduction<br />
In my introduction to the 005 Annual<br />
Report, I described that year as a pivotal<br />
year for <strong>ESO</strong>. This was not least on the<br />
basis of the progress regarding the ALMA<br />
project. Looking at 006, however, it is<br />
impossible not to use similar vocabulary<br />
again. Shortly before Christmas 005 I<br />
had launched a very ambitious plan aiming<br />
to move quickly and decisively towards<br />
the realisation of the European<br />
Extremely Large Telescope (E-ELT). The<br />
task was daunting: the plan foresaw<br />
the establishment of five mixed Community-<strong>ESO</strong><br />
topical Working Groups with-<br />
in the shortest space of time to lay the<br />
groundwork for a set of extremely intense<br />
activities to be conducted within a ‘core’<br />
Working Group, the ELT Science and Engineering<br />
Working Group, supplemented<br />
by an ELT Standing Advisory Committee.<br />
Before the end of 006, and with broad<br />
involvement of the scientific community,<br />
we wanted to be able to present a basic<br />
reference design and ask Council for approval<br />
of a Phase B for the project.<br />
The way the scientific community and the<br />
<strong>ESO</strong> staff embraced the plan was truly<br />
encouraging, with 85 out of 88 invitees<br />
enthusiastically agreeing to board the<br />
‘ELT-train’. Now, 1 months later, the train<br />
has arrived – precisely on schedule.<br />
At the 7 November–1 December conference<br />
in Marseille, which was attended by<br />
more than 50 scientists, the results were<br />
presented to and discussed by the<br />
scientific community. Only a week later,<br />
Council gave the green light to embark<br />
on Phase B, a three-year long detailed<br />
design study that should allow us to present<br />
a proposal for construction to the<br />
<strong>ESO</strong> Council in the 009– 010 time frame.<br />
The basis for the design study is a 4 -m<br />
telescope with a unique five-mirror design.<br />
It constitutes an innovative design<br />
solution that takes account of all the concerns<br />
raised with previous design proposals.<br />
Yet, while pursuing the detailed<br />
studies, we retain the option of the classical<br />
Gregorian telescope as a fallback<br />
possibility.<br />
These twelve months have seen a remarkable<br />
coming together of people,<br />
ideas, policy decisions and much hard<br />
work. The outcome is a tribute to the<br />
ability of Europe’s astronomers to set ambitious<br />
goals but also to forge tenable<br />
compromises – to set their sights on the<br />
sky, while keeping their feet on the<br />
ground.<br />
Aside from the impressive mobilisation<br />
of the scientific community, two other elements<br />
in the jigsaw puzzle should be<br />
mentioned: the inclusion of the ELT in the<br />
so-called ESFRI-list of large future research<br />
infrastructures deemed to be of<br />
European interest, and the setting up at<br />
<strong>ESO</strong> of a dedicated E-ELT project office<br />
with cross-divisional parts in a matrix<br />
structure. The former embeds the E-ELT<br />
decision process in the wider European<br />
science policy scene, a necessary step in<br />
the age of the European Research Area.<br />
The latter is part of preparing <strong>ESO</strong> for<br />
the challenges arising from the fact that<br />
we have become a multi-project organisation.<br />
A new step in the matrix structure<br />
foreseen to cope with this new situation<br />
is the creation of the Software Development<br />
Division, encompassing software<br />
developers from the previous Data Management<br />
Division, the Technological<br />
Division, and ALMA. Meanwhile, the new<br />
Data Management Operations division<br />
serves the VLT/VLTI and the ALMA ARC,<br />
ensuring continued attention to our running<br />
operations.<br />
At Paranal, we introduced in January the<br />
Laser Guide Star (LGS) system on Yepun.<br />
At <strong>ESO</strong>, as elsewhere, success requires<br />
hard work, and indeed it became evident<br />
that the LGS launch-telescope needed<br />
<strong>ESO</strong> Annual Report 006<br />
Photo: Volker Steger<br />
modifications in order to perform as required.<br />
However, with the improvements<br />
carried out, the LGS commissioning<br />
could resume by October, and the facility<br />
will be fully used in scientific observations<br />
early in 007.<br />
Also this year, the fourth Auxiliary Telescope<br />
saw First Light, completing the<br />
suite of ATs for the Very Large Telescope<br />
Interferometer (VLTI) and we thank<br />
the Belgians, the Swiss and the Italians<br />
for providing the additional resources<br />
needed for this significant improvement.<br />
Progress was also achieved with respect<br />
to VISTA, the 4-m survey telescope that<br />
forms a part of the UK entrance fee to<br />
<strong>ESO</strong>. In May 006 most of the structural<br />
parts were shipped to Chile. The telescope<br />
enclosure was accepted in Chile,<br />
while the camera was ready to leave<br />
the UK for Chile at the end of the year.<br />
The coating plant that comes with VISTA<br />
was also being installed. This facility<br />
will prove a useful resource as it will allow<br />
mirrors to be silver rather than alumin-<br />
ium coated. Public Surveys for VISTA<br />
have been selected and I am glad to see<br />
that there were so many proposals, with<br />
the result that a very good set of surveys<br />
have been chosen.<br />
The other survey telescope, the .5-m<br />
VST, remains on the other hand a matter<br />
of concern due to serious, continued<br />
delay. Nonetheless, following a visit by<br />
<strong>ESO</strong> engineers to Naples, plans were<br />
made for shipping of the telescope struc-<br />
7
ture early in 007. The 3 -CCD-mosaic<br />
OmegaCAM wide-field optical camera for<br />
the VST, which was developed by <strong>ESO</strong>,<br />
was, however, finished. The primary<br />
mirror of the telescope is also now ready,<br />
in Moscow.<br />
In June the VLT cryogenic high-resolution<br />
infrared echelle spectrograph CRIRES<br />
was commissioned at the Nasmyth focus<br />
of Antu, marking the completion of the<br />
first-generation VLT instrumentation. First<br />
steps of Science Verification also took<br />
place during the year and work was progressing<br />
very well on developing a de-<br />
dicated pipeline for the CRIRES data reduction.<br />
At the same time, the near-infrared imager<br />
HAWK-I, often described as a VLT<br />
‘generation 1.5’ instrument, was in an<br />
advanced stage, undergoing Assembly<br />
and Integration at <strong>ESO</strong> Garching, paving<br />
the way for a shipment to Chile in 007.<br />
Important progress was also achieved<br />
with respect to the second-generation<br />
instrumentation. In September, an agreement<br />
was signed with an extended<br />
consortium led by LAOG in Grenoble to<br />
develop SPHERE. The revised design<br />
fulfils all the requirements set by the <strong>ESO</strong><br />
Scientific Technical Committee (STC) for<br />
the planet-finder instrument.<br />
Meanwhile, the multi-conjugate adap-<br />
tive optics demonstrator (MAD) was successfully<br />
tested in the laboratory in<br />
Garching, passing its PAE (Preliminary<br />
Acceptance Europe) in December and<br />
thus being ready to go to Chile.<br />
All of these instruments constitute technological<br />
marvels; we are thrilled by their<br />
ingenious design and capabilities, for<br />
they allow us to do science at the cuttingedge.<br />
This is undoubtedly also the case<br />
for AMBER, the interferometric beam<br />
combiner for the VLTI, which was offered<br />
to the scientific community from P 76, and<br />
it is gratifying to see a string of truly impressive<br />
scientific results, scheduled to<br />
appear in a special issue of A&A in March<br />
007.<br />
AMBER is not the only facility to have this<br />
honour, as in July 006 the submillimetric<br />
telescope APEX was also the topic of<br />
8<br />
<strong>ESO</strong> Annual Report 006<br />
a special A&A issue, with no fewer than<br />
6 articles based on early science being<br />
published.<br />
Although some of the great scientific<br />
achievements made with <strong>ESO</strong>’s telescopes<br />
are published in the Research<br />
Highlights, I cannot resist mentioning<br />
a few. In January, the discovery of the<br />
smallest exoplanet found so far, a five-<br />
Earth-mass planet, was announced.<br />
The planet was discovered by microlensing,<br />
with the help of a worldwide network<br />
of telescopes, among which the 1.5-m<br />
Danish telescope at La Silla was the one<br />
that could pick up the signal due to the<br />
planet. This discovery heralds a new era<br />
in the search for exoplanets. The identification,<br />
also at La Silla but with the 3.6-m<br />
telescope this time, of a planetary system<br />
containing three Neptune-mass planets<br />
and an asteroid belt, is also of crucial<br />
importance in this very hot research area.<br />
With the VLT, astronomers have found<br />
possible proofs of stellar vampirism in the<br />
globular cluster 47 Tucanae. Indeed,<br />
some hot, bright, and apparently young<br />
stars in the cluster present less carbon<br />
and oxygen than the majority of their sisters,<br />
indicating that these few stars likely<br />
formed by taking their material from another<br />
star. Farther away, the combination<br />
of adaptive optics techniques with the<br />
new SINFONI integral-field spectrograph<br />
allowed astronomers to study a very distant<br />
galaxy with a record-breaking resolution<br />
of a mere 0.15 arcseconds, giving<br />
an unprecedented detailed view of the<br />
anatomy of such a distant proto-disc galaxy.<br />
The observations imply that large<br />
disc galaxies akin to our Milky Way must<br />
have formed on a rapid timescale, only<br />
three billion years after the Big Bang.<br />
With the VISIR instrument, astronomers<br />
have mapped the disc around a star<br />
more massive than the Sun. The very extended<br />
and flared disc most likely contains<br />
enough gas and dust to spawn planets.<br />
It appears as a precursor of debris<br />
discs such as those around Vega-like<br />
stars and thus provides the rare opportunity<br />
to witness the conditions prevailing<br />
prior to or during planet formation. The<br />
huge gain in resolving power offered<br />
by the VLTI also made a difference. VINCI<br />
and MIDI were used to discover envelopes<br />
around three Cepheids, massive<br />
pulsating stars that play a crucial role<br />
in cosmology, being one of the first steps<br />
on the cosmic distance ladder.<br />
Of course, these are but a few examples<br />
of the science that is based on observations<br />
with <strong>ESO</strong> telescopes. In fact, on<br />
average, our user community produces<br />
close to two papers with <strong>ESO</strong> data a day<br />
all year round, more than any other<br />
ground-based observatory in the world.<br />
<strong>ESO</strong> telescopes generate a large quantity<br />
of data, which are kept for reuse in the<br />
Science Archive. With the coming online<br />
of VISTA, and later of the VST, the flow<br />
of data will considerably increase, reaching<br />
100 TB of data per year. To anticipate<br />
this, <strong>ESO</strong> is preparing a Petabyte-class<br />
archive that will be ready next year.<br />
In July, the first data release of the UKIRT<br />
Infrared Deep Sky Survey (UKIDSS)<br />
was available, providing a year of data to<br />
the <strong>ESO</strong> community of users. The full survey<br />
is expected to take seven years. But<br />
this first set of observations already<br />
shows how powerful the full survey will<br />
be at finding rare objects that hold vital<br />
clues to how stars and galaxies in our<br />
Universe formed. Indeed, the new data<br />
on young galaxies is already challenging<br />
current thinking on galaxy formation,<br />
revealing galaxies that are massive at a<br />
much earlier stage of development than<br />
anticipated.<br />
In 005, the ALMA project was set on<br />
track with major industrial contracts<br />
being awarded. The year 006 was a year<br />
of construction: the road from the highway<br />
to the high site, the AOS, was completed<br />
at its full width, and construction<br />
of the buildings at the OSF, at 900 m<br />
altitude, began at full speed. The road<br />
and the OSF buildings are deliverables for<br />
which <strong>ESO</strong> is responsible.<br />
In Europe, the first cryostats and receivers<br />
for two frequency bands were delivered.<br />
By now, prototypes are available<br />
for all four ALMA frequencies (0.6, 0.9,<br />
1.3 and 3 mm), fulfilling specifications. For<br />
the cryostats, a first series of eight was
manufactured and delivered. The first cartridge<br />
for Band 7 exceeded the specifications,<br />
being much more sensitive than<br />
initially planned. This, in effect, is equivalent<br />
to having many more antennas.<br />
First tests on the SMA on Mauna Kea of<br />
the water vapour radiometers proved<br />
the technology to be highly successful. It<br />
was thus decided to implement these<br />
in ALMA, thereby further increasing the<br />
output of this unique facility.<br />
Another important milestone for the<br />
ALMA project was reached in June with<br />
the signing of the agreement with Japan<br />
(and Taiwan), bringing a Compact Ar-<br />
ray and other wavebands to the project.<br />
According to the agreement, the ALMA<br />
array will thus initially comprise 66 antennas,<br />
54 of them with 1 -m diameter<br />
and 1 7-m antennas.<br />
ALMA is the first quasi-global project in<br />
ground-based astronomy, and it is fitting<br />
that <strong>ESO</strong>, with its international orientation,<br />
plays its part in it. That <strong>ESO</strong> plays an<br />
important role on the international scene<br />
was also visible during the 006 SPIE<br />
conference, with a large involvement in<br />
the organisation and numerous presentations<br />
by <strong>ESO</strong> staff. The SPIE meeting<br />
also allowed for starting most fruitful discussions<br />
with other ELT groups, especially<br />
the TMT, that have since been ongoing.<br />
Equally, in November, a top-level meeting<br />
on exoplanets took place in Washington<br />
D.C. between <strong>ESO</strong>, ESA, NSF and NASA.<br />
Back in Europe, the IAU General Assembly<br />
was held in Prague. These triennial<br />
events always provide a unique opportunity<br />
to experience first-hand the progress<br />
across the entire range of astronomy,<br />
as well as to meet friends and colleagues<br />
from one’s own and other sub-fields, and<br />
this General Assembly certainly lived<br />
up to expectation. Some 800 participants<br />
from around the world attended the<br />
event. Again, <strong>ESO</strong> was well presented,<br />
in the various sessions and also with a<br />
major information stand – fitting in the<br />
context of our ongoing talks with the<br />
Czech Republic.<br />
We continued our collaboration with ESA,<br />
with the publication of two joint reports<br />
on Herschel/ALMA synergies and fundamental<br />
cosmology, respectively, as visible<br />
signs of the coordination efforts in this<br />
field on our continent.<br />
In June, with our Chilean colleagues we<br />
celebrated the 10th anniversary of the<br />
supplementary agreement with Chile,<br />
which not only paved the way for <strong>ESO</strong>’s<br />
operations in Chile in the VLT era, but<br />
also provided strong impulses to Chilean<br />
astronomy. Some of the results are described<br />
in the book “10 Years Exploring<br />
the Universe” that was published on this<br />
occasion. We are pleased that our relations<br />
with Chile, its scientific community<br />
and its people, remain strong and positive.<br />
Moving from international relations in general<br />
to the issue of new member states,<br />
we were happy when, in February, Spain<br />
took a decisive step towards full membership<br />
with the signing in Madrid of a<br />
statement aiming at accession to the<br />
<strong>ESO</strong> Convention effective from 1 July.<br />
As it turned out, the ratification process<br />
needed more time and the last steps remained<br />
to be completed by the end of<br />
the year. Nonetheless, we were assured<br />
by the Spanish authorities of the intent<br />
to respect the accession date, as set out<br />
in the February statement.<br />
In parallel, negotiations with the Czech<br />
Republic progressed rapidly. At the<br />
December meeting, Council approved<br />
the agreement, which foresaw Czech<br />
membership as of 1 January 007. A few<br />
days later, the agreement was also approved<br />
by the Czech Government, and<br />
on December the agreement was<br />
signed at a ceremony in Prague. As in the<br />
case of Spain, however, the parliamentary<br />
approval and the subsequent deposition<br />
of the instrument of ratification remained<br />
to be completed.<br />
<strong>ESO</strong> is a high-tech research organisation<br />
with a global perspective. As such it must<br />
meet the challenges of the dynamic, international<br />
labour market, competing for<br />
the best and most talented staff. With the<br />
opening of the IPP/<strong>ESO</strong> crèche for our<br />
staff in Garching, we have taken further<br />
steps to create a working climate that<br />
is also amenable to family needs. In Chile,<br />
we entered collective bargaining, concluding<br />
collective arrangements valid for<br />
three years.<br />
Having physical surroundings that foster<br />
human and intellectual exchange is another<br />
important element. It is therefore<br />
good that the long-awaited expansion of<br />
our Headquarters building moved clos-<br />
er as, with the help of the German authorities,<br />
we made progress towards securing<br />
the land to the south of the existing<br />
premises.<br />
In its 45th year, <strong>ESO</strong> remains a strong<br />
and dynamic organisation, not just full of<br />
ideas and initiatives but with a clear will<br />
to harness these into projects that can<br />
serve our users. An important tool in this<br />
process is the Medium Range Implementation<br />
Plan, which was endorsed by<br />
Council at its December meeting. This<br />
plan provides a clear path for <strong>ESO</strong>’s development<br />
over the next four years; now<br />
it is for us to turn it into reality.<br />
Catherine Cesarsky<br />
Director General, <strong>ESO</strong><br />
<strong>ESO</strong> Annual Report 006<br />
9
Research Highlights<br />
In 006 <strong>ESO</strong> again proved that it has<br />
the telescopes and instruments to maintain<br />
its lead position in the quest for<br />
exoplanets, that is, planets that orbit a<br />
star other than the Sun. Using a variety<br />
of telescopes, at La Silla and Paranal,<br />
astronomers were able to find the smallest<br />
exoplanet yet discovered — a five-<br />
Earth-mass icy world — as well as a complete<br />
planetary system composed of 3<br />
Neptune-mass planets. Also noteworthy<br />
is the study of free-floating planets that<br />
appear to harbour discs and even form as<br />
twins, thereby sharing many properties<br />
of stars.<br />
The Comet With a Broken Heart<br />
On the night of 3/ 4 April, <strong>ESO</strong>’s Very<br />
Large Telescope observed fragment B of<br />
the comet Schwassmann-Wachmann<br />
3 that had split a few days earlier. To their<br />
great surprise, the <strong>ESO</strong> astronomers<br />
discovered that the piece just ejected by<br />
fragment B was splitting again! Five<br />
other mini-comets are also visible on the<br />
image. The comet seems thus doomed<br />
to disintegrate but the question remains in<br />
how much time.<br />
Comet 73P/Schwassmann-Wachmann 3<br />
(SW 3) is a body with a very tormented<br />
past. This comet revolves around the Sun<br />
in about 5.4 years, in a very elongated<br />
orbit that brings it from inwards of the<br />
Earth’s orbit to the neighbourhood of giant<br />
planet Jupiter. In 1995, when it was<br />
coming ‘close’ to the Earth, it underwent<br />
a dramatic and completely unexpected,<br />
thousandfold brightening. Observations<br />
in 1996, with <strong>ESO</strong>’s New Technology<br />
Telescope and 3.6-m telescope, at La<br />
Silla, showed that this was due to the fact<br />
that the comet had split into three distinct<br />
pieces. Later, in December 1996, two<br />
more fragments were discovered. At the<br />
last comeback, in 001, of these five<br />
10<br />
<strong>ESO</strong> Annual Report 006<br />
Talking about discs, the VISIR instrument<br />
allowed astronomers to map a disc<br />
around a very young star, possibly witnessing<br />
the precursor of a planetary system.<br />
But it is not all about stars and planets.<br />
In 006, astronomers provided unique<br />
insights into two classes of important<br />
objects in cosmology, Cepheids and<br />
Type Ia supernovae.<br />
They also have revealed several cases of<br />
stellar vampirism, including one on a<br />
very big scale. In other studies, they have<br />
provided important clues on the past<br />
of our own Galaxy. Looking farther away,<br />
SINFONI on the VLT made a record<br />
fragments only three were still seen, the<br />
fragments C (the largest one), B and E.<br />
No new fragmentations happened during<br />
this approach, apparently.<br />
Things were different this time, when the<br />
comet moved again towards its closest<br />
approach to the Sun – and to the Earth.<br />
Early in March, seven fragments were<br />
observed, the brightest (fragment C)<br />
being of magnitude 1 , i.e. 50 times<br />
fainter than what the unaided eye can<br />
see, while fragment B was 10 times fainter<br />
still. In the course of March, 6 new<br />
fragments were seen.<br />
Early in April, fragment B went into outburst,<br />
brightening by a factor 10 and<br />
on 7 April, six new fragments were discovered,<br />
confirming the high degree of<br />
fragmentation of the comet. On 1 April,<br />
fragment B was as bright as the main<br />
fragment C, with a magnitude around 9<br />
(16 times fainter than what a keen<br />
observer can see with unaided eyes).<br />
Fragment B seems to have fragmented<br />
again, bringing the total of fragments<br />
close to 40, some being most probably<br />
very small, boulder-sized objects with<br />
irregular and short-lived activity.<br />
observation of a very young galaxy, showing<br />
that it formed very quickly, contrarily<br />
to previous beliefs. The VLT also helped<br />
discover a ‘blob’ twice as large as the<br />
Milky Way and emitting as much as<br />
several billion suns, yet it is invisible in<br />
normal light! In another bout of magic, the<br />
VLT also studied an invisible galaxy, from<br />
the imprint it leaves on the spectrum of a<br />
distant quasar acting as a beacon.<br />
One cannot doubt that the Universe has<br />
still many surprises in store but it seems<br />
also evident from the few Research<br />
Highlights presented here that <strong>ESO</strong><br />
telescopes are revealing more and more<br />
of them every day!<br />
The new observations reveal that this<br />
new small fragment has split again! The<br />
image clearly reveals that below the<br />
main B fragment, there is a small fragment<br />
that is divided into two and a<br />
careful analysis reveals five more tiny fragments<br />
almost aligned. Thus, this image<br />
alone shows at least 7 fragments. The<br />
comet has thus produced a whole set of<br />
mini-comets!<br />
Mini-comets coming off comet SW 3.
An Icy 5 Earth-mass Exoplanet<br />
Driven by the need for increasing efficiency<br />
to address current frontline research<br />
topics, astronomy is moving more and<br />
more in the direction of huge international<br />
teams working together, not unlike what<br />
has been the rule for many years in particle<br />
physics. Nothing can better illustrate<br />
this trend than the discovery of the<br />
smallest exoplanet. This incredible result<br />
is a joint effort of three independent<br />
campaigns: PLANET/RoboNet, OGLE,<br />
and MOA, involving a total of 73 collaborators<br />
affiliated with 3 institutions in 1<br />
countries.<br />
Designated by the unglamorous identifier<br />
of OGLE- 005-BLG-390Lb, the alien<br />
world is a five Earth-mass object located<br />
0 000 lightyears away, not far from the<br />
centre of our Milky Way galaxy.<br />
Contrary to most of the more than 00<br />
exoplanets discovered until now,<br />
OGLE- 005-BLG-390Lb was found using<br />
the ‘microlensing’ technique. This method<br />
is based on the fact that the gravity of<br />
a dim, intervening star can act as a giant<br />
natural telescope, magnifying a more<br />
distant star, which then temporarily looks<br />
brighter. A small ‘glitch’ in the brightening<br />
reveals the existence of a planet around<br />
the lens star. Neither the planet nor the<br />
star that it is orbiting can be seen, only<br />
the effect of their gravity. Such an<br />
intervening star causes a characteristic<br />
brightening that lasts about a month.<br />
Any planets orbiting this star can produce<br />
an additional signal, lasting from days for<br />
giant planets down to hours for Earthmass<br />
planets.<br />
In order to be able to catch and characterise<br />
these planets, nearly-continuous<br />
round-the-clock high-precision monitoring<br />
of ongoing microlensing events is<br />
required. This is the goal of the PLANET<br />
network of 1-m-class telescopes consisting<br />
of the <strong>ESO</strong> 1.54-m Danish at La<br />
Silla (Chile), the Canopus Observatory<br />
1.0-m (Hobart, Tasmania, Australia),<br />
the Perth 0.6-m (Bickley, Western Australia),<br />
the Boyden 1.5-m (South Africa),<br />
and the SAAO 1.0-m (Sutherland, South<br />
Africa). Since 005, PLANET has<br />
operated a common campaign with<br />
RoboNet, a UK-operated network of -m<br />
fully robotic telescopes currently comprising<br />
the Liverpool Telescope (Roque<br />
de Los Muchachos, La Palma, Spain) and<br />
the Faulkes Telescope North (Haleakala,<br />
Hawaii, USA).<br />
The OGLE (Optical Gravitational Lensing<br />
Experiment) search team discovered<br />
the event OGLE- 005-BLG-390 on 11<br />
July 005, triggering the PLANET telescopes<br />
to start taking data. A light curve<br />
consistent with a single lens star peaking<br />
at an amplification of about 3 on 31 July<br />
005 was observed, until 10 August<br />
when a PLANET member, observing at<br />
the Danish 1.54-m at <strong>ESO</strong> La Silla, noticed<br />
a planetary deviation. An OGLE<br />
point from the same night showed the<br />
same trend, while the last half of the planetary<br />
deviation, lasting about a day, had<br />
been covered by images from Perth<br />
Observatory. The MOA (Microlensing<br />
Observations in Astrophysics) collaboration<br />
was later able to identify the source<br />
star on its images and confirmed the<br />
deviation.<br />
The new planet orbits a red star five times<br />
less massive than the Sun in about<br />
10 years. It is the least massive exoplanet<br />
around an ordinary star detected so far,<br />
and also the coolest: its relatively cool<br />
parent star and large orbit implies that<br />
the likely surface temperature of the<br />
planet is 0 degrees Celsius below zero,<br />
too cold for liquid water. It is likely to have<br />
a thin atmosphere, like the Earth, but its<br />
rocky surface is probably deeply buried<br />
beneath frozen oceans. It may therefore<br />
more closely resemble a more massive<br />
version of Pluto, rather than the rocky<br />
inner planets like Earth and Venus.<br />
Astronomers claim that this planet is<br />
actually the first and only planet that<br />
has been discovered so far that is in<br />
agreement with the theories for how<br />
our Solar System formed. The favoured<br />
theoretical explanation for the formation<br />
of planetary systems proposes that solid<br />
‘planetesimals’ accumulate to build up<br />
planetary cores, which then accrete<br />
nebular gas – to form giant planets – if<br />
they are sufficiently massive. Around red<br />
dwarfs, the most common stars of our<br />
Galaxy, this model favours the formation<br />
of Earth- to Neptunemass planets being<br />
between 1 and 10 times the Earth-Sun<br />
distance away from their host.<br />
OGLE- 005-BLG-390Lb is only the third<br />
extrasolar planet discovered so far<br />
through microlensing searches. While the<br />
other two microlensing planets have<br />
masses of a few times that of Jupiter, the<br />
discovery of a 5 Earth-mass planet –<br />
despite being much harder to detect than<br />
more massive ones – is a strong hint<br />
that these lower-mass objects are very<br />
common. In particular, astronomers now<br />
think that such frozen worlds are much<br />
more common than their larger, Jupiterlike<br />
brethren, as otherwise the microlensing<br />
method should have found dozens of<br />
them by now.<br />
There is no doubt that the discovery of<br />
this planet marks a groundbreaking result<br />
in the search for planets that support life.<br />
J.-P. Beaulieu, D. P. Bennett, P. Fouqué, A. Williams,<br />
M. Dominik, U. G. Jørgensen, D. Kubas et al., Nature,<br />
6 January 006.<br />
Artist’s Impression of the Icy Exoplanet.<br />
Light Curve of OGLE- 005-BLG-390.<br />
<strong>ESO</strong> Annual Report 006<br />
11
Trio of Neptunes and their Belt<br />
A most unusual planetary system has<br />
been found, in which a nearby star is hosting<br />
three Neptune-mass planets. The<br />
innermost planet is most probably rocky,<br />
while the outermost is the first known<br />
Neptune-mass planet to reside in the habitable<br />
zone. This unique system is likely<br />
further enriched by an asteroid belt.<br />
A planet in orbit around a star will manifest<br />
its presence by pulling the star in<br />
different directions, thereby changing its<br />
measured velocity by very small amounts.<br />
Astronomers therefore measure the<br />
velocity of a star with very high precision<br />
to detect the signature of one or more<br />
planets. Certainly the best instrument to<br />
do this kind of work is the High Accuracy<br />
Radial velocity Planet Searcher (HARPS)<br />
at the <strong>ESO</strong> La Silla 3.6-m telescope, a<br />
fibre-fed high-resolution echelle spectrograph<br />
that has demonstrated a longterm<br />
precision of about 1 m/s.<br />
During more than two years, a team of<br />
astronomers used HARPS to monitor the<br />
velocity of HD 69830, a rather inconspicuous<br />
nearby star slightly less massive<br />
than the Sun. Located 41 light-years<br />
away towards the constellation of Puppis<br />
(the Stern), it is, with a visual magnitude<br />
of 5.95, just visible with the unaided eye.<br />
Precise measurements allowed the<br />
astronomers to discover the presence of<br />
three tiny companions orbiting their<br />
parent star in 8.67, 31.6 and 197 days.<br />
The detected velocity variations are between<br />
and 3 metres per second,<br />
Increasing the Odds of the Sweep<br />
The VLT has confirmed the extrasolar<br />
planet status of two of the 16 candidates<br />
discovered by the NASA/ESA Hubble<br />
Space Telescope.<br />
The 16 candidates were uncovered<br />
during an international HST survey, called<br />
the ‘Sagittarius Window Eclipsing<br />
Extrasolar Planet Search’, or SWEEPS.<br />
HST couldn’t see the 16 newly found planet<br />
candidates directly. Instead, astronomers<br />
used HST to search for planets by<br />
measuring the slight dimming of a star<br />
due to the passage of a planet in front of<br />
it. This event is called a transit. The<br />
1<br />
<strong>ESO</strong> Annual Report 006<br />
Impression of the planetary system around HD 69830.<br />
corresponding to about 9 km/h! That’s<br />
the speed of a person walking briskly.<br />
Such tiny signals could not have been<br />
distinguished from ‘simple noise’ by most<br />
of today’s available spectrographs.<br />
The newly found planets have minimum<br />
masses between 10 and 18 times the<br />
mass of the Earth. Extensive the oretical<br />
simulations favour an essentially rocky<br />
composition for the inner planet, and a<br />
rocky/gas structure for the middle one.<br />
The outer planet has probably accreted<br />
some ice during its formation, and is likely<br />
to be made of a rocky/icy core surrounded<br />
by a quite massive envelope. Further<br />
calculations have also shown that the<br />
system is in a dynamically stable configuration.<br />
The outer planet also appears to be located<br />
near the inner edge of the habitable<br />
zone, where liquid water can exist<br />
planet would have to be about the size of<br />
Jupiter to block enough starlight, about<br />
1 to 10 per cent, to be measurable by<br />
HST. These objects are called planetary<br />
‘candidates’ because astronomers<br />
cannot be sure of their mass, and hence<br />
of their status, without further spectroscopic<br />
measurements.<br />
For two of the stars, the SWEEPS team<br />
could use the UVES and FLAMES<br />
instruments on the VLT to make an independent<br />
confirmation of a planet’s<br />
presence by spectroscopically measuring<br />
a slight wobble in the star’s motion<br />
due to the gravitational pull of an unseen<br />
at the surface of rocky/icy bodies.<br />
Although this planet is probably not Earthlike<br />
due to its heavy mass, its discovery<br />
opens the way to exciting possibilities.<br />
This alone would make this system already<br />
exceptional. But the recent discovery<br />
by the Spitzer Space Telescope<br />
that the star most likely hosts an asteroid<br />
belt adds the cherry to the cake. With<br />
three roughly equal-mass planets, one<br />
being in the habitable zone, and an asteroid<br />
belt, this planetary system shares<br />
many properties with our own Solar System.<br />
The planetary system around HD<br />
69830 clearly represents a ‘Rosetta<br />
stone’ for our understanding of how<br />
planets form. No doubt it will help us<br />
better understand the huge diversity we<br />
have observed since the first extrasolar<br />
planet was found in 1995.<br />
Christophe Lovis et al., Nature, 18 May 006.<br />
companion. One of the planetary<br />
candidates has a mass below 3.8 Jupiter<br />
masses. It orbits its host star, which<br />
is 5% more massive than the Sun, in 4.<br />
days. The other candidate’s mass is<br />
9.7 Jupiter masses.<br />
These are the faintest stars with planets<br />
that have been confirmed by radial<br />
velocities so far. To confirm the other planet<br />
candidates one would need a much<br />
bigger telescope on Earth, such as<br />
the European Extremely Large Telescope.<br />
Kailash Sahu et al., Nature, 5 October 006.
Do ‘Planemos’ Have Progeny?<br />
Two new studies show that objects only a<br />
few times more massive than Jupiter are<br />
born with discs of dust and gas, the raw<br />
material for planet-making. This suggests<br />
that miniature versions of the Solar<br />
System may circle objects that are some<br />
100 times less massive than our Sun.<br />
What’s more, such objects appear also to<br />
be able to form as twins: an approximately<br />
seven-Jupiter-mass companion<br />
was found orbiting an object that is itself<br />
only twice as hefty. The existence of such<br />
a double system puts strong constraints<br />
on formation theories of free-floating<br />
planetary-mass objects.<br />
Since a few years ago, it has been known<br />
that many young brown dwarfs —<br />
‘failed stars’ that weigh less than 8 per<br />
cent the mass of the Sun — are surrounded<br />
by a disc of material. This may<br />
indicate these objects form in the same<br />
way as our Sun. The new findings confirm<br />
that the same appears to be true for their<br />
even punier cousins, sometimes called<br />
free-floating planetary mass objects or<br />
‘planemos’. These objects have masses<br />
similar to those of extrasolar planets, but<br />
they are not in orbit around stars –<br />
instead, they float freely.<br />
In a way, the new discoveries are not too<br />
surprising – after all, Jupiter must have<br />
been born with its own disc, out of which<br />
its bigger moons formed. Still they may<br />
lead to a revision of our understanding of<br />
planetary formation as, unlike Jupiter,<br />
these planemos are not circling stars.<br />
The first study used two of <strong>ESO</strong>’s telescopes<br />
– Antu, the 8. -metre Unit Telescope<br />
no. 1 of the Very Large Telescope,<br />
and the 3.5-metre New Technology<br />
Telescope – to obtain optical spectra of<br />
six candidates identified recently by<br />
researchers at the University of Texas at<br />
Austin. Two of the six turned out to<br />
have masses between five and 10 times<br />
that of Jupiter while two others are<br />
a tad heftier, at 10 to 15 times Jupiter’s<br />
mass. All four of these objects are<br />
‘newborns’, just a few million years old,<br />
and are located in star-forming regions<br />
about 450 light years from Earth. The<br />
planemos show infrared emission from<br />
dusty discs that may evolve into miniature<br />
planetary systems over time.<br />
The other study also used the Very Large<br />
Telescope, but this time with its adaptive<br />
optics system and infrared camera<br />
NACO, to obtain images and spectra of<br />
a planetary-mass companion discovered<br />
two years ago at <strong>ESO</strong> around a young<br />
brown dwarf that is itself about 5 times<br />
the mass of Jupiter.<br />
This planetary-mass companion is the<br />
first-ever exoplanet to have been imaged.<br />
The brown dwarf, dubbed M1 07 for<br />
short and located 170 light years from<br />
Earth, was known to be surrounded by a<br />
disc. Now, evidence has been found for<br />
a disc around the eight-Jupiter-mass<br />
companion as well.<br />
The pair probably formed together, like a<br />
petite stellar binary, instead of the<br />
companion forming in the disc around the<br />
brown dwarf like a star-planet system.<br />
It is also possible that smaller planets or<br />
asteroids could now form in the disc<br />
around each one.<br />
Astronomers have in fact found a double<br />
system composed of even smaller<br />
objects. Oph 16 5- 40515, or Oph<br />
16 for short, is the first planemo found<br />
to be a double. Researchers discovered<br />
the companion candidate in an optical<br />
image taken with the NTT, then took<br />
optical spectra and infrared images of the<br />
pair with the VLT to make sure that it is a<br />
true companion, instead of a foreground<br />
or background star that happens to be in<br />
the same line of sight. These follow-up<br />
observations indeed confirmed that both<br />
objects are young, at the same distance,<br />
and much too cool to be stars. This<br />
suggests the two are physically associated.<br />
By comparing to widely used theoretical<br />
models, the astronomers estimate<br />
that the companion is about seven times<br />
the mass of Jupiter, while the more<br />
massive object comes in at about 14<br />
times Jupiter’s mass. The newborn pair,<br />
barely a million years old, is separated<br />
by about six times the distance between<br />
the Sun and Pluto, and is located in<br />
the Ophiuchus star-forming region approximately<br />
400 light years away.<br />
Planets are thought to form out of discs<br />
of gas and dust that surround stars,<br />
brown dwarfs, and even some free-floating<br />
planetary mass objects, as described<br />
above. But, it is likely that these planemo<br />
twins formed together out of a contracting<br />
gas cloud that fragmented, like a<br />
miniature stellar binary.<br />
Oph 16 B is only the second or third<br />
directly-imaged planetary-mass companion<br />
to be confirmed spectroscopically,<br />
and the first one around a primary that is<br />
itself a planetary-mass object. Its existence<br />
poses a challenge to a popular<br />
theoretical scenario, which suggests that<br />
brown dwarfs and free-floating planetary-<br />
mass objects are embryos ejected from<br />
multiple protostar systems.<br />
Since the two objects in Oph16 are so<br />
far apart, and only weakly bound to each<br />
other by gravity, they would not have<br />
survived such a chaotic birth.<br />
Recent discoveries have revealed an<br />
amazing diversity of worlds out there.<br />
Still, the Oph16 pair stands out as one<br />
of the most intriguing. Now, the as-<br />
tronomers are curious to find out whether<br />
such pairs are common or rare. The<br />
answer could shed light on how free-<br />
floating planetary-mass objects form.<br />
Ray Jayawardhana & Valentin Ivanov, American<br />
Astronomical Society, June 006, Calgary, Canada.<br />
Ray Jayawardhana & Valentin D. Ivanov, Science, 3<br />
August 006.<br />
Subhanjoy Mohanty et al., American Astronomical<br />
Society, June 006, Calgary, Canada.<br />
Spectra of candidate ‘planemos’.<br />
<strong>ESO</strong> Annual Report 006<br />
13
Watching How Planets Form<br />
The disc around a star more massive<br />
than the Sun has been mapped, revealing<br />
a very extended and flared disc that most<br />
likely contains enough gas and dust to<br />
spawn planets. It appears as a precursor<br />
of debris discs such as the one around<br />
Vega-like stars and so provides the rare<br />
opportunity to witness the conditions<br />
prevailing prior to or during planet<br />
formation.<br />
Planets form in massive, gaseous and<br />
dusty protoplanetary discs that surround<br />
nascent stars. This process must be<br />
rather ubiquitous given the many exoplanets<br />
already known. However, very little<br />
is known about these discs, especially<br />
those around stars more massive than the<br />
Sun. Such stars are much more luminous<br />
and could have a large influence on their<br />
disc, possibly quickly destroying the inner<br />
part.<br />
Astronomers used the VISIR instrument<br />
on the VLT to map the disc surrounding<br />
the young star HD 97048 in the infrared.<br />
HD97048 has an age of a few million<br />
years – a blink of an eye compared to the<br />
age of the Sun (4.6 billion years) – and<br />
belongs to the Chameleon I dark cloud,<br />
a stellar nursery 600 lightyears away.<br />
14<br />
<strong>ESO</strong> Annual Report 006<br />
Sketch of a flared proto-planetary disc such as the one around the young star HD 97048.<br />
The star is 40 times more luminous than<br />
our Sun and is .5 times as massive.<br />
The astronomers could only have<br />
achieved such a detailed view due to the<br />
high angular resolution offered by an 8metre-size<br />
telescope in the infrared,<br />
reaching a resolution of 0.33 arcsecond.<br />
They discovered a very large disc, at<br />
least 1 times more extended than the<br />
or-bit of the farthest planet in the Solar<br />
System, Neptune. The observations suggest<br />
that the disc is flared, the first time<br />
such a structure, predicted by some<br />
theoretical models, has been imaged<br />
around a massive star.<br />
Such geometry can only be explained<br />
if the disc contains a large amount of<br />
gas, in this case, at least as much as 10<br />
times the mass of Jupiter. It should also<br />
contain more than 50 Earth masses in<br />
dust.<br />
The dust mass derived here is more<br />
than thousand times larger than what is<br />
observed in debris discs and Kuiper-<br />
belt-like structures found around older,<br />
‘Vega-like’ stars, such as Beta Pictoris,<br />
Vega, Fomalhaut and HR 4796, and<br />
which is thought to be produced by<br />
collisions of larger bodies.<br />
The dust mass observed around HD<br />
97048 is similar to the mass invoked for<br />
the (undetected) parent bodies in the<br />
more evolved systems. HD 97048’s disc<br />
is thus most likely a precursor of debris<br />
discs observed around older stars.<br />
From the structure of the disc, the astronomers<br />
gather that planetary embryos<br />
may be present in the inner part of the<br />
disc. Follow-up observations at higher<br />
angular resolution with the VLT interferometer<br />
(VLTI) should allow them to probe<br />
these regions.<br />
Pierre-Olivier Lagage et al., Science, 8 September<br />
006.
A Substellar Jonah<br />
Astronomers have discovered a rather unusual<br />
system, in which two planet-size<br />
stars, of different colours, orbit each other.<br />
One is a rather hot white dwarf, weighing<br />
a little bit less than half as much as the<br />
Sun. The other is a much cooler, 55<br />
Jupiter-masses brown dwarf.<br />
The low-mass companion to the white<br />
dwarf (named WD0137-349) was found<br />
using spectra taken with EMMI at the New<br />
Technology Telescope at La Silla. The<br />
astronomers then used the UVES spectrograph<br />
on the VLT to record 0 spectra<br />
and so measure the period and the mass<br />
ratio.<br />
Numerical simulations of a brown dwarf being swallowed by a red giant.<br />
The two objects, separated by less than<br />
/3 of the radius of the Sun, or only a<br />
few thousandths of the distance between<br />
the Earth and the Sun, rotate around<br />
each other in about hours. The brown<br />
dwarf moves on its orbit at the amazing<br />
speed of 800 000 km/h!<br />
The two stars were not so close in their<br />
past. Only when the solar-like star<br />
that has now become a white dwarf was<br />
a red giant did the separation between<br />
the two objects diminish drastically. During<br />
this fleeting moment, the giant engulfed<br />
its companion. The latter, feeling a<br />
large drag similar to trying to swim in<br />
a bath full of oil, spiralled in towards the<br />
core of the giant. The envelope of the<br />
giant was finally ejected, leaving a binary<br />
system in which the companion is in a<br />
close orbit around a white dwarf.<br />
Image: Los Alamos National Laboratory<br />
The existence of the system proves that<br />
the brown dwarf came out almost<br />
unaltered from an episode in which it was<br />
swallowed by a red giant. Models show<br />
that had the companion been less than<br />
0 Jupiter masses, it would have<br />
evaporated during this phase. The brown<br />
dwarf shouldn’t rejoice too quickly to<br />
have escaped this doom, however.<br />
Einstein’s General Theory of Relativity<br />
predicts that the separation between the<br />
two stars will slowly decrease. In about<br />
1.4 billion years, the orbital period will<br />
have decreased to slightly more than one<br />
hour. At that stage, the two objects will<br />
be so close that the white dwarf will work<br />
as a giant ‘vacuum cleaner’, drawing gas<br />
off its companion, in a cosmic cannibal<br />
act.<br />
Pierre Maxted et al., Nature, 3 August 006.<br />
<strong>ESO</strong> Annual Report 006<br />
15
Stellar Vampires Unmasked<br />
Some hot, bright, and apparently young<br />
stars – known as ‘blue stragglers’ – in the<br />
globular cluster 47 Tucanae contain less<br />
carbon and oxygen than the majority of<br />
their sisters. This indicates that these few<br />
stars likely formed by taking their material<br />
from another star, acting as stellar<br />
vampires.<br />
Blue stragglers are unexpectedly younglooking<br />
stars found in stellar aggregates,<br />
such as globular clusters, which are<br />
known to be made up of old stars.<br />
These enigmatic objects are thought to be<br />
created in either direct stellar collisions<br />
or through the evolution and coalescence<br />
of a binary star system in which one<br />
star ‘sucks’ material off the other, rejuvenating<br />
itself. As such, they provide<br />
interesting constraints on both binary stellar<br />
evolution and star-cluster dynamics.<br />
To date, the unambiguous signatures of<br />
either stellar traffic accidents or stellar<br />
vampirism have not been observed, and<br />
the formation mechanisms of blue stragglers<br />
are still a mystery.<br />
16<br />
<strong>ESO</strong> Annual Report 006<br />
Oxygen Abundance<br />
Abundances in blue straggler stars.<br />
The VLT was used to measure the abundance<br />
of chemical elements at the<br />
surface of 43 blue straggler stars in the<br />
globular cluster 47 Tucanae, an impressive<br />
globular cluster that has a total<br />
mass of about 1 million times the mass of<br />
the Sun and is 1 0 light years across.<br />
Measurements of so many faint stars are<br />
only possible since the advent of 8-m-<br />
class telescopes equipped with spectrographs<br />
which have multiplexing capability.<br />
In this case, the astronomers used<br />
the FLAMES/GIRAFFE instrument, that<br />
allows the simultaneous observation of<br />
up to 130 targets at a time, making it<br />
ideally suited for surveying individual stars<br />
in closely populated fields.<br />
Six of these blue straggler stars were<br />
found to contain less carbon and oxygen<br />
than the majority of these peculiar<br />
objects. Such an anomaly indicates that<br />
the material at the surface of the blue<br />
stragglers comes from the deep interiors<br />
of a parent star. Such deep material can<br />
reach the surface of the blue straggler<br />
only during the mass transfer process<br />
occurring between two stars in a binary<br />
system. Numerical simulations indeed<br />
show that the coalescence of stars should<br />
not result in anomalous abundances.<br />
Carbon Abundance<br />
In the core of a globular cluster, stars are<br />
packed extremely close to each other:<br />
more than 4 000 stars are found in the innermost<br />
lightyear-sized cube of 47<br />
Tucanae. Thus, stellar collisions are<br />
thought to be very frequent and the collision<br />
channel for the formation of blue<br />
stragglers should be extremely efficient.<br />
The chemical signature detected by these<br />
observations demonstrates that the<br />
binary mass-transfer scenario is also fully<br />
active, even in a high-density cluster like<br />
47 Tucanae.<br />
This is the first detection of a chemical signature<br />
clearly pointing to a specific<br />
scenario to form blue straggler stars and<br />
therefore a fundamental step toward the<br />
solution of the long-standing mystery of<br />
blue-straggler formation in globular<br />
clusters.<br />
Francesco R. Ferraro et al. 006, Astrophys. Journal<br />
Lett., 647, L53.
Cepheids and their ‘Cocoons’<br />
Combining data from the Very Large<br />
Telescope Interferometer (VLTI) and the<br />
CHARA Interferometer at Mount Wilson,<br />
California, astronomers have discovered<br />
envelopes around three Cepheids, including<br />
the Pole Star. This is the first time<br />
that matter has been found surrounding<br />
members of this important class of rare<br />
and very luminous stars whose luminosity<br />
varies in a very regular way.<br />
Cepheids are commonly used as distance<br />
indicators, thanks to the existence<br />
of a basic relation between their intrinsic<br />
brightness and their pulsation period. By<br />
measuring the period of a Cepheid star,<br />
its intrinsic brightness can be deduced,<br />
and from the observed apparent brightness<br />
the distance may then be calculated.<br />
As they are intrinsically very bright<br />
stars, and can be observed in distant<br />
galaxies, this remarkable property has<br />
turned these yellow supergiant stars into<br />
primary ‘standard candles’ for extragalactic<br />
distance estimations. Cepheids<br />
thus play a crucial role in cosmology,<br />
being one of the first ‘steps’ on the<br />
cosmic distance ladder.<br />
The southern Cepheid L Carinae was observed<br />
with the VINCI and MIDI instrument<br />
at the VLTI, while Polaris (the Pole<br />
Star) and Delta Cephei were scrutinised<br />
with FLUOR on CHARA, located on the<br />
other side of the equator. FLUOR is the<br />
prototype instrument of VINCI, both being<br />
built by the Paris Observatory (France).<br />
L Carinae is the brightest Cepheid in the<br />
sky, and also the one that presents<br />
the largest apparent angular diameter.<br />
It is a massive supergiant star, having<br />
about 10 times the mass of the Sun and<br />
approximately 180 times its radius.<br />
Polaris is a peculiar star located very close<br />
to the north celestial pole (hence its<br />
name). It is classified as a Cepheid, but it<br />
shows very weak pulsations compared<br />
to the other stars of its class. Delta<br />
Cephei is the prototype of the Cepheids.<br />
It was discovered to be a variable star in<br />
the 18th century by the English amateur<br />
John Goodricke, and it is still one of the<br />
brightest members of the Cepheid class.<br />
Its short period is characteristic of a<br />
relatively small supergiant, with a radius<br />
of ‘only’ 43 times that of the Sun.<br />
Although such stars are thus rather large,<br />
they are so far away that they cannot<br />
be resolved by single telescopes. Indeed,<br />
even the largest Cepheids in the sky<br />
subtend an angle of only 0.003 arc second.<br />
To resolve this would be similar to<br />
viewing a two-storey house on the Moon.<br />
Astronomers therefore have to rely on the<br />
interferometric technique, which combines<br />
the light of two or more distant telescopes,<br />
providing the angular resolution<br />
of a single telescope as large as the<br />
separation between them. With the VLTI,<br />
it is possible to achieve a resolution of<br />
0.001 arcsecond or less.<br />
For most stars, the observations made<br />
with interferometers follow the theoretical<br />
stellar models very closely. However, for<br />
these three stars a tiny deviation was<br />
detected, revealing the presence of an<br />
envelope. The envelopes were found to<br />
be to 3 times as large as the star itself.<br />
The fact that such deviations were found<br />
for all three stars, which have very<br />
different properties, seems to imply that<br />
envelopes surrounding Cepheids are<br />
a widespread phenomenon. The physical<br />
processes that have created these<br />
envelopes are still uncertain, but, in analogy<br />
to what happens around other<br />
classes of stars, it is most probable that<br />
the environments were created by matter<br />
ejected by the star itself. Cepheids<br />
pulsate with periods of a few days.<br />
As a consequence, the star goes regularly<br />
through large-amplitude oscillations<br />
that create very rapid motions of its<br />
apparent surface (the photosphere) with<br />
velocities up to 30 km/s, or 108 000 km/<br />
h! While this remains to be established,<br />
there could be a link between the<br />
pulsation, the mass loss and the formation<br />
of the envelopes.<br />
P. Kervella et al. 006, Astronomy and Astrophysics,<br />
448, 6 3.<br />
Antoine Mérand et al. 006, Astronomy and<br />
Astrophysics, 453, 155.<br />
Model image of the Cepheid L Carinae.<br />
<strong>ESO</strong> Annual Report 006<br />
17
To Be or Not to Be: Is It All About Spinning?<br />
A study of the active hot star Alpha Arae<br />
solves a 140-year-old mystery.<br />
Lying about 300 light years away from the<br />
Sun, Alpha Arae is the closest member of<br />
the class of active stars known as ‘Be<br />
stars’. Be stars are very luminous,<br />
massive and hot stars that rotate rapidly.<br />
They are losing mass along the poles<br />
through a strong stellar wind and are<br />
surrounded at the equator by a disc of<br />
matter. Alpha Arae has ten times the mass<br />
of the Sun, is three times hotter and 6 000<br />
times as luminous.<br />
With AMBER on the VLTI, the team of astronomers<br />
were able to examine the<br />
structure of the disc surrounding Alpha<br />
Arae in detail. Moreover, because AMBER<br />
also provides spectra, the astronomers<br />
could study the motion of the gas in the<br />
disc and so understand how it rotates.<br />
The disc surrounding Alpha Arae was<br />
found to be in ‘Keplerian rotation’, that is,<br />
obeying the same rules as discovered by<br />
Johannes Kepler for the planets circling<br />
the Sun: the velocity of the material<br />
decreases with the square root of the<br />
distance from the star. The new result<br />
rules out the possibility of the disc<br />
rotating with a uniform velocity, as would<br />
be the case if a strong magnetic field<br />
were present which forced the matter to<br />
spin at the same rate as the star.<br />
Combining the new data with previous<br />
studies, the astronomers also show that<br />
the star Alpha Arae rotates 50 times<br />
faster than our Sun. In fact, with a speed<br />
at the equator of 470 km/s, it is spinning<br />
so quickly that it is near its break-up<br />
velocity. Matter having such a critical<br />
velocity would be able to freely escape<br />
from the star, in the same way that we<br />
would be ejected from a merry-go-round<br />
that has gone out of control. This could<br />
be the clue to the ‘Be phenomenon’.<br />
A. Meilland et al., 007, Astronomy and Astrophysics,<br />
464, 549.<br />
18<br />
<strong>ESO</strong> Annual Report 006<br />
Artist’s rendering of the Be star Alpha Arae.
Asymmetric Ashes<br />
Astronomers are reporting remarkable<br />
new findings that shed light on a decadelong<br />
debate about one type of the<br />
supernova explosions that mark a star’s<br />
final demise: does the star die in a slow<br />
burn or with a fast bang? From their<br />
observations, the scientists find that the<br />
matter ejected by the explosion shows<br />
significant peripheral asymmetry but a<br />
nearly spherical interior, most likely implying<br />
that the explosion finally propagates<br />
at supersonic speed.<br />
Using observations of 17 supernovae<br />
made over more than 10 years with the<br />
VLT for one part and the McDonald<br />
Observatory’s Otto Struve Telescope for<br />
another, astronomers inferred the shape<br />
and structure of the debris cloud thrown<br />
out from Type Ia supernovae. Such<br />
supernovae are thought to be the result<br />
of the explosion of a small and dense star<br />
– a white dwarf – inside a binary system.<br />
As its companion continuously spills<br />
matter onto the white dwarf, the white<br />
dwarf reaches a critical mass, leading to<br />
a fatal instability and the supernova. But<br />
what sparks the initial explosion, and how<br />
the blast travels through the star have<br />
long been thorny issues.<br />
Artist’s impression of a clumpy SN Ia explosion.<br />
The supernovae that were observed occurred<br />
in distant galaxies, and because<br />
of the vast cosmic distances could not be<br />
studied in detail using conventional<br />
imaging techniques, including interferometry.<br />
Instead, the team of researchers<br />
determined the shape of the exploding<br />
cocoons by recording the polarisation<br />
of the light from the dying stars.<br />
Polarimetry relies on the fact that light is<br />
composed of electromagnetic waves that<br />
oscillate in certain directions. Reflection<br />
or scattering of light favours certain orientations<br />
of the electric and magnetic<br />
fields over others. This is why polarising<br />
sunglasses can filter out the glint of<br />
sunlight reflected off a pond. When light<br />
scatters through the expanding debris of<br />
a supernova, it retains information about<br />
the orientation of the scattering layers. If<br />
the supernova is spherically symmetric, all<br />
orientations will be present equally and<br />
will average out, so there will be no net<br />
polarisation. If, however, the gas shell is<br />
not round, a slight net polarisation will be<br />
imprinted on the light.<br />
This is what broadband polarimetry can<br />
accomplish. If additional spectral in-<br />
formation is available (‘spectropolarimetry’),<br />
one can determine whether the<br />
asymmetry is in the continuum light or in<br />
some spectral lines. In the case of the<br />
Type Ia supernovae, the astronomers<br />
found that the continuum polarisation is<br />
very small, implying that the overall shape<br />
of the explosion is crudely spherical. But<br />
the much larger polarisation in strongly<br />
blue-shifted spectral lines shows the<br />
presence, in the outer regions, of fast-<br />
moving clumps with peculiar chemical<br />
composition.<br />
The study reveals that explosions of Type<br />
Ia supernovae are truly three-dimensional<br />
phenomena. The outer regions of the<br />
blast cloud are asymmetric, with different<br />
materials found in ‘clumps’, while the<br />
inner regions are smooth.<br />
The research team first spotted this<br />
asymmetry in 003, as part of the same<br />
observational campaign. The new, more<br />
extensive results show that the degree of<br />
polarisation, and hence the asphericity,<br />
correlates with the intrinsic brightness of<br />
the explosion. The brighter the supernova,<br />
the smoother, or less clumpy, it is.<br />
This has some impact on the use of Type<br />
Ia supernovae as standard candles.<br />
This kind of supernovae is used to measure<br />
the rate of acceleration of the expansion<br />
of the Universe, assuming these<br />
objects behave in a uniform way. But<br />
asymmetries can introduce dispersions in<br />
the quantities observed.<br />
The discovery also puts strong constraints<br />
on any successful models of<br />
thermonuclear supernova explosions.<br />
Models have suggested that the clumpiness<br />
is caused by a slow-burn process,<br />
called ‘deflagration’, and leaves an irregular<br />
trail of ashes. The smoothness of<br />
the inner regions of the exploding star<br />
implies that at a given stage, the deflagration<br />
gives way to a more violent process,<br />
a ‘detonation’, which travels at supersonic<br />
speeds – so fast that it erases all<br />
the asymmetries in the ashes left behind<br />
by the slower burning of the first stage,<br />
resulting in a smoother, more homogeneous<br />
residue.<br />
Lifan Wang, Dietrich Baade and Ferdinando Patat,<br />
Science Express, 30 November 006.<br />
<strong>ESO</strong> Annual Report 006<br />
19
How to Steal a Million Stars?<br />
In another bout of stellar vampirism, but<br />
on a grand scale, astronomers found that<br />
the stellar cluster Messier 1 must have<br />
lost close to one million low-mass stars to<br />
the rest of the Milky Way galaxy.<br />
The astronomers measured the brightness<br />
and colours of more than 16 000<br />
stars within the globular cluster Messier<br />
1 with the FORS1 multimode instrument<br />
attached to one of the Unit Telescopes of<br />
<strong>ESO</strong>’s VLT at Cerro Paranal (Chile). The<br />
astronomers could study stars that are<br />
40 million times fainter than what the<br />
unaided eye can see.<br />
Messier 1 is one of about 00 globular<br />
clusters known in our Galaxy. These are<br />
large groupings of from 10 000 to more<br />
than a million stars that were formed<br />
together in the youth of the Milky Way,<br />
about 1 to 13 billion years ago. Globular<br />
clusters are a key tool for astronomers,<br />
because all the stars in a globular cluster<br />
share a common history. They were<br />
all born together, at the same time and<br />
place, and only differ from one another in<br />
their mass. By accurately measuring<br />
the brightness of the stars, astronomers<br />
can determine their relative sizes and<br />
stage of evolution precisely. Globular<br />
clusters are thus very helpful for testing<br />
theories of how stars evolve.<br />
Located at a distance of 3 000 light<br />
years in the constellation Ophiuchus<br />
(The Serpent-holder), Messier 1 got its<br />
name by being the 1 th entry in the catalogue<br />
of nebulous objects compiled in<br />
1774 by French astronomer and comet<br />
chaser Charles Messier. It is also known<br />
to astronomers as NGC 6 18 and<br />
contains about 00 000 stars, most<br />
of them having a mass between 0 and<br />
80 per cent of the mass of the Sun.<br />
It is however clear that Messier 1 is<br />
surprisingly devoid of low-mass stars.<br />
For each solar-like star, we would expect<br />
roughly four times as many stars with half<br />
that mass. The VLT observations only<br />
show an equal number of stars of different<br />
masses.<br />
In the solar neighbourhood and in<br />
most stellar clusters, the least massive<br />
0<br />
<strong>ESO</strong> Annual Report 006<br />
The Central Part of Messier 1 .<br />
stars are by far the most common.<br />
The new observations show this is not<br />
the case for Messier 1 .<br />
Globular clusters move in extended<br />
elliptical orbits that periodically take them<br />
through the densely populated plane<br />
of our Galaxy, then high above and below,<br />
in the ‘halo’. When venturing too<br />
close to the innermost and denser ‘bulge’<br />
of the Milky Way a globular cluster can be<br />
perturbed, with the smallest stars being<br />
ripped away.<br />
The astronomers estimate that Messier<br />
1 lost four times as many stars as it still<br />
has. That is, roughly one million stars<br />
must have been ejected into the halo of<br />
our Milky Way.<br />
The total remaining lifetime of Messier 1<br />
is predicted to be about 4.5 billion years,<br />
i.e. about a third of its present age. This<br />
is very short compared to the typical<br />
expected globular cluster’s lifetime, which<br />
is about 0 billion years.<br />
The scientists now hope to discover and<br />
study many more clusters like this, since<br />
catching clusters while they are being<br />
disrupted should clarify the dynamics of<br />
the process that shaped the halo of our<br />
home galaxy, the Milky Way.<br />
Guido de Marchi, Luigi Pulone, and Francesco<br />
Paresce, 006, Astronomy and Astrophysics, 449,<br />
161.
A ‘Genetic Study’ of the Galaxy<br />
Looking in detail at the composition of<br />
stars with the VLT, astronomers are<br />
providing a fresh look at the history of<br />
the Milky Way. They reveal that the<br />
central part of our Galaxy formed not<br />
only very quickly but also independently<br />
of the rest.<br />
For the first time, it has been possible<br />
to clearly establish a ‘genetic difference’<br />
between stars in the disc and the bulge<br />
of our Galaxy. From this one can infer<br />
that the bulge must have formed more<br />
rapidly than the disc, probably in less<br />
than a billion years and when the<br />
Universe was still very young.<br />
The Milky Way is a spiral galaxy, having<br />
a pinwheel shape with arms of gas, dust,<br />
and stars lying in a flattened disc, and<br />
extending directly out from a spherical<br />
nucleus of stars in the central region, the<br />
bulge. While the disc of our Galaxy is<br />
made up of stars of all ages, the bulge<br />
contains old stars dating from the time<br />
the galaxy formed, more than 10 billion<br />
years ago. Thus, studying the bulge<br />
allows astronomers to know more about<br />
how our Galaxy formed.<br />
The Oxygen abundance in the bulge of our Galaxy.<br />
To do this, an international team of<br />
astronomers analysed in detail the chemical<br />
composition of 50 giant stars in four<br />
different areas of the sky towards the<br />
Galactic bulge. They made use of the<br />
FLAMES/UVES spectrograph on the VLT<br />
to obtain high-resolution spectra.<br />
The chemical composition of stars carries<br />
the signature of the enrichment processes<br />
undergone by the interstellar matter<br />
up to the moment of their formation.<br />
It depends on the previous history of star<br />
formation and can thus be used to infer<br />
whether there is a ‘genetic link’ between<br />
different stellar groups. In particular,<br />
comparison between the abundance of<br />
oxygen and iron in stars is very illustrative.<br />
Oxygen is predominantly produced<br />
in the explosion of massive, short-lived<br />
stars (so-called Type II supernovae), while<br />
iron instead originates mostly in Type Ia<br />
supernovae, which can take much longer<br />
to develop. Comparing oxygen with iron<br />
abundances therefore gives insight into<br />
the star-birth rate in the Milky Way’s past.<br />
The larger size and iron-content coverage<br />
of the new sample allowed the astronomers<br />
to draw much more robust conclusions<br />
than were possible until then.<br />
They clearly established that, for a given<br />
iron content, stars in the bulge possess<br />
more oxygen than their disc counterparts.<br />
This highlights a systematic, hereditary<br />
difference between bulge and disc stars.<br />
In other words, bulge stars did not originate<br />
in the disc and then migrate inward<br />
to build up the bulge but rather formed<br />
independently of the disc. Moreover, the<br />
chemical enrichment of the bulge, and<br />
hence its formation timescale, was faster<br />
than that of the disc. Comparisons with<br />
theoretical models indicate that the<br />
Galactic bulge must have formed in less<br />
than a billion years, most likely through a<br />
series of starbursts when the Universe<br />
was still very young.<br />
Manuela Zoccali et al. 006, Astronomy and<br />
Astrophysics, 457, L1.<br />
<strong>ESO</strong> Annual Report 006<br />
1
Cut from Different Cloth<br />
A large survey has shed light on our Galaxy’s<br />
ancestry. After determining the<br />
chemical composition of over 000 stars<br />
in four of the nearest dwarf galaxies<br />
to our own, astronomers have demonstrated<br />
fundamental differences in their<br />
make-up, casting doubt on the theory<br />
that these diminutive galaxies could ever<br />
have formed the building blocks of our<br />
Milky Way Galaxy.<br />
Our Milky Way Galaxy is surrounded by<br />
a number of dwarf satellite galaxies,<br />
which because of their loosely rounded<br />
shape are referred to as ‘dwarf spheroidal’<br />
galaxies. Faint and diffuse, these<br />
dwarf galaxies are a thousand times<br />
fainter than the Milky Way itself, making<br />
them the least luminous galaxies known.<br />
Modern cosmological models predict<br />
that small galaxies form first, and later<br />
assemble into larger systems like our Galaxy.<br />
Since the Universe initially only<br />
The Topsy-Turvy Galaxy<br />
This FORS image of the central parts of<br />
NGC 1313 shows a stunning natural<br />
beauty. The galaxy bears some resemblance<br />
to some of the Milky Way’s closest<br />
neighbours, the Magellanic Clouds.<br />
NGC 1313 has a barred spiral shape,<br />
with the arms emanating outwards in a<br />
loose twist from the ends of the bar.<br />
The galaxy lies just 15 million light years<br />
away from the Milky Way – a mere skip<br />
on cosmological scales. The spiral arms<br />
are a hotbed of star-forming activity, with<br />
numerous young clusters of hot stars<br />
being born continuously at a staggering<br />
rate out of the dense clouds of gas and<br />
dust. Their light blasts through the<br />
surrounding gas, creating an intricately<br />
beautiful pattern of light and dark<br />
nebulosity.<br />
<strong>ESO</strong> Annual Report 006<br />
contained hydrogen and helium (most of<br />
all other chemical elements being<br />
synthesized inside stars), dwarf galaxies<br />
should have the lowest heavy element<br />
content. Not so, reveal the observations.<br />
As part of a large observational programme,<br />
called the Dwarf galaxies Abundances<br />
and Radial-velocities Team<br />
(DART), astronomers from institutes in 9<br />
different countries used FLAMES on the<br />
VLT to measure the amount of iron in over<br />
000 individual giant stars in the Fornax,<br />
Sculptor, Sextans and Carina dwarf<br />
spheroidals.<br />
Their data unearthed fundamental differences<br />
in the dwarf galaxy stars’ chemical<br />
composition compared with those<br />
in our galactic halo, calling into question<br />
the merger theory as the origin of large<br />
galaxies’ haloes. Whilst the average<br />
abundances of elements in the dwarf<br />
spheroidals is comparable with that seen<br />
NGC 1313’s appearance suggests it<br />
has seen troubled times: its spiral arms<br />
look lop-sided and gas globules are<br />
spread out widely around them. Moreover,<br />
observations with <strong>ESO</strong>’s 3.6-m<br />
telescope at La Silla have revealed that<br />
its ‘real’ centre, around which it rotates,<br />
does not coincide with the central bar.<br />
Its rotation is therefore also out of kilter.<br />
Strangely enough, NGC 1313 seems to<br />
be an isolated galaxy. It is not part of a<br />
group and has no neighbour, and it is not<br />
clear whether it may have swallowed a<br />
small companion in its past. So what<br />
caused its asymmetry and stellar baby<br />
boom?<br />
Chemical abundance in several dwarf galaxies.<br />
in the Galactic halo, the former are<br />
lacking the very metal-poor stars that are<br />
seen in the Milky Way – the two types<br />
of systems, contrary to theoretical predictions,<br />
are essentially of different descent.<br />
Amina Helmi et al. 006, Astrophysical Journal<br />
Letters, 651, L1 1-L1 4.<br />
The Topsy-Turvy Galaxy NGC 1313.
<strong>ESO</strong> Annual Report 006<br />
3
Long-lasting but Dim Brethren of Cosmic Flashes<br />
For the first time, it has been possible to<br />
make the link between an X-ray flash<br />
and a supernova. Such flashes are the little<br />
siblings of gamma-ray bursts (GRB)<br />
and this discovery suggests the existence<br />
of a population of events less luminous<br />
than ‘classical’ GRBs, but possibly much<br />
more numerous. This also implies a<br />
common origin for these two classes of<br />
events.<br />
The event began on 18 February 006:<br />
the NASA/PPARC/ASI Swift satellite<br />
detected an unusual gamma-ray burst,<br />
about 5 times closer and 100 times<br />
longer than the typical gamma-ray burst.<br />
GRBs release in a few seconds more<br />
energy than that of the Sun during its entire<br />
lifetime of more than 10 000 million<br />
years. The GRBs are thus the most powerful<br />
events known in the Universe since<br />
the Big Bang.<br />
The explosion, called GRB 060 18<br />
after the date it was discovered, originated<br />
in a star-forming galaxy about 440<br />
million light years away toward the<br />
constellation Aries. This is the secondclosest<br />
gamma-ray burst ever detected.<br />
Moreover, the burst of gamma rays lasted<br />
for nearly 000 seconds; most bursts<br />
last a few milliseconds to tens of seconds.<br />
The explosion was surprisingly<br />
dim, however.<br />
Using several telescopes, among them the<br />
VLT, the scientists watched the afterglow<br />
of this burst grow brighter in optical light.<br />
This brightening, along with other telltale<br />
spectral characteristics in the light,<br />
strongly suggests that a supernova was<br />
unfolding. Within days, the supernova<br />
became apparent.<br />
The observations with the VLT started on<br />
1 February 006, just three days after<br />
the discovery. Spectroscopy was then<br />
performed nearly daily for seventeen<br />
days, providing the astronomers with a<br />
large data set to document this new class<br />
of events.<br />
4<br />
<strong>ESO</strong> Annual Report 006<br />
The field around SN 006aj.<br />
The astronomers could finally confirm that<br />
the event was tied to a supernova called<br />
SN 006aj which was observed a few<br />
days later. The newly discovered supernova<br />
is dimmer by about a factor of two<br />
than the hypernovae associated with<br />
normal long gamma-ray bursts, but it is<br />
still a factor of -3 times more luminous<br />
than regular core-collapse supernovae.<br />
All together, these facts point to a<br />
substantial diversity between supernovae<br />
associated with GRBs and supernovae<br />
associated with X-ray flashes. This<br />
diversity may be related to the masses<br />
of the exploding stars.<br />
Whereas gamma-ray bursts probably<br />
mark the birth of a black hole, X-ray<br />
flashes appear to signal the type of star<br />
explosion that leaves behind a neutron<br />
star. Based on the VLT data, another<br />
team of astronomers postulate that the<br />
18 February event might have led to a<br />
highly magnetic type of neutron star<br />
called a magnetar.<br />
They find indeed that the star that<br />
exploded had an initial mass of ‘only’ 0<br />
times the mass of the Sun. This is<br />
smaller, by about a factor of two at least,<br />
than those estimated for the typical GRBsupernovae.<br />
The properties of GRB 060 18 suggest<br />
the existence of a population of events<br />
less luminous than ‘classical’ GRBs, but<br />
possibly much more numerous. Indeed,<br />
these events may be the most abundant<br />
form of X- or gamma-ray bursts in the<br />
Universe, but instrumental limits allow us<br />
to detect them only locally. The astronomers<br />
find that the number of such events<br />
could be about 100 times more numerous<br />
than typical gamma-ray bursts.<br />
Elena Pian et al., Nature, 31 August 006.<br />
Paolo Mazzali et al., Nature, 31 August 006.
Faraway Galaxy Under the Microscope<br />
Some large-disc galaxies akin to our<br />
Milky Way have formed on a rapid time-<br />
scale, only 3 billion years after the<br />
Big Bang, reveals a study made with the<br />
new SINFONI spectrograph on VLT.<br />
Over the past decade astronomers have<br />
established an overall model of how<br />
galaxies formed and evolved when the<br />
Universe was only a few billion years old.<br />
Gas made of ordinary matter cooled and<br />
collected in concentrations of the<br />
mysterious ‘dark’ matter (so-called dark-<br />
matter halos). Since that time, and up to<br />
the present epoch, collisions and<br />
mergers of galaxies subsequently led to<br />
the hierarchical build-up of galaxy mass.<br />
This general picture leaves open,<br />
however, on what timescales galaxies<br />
were assembled and when and how<br />
bulges and discs, the primary components<br />
of present-day galaxies, were<br />
formed.<br />
A major study of distant, luminous starforming<br />
galaxies at the VLT, the ‘SINS’<br />
(Spectroscopic Imaging survey in the<br />
Near-infrared with SINFONI) survey, has<br />
now resulted in a major breakthrough on<br />
these questions. This study exploited<br />
SINFONI, a novel infrared ‘integral-field<br />
spectrometer’ that simultaneously<br />
delivers sharp images, with adaptive<br />
optics, and highly resolved spectra of an<br />
object on the sky.<br />
In one case, studying the galaxy<br />
BzK155043 at cosmological redshift of<br />
.4, the SINFONI observations achieved<br />
an angular resolution of 0.15 arcsecond,<br />
a mere 4 000 light years at the distance<br />
of this high-redshift galaxy. With this<br />
superior angular resolution the data<br />
reveal the physical and dynamical<br />
properties in unprecedented detail.<br />
Surprisingly, instead of showing mostly<br />
irregular and perhaps even chaotic<br />
motions caused by the frequent merger<br />
activity in the young Universe, the<br />
observations reveal a large and massive<br />
rotating protodisc that is channelling gas<br />
toward a growing central stellar bulge.<br />
The high gas surface densities, the large<br />
star-formation rate and the moderately<br />
young stellar ages derived from these<br />
observations suggest that the system<br />
was assembled rapidly, by fragmentation<br />
and star formation in an initially very gas<br />
rich protodisc. SINS observations of<br />
several other massive, high-redshift<br />
galaxies give similar results.<br />
The fact that these galaxies are so large<br />
and rotate rapidly indicates that the gas<br />
has a similar amount of rotation as the<br />
dark matter halo from which it cooled,<br />
thus empirically solving an important<br />
question of galaxy formation.<br />
The SINFONI data suggest that the protodiscs<br />
may have eventually been transformed<br />
to dense elliptical galaxies, either<br />
by internal processes, such as the<br />
spectacular gas inflows observed in BzK-<br />
15504, or by collisions and mergers with<br />
other galaxies, which were frequent in the<br />
dense environments in which the highredshift<br />
luminous star-forming galaxies<br />
appear to reside.<br />
Another important aspect of the work is<br />
the deduction of very high star-formation<br />
rates for many of the luminous starforming<br />
high-redshift galaxies, about one<br />
hundred times greater than in the<br />
present-day Milky Way.<br />
Astronomers have a growing body of<br />
evidence that massive galaxies formed<br />
much more rapidly in the redshift range<br />
-3 than originally anticipated. The new<br />
SINFONI data give us a first glimpse of<br />
what processes might be involved.<br />
SINFONI maps of emission in BzK-15504.<br />
In fact, the SINS programme on the VLT<br />
is a stunning demonstration of what is<br />
going to be possible in the next few years<br />
with the combination of integral-field<br />
spec-troscopy and adaptive optics.<br />
N.M. Förster Schreiber et al. 006, Astrophys.<br />
Journal 645, 106 .<br />
R. Genzel et al., Nature, 17 August 006.<br />
X. Kong et al. 006, Astrophys.J. 638, 7 .<br />
Emission of the galaxy BzK-15504.<br />
<strong>ESO</strong> Annual Report 006<br />
5
The Invisible Galaxies That Could Not Hide<br />
Astronomers have found a metal-rich hydrogen<br />
cloud in the distant universe.<br />
The result may help to solve the missing<br />
metal problem and provides insight on<br />
how galaxies form. This discovery shows<br />
that significant quantities of metals are to<br />
be found in very remote galaxies that are<br />
too faint to be directly seen.<br />
Metal shouldn’t however be taken too literally<br />
as, for astronomers, metals are all<br />
chemical elements heavier than helium.<br />
The Sun, for example, is made mostly of<br />
hydrogen (73%) and helium ( 5%), and<br />
% of ‘metals’.<br />
Almost all of the elements present in the<br />
Universe were formed in stars, which<br />
themselves are members of galaxies. By<br />
estimating how many stars formed over<br />
the history of the Universe, it is possible<br />
to estimate how much of the metals<br />
should have been produced. However,<br />
this apparently straightforward reasoning<br />
has been confronted for several years<br />
with an apparent contradiction: adding<br />
up the amount of metals observable<br />
today in distant astronomical objects falls<br />
Falling Onto the Dark<br />
Using the FORS1 instrument on the VLT,<br />
an international team of astronomers<br />
have discovered a new ‘blob’ located at a<br />
distance of 11.6 billion light years (redshift<br />
3.16). It is thus seen as it was when<br />
the Universe was only billion years old,<br />
or less than 15% its present age. The<br />
newly discovered object is located in the<br />
well-studied GOODS South field.<br />
With a diameter of 00 000 light years,<br />
the blob is twice as big as our Milky Way<br />
and the total energy emitted is equivalent<br />
to that of about billion suns. Despite<br />
this, the object is invisible in images taken<br />
with various telescopes observing from<br />
the infrared to the X-ray wavebands,<br />
making it a very peculiar object indeed.<br />
This is because the object emits most of<br />
its light in the Lyman-alpha hydrogen line,<br />
while its continuum emission is too low to<br />
be detected. It is also the only such<br />
object found by the astronomers in their<br />
survey.<br />
6<br />
<strong>ESO</strong> Annual Report 006<br />
short of the predicted value. When the<br />
contribution of galaxies now observed at<br />
cosmological distances is added to that<br />
of the intergalactic medium, the total<br />
amounts for no more than a tenth of the<br />
metals expected.<br />
Studying distant galaxies is however a<br />
difficult task. The further a galaxy, the<br />
fainter it is, and the smallest or intrinsically<br />
faintest ones will not be observed.<br />
This may introduce severe biases in the<br />
observations as only the largest and most<br />
active galaxies are picked up.<br />
Astronomers therefore came up with<br />
other ways to study distant galaxies: they<br />
use quasars, most probably the brightest<br />
distant objects known, as beacons in the<br />
Universe.<br />
Interstellar clouds of gas in galaxies, located<br />
between the quasars and us on the<br />
same line of sight, absorb parts of the<br />
light emitted by the quasars. The<br />
resulting spectrum consequently presents<br />
dark ‘valleys’ that can be attributed to<br />
well-known elements. Thus, astronomers<br />
Trying to explain this blob by invoking<br />
a powerful galaxy as the cause for the<br />
object to emit so much radiation proved<br />
impossible. The astronomers are instead<br />
led to the conclusion that the observed<br />
hydrogen emission comes from primordial<br />
gas falling onto a clump of dark<br />
HST Image Narrow-band<br />
A Rare Blob.<br />
can measure the amount of metals<br />
present in these galaxies – that are otherwise<br />
invisible – at various epochs.<br />
This can best be done by high-resolution<br />
spectrographs on the largest telescopes,<br />
such as UVES on the VLT.<br />
Astronomers thus studied, with the<br />
UVES spectrograph on the VLT, the light<br />
emitted by the quasar SDSS J13 3-00 1.<br />
Located 9 billion light years away, its<br />
light is partially absorbed by an otherwise<br />
invisible galaxy sitting 6.3 billion light years<br />
away along the line of sight.<br />
The analysis of the spectrum shows that<br />
this galaxy has four times more metals<br />
than the Sun. This is the first time one<br />
finds such a large amount of ‘metals’<br />
in a very distant object, giving encouragement<br />
to astronomers. If a large number of<br />
such ‘invisible’ galaxies with high metal<br />
content were to be discovered, they<br />
might well alleviate the missing metals<br />
problem considerably.<br />
C. Péroux et al., 006, Astronomy and Astrophysics,<br />
450, 53.<br />
matter. They could thus be literally seeing<br />
the building up of a massive galaxy, like<br />
our own, the Milky Way.<br />
K.K. Nilsson et al. 006, Astronomy and Astrophysics,<br />
45 , 3.<br />
Red Blue
A 1.8-m Auxiliary Telescope at Paranal.<br />
<strong>ESO</strong> Annual Report 006<br />
7
8<br />
<strong>ESO</strong> Annual Report 006
Venus and the Moon setting over Paranal.<br />
<strong>ESO</strong> Annual Report 006<br />
9
La Silla Paranal Observatory<br />
In 006 the La Silla Paranal Observatory<br />
has been routinely operating a total of<br />
10 telescopes with 19 optical, near-infrared<br />
and mid-infrared instruments. On<br />
Paranal these are nine VLT instruments at<br />
the four 8. -m Unit Telescopes (UTs).<br />
There are also two instruments at the VLT<br />
Interferometer (VLTI), which coherently<br />
combine the light of the UTs or the 1.8-m<br />
Auxiliary Telescopes (ATs). On La Silla, a<br />
total of eight instruments are operated on<br />
the 3.5-m NTT, the 3.6-m, and the MPG/<br />
<strong>ESO</strong> . -m telescopes.<br />
The observatory has also supported the<br />
operation of the Atacama Pathfinder<br />
Experiment (APEX). The 1 -m APEX<br />
antenna is located on the high plateau<br />
of Chajnantor at an altitude of 5100 m.<br />
APEX and its two workhorse instruments,<br />
APEX a and FLASH, have been<br />
operated from the base camp in the village<br />
of Sequitor near San Pedro de<br />
Atacama. During this first year of regular<br />
operation about 10 nights of mostly<br />
Service Mode observations were carried<br />
out at APEX with an average observing<br />
time of 13 hours per night.<br />
In 006 more than 630 peer-reviewed articles<br />
and papers were published in scientific<br />
journals in which the authors have<br />
made use of astronomical data collected<br />
with telescopes and instruments available<br />
at the three sites of the La Silla Paranal<br />
Observatory. This number translates into<br />
an impressive publication rate of nearly<br />
two refereed papers for every day of the<br />
year. APEX alone in its very first year of<br />
routine operations has produced the respectable<br />
number of 1 publications – all<br />
contained in a special edition of the Astronomy<br />
& Astrophysics journal.<br />
One of the important ingredients for such<br />
a high productivity of the observatory is<br />
the high availability of its telescopes and<br />
instruments to carry out scientific observations.<br />
In this respect the observatory<br />
had another excellent year, with a total of<br />
410 nights scheduled for scientific<br />
observations with the four UTs at the VLT<br />
and with the three major telescopes at<br />
La Silla. In addition, the VLTI was oper-<br />
30<br />
<strong>ESO</strong> Annual Report 006<br />
ated for about 140 nights, executing scientific<br />
observations with its MIDI and<br />
AMBER instruments. This total number of<br />
nights scheduled for scientific observations<br />
is equivalent to about 90% of the<br />
theoretically available total time.<br />
The remaining 10 % were scheduled<br />
for planned engineering and maintenance<br />
activities to guarantee the continuous<br />
performance of the telescopes and instruments.<br />
Technical time further includes<br />
the time slots required to commission<br />
the new instruments and facilities, which<br />
keep arriving in particular on Paranal for<br />
the VLT.<br />
Of the available science time on Paranal,<br />
only .3% was lost due to technical problems<br />
and about 6% due to bad weather.<br />
On La Silla bad weather accounted for a<br />
loss of about 11%, and technical<br />
problems for 5.4%. This comparatively<br />
high figure for the technical downtime in<br />
La Silla was solely due to a major problem<br />
of the aged dome rotation system of<br />
the 3.6-m telescope, which required extended<br />
periods of corrective maintenance<br />
during which no operation of the<br />
telescope was possible. Otherwise, the<br />
downtime figure would have been reduced<br />
to an excellent .6 %.<br />
One of the great technical achievements<br />
of the year has been the first-ever recoating<br />
of a secondary mirror (M ) of the<br />
VLT with a few-nanometre-thick layer of<br />
fresh aluminium (Al). The M of the VLT is<br />
a lightweight 1. -m hyperbolic mirror,<br />
made of beryllium in order to minimise its<br />
mass to allow precise and fast tilt motions<br />
(‘field stabilisation’) and chopping<br />
with frequencies of up to several hertz.<br />
The optical surface of the M is protected<br />
by a thin layer of nickel (Ni) onto which<br />
the reflective layer of Al is superimposed.<br />
The challenges are first to develop and<br />
define the M recoating procedure, then<br />
to actually remove the old Al layer without<br />
affecting the Ni layer, and finally to recoat<br />
the surface with fresh Al. The engineering<br />
department mastered these<br />
challenges for the M of Antu (UT1), in<br />
May 006. Recoating of the secondary<br />
mirrors of the UTs has now become part<br />
of the regular maintenance of the VLT<br />
to ensure the optimal long-term performance<br />
of the telescope optics. The scheduled<br />
recoating of the primary and tertiary<br />
mirrors of Kueyen (UT ) and Yepun (UT4)<br />
were also successfully performed.<br />
Cleaning a mirror at La Silla.
New Instruments and Facilities<br />
With the installation and commissioning<br />
of the CRIRES instrument on the Nasmyth<br />
A focus of Antu (UT1) a major milestone<br />
of the VLT programme was<br />
reached this year: the completion of the<br />
first generation of VLT instruments.<br />
CRIRES is a cryogenic high-resolution<br />
infrared échelle spectrograph, that provides<br />
a resolving power of up to 10 5 in the<br />
spectral range from 1 to 5 μm when used<br />
with a narrow slit of 0. arcseconds. After<br />
its successful commissioning in 006,<br />
CRIRES was offered for the first time to<br />
the astronomical community for Period<br />
79, which starts in April 007.<br />
The sixth <strong>ESO</strong> standard adaptive optics<br />
system, Multi-Applications Curvature<br />
Adaptive Optics (MACAO), was deployed<br />
on Paranal to feed the narrow CRIRES<br />
slit, and to optimise the achievable signalto-noise<br />
ratio and spatial resolution. Four<br />
MACAO systems were already installed<br />
in the Coudé feeds to VLTI, and a similar<br />
system has been installed in the Cassegrain<br />
focus of UT4 feeding the SINFONI<br />
instrument.<br />
Maximum concentration during the CRIRES Commissioning.<br />
The Laser Guide Star Facility (LGSF)<br />
achieved its ‘First Light’ in early 006 and<br />
created the first artificial star in the Paranal<br />
sky. The LGSF provides the adaptive<br />
optics (AO) systems of instruments like<br />
SINFONI and NACO with bright reference<br />
stars in regions of the sky where sufficiently<br />
bright natural stars cannot be<br />
found close enough to the scientific targets<br />
for the AO system to perform. The<br />
path from having seen the first artificial<br />
laser star to regular operations turned out<br />
to be longer and harder than expected<br />
after the initial success. Several modifications<br />
and improvements of the LGSF<br />
were required over the course of the year<br />
until the facility was successfully commissioned<br />
by the end of the year. The<br />
very first observations with SINFONI and<br />
NACO in the new LGS mode immediately<br />
gave a taste of the exciting new possibilities<br />
this facility will provide to the observatory<br />
in early 007 when the LGSF<br />
will be fully commissioned together with<br />
the AO instruments.<br />
The VLT welcomed its second Visitor<br />
Instrument, DAZLE (Dark Age ‘Z’ Lymanalpha<br />
Explorer). DAZLE is an innovative<br />
narrowband imaging instrument, specifically<br />
developed by the Institute of Astronomy<br />
(Cambridge, UK) and the Anglo-<br />
Australian Observatory for use on the<br />
Visitor focus of UT3 (Melipal) in order to<br />
detect the most distant objects in the<br />
Universe. Nine nights of data were taken<br />
with the VLT and first results from this<br />
ambitious search project are eagerly expected.<br />
On La Silla the mid-infrared instrument<br />
TIMMI was decommissioned after the<br />
corresponding mid-infrared instrument<br />
VISIR at the VLT had begun full operation.<br />
A new telescope has joined the suite of<br />
gamma-ray burst (GRB) hunters on<br />
La Silla: the very fast moving and robotic<br />
TAROT-S telescope has been installed<br />
by a consortium led by Observatoire de<br />
Haute-Provence to follow-up GRBs within<br />
seconds of their detection by dedicated<br />
satellites in the Earth’s orbit. The new<br />
telescope delivered first results on newlydetected<br />
GRBs only a few days after its<br />
installation.<br />
The . -m telescope on La Silla was prepared<br />
over the year to receive the GRB<br />
follow-up instrument GROND, which<br />
is being built by the Max-Planck-Institut<br />
für Extraterrestrische Physik and will be<br />
commissioned in early 007.<br />
GRBs also triggered several fast followup<br />
observations with the VLT using<br />
the novel Rapid-Response Mode (RRM),<br />
which allows authorised VLT users<br />
to interrupt ongoing observations and to<br />
point the UTs to a transient target of<br />
interest. On 7 June 006, the Rapid-Response<br />
Mode triggered UVES observations<br />
of the quickly fading afterglow of<br />
a distant gamma-ray source. Integrations<br />
with the high-resolution spectrograph<br />
started a mere 7.5 minutes after the detection<br />
of the GRB by the SWIFT satellite<br />
– to date, still a record for the spectroscopic<br />
follow-up of any GRB.<br />
APEX is expecting its final suite of facility<br />
instruments, including new heterodyne<br />
receivers from the Onsala Space Observatory<br />
to cover all atmospheric windows<br />
from 00 to 1000 GHz, and the Large<br />
<strong>ESO</strong> Annual Report 006<br />
31
APEX Bolometer Camera (LABOCA) developed<br />
by the Max-Planck-Institut für<br />
Radioastronomie. LABOCA, a detector<br />
array with 95 pixels operating at a wavelength<br />
of 870 μm, has been extensively<br />
tested during the year at Chajnantor. We<br />
expect regular science operation for all<br />
new instruments to start in 007.<br />
In addition to these workhorse instruments,<br />
several experimental receivers<br />
covering selected windows above 1 THz<br />
are under development. This frequency<br />
regime has so far been considered to<br />
be only accessible from space. However,<br />
the exceptional site of Chajnantor at<br />
an altitude of 5100 m, and the excellent<br />
quality of the APEX antenna, will allow<br />
us soon to explore the sky at the shortest<br />
radio wavelengths from the ground.<br />
The VLT Interferometer<br />
In 006 the VLT Interferometer (VLTI) executed<br />
about 140 nights of scientific<br />
observations with MIDI and AMBER using<br />
both UT and AT baselines. The other<br />
nights were used for intensive engineering<br />
and commissioning activities to<br />
complete and improve the interferometer<br />
infrastructure and to fully exploit the<br />
capabilities of the VLTI Sub-Array (VISA).<br />
The VISA feeds the VLTI infrastructure<br />
and instruments with the light from the<br />
1.8-m Auxiliary Telescopes (AT) when the<br />
individual UTs are used for stand-alone<br />
VLT observations. By the end of 006,<br />
VISA was completed with the arrival<br />
of the fourth AT and has become integral<br />
part of the VLTI science operation. Because<br />
it is now possible to choose between<br />
any six baselines and switch from<br />
one to another during the same night,<br />
AT4 provides the VLTI operations with<br />
ad-ditional flexibility in the selection of different<br />
and complementary AT baselines<br />
without having to physically reconfigure<br />
the array of telescopes. This capability, in<br />
combination with AMBER phase-closure<br />
on three telescopes, is an important step<br />
toward imaging with the VLTI.<br />
3<br />
<strong>ESO</strong> Annual Report 006<br />
The AMBER instrument allows the interferometric<br />
combination of up to three<br />
beams, and could be offered to the community<br />
for the first time with three ATs<br />
starting in Period 79 after first fringes<br />
were obtained on 3 August 006. The<br />
VLTI infrastructure was prepared accordingly<br />
and the three delay lines numbered<br />
4, 5 and 6 were equipped with<br />
Variable Curvature Mirrors (VCM) to control<br />
the longitudinal position of the pupil<br />
of the individual interferometric beams.<br />
The delay lines themselves were put under<br />
an intensive preventive maintenance<br />
plan in order to keep them literally in the<br />
best possible shape.<br />
These were all necessary steps towards<br />
the VLTI team’s ambitious goal of offering<br />
AMBER on three ATs with FINITO<br />
fringe-tracking for the call for proposals<br />
for Period 80, and to eventually bring<br />
AMBER close to the expected sensitivities<br />
in its different spectroscopic modes.<br />
A major milestone in this direction was<br />
reached when, for the first time, FINITO<br />
fringe-tracking with AMBER and three<br />
ATs was achieved on 1 December 006<br />
on the bright star b Ceti.<br />
The investigation and improvement of<br />
the stability of the interferometric beams,<br />
and in particular of the vibration-induced<br />
variations in the optical path differences<br />
(OPD) of the interferometric beams<br />
delivered by the 8. -m UTs, continued in<br />
parallel to the implementation of new VLTI<br />
observing modes with the VISA and the<br />
ATs.<br />
Working on APEX.<br />
Beam instabilities and vibrations of the<br />
UTs transmitted to the VLTI were identified<br />
as the primary reasons that prevented<br />
fringe-tracking with the UTs in the<br />
past. While the beam stability was recently<br />
improved dramatically through the<br />
introduction of fast beam control with the<br />
VLTI Infrared Image Sensor IRIS, the<br />
elimination of vibrations or their compensation<br />
remained the primary goal of the<br />
VLTI team during 006. Active suppression<br />
of the OPD variations as introduced<br />
by the vibrating optical surfaces of the<br />
Unit Telescopes was achieved through a<br />
novel Vibration Tracking (VTK) system.<br />
The performance of this vibration-suppression<br />
system was further enhanced by<br />
the installation of accelerometers close to<br />
the vibrating optical surfaces of the UTs.
User Support<br />
The User Support Department (USD) of the<br />
<strong>ESO</strong> Data Management and Operations<br />
Division, based in Garching, represents the<br />
primary link between the <strong>ESO</strong> community and<br />
the Observatory and its operation groups. It<br />
provides support primarily to Service Mode<br />
users of <strong>ESO</strong> facilities and to the operations<br />
teams of the La Silla Paranal Observatory. In<br />
006, Service Mode continued to be the most<br />
requested observing mode at the VLT (a<br />
factor of .5 higher than the time requested<br />
for Visitor Mode during Period 77 and 78).<br />
This clearly shows that the community has<br />
recognised the advantages of this observing<br />
mode for many different types of projects.<br />
Period 77 also marked the beginning of<br />
Service Mode observing at the APEX facility,<br />
the <strong>ESO</strong> Project Scientist of which is a<br />
member of the User Support Department.<br />
A total of 1054 Service Mode runs were<br />
supported by USD at the VLT, VLTI, and<br />
MPG/<strong>ESO</strong> . -m telescope during 006,<br />
which includes all runs approved during<br />
Period 77 and 78, including those that were<br />
granted telescope time via the Director’s<br />
Discretionary Time channel.<br />
Data Processing and Quality Control<br />
Ensuring that data taken on Paranal are of<br />
certified and predictable quality, and<br />
continuously monitoring the ‘health’ of the<br />
instruments, are cornerstone concepts in the<br />
<strong>ESO</strong> end-to-end data flow model. The DFO<br />
Quality Control (QC) group is responsible<br />
primarily for the monitoring and reporting of<br />
basic instrument performance for all VLT/VLTI<br />
instruments as well as the creation of various<br />
calibration and science data products for<br />
these instruments. Raw calibration data are<br />
processed into master calibration products<br />
that are used not only to monitor instrument<br />
performance but also to process science<br />
data. These master calibration products are<br />
stored in the <strong>ESO</strong> archive and are available to<br />
the scientific community at large.<br />
For Service Mode users, the QC group<br />
provides two additional services. First,<br />
Service Mode science data are processed<br />
into science products using standard<br />
pipelines which, by now, cover virtually 100 %<br />
of the Paranal data stream. Second, QC<br />
creates data packages that include all raw<br />
data, resultant products, and associated<br />
information for each and every Service Mode<br />
observing run. These packages are burned<br />
onto DVDs and shipped to users by the DFO<br />
SAO group.<br />
During 006 QC processed 5 TB of raw data<br />
in 156 500 processing jobs to create 1014<br />
service mode packages – an increase of 13 %<br />
compared to 005 – which were distributed<br />
to their respective Principal Investigators on<br />
100 DVDs. The quality control processing of<br />
the expected 150 TB/year of VISTA/VIRCAM<br />
data will certainly be challenging. New<br />
concepts and tools were developed and<br />
tested in 006 both to cope with the<br />
computing challenges posed by the high data<br />
rate itself and to efficiently monitor the quality<br />
of a large number of images.<br />
The Data Flow System<br />
The Data Flow System Department is responsible<br />
for the design, the implementation<br />
and the maintenance of the Data Flow System<br />
software components, that are critical for the<br />
end-to-end operation of the VLT, VLTI, VST,<br />
VISTA and some of the La Silla telescopes.<br />
The Data Flow System consists of two kinds<br />
of modules or tools. Some of them (e.g.<br />
P PP) are generic and provide a uniform<br />
interface to all instruments, while others, e.g.<br />
pipelines, are instrument specific. The<br />
department delivers its tools to a variety of<br />
customers: the astronomical community (e.g.<br />
P PP, Exposure Time Calculators, Archive<br />
Interface), VISAS and OPC, User Support<br />
Department (P PP, Observing Tool), and<br />
Science Operations and Data Flow Operation<br />
(Instrument Pipelines, data packing tools).<br />
The Data Flow System Department is also<br />
responsible for the installation and the<br />
commissioning of its software modules<br />
on-site.<br />
The front-end and back-end teams continued<br />
to concentrate their efforts on the design and<br />
implementation of software components<br />
required to support survey facilities. This<br />
includes an upgrade of the Observation<br />
Preparation Tools to introduce new scheduling<br />
concepts such as groups and links of<br />
Observation Blocks. The development of the<br />
User Portal, which will provide the user<br />
community with one registration system for all<br />
services provided by the Observatory, is<br />
progressing well. The pipeline team released<br />
three instrument pipelines to the community:<br />
the ISAAC, VISIR and GIRAFFE packages,<br />
based on the Common Pipeline Library. At the<br />
same time, the CRIRES pipeline was verified<br />
and validated during the commissioning<br />
phases of the instrument. The pipeline team<br />
developed an innovative algorithm based on<br />
pattern-matching for the wavelength calibration<br />
of spectroscopic data. This algorithm was<br />
implemented in the new FORS pipeline, which<br />
is now fully operational and will become<br />
publicly available in the first quarter of 007.<br />
During 006 the SAMPO work has focused on<br />
addressing the requirements within the <strong>ESO</strong><br />
community for more flexible access to the<br />
<strong>ESO</strong> reduction pipeline recipes. Following a<br />
review of the available options an open source<br />
graphical workflow system (Taverna) was<br />
selected and extensively extended to interface<br />
to <strong>ESO</strong> software components. This workflow<br />
system has been named <strong>ESO</strong> Reflex (<strong>ESO</strong><br />
Recipe Flexible Execution Workbench). The<br />
FORS spectroscopy and AMBER recipes have<br />
been integrated in a beta-test version of<br />
Reflex.<br />
The Reflex scientific workflow allows users to run<br />
instrument recipes as a sequence of reduction steps<br />
while inspecting intermediate products and calling<br />
external applications.<br />
<strong>ESO</strong> Annual Report 006<br />
33
The accelerometers enable the feeding of<br />
direct measurements of the actual vibration<br />
signals to the VTK system. Through<br />
this effort the original residual OPD variations<br />
of 480 nm were reduced by the end<br />
of the year to 30 nm. The VLTI team is<br />
confident that, with a robust implementation<br />
of these new vibration-suppression<br />
techniques and further elimination of the<br />
major vibration sources, fringe-tracking<br />
with three UTs and AMBER can be delivered<br />
to science operations by the end<br />
of 007 – just in time for the observatory<br />
to receive PRIMA, the next VLTI facility,<br />
which is expected to further push the<br />
sensitivity of the VLTI and provide relative<br />
astrometric measurements of the highest<br />
precision.<br />
VST and VISTA Survey Telescopes<br />
The construction, integration and test-<br />
ing of the .4-m optical VLT Survey Telescope<br />
(VST) and its subsystems con-<br />
tinued in Naples during 006 by the<br />
Osservatorio di Capodimonte. The disassembly<br />
of the main telescope structure<br />
started in collaboration with <strong>ESO</strong> at the<br />
end of the year, to prepare for the shipment<br />
to Paranal where the reintegration<br />
of the telescope is planned during the<br />
second half of 007.<br />
34<br />
<strong>ESO</strong> Annual Report 006<br />
The primary mirror cell and the secondary<br />
mirror unit, however, remain in Naples for<br />
their completion. The VST secondary<br />
mirror optics were completed and shipped<br />
to Paranal early this year while the .4-m<br />
primary mirror remained at the manufacturer’s<br />
premises for its completion.<br />
The 4. -m infrared survey telescope<br />
VISTA is currently under construction by<br />
the VISTA project office on its own peak<br />
about 1500 m from the Paranal summit.<br />
The enclosure was essentially completed<br />
and accepted before the telescope<br />
structure arrived on 11 May 006. Since<br />
then, the telescope assembly progressed<br />
rapidly and the VISTA telescope had<br />
entered a phase of intensive testing and<br />
tuning by the end of the year. At the same<br />
time, the VISTA facility was integrated<br />
into the power and computer networks of<br />
the Paranal site to prepare for its future<br />
operation. VISTA – as all telescopes on<br />
Paranal – will eventually be operated from<br />
the same common control room as the<br />
VLT and the VLTI.<br />
A dedicated coating unit arrived in September<br />
and was successfully commissioned<br />
in the following months. The<br />
VISTA coating unit is the only facility<br />
on Paranal that allows the coating of<br />
mirror surfaces with a layer of silver (instead<br />
of aluminium as used for the<br />
VLT mirrors) to provide highest reflectivity<br />
of the optical surfaces in the near-infrared<br />
wavelengths where VISTA is going to<br />
survey the sky.<br />
The VISTA telescope is now awaiting the<br />
arrival of its optics and its instrument.<br />
The primary and secondary mirrors are<br />
still in the phase of final polishing in Europe,<br />
and are now only expected to arrive<br />
on Paranal in the second quarter of 007.<br />
Commissioning of the telescope and the<br />
formal handover to <strong>ESO</strong> are planned to<br />
take place in the second half of 007.<br />
In December, the IR Camera that was<br />
developed at the Rutherford Appleton<br />
Laboratory in the UK was also shipped to<br />
Paranal for arrival in mid-January 007.<br />
VISTA enclosure. The VISTA telescope.
<strong>ESO</strong> Annual Report 006<br />
35
36<br />
Llano de Chajnantor<br />
<strong>ESO</strong> Annual Report 006
<strong>ESO</strong> Annual Report 006<br />
37
Atacama Large Millimeter/submillimeter Array<br />
The Atacama Large Millimeter/submillimeter<br />
Array (ALMA) is a very sensitive,<br />
high-resolution aperture-synthesis array<br />
telescope, which will work at millimetre<br />
and submillimetre wavelengths. It is an<br />
international facility, constructed and<br />
operated as a partnership between<br />
Europe (through <strong>ESO</strong>), North America<br />
(through the National Radio Astronomy<br />
Observatory, NRAO) and Japan (through<br />
the National Astronomical Observatory of<br />
Japan, NAOJ), in cooperation with the<br />
Republic of Chile.<br />
The initial plan was to install and operate<br />
64 antennas of 1 metres diameter, but<br />
detailed design studies and prototype<br />
research showed that this project could<br />
not be realised with the funds foreseen<br />
by the agreement between the North<br />
American and European partners. During<br />
005, in-depth studies were made to<br />
redefine the ALMA baseline project with<br />
acceptable cost, while still maintaining<br />
the prime scientific objectives. By the<br />
middle of 006, the North American<br />
partners received approval from their<br />
Funding Agency (the US National Science<br />
Foundation, NSF) for the rebaselined<br />
ALMA project, which had already been<br />
approved by <strong>ESO</strong> Council towards the<br />
end of 005.<br />
In parallel, Japanese scientists, through<br />
the NAOJ, continued to define their<br />
participation in the ALMA project. The<br />
European and North American partners<br />
in ALMA spent a considerable amount of<br />
time with their Japanese partners in<br />
identifying the Japanese participation and<br />
reviewed various subsystems, in particular<br />
the correlator, receivers and antennas.<br />
Details of the partnerships were defined<br />
and a trilateral agreement between <strong>ESO</strong>,<br />
the NSF, and the National Institute for<br />
Natural Sciences (NINS, Japan) was<br />
signed in summer 006. In addition to the<br />
equipment that NAOJ will provide for the<br />
bilateral ALMA configuration of 50<br />
antennas, NAOJ will provide four antennas<br />
of 1 metre diameter, twelve antennas<br />
of 7 metre diameter, and two receiver<br />
bands for all 66 antennas of ALMA.<br />
Approval of funds required for the<br />
Japanese participation in ALMA is<br />
38<br />
<strong>ESO</strong> Annual Report 006<br />
expected by spring 007. With the<br />
inclusion of the Japanese partners,<br />
ALMA becomes a truly global astronomy<br />
facility, involving scientists from four<br />
different continents.<br />
Construction Work<br />
The ALMA Array Operations Site (AOS)<br />
will be located at a truly unique and<br />
unusual place: the Altiplano de Chajnantor,<br />
a plateau at an altitude of 5 000<br />
metres above sea level, in the Atacama<br />
Desert in Chile. This location was<br />
selected for scientific reasons, particularly<br />
dryness and altitude. Considering<br />
these aspects, the ALMA Observatory<br />
will not only be unique because of its<br />
ambitious scientific goals and the<br />
unprecedented technical requirements.<br />
It will also be unique because of the<br />
harsh environment and living conditions<br />
in which the array has to operate with<br />
high efficiency and accuracy.<br />
A second site, the ALMA Operations<br />
Support Facilities (OSF), will be the base<br />
camp for the day-to-day operation of the<br />
observatory. It is located at an altitude of<br />
about 900 metres, quite high compared<br />
to standard living conditions, but still<br />
acceptable for scientific projects in<br />
astronomy of similar scope. However, the<br />
OSF will not only serve as the location for<br />
operating the ALMA Observatory: it will<br />
also be the site for Assembly, Integration<br />
and Verification (AIV) of all the hightechnology<br />
equipment before this is<br />
moved to the Array Operations Site.<br />
The AOS Technical Building.<br />
Both the AOS and OSF are remote<br />
locations. The 900-metre OSF site is<br />
about 15 kilometres away from the<br />
closest public road, the Chilean highway<br />
No. 3. The AOS is another 8 kilometres<br />
away from the OSF site. Thus, one of the<br />
first ALMA projects was to construct an<br />
access road not only to the OSF but also<br />
to the AOS. This road, 43 kilometres long<br />
and at high altitude, with sufficient width<br />
for the regular transport of many large<br />
radio telescopes with diameters of 1<br />
metres, was completed in the course of<br />
006.<br />
The OSF is in many ways the centre of<br />
activities of the ALMA project, and will<br />
remain so in the future. The focus there<br />
will, however, change as ALMA moves<br />
through the different phases of construction<br />
and operations.<br />
Presently, the OSF site is the area where<br />
all ALMA Site contractors and their staff<br />
are accommodated – the base camp for<br />
work on the OSF and AOS infrastructure.<br />
Local contractors’ staff live there and<br />
start their work either at the OSF, the<br />
road construction (between the Chilean<br />
Highway No. 3 and the AOS) or at the<br />
AOS itself. Work is organised in 0 days<br />
working/10 days rest periods. Special<br />
facilities for board and lodging have had<br />
to be organised for such a large activity.<br />
Camps have been erected and by now<br />
can accommodate the maximum<br />
required capacity of 500 workers.
Construction of the OSF Technical Buildings.<br />
The construction of the multi-purpose<br />
OSF, intended to serve over the lifetime of<br />
the observatory, is a challenging task. It<br />
requires taking into account many<br />
aspects of the functionality of these<br />
facilities over a period of 30 years. During<br />
the years 005 and 006 the Technical<br />
Specifications and Statements of Work<br />
for the OSF construction were defined,<br />
refined and adapted to the requirements<br />
and resources of ALMA. <strong>ESO</strong> signed a<br />
very important contract for the construction<br />
of the OSF Technical Facilities in<br />
August 006. Construction work has<br />
started, and during the first five months of<br />
this unique endeavour no major problems<br />
or delays occurred. As specified in the<br />
construction schedule, foundations have<br />
been prepared and the erection of the<br />
first walls started in November 006.<br />
Provisional Acceptance of all facilities is<br />
foreseen for the first quarter of 008.<br />
The construction of the AOS Technical<br />
Building, a project to be delivered by the<br />
North American partner in ALMA, started<br />
in October 005 and the outer shell was<br />
completed by mid- 006. After this date<br />
installation of the interior infrastructure<br />
started.<br />
Antennas<br />
The four antennas of 1 metre diameter<br />
to be provided by Japan have been<br />
ordered from Mitsubishi Electrical<br />
Company by NAOJ. The twelve remaining<br />
antennas of 7 metre diameter will be<br />
ordered during the year 007.<br />
The Preliminary Production Design<br />
Review for antennas to be produced by<br />
Vertex SRL was held in September 006.<br />
The corresponding review for the AEM<br />
antennas contracted by <strong>ESO</strong> is scheduled<br />
for the end of January 007.<br />
The design of the antenna transporter<br />
vehicle has progressed well. Some<br />
delays, due to long delivery time for<br />
materials, have arisen. The first transporter<br />
is expected to be delivered to the<br />
OSF in October 007, about three<br />
months later than originally foreseen.<br />
Front End<br />
The ALMA Front End system is the first<br />
element in a complex chain of signal<br />
reception, conversion, processing and<br />
recording. The Front End is designed to<br />
receive signals in ten different frequency<br />
bands. In the initial phase of operation<br />
the antennas will be equipped with six<br />
bands. These are Bands 3, 4, 6, 7, 8 and<br />
9. <strong>ESO</strong> is in charge of providing Bands 7<br />
and 9. It is planned to equip the antennas<br />
with the missing bands at a later stage of<br />
ALMA operation.<br />
The ALMA Front Ends are superior to<br />
almost all existing systems. Indeed,<br />
development work for the ALMA prototypes<br />
has also led to improved receivers<br />
for existing millimetre and submillimetre<br />
observatories.<br />
The Front End units are comprised of<br />
numerous elements, produced at<br />
different locations in Europe, North America<br />
and East Asia. In the initial phase of<br />
construction after the prototyping and<br />
developing stage, it was decided to build<br />
a set of eight pre-production units before<br />
moving to mass production. This initial<br />
phase started in the years 00 and<br />
003. The pre-production phase has<br />
advanced well and 006 was an especially<br />
important year, because it marked<br />
the start of the transition from this preproduction<br />
to the final series production<br />
phase.<br />
<strong>ESO</strong> Annual Report 006<br />
39
ALMA FE No. 1 rear view (chassis covers removed)<br />
with receiver cartridges for Bands 3, 6, 7 and 9<br />
installed.<br />
In 006, the European groups made<br />
essential contributions to the integration<br />
of the first ALMA front end. In early 006,<br />
the Band 7 Cartridge delivered by IRAM<br />
(Grenoble, France) was the first of all the<br />
cartridges to be accepted by the North<br />
American Front End Integration Centre<br />
(NAFEIC), which is based at NRAO<br />
(Charlottesville, Virginia, USA). The first<br />
Band 9 Cartridge, manufactured by<br />
NOVA (Groningen, the Netherlands), was<br />
successfully delivered and accepted by<br />
the NAFEIC at the end of 006.<br />
Receiver noise performance for three Band 9 Cartridge (pre-production) units.<br />
40<br />
<strong>ESO</strong> Annual Report 006<br />
In 003, <strong>ESO</strong> and the Rutherford<br />
Appleton Laboratory (RAL, UK) launched<br />
a development and pre-production<br />
programme for the manufacture of eight<br />
operational cryostats. By the end of<br />
006, six cryostats had been fully<br />
assembled. The remaining two units are<br />
in manufacture and will be completed in<br />
early 007.<br />
With the end of the pre-production phase<br />
of these cryostats in sight, efforts were<br />
made to prepare the final series production<br />
phase. This resulted in the approval<br />
by <strong>ESO</strong> Finance Committee at its<br />
November 006 meeting of a proposal to<br />
place a contract for 45 production units<br />
to cover the needs of the ALMA Baseline.<br />
With the ongoing production of ALMA<br />
receiver cartridges, more insight was also<br />
obtained into the repeatability of their<br />
performance. Collecting this information<br />
was one of the main goals of the preproduction<br />
phase, and is essential for<br />
increasing the accuracy of the series<br />
production schedule. The graph below<br />
shows the receiver noise performance for<br />
three Band 9 Cartridges, each having<br />
two independent polarisation channels.<br />
Besides the exceptionally good noise<br />
performance for reach of the cartridges –<br />
well within the specified project requirements<br />
– the repeatability is very good.<br />
Pre-production 4-8 GHz cryogenic low-noise amplifier.<br />
In the framework of an EC FP6 programme,<br />
<strong>ESO</strong> is leading a group of<br />
European institutes to develop and build<br />
six Band-5 receiver cartridges and to<br />
develop associated software. This<br />
project, “Enhancement of ALMA Early<br />
Science”, was approved by the European<br />
Commission at the end of 005 and<br />
actual work started in January 006. The<br />
Band 5 receiver design is being developed<br />
by the Onsala Space Observatory<br />
(OSO, Sweden). By the end of 006,<br />
most of the receiver design concept had<br />
been finalised.<br />
Discussions have been initiated between<br />
<strong>ESO</strong>, OSO, and RAL to provide the local<br />
oscillator as needed in this Band 5<br />
receiver. An initial plan for this activity has<br />
been provided by RAL and it is planned<br />
to include them as a participant in the<br />
FP6 programme.<br />
The pre-production phase of the cryogenic<br />
low-noise amplifiers used in the IF<br />
of the Band 7, 4-8 GHz bandwidth, and<br />
Band 9, 4-1 GHz bandwidth receivers<br />
has been successfully completed by<br />
Centro Astronómico de Yebes (CAY,<br />
Spain). Amplifier production for the Band<br />
7 cartridges (198 units) by industry will<br />
commence in early 007. A proposal was<br />
received and approved by the <strong>ESO</strong><br />
Finance Committee at its meeting in<br />
November 006.<br />
Production of the more complex 4-1<br />
GHz cryogenic amplifiers will remain at<br />
CAY. It is planned to start this series<br />
production phase in early 007.
Water Vapour Radiometers (WVRs)<br />
operating at 183 GHz are essential for<br />
ALMA to improve the fidelity of highresolution<br />
radio maps when using<br />
baselines longer than 300 metres. These<br />
radiometers provide a correction of the<br />
signal phase due to atmospheric water<br />
vapour fluctuations. The development of<br />
two prototype WVRs, a joint undertaking<br />
by the University of Cambridge and OSO,<br />
has been completed and they are<br />
undergoing intensive tests at the Submillimeter<br />
Array (SMA) on Mauna Kea<br />
(Hawaii). This field test of the WVRs has<br />
shown that it is feasible to do this<br />
correction of the atmospheric phase<br />
fluctuations with the necessary accuracy.<br />
The performance of both prototypes<br />
meets the requirements, and a simpler,<br />
more cost-effective, single-channel Dicke<br />
switched radiometer design has been<br />
adopted as the baseline for production.<br />
By the end of 006 a Call for Tender had<br />
been prepared for the final detailed<br />
design phase and production phase of<br />
53 units. This Call will be issued to<br />
industry in early 007.<br />
Back End<br />
The ALMA Back End systems deliver<br />
signals generated by Front End units<br />
installed in each antenna to the central<br />
Correlator at the AOS Technical Building.<br />
At any time, 8 GHz of signal bandwidth in<br />
each of two orthogonal linear polarisations<br />
can be processed and recorded.<br />
Analogue data, produced by the Front<br />
End electronics, are processed and<br />
digitised before entering first the data<br />
encoder, and then the optical transmitter<br />
Pre-production ALMA cryostat lined up for delivery<br />
at the Rutherford Appleton Laboratory.<br />
units and multiplexers. All these elements<br />
are installed in the receiver cabins of<br />
each antenna. Optical signals are then<br />
transmitted by fibres to the AOS Technical<br />
Building. The total distance in the<br />
most extended antenna configuration is<br />
about 15 kilometres. At the AOS Technical<br />
Building the incoming optical signals<br />
are de-multiplexed and de-formatted<br />
before entering the Correlator.<br />
The European deliverables in the ALMA<br />
Back End project are various components,<br />
which are produced by several<br />
European institutes, working closely with<br />
<strong>ESO</strong> and NRAO. These deliverables are:<br />
– digitiser chip production<br />
– digitiser chip assembly,<br />
– digitiser clock and assembly,<br />
– optical data transmission system<br />
design,<br />
– fibre patch panel,<br />
– optical multiplexers (MUX), amplifiers<br />
(EDFA), and de-multiplexers (De-MUX),<br />
and<br />
– photonic local oscillator photomixers.<br />
Development and pre-production of<br />
these components has either been<br />
successfully completed or is so far<br />
advanced that completion will happen in<br />
the first few months of 007. The components<br />
will be integrated at the Back End<br />
Integration Center at Socorro (New<br />
Mexico) and installed in the European<br />
and North American prototype antennas<br />
for tests at the ALMA Test Facility.<br />
Correlator<br />
The ALMA Correlator, to be installed in<br />
the AOS Technical Building, is the last<br />
component in the receiving end of the<br />
data transmission. It takes as input the<br />
digitised signals from the individual<br />
antennas, and outputs amplitude and<br />
phase on all of the interferometer<br />
baselines in each of a large number of<br />
spectral channels. It is a very large data-<br />
processing system, composed of four<br />
quadrants, each of which can process<br />
data coming from up to 16 different<br />
antennas. The complete correlator will<br />
have 91 printed circuit boards, 5 00<br />
interface cables, and more than 0<br />
million solder joints. The first quadrant<br />
was completed at NRAO in the third<br />
quarter of 006. Work on the second<br />
quadrant is progressing on schedule.<br />
Integral parts of the Correlator are<br />
Tunable Filter Bank (TFB) cards, which<br />
allow a major increase in the flexibility by<br />
subdividing the frequency range into 3<br />
independently configurable sub-channels.<br />
The layout is such that four TFB<br />
cards are needed for the data coming<br />
from a single antenna. The TFB cards<br />
have been developed and optimised by<br />
the University of Bordeaux over the last<br />
few years. Prototypes and pre-production<br />
units have been extensively tested and<br />
their performance was critically reviewed<br />
in the first half of 006. In the meantime,<br />
series production has started and the first<br />
batch of 36 cards has been produced.<br />
Software Development<br />
The ALMA software is planned from the<br />
beginning as an end-to-end software<br />
system, which goes from proposal<br />
preparation to data reduction, including<br />
all the necessary control software for<br />
antennas and correlator. The computing<br />
work in Europe is organised through<br />
<strong>ESO</strong>. Many developments are done<br />
directly by <strong>ESO</strong>; others are done in<br />
collaboration with European institutes in<br />
Spain, France, Italy, Germany and the<br />
United Kingdom.<br />
In 006, the ALMA software was tested<br />
end-to-end in different observing modes,<br />
starting from proposals consisting of<br />
Scheduling Blocks up to reducing data<br />
obtained with the ALMA prototype<br />
antennas at the ALMA Test Facility (ATF)<br />
located at the site o the Very Large Array<br />
(VLA) in Socorro. <strong>ESO</strong> and its associated<br />
institutes not only provided their software<br />
for this, but also actively participated in<br />
the testing campaigns.<br />
The next goal is to perform interferometry<br />
tests with the two prototype antennas at<br />
the ATF, while preparing to support<br />
integration and tests of the first European<br />
ALMA antenna to be delivered to Chile in<br />
the second part of 007.<br />
<strong>ESO</strong> Annual Report 006<br />
41
System Engineering (SE)<br />
Substantial progress was achieved on<br />
project-wide requirements and Interface<br />
Control Document (ICD) completion,<br />
which are now 93% and 80% completed,<br />
respectively. The ALMA system requirement<br />
version B was released, and is now<br />
consistent with the refined science<br />
requirements document and much more<br />
complete. Progress was also made on<br />
the Front End and Back End requirements<br />
and these will be formally released<br />
at the beginning of 007. The requirements<br />
database DOORS was updated<br />
and enhanced, and more requirements<br />
were added.<br />
The 3-dimensional models of the AEM<br />
and Vertex Antenna receiver cabins with<br />
their interiors have been developed and<br />
documented. The Antenna cabling<br />
designs for these antennas were done<br />
and released. Support was given to all<br />
Integrated Project Teams (IPTs) for their<br />
technical activities, e.g. for the ridges<br />
procurement and for the design and<br />
manufacturing of the ridges alignment<br />
tool. The mechanical tolerance budget<br />
was refined. Master Frequency Standard<br />
specification was prepared and the<br />
procurement process was initiated.<br />
ALMA system block diagrams have been<br />
updated, refined and distributed. The<br />
sensitivity budget was further refined and<br />
used for system design trade-offs and<br />
analysis tasks.<br />
System Engineering participated in<br />
several review meetings, such as maser<br />
laser review, and organised and chaired<br />
the Antenna Transporter PDR, Band 7<br />
Cartridge CDR, 1st Local Oscillator CDR,<br />
System Requirement review, Vertex<br />
antenna Pre-production review (PPDR),<br />
and the ACA correlator CDR.<br />
4<br />
<strong>ESO</strong> Annual Report 006<br />
The ALMA optical analysis led by SE<br />
started. The goal is to perform a detailed<br />
analysis of the antenna optical performance<br />
including polarisation, sidelobe<br />
patterns, and subreflector scattering<br />
cone under load conditions to predict<br />
antenna performance and the science<br />
case of polarisation mosaicing.<br />
A new ALMA Product Assurance (PA)<br />
manager was hired in mid- 006. His main<br />
task was to organise PA to be ready for<br />
the production contracts. This was<br />
achieved through close cooperation and<br />
meeting with all IPTs. Also, Statements of<br />
Work, verification plans and PA plans<br />
were reviewed and updated.<br />
System prototyping in the laboratory<br />
continued until November. A lot of<br />
detailed technical work was done to<br />
finally achieve continuity of the signal<br />
chain in the laboratory. Millimetrewavelength<br />
cross-correlation was<br />
achieved in the lab using both the AEM<br />
and Vertex antenna racks. For this a<br />
signal at 86 GHz was injected into each<br />
leg of the RF simulator. Then, system<br />
level testing, leading to phase tracking<br />
and delay switching interferometry, was<br />
achieved in the lab.<br />
After that the Back End antenna racks<br />
were removed from the lab in November,<br />
moved onto the antennas, and installed.<br />
The Evaluation Front Ends were also<br />
installed on both antennas, on which the<br />
signal path through the Front End to the<br />
Correlator is functional; the evaluation<br />
Front Ends were cooled down; and<br />
monitoring and control is functional via<br />
control software. The Central Local<br />
Oscillator racks and Correlator were<br />
installed, populated, powered up, and<br />
monitoring and control was established.<br />
First on-the-sky fringes are expected in<br />
the first quarter of 007.<br />
Other activities of PSI staff were the<br />
support of the holography system at the<br />
ATF and the support of the photogrammetry<br />
mission.<br />
System integration planning in Chile<br />
progressed well. Discussions with all IPTs<br />
about deliveries and acceptance of<br />
equipment for Chilean Assembly,<br />
Integration and Verification (AIV) were<br />
held and documented. The Japanese AIV<br />
involvement, deliverable and schedule<br />
were agreed. The interface between the<br />
ALMA Back End engineers at work.<br />
IPTs delivering the equipment and the<br />
commissioning team receiving the system<br />
from AIVS was agreed and documented.<br />
The AIV Interim Lab construction, needed<br />
because the OSF technical building will<br />
only be ready at the beginning of 008,<br />
was completed. The Holography Tower<br />
construction was completed. In total 11<br />
AIV engineers have been employed. All<br />
are posted at the executives (Socorro,<br />
Charlottesville, Garching) for training.<br />
Science Activities<br />
One of the main roles of the Science IPT<br />
is to define the top-level science requirements<br />
for ALMA and, in close collaboration<br />
with the System Engineering team, to<br />
ensure that they can be met by the<br />
hardware and software. The year 006<br />
saw the completion of a comprehensive<br />
System Requirements Review, covering<br />
all aspects of the specification. The major<br />
conclusion was that the current design<br />
would indeed meet (and in several areas<br />
such as receiver sensitivity even exceed)<br />
the demanding specification.
The calibration of ALMA is a challenging<br />
problem. The Science IPT has produced<br />
a comprehensive series of examples<br />
which demonstrate how key quantities<br />
such as amplitude, phase, antenna<br />
location and instrumental polarisation can<br />
be calibrated in practice. Even on the<br />
excellent Chajnantor site, water vapour in<br />
the atmosphere both absorbs and<br />
refracts millimetre waves from astronomical<br />
sources. To correct the fast fluctuations<br />
of phase which would otherwise<br />
limit imaging, ALMA will use a combination<br />
of two methods: fast switching<br />
between the object of interest and a<br />
nearby point calibrator, and water vapour<br />
radiometry. The latter technique measures<br />
emission from the 183-GHz atmospheric<br />
water line, using receivers<br />
mounted on each antenna and infers the<br />
resulting phase differences on all<br />
baselines.<br />
ALMA Regional Centre<br />
The European ALMA Regional Centre<br />
(ARC) is part of <strong>ESO</strong>’s Data Management<br />
Operations Division and started its activities<br />
on 1 June 006. The ARC’s mission<br />
is to provide the science and technical<br />
support services necessary for<br />
the European user community to exploit<br />
ALMA to its full scientific potential. The<br />
ARC will form the interface between<br />
the ALMA Observatory in Chile and the<br />
European user community. Similar ARCs<br />
are currently being established in North<br />
America and East Asia, <strong>ESO</strong>’s partners in<br />
the trilateral ALMA project. For Europe-<br />
an users, the ARC is being set up as a<br />
cluster of nodes located throughout Europe,<br />
with the main coordinating centre at<br />
the <strong>ESO</strong> Headquarters in Garching. In<br />
this distributed network, user support<br />
and operations experience at <strong>ESO</strong> can<br />
be mixed with millimetre-wave astronomy<br />
experience that exists in the communi-<br />
ty to create optimal science support services.<br />
The European ARC will be the point of<br />
contact for European ALMA users<br />
from the moment of proposal submission<br />
to the actual distribution of calibrated<br />
data and consequent analysis. The core<br />
of the ARC activities will consist of running<br />
a help desk for the proposal submission<br />
and submission of observing programmes,<br />
the delivery of data to principal<br />
investigators, the maintenance and refinement<br />
of the ALMA data archive, and<br />
the feedback to the data reduction pipeline<br />
and the off-line reduction software<br />
systems that surround it.<br />
Among the tasks of the ARC Manager is<br />
the contribution to the preparation of<br />
the ALMA Operations Plan (AOP), which<br />
describes both the science operations<br />
and the technical services provided by<br />
the technical staff when ALMA becomes<br />
operational, and its implementation within<br />
<strong>ESO</strong>.<br />
Fundamental to ALMA’s success in Europe<br />
are the enhanced services provided<br />
by the network of ARC nodes. These are<br />
required to fully realise the potential of<br />
ALMA and to maximise the scientific return<br />
for the European community. Fostering<br />
community development and guid-<br />
ing the future evolution of ALMA’s use<br />
are among the primary tasks for the<br />
nodes. The nodes will provide face-toface<br />
help and additional support, beyond<br />
what are called the ARC core functions.<br />
This help includes, for example,<br />
advanced user support for special projects,<br />
and refinement in the data reduction<br />
process. To achieve these goals,<br />
the nodes will conduct fellowship, user<br />
grant, student and postdoctoral programmes,<br />
as well as promote the organisation<br />
of workshops, schools, and any<br />
other support facilities for users.<br />
The ARC Manager coordinates this network<br />
of nodes. Activities have been<br />
started with a face-to-face meeting with<br />
representatives of the ARC nodes, held<br />
at <strong>ESO</strong> on 9 August. Most of these activities<br />
are described on the ARC web<br />
page (www.eso.org/projects/alma/ARC),<br />
whereas internal information is shared<br />
and exchanged via a ‘wiki’.<br />
<strong>ESO</strong> Annual Report 006<br />
Organisational structure<br />
of the European<br />
ALMA Regional Centre.<br />
43
44<br />
<strong>ESO</strong> Annual Report 006
The European Extremely Large Telescope<br />
Extremely Large Telescopes – telescopes<br />
with a diameter of 30 m or more – are<br />
seen worldwide as one of the highest priorities<br />
in ground-based astronomy. They<br />
will vastly advance astrophysical knowledge,<br />
allowing detailed studies of, inter<br />
alia, planets around other stars, the first<br />
objects in the Universe, supermassive<br />
black holes, and the nature and distribution<br />
of the dark matter and dark energy<br />
which dominate the Universe. The European<br />
Extremely Large Telescope project<br />
will maintain and reinforce Europe’s position<br />
at the forefront of astrophysical research<br />
and, as such, it is no surprise that<br />
it was included in the European Strate-<br />
gy Forum on Research Infrastructures<br />
(ESFRI) Roadmap in October 006. This<br />
European Roadmap, defined at the<br />
request of the European Union Council,<br />
identifies new Research Infrastructures<br />
of pan-European interest corresponding<br />
to the long-term needs of the European<br />
research communities which are likely to<br />
be realised in the next 10 to 0 years,<br />
covering all scientific areas and regardless<br />
of possible location.<br />
The European Extremely Large Telescope<br />
(E-ELT) project made large strides in<br />
006. In the first half of the year, five working<br />
groups composed of over 100 scientists<br />
and engineers from <strong>ESO</strong> and its<br />
community of users elaborated a new<br />
vision for the project. These ELT Science<br />
and Engineering (ESE) working groups<br />
focused on the scientific case, telescope<br />
design, site, adaptive optics and instrumentation.<br />
Chaired by members of the<br />
community, the working groups produced<br />
their reports, which were collected into<br />
a ‘tool box’ to guide the further design activities.<br />
The chairs of the working groups, augmented<br />
by members of the <strong>ESO</strong> Scientific<br />
Technical Committee (STC), formed a<br />
subcommittee of the STC naturally<br />
named ESE to monitor the project and<br />
advise both the STC and <strong>ESO</strong> on the<br />
work. In parallel to this community-wide<br />
consultation, the <strong>ESO</strong> Council established<br />
an ELT Standing Review Committee<br />
(ESRC) composed of external experts<br />
to advise on a broad variety of aspects to<br />
do with the project.<br />
With the tool box in place, <strong>ESO</strong> formed a<br />
telescope project office in the middle<br />
of the year and tasked it with absorbing<br />
the recommendations of the ESE working<br />
groups and developing a coherent<br />
proposal for a telescope – a baseline reference<br />
design – and associated instrumentation<br />
to be elaborated upon in the<br />
coming years. The <strong>ESO</strong> ELT programme<br />
is in fact split into three parallel activities<br />
on telescope, instrumentation and operations,<br />
each with its own office within the<br />
respective divisions at <strong>ESO</strong>: Telescope<br />
Systems, Instrumentation, and Data Management<br />
and Operations.<br />
Innovative Design<br />
The baseline reference design of the telescope<br />
is to have adaptive optics as<br />
an integral part of the system, to provide<br />
instrumentation with gravity-invariant<br />
foci, to have an instrumentation-friendly<br />
focal plane and to avoid the areas considered<br />
high-risk by the OWL review undertaken<br />
in late 005. The telescope<br />
design working group activities focused<br />
on establishing the viability and relative<br />
merits of the two front-runners in the designs<br />
that could address these basic<br />
requirements. The first design was a classical<br />
Gregorian telescope and the second<br />
a novel five-mirror design. The activities<br />
at <strong>ESO</strong> focused on establishing the<br />
viability of a mechanical structure to support<br />
a mirror diameter of 4 metres and<br />
the rest of the optics required to relay the<br />
beam back to a focal station. Sophisticated<br />
finite-element modelling and analysis,<br />
as well as preliminary control engineering<br />
work, were used to develop a<br />
mechanical structure that could host<br />
either of the two designs with comparable<br />
performance. The size of 4 metres<br />
was considered by the ESE as a good<br />
compromise between ambition and technical<br />
feasibility.<br />
In parallel, <strong>ESO</strong> contracted European industrial<br />
firms to develop conceptual designs<br />
for the adaptive optics systems that<br />
are going to be built into the telescope.<br />
External consultants worked on developing<br />
concepts for the dome to house the<br />
telescope and within <strong>ESO</strong> a great deal of<br />
attention has been placed on the interfaces<br />
of the telescope and its infrastructure<br />
with instrumentation. Industrial firms<br />
were contacted to establish a first topdown<br />
cost estimate for the telescope.<br />
The two optical designs considered during the Basic Reference Design development: five-mirror (left) and<br />
Gregorian (right).<br />
<strong>ESO</strong> Annual Report 006<br />
45
The activities within the EU FP6-supported<br />
ELT Design Studies programme,<br />
led by <strong>ESO</strong> but largely executed in<br />
industry and academia outside the<br />
organisation, are aligned with the<br />
activities of the E-ELT programme and in<br />
all areas much progress is being made.<br />
Actuator prototypes, edge sensors, phasing<br />
techniques, wind evaluation systems,<br />
dome designs, site testing and many<br />
other such activities are all contributing to<br />
the knowledge we require to advance the<br />
project into the next phase. Integral to<br />
this planning is the membership of Spain<br />
in <strong>ESO</strong> and the expertise that the Spanish<br />
community will bring. Spain has just<br />
completed the segmented 10.4-m Gran<br />
Telescopio Canarias (GTC) telescope<br />
and, with Spain’s membership, <strong>ESO</strong><br />
engineers will gain technical access to<br />
that system.<br />
Participants to the E-ELT conference in Marseille.<br />
46<br />
<strong>ESO</strong> Annual Report 006<br />
The baseline reference design selected<br />
and approved by the <strong>ESO</strong> Council to<br />
move into the Phase B of the project is<br />
the five-mirror design. While the Gregorian<br />
design had advantages in a better<br />
theoretical performance in adaptive optics,<br />
a smaller mirror count and smaller<br />
central obstruction, the five-mirror design<br />
was considered to have advantages in<br />
the image quality across the focal plane,<br />
the control of the wavefront using laser<br />
guide stars, the flexibility of the focal stations,<br />
the deployment of atmospheric<br />
dispersion compensators, the smaller<br />
dome and the relative ease with which it<br />
could be upgraded to follow the development<br />
of technology in the future. Most<br />
critically however, the five-mirror design<br />
was considered to have much lower risk<br />
in the area of adaptive optics by virtue<br />
of the separation of the field-stabilisation<br />
and adaptive-optics functions, a key recommendation<br />
of the OWL review.<br />
Into Phase B<br />
The results of this burst of activity came<br />
together during November 006 in preparation<br />
for a series of presentations of<br />
the Project Office conclusions to ESE,<br />
ESRC, STC, to 50 astronomers at the<br />
Marseilles meeting on the E-ELT and, finally,<br />
to the <strong>ESO</strong> Council. The endorsement<br />
of the Project Office proposal by<br />
this broad spectrum of the community<br />
and decision makers reflects not only the<br />
good progress <strong>ESO</strong> made during 006<br />
in the elaboration of the design but also<br />
the clear scientific need to advance<br />
rapidly and effectively in the area of E-<br />
ELTs and the commitment of the user<br />
community.
The baseline reference design selected and<br />
approved by the <strong>ESO</strong> Council to move into<br />
the Phase B of the project is the five-mirror<br />
design. While the Gregorian design had<br />
advantages in a better theoretical performance<br />
in adaptive optics, a smaller mirror<br />
count and smaller central obstruction, the<br />
five-mirror design was considered to have<br />
advantages in the image quality across the<br />
focal plane, the control of the wavefront<br />
using laser guide stars, the flexibility of the<br />
focal stations, the deployment of atmospheric<br />
dispersion compensators, the<br />
smaller dome and the relative ease with<br />
which it could be upgraded to follow the<br />
development of technology in the future.<br />
Most critically however, the five-mirror<br />
design was considered to have much lower<br />
risk in the area of adaptive optics by virtue<br />
of the separation of the field-stabilisation<br />
and adaptive optics functions, a key recommendation<br />
of the OWL review.<br />
The E-ELT is now in Phase B, a period<br />
during which the design will be elaborated<br />
further. Together with academic and<br />
industrial partners, and with continuous<br />
consultation with its user community,<br />
<strong>ESO</strong> expects that a proposal for the<br />
construction of this ambitious project can<br />
be ready by the end of this decade.<br />
A Revolutionary Concept<br />
The present concept features as a<br />
base-line a 4 -m diameter mirror<br />
telescope, and is revolutionary. The<br />
primary mirror is composed of 906<br />
segments, each 1.45 m wide, while the<br />
secondary mirror is as large as 6 m in<br />
diameter. In order to overcome the<br />
fuzziness of stellar images due to<br />
atmospheric turbulence the telescope<br />
needs to incorporate adaptive mirrors<br />
into its optics, and a tertiary mirror, 4.<br />
m in diameter, relays the light to the<br />
adaptive optics system, composed of<br />
two mirrors: a .5-m mirror supported<br />
by 5 000 or more actuators so as to be<br />
able to distort its own shape a<br />
thousand times per second, and one<br />
.7 m in diameter that allows for the<br />
final image corrections. This five-mirror<br />
approach results in an exceptional<br />
image quality, with no significant<br />
aberrations in the field of view.<br />
<strong>ESO</strong> Annual Report 006<br />
47
48<br />
<strong>ESO</strong> Annual Report 006
Organisation and Personnel<br />
The main organisational and managerial<br />
units of <strong>ESO</strong> are the Divisions which<br />
currently include: the Office of the<br />
Director-General, the Administration, the<br />
Space Telescope/European Coordinating<br />
Facility, the La Silla Paranal Observatory,<br />
and the Instrumentation, Telescope<br />
Systems, Technology, Data Management<br />
and Operations, Software Development,<br />
and ALMA Divisions. Most divisions are<br />
organised in Departments, some of which<br />
consist of two or more Groups.<br />
<strong>ESO</strong> Annual Report 006<br />
49
List of Personnel<br />
Office of the Director<br />
General 1<br />
Catherine Cesarsky<br />
Fatme Allouche<br />
Catarina Alves de<br />
Oliveira<br />
Gonzalo Argandoña<br />
Lazo<br />
Mustafa Basbilir<br />
Mary Bauerle Blandford<br />
Luigi Bedin<br />
Yuri Beletsky<br />
Angelika Beller<br />
Adrianus Bik<br />
Michael Böcker<br />
Henri Boffin<br />
Konstantina Boutsia<br />
Jutta Boxheimer<br />
Pamela Bristow<br />
Benoît Carry<br />
Mary Cesetti<br />
Gaël Chauvin<br />
Lise Bech Christensen<br />
Blair Campbell Conn<br />
Silvia Cristiani<br />
Itziar De Gregorio<br />
Monsalvo<br />
Gayandhi Manomala<br />
De Silva<br />
Eric Depagne<br />
Jörg Dietrich<br />
Michelle Doherty<br />
Michaela Döllinger<br />
Brigitta Eder<br />
Christopher Erdmann<br />
Davide Fedele<br />
Cedric Foellmi<br />
Audrey Galametz<br />
Emmanuel Galliano<br />
Kerstin Geissler<br />
Mark Gieles<br />
Carla Gil<br />
Rachel Emily Gilmour<br />
Raphael Gobat<br />
María Eugenia<br />
Gómez Carrasco<br />
Luis Goncalves Calçada<br />
Claudio Grillo<br />
Uta Grothkopf<br />
Karin Hansen<br />
Markus Hartung<br />
Hans Hermann Heyer<br />
Renate Hoppe-Lentner<br />
Hannes Horst<br />
Gaël James<br />
Edmund Janssen<br />
Paulina Jiron Planella<br />
Andres Jordan<br />
Eric Jullo<br />
Georg Junker<br />
Jouni Kainulainen<br />
Katarina Kiupel<br />
Karina Kjær<br />
Rubina Kotak<br />
Isolde Kreutle<br />
Daniel Kubas<br />
Jean Baptiste<br />
Le Bouquin<br />
Bruno Leibundgut<br />
Silvia Leurini<br />
Cristian Lopez<br />
Paul Lynam<br />
1 Including all the<br />
Fellows and Students<br />
under the Studentship<br />
programme.<br />
50<br />
<strong>ESO</strong> Annual Report 006<br />
Mariya Lyubenova<br />
Claus Madsen<br />
Vincenzo Mainieri<br />
Gautier Mathys<br />
Jorge Melnick<br />
Maria Messineo<br />
Steffen Mieske<br />
Igor-Felix Mirabel<br />
Lorenzo Monaco<br />
Marcelo Mora<br />
Dominique Naef<br />
Thomas Naets<br />
Kim Nilsson<br />
Pasquier Noterdaeme<br />
Christina Papadaki<br />
Laura Catherine Parker<br />
Enikö Patkos<br />
Silvia Pedicelli<br />
Douglas Pierce-Price<br />
Olga Pinto Moreira<br />
Farid Rahoui<br />
Suzanna Randall<br />
Jaroslaw P. Rzepecki<br />
Francesco Saitta<br />
Hugues Sana<br />
Julia Scharwächter<br />
Andreas Seifahrt<br />
Zhixia Shen<br />
Rodolfo Silva Smiljanic<br />
Colin Snodgrass<br />
Veronica Sommariva<br />
Thomas Stanke<br />
Christina Stoffer<br />
Gabriel Szasz<br />
Svea Teupke<br />
Sune Toft<br />
Ezequiel Treister<br />
Stefan Uttenthaler<br />
Stefano Valenti<br />
Elena Valenti<br />
Gerrit van der Plas<br />
Martin Vannier<br />
Stefan Vehoff<br />
Daniela Villegas Mansilla<br />
Elisabeth Völk<br />
Rein Warmels<br />
Michael Weigand<br />
Thomas Wilson<br />
Gabriele Zech<br />
Administration Division<br />
Hans Jahreiss<br />
Hugo Freddy Aguilera<br />
Eduardo Arenas<br />
Paredes<br />
Andres Arias<br />
Angela Arndt<br />
Roland Block<br />
Jean-Michel Bonneau<br />
Renate Brunner<br />
Cecilia Carrasco Cruz<br />
Laura Comendador<br />
Frutos<br />
Walter Demartis<br />
Tommaso Di Dio<br />
Günther Dremel<br />
Willem Arie Dirk Eng<br />
Robert Fischer<br />
Nicolás Fischman Rajii<br />
Sonia Gárnica Plaza<br />
Rebonto Guha<br />
Priya Nirmala Hein<br />
Charlotte Hermant<br />
Hans Jahreiss<br />
Nathalie Kastelyn<br />
Elizabeth Kerk<br />
Hans-Jürgen Kraus<br />
Katjuscha Lockhart<br />
Ignacio Lopez Gil<br />
Maria Madrazo<br />
Silvia Madrid Pariente<br />
Jorge Moreno González<br />
María Angélica Moya<br />
Helene Neuville<br />
Christine Nieuwenkamp<br />
Mauricio Quintana<br />
Ipinza<br />
Rolando Quintana<br />
Ipinza<br />
André Louis Ritz Solari<br />
Rosa Ivonne Riveros<br />
Cárdenas<br />
Francky Rombout<br />
Nadja Sababa<br />
María Soledad Silva<br />
Castán<br />
Erich Siml<br />
Beatrice Sivertsen<br />
Roswitha Slater<br />
Albert Triat Saurat<br />
Ullrich Urban<br />
Lone Vedsø Marschollek<br />
Sabine Weiser<br />
Yves Wesse<br />
Gerd Wieland<br />
La Silla Paranal<br />
Observatory<br />
Andreas Kaufer<br />
Nancy Ageorges<br />
Luis Águila Vargas<br />
Claudio Agurto<br />
Bernardo Ahumada<br />
Héctor Alarcón Ramírez<br />
Mario Alfaro Varela<br />
Jaime Alonso Torrini<br />
Nilso Alquinta Espejo<br />
Jose Luis Alvarez<br />
Paola Amico<br />
Michel Anciaux<br />
Andreas Andersson<br />
Lundgren<br />
Gaetano Andreoni<br />
Ernesto Araya Troncoso<br />
Juan Carlos Arcos<br />
Álvarez<br />
Javier Argomedo<br />
Karla Aubel<br />
Francisco Azagra<br />
Jose Baez<br />
Stefano Bagnulo<br />
Pedro Baksai<br />
Emilio Barrios Rojas<br />
Rogelio Bascunan<br />
Bertrand Bauvir<br />
Eduardo Bendek<br />
Per Mikael Bergman<br />
Guillame Blanchard<br />
Carlos Bolados<br />
Henri Bonnet<br />
Stephane Brillant<br />
Armando Bruna Bruna<br />
Erich Bugueño<br />
Blanca Camucet Ortiz<br />
Massimiliano Camuri<br />
Luis Alejandro<br />
Caniguante<br />
Michael Cantzler<br />
Ruben Carcamo<br />
Cesar Cardenas<br />
Johan Carstens<br />
Fabio Caruso<br />
Duncan Castex<br />
Roberto Castillo Ladrón<br />
De Guevara<br />
Mónica Castillo Cortés<br />
Jorge Castizaga<br />
Cáceres<br />
Susana Cerda<br />
Hernández<br />
Cecilia Cerón Canelo<br />
Claudia Cid Fuentes<br />
Florentino Contreras<br />
Alex Correa Gutiérrez<br />
José Ignacio Cortés<br />
Mandiola<br />
Ángela Cortés Carvallo<br />
Jaime Costa Abarca<br />
Claudio De Figueiredo<br />
Melo<br />
Reinaldo Donoso Marín<br />
Javier Duk Díaz<br />
Christophe Dumas<br />
Michael Dumke<br />
Domingo Durán Cortés<br />
Carlos Durán Urrutia<br />
Yves Durand<br />
Carlos Ebensperger Eliz<br />
Cristian Esparza<br />
Morales<br />
Loreno Esparza Morales<br />
Erito Flores Arias<br />
Juan Carlos Fluxá<br />
Nadeau<br />
Patrick Francois<br />
Sergio Gaete Román<br />
Enrique Garcia<br />
José Gardiazabal<br />
Schilling<br />
Gordon Gillet<br />
Alain Gilliotte<br />
Percy Glaves Peters<br />
Leonardo González<br />
Hernández<br />
Domingo González<br />
Leyton<br />
Andrés González López<br />
Sergio Gonzalez Burgus<br />
Víctor González Toro<br />
Charlotte Groothuis<br />
Patricia Guajardo<br />
Obando<br />
Carlos Guerra Escobar<br />
Stephane Guisard<br />
Serge Guniat<br />
Flavio Gutiérrez Willer<br />
Fernando Gutierrez<br />
Nicolas Haddad<br />
Salcedo<br />
Juan Pablo Haddad<br />
Ferretto<br />
Pierre Haguenauer<br />
Olivier Hainaut<br />
George Harding<br />
Juan Pablo Henriquez<br />
León<br />
Cristian Herrera<br />
González<br />
Leonardo Herrera<br />
González<br />
Herrera Mena, Leonardo<br />
Swetlana Hubrig<br />
Gerhard Hüdepohl<br />
Rodrigo Huerta<br />
Ramón Huidobro<br />
Nordenflycht<br />
Christian Hummel<br />
Gerardo Ihle<br />
Valentin Ivanov<br />
Emmanuel Jehin<br />
Jorge Jiménez Rojas<br />
Nestor Jiménez Odgers<br />
Ismo Kastinen<br />
Andreas Kaufer<br />
Nicholas Charles<br />
Kornweibel<br />
Carlos La Fuente Peña<br />
Francisco Labraña<br />
Zamorano<br />
Octavio Lavín Catril<br />
Paul Le Saux<br />
Cedric Ledoux<br />
Alfredo Leiva Becerra<br />
Ramón Leyton Muñoz<br />
Christopher Lidman<br />
Gaspare Lo Curto<br />
Ignacio López Vilches<br />
Ariel Lopez Ortega<br />
Fernando Luco<br />
Meneses<br />
Javier Luhrs Middleton<br />
Felipe Mac-Auliffe Prieto<br />
Agustín Macchino Farías<br />
Massimiliano Marchesi<br />
Gianni Marconi<br />
Pedro Mardones Ojeda<br />
Pedro Marín Fuentes<br />
Kiriako Markar Aros<br />
Mauricio Martinez<br />
Parada<br />
Elena Mason<br />
Eduardo Matamoros<br />
Pastén<br />
Rolando Medina Zanetta<br />
Juan Alberto Mella<br />
Angel Mellado González<br />
Alejandra Mena Briceño<br />
Jorge Miranda Mery<br />
Juan Molina Watanabe<br />
Nelson Montano Ortiz<br />
Alex Morales Agurto<br />
Sebastien Morel<br />
Merilio Morell Rodríguez<br />
Manfred Mornhinweg<br />
Krohmer<br />
Ivan Muñoz Máximo<br />
Julio Navarrete Lavín<br />
Jean-Luc Nicoud<br />
Hernan Nievas<br />
Fernández<br />
Dieter Nürnberger<br />
Herman Nuñez Portilla<br />
Lars A. Nyman<br />
Kieran O’Brien<br />
Rodrigo Olivares Álvarez<br />
Francisco Olivares<br />
González<br />
Ernesto Orrego<br />
Cisternas<br />
Óscar Orrego Sandoval<br />
Juan Osorio Escrich<br />
Juan Carlos Palacio<br />
Valenzuela<br />
Ricardo Parra Paz<br />
José Parra Ortiz<br />
Andrés Parraguez<br />
Cárcamo<br />
Marcus Pavez Hubner<br />
Eduardo Peña<br />
Juan Pineda Hernández<br />
Andres Pino<br />
Manuel Pizarro López<br />
De Maturana<br />
Aldo Pizarro Hess<br />
Andrés Pizarro Pavez<br />
Emanuela Pompei<br />
Hugo Quijón Duarte<br />
Andrés Ramírez Molina<br />
Fredrik Rantakyrö<br />
Johnny Reveco Arias<br />
Vincent Reveret<br />
Miguel Riquelme Oyarce<br />
Christophe Risacher<br />
Thomas Rivinius<br />
Luis Roa Figueroa<br />
Pascal Robert<br />
William Robinson<br />
Chester Rojas<br />
Gorky Román Delgado<br />
José Rosas Ávalos<br />
Felix Alberto Rozas<br />
Francisco G. Ruseler<br />
Claudio Sagüez García<br />
Daniel Salazar Barrera<br />
Fernando Salgado<br />
Ibarra<br />
Alejandro Salinas<br />
Fenero<br />
Ariel Sánchez Peñailillo<br />
Stefan Sandrock<br />
Roberto Sanhueza<br />
Slater
Pierre Sansgasset<br />
Jorge Santana<br />
Marambio<br />
Ivo Saviane<br />
Linda Schmidtobreic<br />
Ricardo Schmutzer Von<br />
Oldershausen<br />
Markus Schöller<br />
Oliver Schuetz<br />
Fernando Selman<br />
Jorge Sepúlveda Ortega<br />
Tzu Chiang Shen<br />
Waldo Siclari Bordones<br />
Peter Sinclaire Aguirre<br />
Alain Smette<br />
Fabio Somboli<br />
Rubén Soto Troncoso<br />
Mauro Stefanon<br />
Stanislav Stefl<br />
Michael Fritz Sterzik<br />
Sandra Strunk<br />
Thomas Szeifert<br />
Roberto Tamai<br />
Mario Tapia Gonzáles<br />
Manuel Torres<br />
Zamorano<br />
Soraya Torres López<br />
Guillermo Valdés<br />
José Javier Valenzuela<br />
Soto<br />
Karen Vallejo Cerda<br />
Leonardo Vanzi<br />
Oscar Varas Mella<br />
Enrique Vera Diaz<br />
Jorge Vilaza Méndez<br />
Stefan Wehner<br />
Ueli Weilenmann<br />
Luis Wendegass<br />
Mellado<br />
Andrew Wright<br />
Juan Christóbal Zagal<br />
ALMA Division<br />
Hans Rykaczewski<br />
Gareth Aspinall<br />
Fabio Biancat Marchet<br />
Claus Dierksmeier<br />
Jörg Eschwey<br />
Preben Grosbøl<br />
Christoph Haupt<br />
Jorge Ibsen<br />
Andreas Kempf<br />
Hervé Kurlandczyk<br />
Robert Alexander Laing<br />
Pascal Lapeyre<br />
Pascal Martinez<br />
Angel Otárola Medel<br />
Eric Pangole<br />
Ferdinand Patt<br />
Gianni Raffi<br />
Silvio Rossi<br />
Hans Rudolf<br />
Joseph Schwarz<br />
Stefano Stanghellini<br />
Donald Tait<br />
Gie Han Tan<br />
Nathalie Thebaud<br />
Eugenio Ureta Bravo<br />
Elena Zuffanelli<br />
Jennifer Hewitson<br />
Manuel de Menezes<br />
Telescope System<br />
Division<br />
Roberto Gilmozzi<br />
Constanza Araujo<br />
Hauck<br />
Robin Arsenault<br />
Domenico Bonaccini<br />
Calia<br />
Jeroen de Jong<br />
Françoise Delplancke<br />
Frédéric Derie<br />
Philippe Dierickx<br />
Robert Donaldson<br />
Enrico Fedrigo<br />
Yan Feng<br />
Andreas Glindemann<br />
Wolfgang Hackenberg<br />
Ronald Holzlöhner<br />
Norbert Hubin<br />
Markus Kasper<br />
Bertrand Koehler<br />
Johann Kolb<br />
Visa Korkiakoski<br />
Miska Kristian Le Louarn<br />
Samuel Leveque<br />
Jochen Liske<br />
Enrico Marchetti<br />
Patrice Martinez<br />
Serge Menardi<br />
Samantha Milligan<br />
Guy Monnet<br />
Riccardo Muradore<br />
Sylvain Oberti<br />
Jérôme Paufique<br />
Duc Thanh Phan<br />
Florence Puech<br />
Mark Robinson<br />
Tatyana Sadibekova<br />
Marc Sarazin<br />
Kevin Scales<br />
Nicolas Schuhler<br />
Christian Soenke<br />
Jason Spyromilio<br />
Josef Strasser<br />
Stefan Ströbele<br />
Isabelle Surdej<br />
Arkadiusz Swat<br />
Luke Taylor<br />
Gautam Vasisht<br />
Christophe Verinaud<br />
Elise Vernet<br />
Anders Wallander<br />
Nataliya Yaitskova<br />
Davide Zil<br />
Data Management and<br />
Operations Division<br />
Fernando Comerón<br />
Paola Andreani<br />
Fabien Chereau<br />
Fernando Comeron<br />
Carlos De Breuck<br />
Nausicaa Delmotte<br />
Danuta Dobrzycka<br />
Adam Dobrzycki<br />
Markus Dolensky<br />
Nina Felber<br />
Nathalie Fourniol<br />
Monika Gotzens<br />
Reinhard Hanuschik<br />
Paul Harrison<br />
Evanthia Hatziminaoglou<br />
Michael Hilker<br />
Wolfgang Hummel<br />
John Lockhart<br />
Jean-Christophe<br />
Malapert<br />
Stephane Marteau<br />
Sabine Mengel<br />
Sabine Moehler<br />
Palle Møller<br />
Petra Nass<br />
Mark Neeser<br />
Paolo Padovani<br />
Ferdinando Patat<br />
Isabelle Percheron<br />
Francesca Primas<br />
John Pritchard<br />
Marina Rejkuba<br />
Jörg Retzlaff<br />
Bruno Rino<br />
Charles Rite<br />
Jesus Rodriguez Ulloa<br />
Martino Romaniello<br />
Piero Rosati<br />
Remco Slijkhuis<br />
Dieter Suchar<br />
Lowell Tacconi-Garman<br />
Mario Van Den Ancker<br />
Benoît Vandame<br />
Andreas Wicenec<br />
Markus Wittkowski<br />
Burkhard Wolff<br />
Martin A. Zwaan<br />
Space Telescope –<br />
European Coodination<br />
Facility<br />
Lars Lindberg<br />
Christensen<br />
Wolfram Freudling<br />
Francesca Granato<br />
Jonas Haase<br />
Richard Hook<br />
Martin Kornmesser<br />
Martin Kümmel<br />
Harald Kuntschner<br />
Marco Lombardi<br />
Paola Popesso<br />
Britt Sjöberg<br />
Aitana Vargas<br />
Jeremy Walsh<br />
Software Development<br />
Division<br />
Michele Peron<br />
Roberto Abuter<br />
Eric Allaert<br />
Luigi Andolfato<br />
Pascal Ballester<br />
Klaus Banse<br />
Peter Biereichel<br />
Alessandro Caproni<br />
Sandra Maria Castro<br />
Maurizio Chavan<br />
Gianluca Chiozzi<br />
Mauro Comin<br />
Livio Condorelli<br />
Stéphane Di Cesare<br />
Gabriele Donino<br />
Dario Dorigo<br />
Philippe Duhoux<br />
Sylvie Feyrin<br />
Robert Frahm<br />
Bruno Gilli<br />
Carlos Guirao Sanchez<br />
Birger Gustafsson<br />
Karim Haggouchi<br />
Carlo Izzo<br />
Bogdan Jeram<br />
Yves Jung<br />
Robert Karban<br />
Mario Kiekebusch<br />
Maurice Klein Gebbinck<br />
Jens Knudstrup<br />
Antonio Longinotti<br />
Henning Lorch<br />
Lars Kristian Lundin<br />
Holger Meuss<br />
Andrea Modigliani<br />
Christophe Moins<br />
Ralf Palsa<br />
Moreno Pasquato<br />
Martine Peltzer<br />
Werther Pirani<br />
Dan Popovic<br />
Eszter Pozna<br />
Marcus Schilling<br />
Diego Sforna<br />
Paola Sivera<br />
Fabio Sogni<br />
Heiko Andreas Sommer<br />
Stefano Turolla<br />
Jakob Vinther<br />
Krister Wirenstrand<br />
Michele Zamparelli<br />
Stefano Zampieri<br />
Instrumentation<br />
Division<br />
Alan Moorwood<br />
Matteo Accardo<br />
Gerardo Avila<br />
Dietrich Baade<br />
Andrea Balestra<br />
Paul Bristow<br />
Iris Bronnert<br />
Mark Casali<br />
Claudio Cumani<br />
Sebastian Deiries<br />
Klaas Johannes Dekker<br />
Sandro D’Odorico<br />
Reinhold Dorn<br />
Mark Desmond<br />
Downing<br />
Christophe Dupuy<br />
Siegfried Eschbaumer<br />
Gert Finger<br />
Christoph Geimer<br />
Stefan Hötzl<br />
Olaf Iwert<br />
Hans-Ulrich Käufl<br />
Florian Kerber<br />
Jean Paul Kirchbauer<br />
Jean-Louis Lizon à<br />
L’Allemand<br />
Antonio Ramon<br />
Manescau Hernandez<br />
Leander H. Mehrgan<br />
Manfred Meyer<br />
Luca Pasquini<br />
Markus Patig<br />
Jean-François Pirard<br />
Roland Reiss<br />
Javier Reyes<br />
Andrea Richichi<br />
Gero Rupprecht<br />
Ralf Siebenmorgen<br />
Armin Silber<br />
Jörg Stegmeier<br />
Sebastien Tordo<br />
Joel Daniel Roger Vernet<br />
Technology Division<br />
Martin Cullum<br />
<strong>ESO</strong> Annual Report 006<br />
Roland Brast<br />
Enzo Brunetto<br />
Bernard Buzzoni<br />
Ralf Dieter Conzelmann<br />
Bernard-Alexis Delabre<br />
Nicola Di Lieto<br />
Canio Dichirico<br />
Martin Dimmler<br />
Michel Duchateau<br />
Toomas Erm<br />
Raul Esteves<br />
Giorgio Filippi<br />
Gerhard Fischer<br />
Christoph Frank<br />
Philippe Gitton<br />
Domingo Gojak<br />
Frederic Yves Joseph<br />
Gonté<br />
Ivan Maria Guidolin<br />
Volker Heinz<br />
Florian Heissenhuber<br />
Guy Hess<br />
Georgette Hubert<br />
Gotthard Huster<br />
Georg Igl<br />
Andreas Jost<br />
Franz Koch<br />
Heinz E. Kotzlowski<br />
Maximilian Kraus<br />
Simon Lowery<br />
Christian Lucuix<br />
Ruben Mazzoleni<br />
Jean-Michel Moresmau<br />
Michael Müller<br />
Michael Naumann<br />
Lothar Noethe<br />
Edouard Pomaroli<br />
Marco Quattri<br />
Jutta Quentin<br />
Michael Schneermann<br />
Babak Sedghi<br />
Barbara Sokar<br />
Jesper Thillerup<br />
Arno Van Kesteren<br />
Véronique Ziegler<br />
Seconded Staff<br />
Members<br />
Joint ALMA Office<br />
Massimo Tarenghi<br />
Alejandra Araya<br />
Ann Edmunds<br />
Jacques Lassalle<br />
Russell Smeback<br />
51
Personnel Services<br />
The ‘Five-Yearly Review’ of the conditions<br />
of employment for International Staff<br />
Members was completed, in close interaction<br />
with CERN. The results of the<br />
study led to further reviews and amendments,<br />
in particular regarding: the definition<br />
of family, now recognising same-sex<br />
marriages and same-sex or opposite-<br />
sex partnerships; maternity leave, parental<br />
leave and further options to facilitate<br />
and increase the harmonisation of family<br />
and professional career; education grants<br />
and expatriation allowances.<br />
The Personnel Department in Garching<br />
and Vitacura prepared and concluded the<br />
collective bargaining with the representatives<br />
of the Unions of La Silla and Paranal<br />
as well as with the representatives of the<br />
Administration in Santiago. The new Collective<br />
Contracts are effective as of 1 December<br />
006 for a period of three years.<br />
The process of the creation and implementation<br />
of the Software Development<br />
Division and reorganisation of the Data<br />
Management and Operations Division<br />
was accomplished. Personnel also participated<br />
in the review and restructur-<br />
ing of the Administration Division, all the<br />
related decisions being implemented by<br />
1 July 006.<br />
5<br />
Others<br />
9.4 %<br />
Sweden<br />
.3 %<br />
Portugal<br />
0.3 %<br />
The Netherlands<br />
3.7 %<br />
Italy<br />
18.9 %<br />
United Kingdom<br />
5.7 %<br />
<strong>ESO</strong> Annual Report 006<br />
Personnel Services was greatly involved<br />
in matters regarding the ALMA project.<br />
We participated in the recruitment of key<br />
positions of the Joint ALMA Observatory,<br />
in the foundation of the ALMA Human<br />
Resource Advisory Group, and in the<br />
completion of the Internal Regulations as<br />
well as the Compensation and Benefits<br />
for ALMA Local Staff.<br />
The ‘leave module’ was implemented for<br />
Garching on 1 July 006 in the ERP system.<br />
To make this process smooth, training<br />
was provided for all the Staff.<br />
To make new staff members in Garching<br />
more used to all the aspects of the organisation,<br />
from an overview of its different<br />
activities to very practical questions,<br />
an induction day was established with<br />
support from all Divisions at <strong>ESO</strong>. Conditions<br />
in Garching have also been improved<br />
for young parents with the opening<br />
of the IPP/<strong>ESO</strong> Crèche on 1 April<br />
006.<br />
Other activities included participating in<br />
the recruitment of key management<br />
positions in Garching and Chile, making<br />
regular visits to the sites in Chile in or-<br />
der to keep close contact with the International<br />
and Local Staff Members and<br />
their representatives, organising common<br />
training in ‘managing people’ for about<br />
Belgium<br />
4.9 %<br />
Switzerland<br />
1.4 %<br />
Germany<br />
3 .6 %<br />
Denmark<br />
3.1%<br />
France<br />
17.7%<br />
5 team leaders of the La Silla Paranal<br />
Observatory during the month of November<br />
006, and providing short-term and<br />
long-term office accommodation in<br />
Garching.<br />
The employment conditions and further<br />
guidelines for International Staff Members<br />
and Local Staff in Chile were revised, particularly<br />
with respect to:<br />
– The calculation and adjustment of<br />
the Cost of Living for International Staff<br />
Members in Chile;<br />
– Contract Policy for International Staff<br />
Members;<br />
– Regular medical examinations for Staff<br />
in Chile and Garching;<br />
– Equal Opportunity Statement;<br />
– Recruitment Policy Statement and its<br />
guidelines;<br />
– The application of the Social Activity<br />
Day;<br />
– Limitation of claims;<br />
– Home leave regulation;<br />
– The application of official holidays<br />
during duty travels.<br />
In the course of the year, 9 Local Staff<br />
and 34 International Staff Members were<br />
recruited. In addition, 101 Students, Fellows,<br />
and Paid and Unpaid Associates<br />
joined <strong>ESO</strong>. The diagramme below shows<br />
the International Staff Members of <strong>ESO</strong>,<br />
by nationality, as of December 006.<br />
Distribution of International<br />
Staff Members<br />
by Nationality as of<br />
31 December 006.
Instrumentation<br />
Highlights of the year were the installation<br />
and commissioning on Antu (UT1) of the<br />
Cryogenic Infrared Spectrometer (CRI-<br />
RES), the last of the first-generation VLT<br />
instruments, and the successful commissioning<br />
of the laser guide-star facility<br />
on Yepun (UT4), which will substantial-<br />
ly increase the sky coverage achievable<br />
with the adaptive optics assisted instruments<br />
NACO and SINFONI. The Omega-<br />
CAM camera was completed in advance<br />
of the VLT Survey Telescope for which it<br />
has been built; integration of the HAWK-I<br />
infrared camera for the VLT started in<br />
Garching; work on PRIMA continued;<br />
the approved second-generation VLT<br />
instruments X-Shooter, KMOS, MUSE<br />
and SPHERE, plus the Adaptive Optics<br />
Facil-ity (AOF) and the new NGC detector<br />
con-troller all progressed well, and Phase<br />
A studies were launched of three<br />
potential second-generation VLT interferometric<br />
instruments to eventually<br />
replace MIDI and AMBER. In addition,<br />
work ramped up on defining the ELT<br />
instrument interfaces and the design of<br />
possble instruments both within the <strong>ESO</strong><br />
E-ELT Instrument Project Office and the<br />
FP6 ELT Design Study.<br />
The leadership and know-how in astronomical<br />
instrumentation of <strong>ESO</strong> and<br />
its partners was very visible at the 006<br />
SPIE Astronomical Telescopes and<br />
Instrumentation Symposium that took<br />
place in Orlando, Florida, bringing together<br />
1700 astronomy, technology, and<br />
engineering experts from all over the<br />
world. <strong>ESO</strong> staff played a key role in the<br />
numerous meetings, either as organisers<br />
or speakers, and many <strong>ESO</strong> projects<br />
were discussed.<br />
CRIRES, the infrared (1–5 μm), high resolution<br />
(R = 10 5 ), adaptive optics assisted<br />
spectrograph built for the VLT by <strong>ESO</strong><br />
was integrated, extensively tested and<br />
formally passed its Preliminary Acceptance<br />
Europe (PAE) review in Garching on<br />
13 April. In order to optimise the installation<br />
and commissioning process the<br />
adaptive optics part was reviewed first,<br />
and released for shipment to Chile by the<br />
end of February. First light was achieved<br />
with an infrared test camera on 6 April<br />
when the adaptive optics control loop<br />
was closed on the star b Muscae. Although<br />
packing of the cryogenic spectrograph<br />
only started on 5 April, first astro-<br />
nomical spectra were already obtained<br />
together with the adaptive optics feed on<br />
4 June. We believe that this constitutes<br />
a record time for such a complex installation.<br />
By year’s end, commissioning was<br />
almost complete and the first scientific<br />
results had already been obtained through<br />
a highly successful set of science verification<br />
observations conducted to test the<br />
end-to-end system including the proposal<br />
preparation, instrument operation, and<br />
data handling and analysis tools and procedures.<br />
Following final commissioning<br />
and calibration in early 007, CRIRES will<br />
officially enter full science operations at<br />
the start of Period 79 on 1 April.<br />
The Laser Guide Star Facility (LGSF) had<br />
first light on 8 January. During the first<br />
commissioning a degradation of the image<br />
quality of the projected artificial star<br />
was detected. This was found to be due<br />
to the deformation of the flange at the<br />
interface between the launch telescope<br />
and the secondary mirror of UT4. The<br />
flange was redesigned and replaced in<br />
April. This solved much of the image quality<br />
problem although a second problem<br />
appeared: at low temperatures the<br />
supports of the launch telescope’s primary<br />
mirror caused an aberration that<br />
also affected the image quality of the artificial<br />
star. The launch telescope was<br />
dismounted, tested and shipped back to<br />
Garching for repairs. A task force was<br />
created to manage the recovery actions.<br />
A new mirror support was designed<br />
and mounted in the launch telescope. A<br />
more advanced focusing mechanism<br />
was also developed and mounted. A comprehensive<br />
set of realistic tests was then<br />
performed in a controlled environment<br />
to check the quality of the refurbishment<br />
before sending the launch telescope<br />
back to Paranal in October. All recovery<br />
activities were done in collaboration<br />
with the telescope provider. The LGSF<br />
went back ‘on sky’ in October, and<br />
commissioning resumed together with<br />
the NACO and SINFONI instruments.<br />
Although not yet fully within specifications,<br />
the LGSF was starting to produce<br />
scientific results at the end of the year.<br />
The OmegaCAM wide-field optical camera<br />
for the VST was finished and passed<br />
its PAE. The camera itself has been<br />
built by a German/Dutch/Italian consortium<br />
and the detector system, compris-<br />
ing a mosaic of 3 CCDs, by <strong>ESO</strong>. The<br />
instrument is now being stored in Garching,<br />
awaiting the installation and commissioning<br />
on Paranal in 007 of the<br />
.6-m VST, being supplied by INAF in<br />
Italy.<br />
Manufacturing and procurement of essentially<br />
all the components of the<br />
HAWK-I infrared camera for the VLT proceeded<br />
well. In particular, all four of its<br />
k × k Hawaii RG infrared detectors<br />
were delivered and fully tested with excellent<br />
results. They were mounted together<br />
to form a mosaic similar to that planned<br />
for the James Webb Space Telescope.<br />
The radiation shield was installed in the<br />
vacuum vessel in Garching, resulting in a<br />
rather large camera system. The reflecting<br />
optics were also mounted and found<br />
to exhibit excellent optical quality at room<br />
temperature. The first cool-down and<br />
test of the complete system at cryogenic<br />
temperatures is expected in January<br />
007 and, if all goes well in the following<br />
few months, HAWK-I will be commissioned<br />
in the period June–September<br />
007 at one of the Nasmyth foci of Yepun<br />
(UT4). After around three years use for<br />
direct imaging it is planned to install four<br />
wavefront sensors to exploit the possibility<br />
of ground layer adaptive optics correction<br />
with the AOF.<br />
Installation of the radiation shield in the HAWK-I<br />
vacuum vessel in Garching.<br />
<strong>ESO</strong> Annual Report 006<br />
53
The Adaptive Optics Facility<br />
The AOF is a project to upgrade one of<br />
the VLT 8. -m telescopes, Yepun (UT4),<br />
with an adaptive secondary mirror, multiple<br />
Laser Guide Stars and two adaptive<br />
optics modules: GRAAL for HAWK-I and<br />
GALACSI for MUSE. The aim is to provide<br />
both instruments with ‘enhanced seeing’<br />
performance in a large field of view and<br />
to achieve diffraction-limited performance<br />
in a small field of view for MUSE. An optical<br />
test-bench, ASSIST, built by a Dutch<br />
partner, will be used to test the complete<br />
system in Europe before sending it to the<br />
observatory.<br />
Substantial progress was achieved in the<br />
design of the various subsystems during<br />
the year. The Deformable Secondary<br />
Mirror (DSM) preliminary design has advanced<br />
well and major design difficulties<br />
– such as procedures for safe handling of<br />
the thin mirror shell, design of a stiff hexapod<br />
structure with sophisticated flexible<br />
joints, manufacture of a light-weight<br />
reference body – have been solved. The<br />
end of the year has been used to write<br />
the documentation for the DSM Preliminary<br />
Design Review (PDR) planned for<br />
early 007. A complete design for GRAAL<br />
has been produced, including the large<br />
bearing which allows rotation of the<br />
wavefront sensors. Preliminary inquiries<br />
have taken place for specifications and<br />
cost-estimate of such a device, opening<br />
the way for the GRAAL PDR in early<br />
007. GALACSI and 4LGSF preliminary<br />
designs are in line for reviews planned<br />
in autumn 007. The synergy between<br />
GRAAL and GALACSI (e.g. their similar<br />
real-time computer and wavefront sensor)<br />
allows GALACSI to benefit from the<br />
GRAAL progress. Moreover, the results<br />
and lessons learned from the LGSF commissioning<br />
in Paranal are retrofitted to<br />
the actual 4LGSF design. The ASSIST<br />
test-bench has undergone Optical PDR in<br />
October 006 and a reliable optical design<br />
is on hand for the ‘DSM main tower’.<br />
The mirror blank for the Thin Shell prototype<br />
has been prepared by a contractor<br />
and is ready to undergo aspherical polishing.<br />
Concerning the Very Large Telescope<br />
Interferometer (VLTI), several parts of the<br />
PRIMA (Phase-Referenced Imaging and<br />
Micro-arcsecond Astrometry facility)<br />
54<br />
<strong>ESO</strong> Annual Report 006<br />
CRIRES installed at a Nasmyth focus of Antu. The large vacuum vessel houses the cryogenically<br />
cooled, high-resolution infrared spectrometer, and the enclosure between it and the<br />
telescope contains adaptive optics and calibration systems.<br />
hardware have been delivered and are<br />
undergoing intensive tests in the Garching<br />
laboratories. The PRIMA facility is a<br />
sys-tem designed to enable simultaneous<br />
interferometric observations of two objects<br />
– each with size of at most arcseconds<br />
– that are separated by up to<br />
1 arcminute. PRIMA can be used to increase<br />
the sensitivity of the VLTI, to image<br />
faint objects with a high angular resolution<br />
and to perform high-precision<br />
astrometry, mainly for planet detection.<br />
The principal components of PRIMA<br />
are: a Star Separator per telescope, a<br />
system of laser metrology, two Fringe-<br />
Sensor Units, and four Differential Delay<br />
Lines.<br />
One Star Separator for the Auxiliary Telescopes<br />
and one for the Unit Telescopes<br />
have been delivered within specifications.<br />
The second of each type will be delivered<br />
in early 007. Two additional Star Separators<br />
for the Unit Telescopes are under<br />
manufacturing and should be delivered in<br />
008. The Fringe Sensor Units (FSU) are<br />
under intensive tests at a laboratory in<br />
the Max-Planck-Institut für Extraterrestrische<br />
Physik. Some specifications are not<br />
yet met but several solutions are being<br />
worked out and implemented in collaboration<br />
with the contractor. The laser metrology,<br />
the system measuring the phase<br />
and delay that is at the basis of the<br />
PRIMA concept, is regularly used in the<br />
testing of the FSU. Its interface with<br />
the Star Separators has also been proven<br />
adequate. Continuous improvement of<br />
this essential device is ongoing as the<br />
lessons learned from the Interferomet-<br />
ric Task Force in Paranal are taken into<br />
account and used to improve the PRIMA<br />
reliability. The Differential Delay Lines are<br />
under manufacturing and currently no<br />
problem has been encountered. Finally,<br />
the PRIMA Astrometric Software, a detailed<br />
data analysis software and calibration<br />
package needed to reach the ambitious<br />
10 micro-arcsecond accuracy, is<br />
under development. A first version of the<br />
software will be available for the integration<br />
and commissioning of PRIMA during<br />
008.<br />
Second-generation Instruments<br />
Design work advanced well on the four<br />
approved second-generation VLT in-<br />
struments. X-Shooter, the wideband UV-<br />
IR spectrograph being developed by a<br />
Danish/Dutch/French/Italian consortium<br />
led by <strong>ESO</strong>, is the most advanced. It<br />
passed its Final Design Review (FDR) in<br />
June 006 and its optical CCDs and<br />
infrared array detector have already been<br />
successfully tested. KMOS, the multiple,<br />
deployable integral-field infrared spectrometer<br />
being developed by a UK/German<br />
consortium (with <strong>ESO</strong> providing the<br />
detector system) passed its PDR in Sep-
Assembling the Hawk-I 4K x 4K detector mosaic.<br />
<strong>ESO</strong> Annual Report 006<br />
55
tember following successful tests of a<br />
prototype cryogenic pick-off arm – one of<br />
4 to be installed in the final instrument –<br />
and of diamond machined optical components<br />
representative of those needed<br />
for its image slicer systems. The agreement<br />
between <strong>ESO</strong> and the French/<br />
Swiss/German MUSE consortium was<br />
signed and the instrument itself continued<br />
in its preliminary design phase.<br />
MUSE is an integral-field optical spectrograph<br />
– actually 4 spectrographs –<br />
with <strong>ESO</strong> again responsible for the design<br />
and procurement of the detector<br />
systems. An important milestone in 006<br />
was the optical PDR, which paved the<br />
way for the production of a prototype of<br />
one of the 4 spectrographs. MUSE is<br />
also designed to be used together with<br />
the AOF described above in order to<br />
enhance the delivered image quality and<br />
hence sensitivity and resolution.<br />
The aim of SPHERE is to directly detect<br />
extrasolar planets, possibly down to<br />
Jupiter masses, achieving a contrast of at<br />
least 1/100 000 at 0.1 arcsecond from a<br />
bright central star. This will be made possible<br />
by an ‘extreme’ adaptive optics system<br />
to correct atmospheric turbulence<br />
effects, by suppression of the diffraction<br />
pattern using state-of-the-art coronagraphs,<br />
and by advanced differential techniques<br />
aimed at reducing the speckle<br />
noise. The corrected beam will feed three<br />
scientific instruments which will work<br />
at optical and near-infrared wavelengths.<br />
The SPHERE consortium comprises partners<br />
from France, Germany, Switzerland,<br />
Italy, and the Netherlands. <strong>ESO</strong> is a full<br />
partner in the project, which also includes<br />
significant support by the OPTICON FP6<br />
network. During 006, the preliminary<br />
design of systems and subsystems has<br />
advanced well at the various institutes.<br />
The PDR of the Optics is planned for<br />
March 007, with the overall PDR planned<br />
for July 007. The development of the<br />
extreme AO deformable mirror, its drive<br />
electronics and the digital detectors necessary<br />
to analyse the wavefront is proceeding.<br />
The delivery of these critical<br />
components is expected in autumn 007.<br />
The High Order Test-bench (HOT), supported<br />
by OPTICON and dedicated to the<br />
verification of high-contrast imaging concepts,<br />
has been set up at <strong>ESO</strong> and first<br />
closure of the AO loop has been achieved.<br />
56<br />
<strong>ESO</strong> Annual Report 006<br />
A formal call for second-generation VLT<br />
interferometric instruments yielded three<br />
Proposals in January: for GRAVITY,<br />
MATISSE and VSI (down from nine possible<br />
concepts at the start of the selection<br />
process in 005). Following a recommendation<br />
of the STC committee, Phase A<br />
study contracts were let for all of them<br />
with final study reports being due in summer<br />
007.<br />
In addition to specific instrumentation<br />
projects, detector and other development<br />
work was undertaken to ensure that<br />
<strong>ESO</strong> remains at the forefront in this critical<br />
area. Most visibly, development of<br />
the Next General detector Controller<br />
(NGC) continued to advance. The NGC is<br />
designed to meet the needs of all foreseeable<br />
visible and infrared detector systems<br />
for the coming years – both to<br />
achieve the noise, speed and other performance<br />
requirements and also to provide<br />
the maintenance benefits of a single<br />
type of system at the La Silla Paranal<br />
Observatory. Furthermore, detector developments<br />
and characterisation together<br />
with industry continued in various areas<br />
aimed at improving the quantum efficiency,<br />
noise, speed and other properties<br />
of both visible and infrared detectors. In<br />
addition to the science detectors themselves,<br />
new drivers for these improvements<br />
have come from the requirements<br />
for adaptive optics wavefront sensors<br />
and fringe-tracking systems needed for<br />
interferometric applications.<br />
MAD, the Multi-Conjugate Adaptive Optics<br />
Demonstrator, is a bench instrument<br />
to demonstrate and study, both in the<br />
Laboratory and on-sky, many of the new<br />
AO approaches proposed in the last<br />
years, which are needed for some second-generation<br />
VLT instruments and<br />
which are crucial for the future European<br />
Extremely Large Telescope. The most<br />
important approaches to be demonstrated<br />
by MAD are the Multi-Conjugate<br />
AO and the Ground Layer AO, both aiming<br />
at enlarging the field of view of the<br />
correction, which is typically very small in<br />
traditional AO systems. During the year<br />
MAD completed its test and characterisation<br />
phase in the laboratory for both the<br />
‘classical’ wavefront-sensing mode developed<br />
at <strong>ESO</strong> and the layer-oriented mode<br />
developed by an Italian consortium.<br />
The laboratory results have shown that<br />
Multi-Conjugate AO has diffractionlimited<br />
capabilities and good correction<br />
uniformity across a field of view up to<br />
arcminutes, under Paranal median seeing<br />
conditions. Ground Layer AO has shown<br />
its great potential in increasing the energy<br />
concentration on similar fields of view.<br />
On-sky demonstration will be extremely<br />
helpful in understanding how the two<br />
correction approaches will perform under<br />
real atmospheric conditions. MAD<br />
achieved Preliminary Acceptance in<br />
Europe (PAE) in December. The infrared<br />
camera produced by the Portuguese<br />
partner also achieved PAE, in September.<br />
MAD has been sent to Paranal to be<br />
reintegrated and should perform first onsky<br />
runs in March/April 007.
Technical Developments<br />
The Technology Division provided engineering<br />
support to over 150 different <strong>ESO</strong><br />
projects and workpackages in 006 –<br />
a 50 % increase over 005. The increase<br />
has been largely due to the start of the<br />
production phases of major on-going<br />
projects like ALMA, second-generation<br />
VLT instrumentation, and VLTI instruments,<br />
as well as the demands of new<br />
workpackages related to the E-ELT and<br />
FP6. Support for VLT operations at<br />
Paranal also continues as an important<br />
background activity for the Division.<br />
Electronic Engineering<br />
The introduction of the EU RoHS Directive<br />
(Restriction on the use of Hazardous<br />
Substances) has had an impact not only<br />
on internal electronic developments at<br />
<strong>ESO</strong> but also on the availability of many<br />
commercial electronic units. This relates,<br />
in particular, to the requirement for leadfree<br />
soldering. In some cases compatible<br />
alternative commercial units that conform<br />
to RoHS are available, but others, like<br />
the <strong>ESO</strong>-standard Maccon motor control<br />
units that are used within all VLT instruments,<br />
are now no longer available. The<br />
Electronics Department has therefore ordered<br />
a sufficient stock of these and<br />
other operations-critical modules to provide<br />
for long-term maintenance sup-<br />
port for the VLT and its instrumentation.<br />
A new standard motor-control suite for<br />
instrumentation based on the CAN-bus<br />
standard has been developed and, in<br />
006, a pre-production series of the DC<br />
motor controllers and prototypes of the<br />
stepper motor controllers were produced<br />
and tested in Garching. These will complement<br />
the existing Maccon boards and<br />
will be particularly suitable for new applications<br />
where distributed motors are to<br />
be controlled.<br />
In order to be able to assure reliable operation<br />
of electronic systems over the entire<br />
range of operational temperatures,<br />
the Electronics Department has acquired<br />
a new climatically controlled enclosure to<br />
allow thermal stress-testing all new electronics<br />
designs as well as commercially<br />
bought equipment. Although electronic<br />
reliability has not been a serious problem<br />
in the past, the new equipment will contribute<br />
to our goal of improving quality assurance<br />
procedures throughout the organisation.<br />
Systems Engineering<br />
Computer modelling of opto-mechanical<br />
systems is an important aspect of <strong>ESO</strong>’s<br />
systems engineering work. To enable increasingly<br />
complex systems such as the<br />
E-ELT to be modelled, the analysis tools<br />
used at <strong>ESO</strong> have to be continually extended<br />
to keep pace with project requirements.<br />
A particular example in 006 is<br />
the Structural Modelling Interface (SMI)<br />
tool developed jointly at <strong>ESO</strong> and the<br />
Technical University in Munich. The SMI<br />
Test chassis with multiple units of the <strong>ESO</strong>-developed CAN-bus DC motor drive module.<br />
can reduce the complexity of large FEM<br />
models produced in ANSYS to levels<br />
that permit control simulations using Matlab/Simulink<br />
to be carried out, but without<br />
significant losses in model fidelity.<br />
Another analysis tool that has been developed<br />
over a number of years at <strong>ESO</strong>, together<br />
with Astrium, is Beam Warrior. A<br />
limitation of classical optical design tools<br />
like Code-V and Zemax is that they produce<br />
optical models but these are not<br />
linked to the mechanical and other perturbations<br />
of the complete system. By combining<br />
optical design parameters from<br />
these programs with flexure information<br />
obtained from a FE Analysis, Beam Warrior<br />
can calculate parameters like the<br />
point-spread functions or Zernike coefficients<br />
for a variety of telescope orientations<br />
and load conditions. It allows optical<br />
models to be integrated into control-loop<br />
simulations and can also handle segmented-mirror<br />
telescopes. Beam Warrior<br />
will thus be an important element of the<br />
E-ELT integrated model.<br />
Systems Engineering is an important discipline<br />
for all complex projects, and for<br />
major projects like ALMA and the E-ELT it<br />
is indispensable. Keeping track of the<br />
continually evolving projects requirements<br />
throughout the development cycle is a<br />
challenging task and is an area where<br />
a Requirement Management Tool can be<br />
very useful. DOORS is such a tool that<br />
has been successfully used within the<br />
Software Department for several years for<br />
the ALMA software documentation and<br />
requirement management. Requirement<br />
Management promotes a formal approach<br />
to the definition of project requirements<br />
at different levels (stakeholder<br />
requirements, systems requirements,<br />
operational requirements, etc.), and links<br />
these to subsystems requirements,<br />
design documentation, verification procedures,<br />
and so on. It allows transparent<br />
requirement traceability for change control<br />
and helps with the early identifica-<br />
tion of errors that can be expensive to<br />
correct later on in the project.<br />
In 006, a pilot project has been started<br />
to apply DOORS to the E-ELT project.<br />
The Level 1 project requirements have<br />
been identified and integrated into the<br />
DOORS requirements management process<br />
framework, and linking has started.<br />
<strong>ESO</strong> Annual Report 006<br />
57
Opto-Mechanics<br />
During 006, several background developments<br />
have been pursued in technologies<br />
that could be of potential interest<br />
for future <strong>ESO</strong> projects. One area of key<br />
importance for an ELT project is fine mirror-shape<br />
control and, with this in mind,<br />
two parallel development projects have<br />
been undertaken to evaluate piezoelectric<br />
actuators. The first project used piezo<br />
fibres attached to a bar. The test results<br />
obtained showed bending that was in<br />
good agreement with a FE analysis and,<br />
in particular, showed no significant hysteresis.<br />
The second development, which<br />
is still ongoing, uses piezo stack actuators<br />
attached to a dummy mirror blank.<br />
Both these techniques show good potential<br />
for a precise and economic means of<br />
mirror deformation control.<br />
A design challenge for any large exposed<br />
structure like the ELT is wind buffeting<br />
control. Although wind tunnel testing and<br />
CFD (Computational Fluid Dynamics)<br />
models are both valuable techniques,<br />
there always remains a problem of validating<br />
these models, both in terms of scaling<br />
and understanding the correct disturbance<br />
spectra to apply. In order to<br />
obtain realistic test data for an extremely<br />
large telescope, an experiment has been<br />
undertaken with the support of the University<br />
of Manchester to attach some 00<br />
pressure sensors on the surface of the<br />
Jodrell Bank 70-m Lovell radio telescope<br />
in the UK. These allow not only the absolute<br />
pressure variations to be determined<br />
over a period of one year, but also enable<br />
us to gain a good understanding of the<br />
pressure correlations across the reflector<br />
surface, that have an important impact<br />
on the overall telescope design. During<br />
the course of 006, the sensors and their<br />
readout electronics were installed on the<br />
telescope by <strong>ESO</strong>’s partner firm GBF, and<br />
analysis of the initial data is already underway.<br />
58<br />
<strong>ESO</strong> Annual Report 006<br />
Software Engineering<br />
The 15th release of the VLT Software, i.e.<br />
the January 006 release, was the last to<br />
support HP-UX and Sun Solaris operating<br />
systems. The next planned release, in<br />
February 007, will support Linux only.<br />
This change will considerably reduce the<br />
amount of software testing to be carried<br />
out and contribute to improved reliability.<br />
<strong>ESO</strong> Videoconferences from 000 to 006<br />
3 000<br />
500<br />
000<br />
1500<br />
1000<br />
500<br />
0<br />
TBytes<br />
70<br />
60<br />
50<br />
40<br />
30<br />
0<br />
10<br />
0<br />
Software updates are needed primarily to<br />
meet the specific requirements of new<br />
VLT instruments as well to cater for various<br />
hardware configuration changes.<br />
For real-time control environments, <strong>ESO</strong><br />
has now moved from WindRiver VxWorks<br />
release 5.5 to release 6.0. This step<br />
was necessary, not only to be able to use<br />
the latest real-time processor boards,<br />
but also because release 6, unlike its predecessors,<br />
supports Linux as a development<br />
platform.<br />
110 141 44 363 496 1 06 568<br />
000 001 00 003 004 005 006<br />
003<br />
004 005 006<br />
Above: The total number of yearly <strong>ESO</strong><br />
videoconferences since the year 000.<br />
TBytes transmitted<br />
TBytes received<br />
Growth of Garching Internet traffic in<br />
Terabytes over the last four years.<br />
The dark blue bars show outgoing<br />
data and the light blue incoming data.
In December 006, an internal reorganisation<br />
in Garching led to the transfer<br />
of staff of the Software Department from<br />
the Technology Division to the newly<br />
formed Software Development Division.<br />
There they join software engineers who<br />
were previously in the software development<br />
group of the former Data Management<br />
Division. This move is intend-<br />
ed to consolidate software developers<br />
within the organisation and provide improved<br />
synergy.<br />
IT Services<br />
A major event for IT services was the<br />
change of outsource service provider in<br />
April 006. The new contractor has<br />
taken over responsibility for providing IT<br />
support not only in Garching but also<br />
in Santiago, La Silla and Paranal. Previously,<br />
three separate contractors were<br />
responsible for providing IT support in<br />
Garching, Paranal and Santiago respectively,<br />
with La Silla being supported by<br />
<strong>ESO</strong> staff. This change will greatly assist<br />
inter-site coordination and the rationalisation<br />
of IT services.<br />
The use of <strong>ESO</strong> communications systems<br />
continues to rise rapidly. Since videoconference<br />
systems were first introduced at<br />
<strong>ESO</strong> in 000, their usage has increased<br />
dramatically. Today, videoconferencing is<br />
an indispensable part of <strong>ESO</strong>’s activities,<br />
not only for internal <strong>ESO</strong> meetings between<br />
Europe and Chile, but also for regular<br />
contacts with our project partners<br />
in Europe and beyond. Videoconferences<br />
not only facilitate closer contact between<br />
staff in Europe and Chile but also lead to<br />
reduced travel costs. In 006, an average<br />
of 10 videoconferences took place each<br />
working day.<br />
Similarly, network traffic has also increased<br />
steadily over the last few years,<br />
fuelled by higher available bandwidths<br />
and cheaper access costs. In 006, the<br />
total incoming and outgoing traffic<br />
through the Garching Internet portal was<br />
about 90 Terabyte/year.<br />
The Spiral Galaxy NGC 3190 (FORS/<strong>ESO</strong>).<br />
<strong>ESO</strong> Annual Report 006<br />
59
Science Archive Operation<br />
The Science Archive Operation (SAO)<br />
group is responsible for receiving, storing<br />
and redistributing <strong>ESO</strong> and Hubble<br />
Space Telescope (HST) data, as well as<br />
providing front-line archive user sup-<br />
port. The current total archive holding is<br />
53. terabytes (TB) of <strong>ESO</strong> data and<br />
in excess of TB of HST data. Roughly<br />
13 TB of new data were archived during<br />
006, a 10 % increase over 005. While<br />
the volume of HST data is rather small<br />
compared to that of <strong>ESO</strong> data, the number<br />
of files archived for the two observatories<br />
is comparable: 6 million <strong>ESO</strong> files<br />
and 4 million from HST, for a grand total<br />
holding in excess of 10 million files hosted<br />
in the <strong>ESO</strong> Archive. Users around the<br />
world can access the <strong>ESO</strong> archive via a<br />
web-based data request submission<br />
system. In addition to the general archive<br />
web interface, all current VLT instruments,<br />
the VLTI MIDI instrument, the<br />
HARPS instrument on La Silla, and APEX<br />
on Chajnantor have dedicated instrumentspecific<br />
forms to query the data. More<br />
than 16 600 unique archive requests were<br />
served in 006, totalling 4 TB of data<br />
(a 4 % increase with respect to 005). Of<br />
those requests, 14 900 were for <strong>ESO</strong><br />
data, while the remaining 1700 were for<br />
HST data. In addition we have prepared<br />
1 11 data packages that were delivered<br />
to Principal Investigators on 733 CDs<br />
or DVDs. Finally, 140 calibrated pre-imaging<br />
data sets from the two FORS instruments,<br />
VIMOS, VISIR and, as of the third<br />
quarter of 006, ISAAC, NACO and SIN-<br />
FONI were delivered automatically within<br />
48 hours of acquisition at the telescope.<br />
Raw data from the UKIRT Infrared Deep<br />
Sky Survey (UKIDSS) executed with the<br />
WFCAM instrument at the UK Infrared<br />
Telescope (UKIRT) have kept flowing into<br />
the <strong>ESO</strong> archive. During 006 we have<br />
received .5 TB worth of UKIDSS data,<br />
mostly concentrated in the first part of<br />
the year.<br />
The year 006 marked the beginning of<br />
operations of the APEX submillimetre<br />
antenna on the Llano de Chajnantor. The<br />
data belonging to two out of the three<br />
APEX partners – <strong>ESO</strong> itself and the<br />
Onsala Space Observatory in Sweden –<br />
are stored in the <strong>ESO</strong> archive. As with<br />
any other <strong>ESO</strong> data, APEX files will also<br />
be made public to the community at<br />
large, once the usual proprietary period<br />
has expired. The <strong>ESO</strong> archive currently<br />
60<br />
<strong>ESO</strong> Annual Report 006<br />
holds 75 GB of APEX data, as produced<br />
by the Science Verification runs and<br />
the first round of <strong>ESO</strong> and Onsala General<br />
Observer programmes.<br />
A major milestone for 007 will be the<br />
archiving of data from VISTA/VIRCAM,<br />
the new wide-field infrared imager scheduled<br />
to start operating in the course<br />
of the year. With an expected data rate of<br />
150 TB a year, this instrument alone<br />
will produce a tenfold increase of data<br />
volume compared to all other instruments<br />
combined!<br />
In order to cope with this massive flow of<br />
data, the way data themselves are transferred<br />
from Paranal to Garching was<br />
overhauled in 006. In fact, the traditional<br />
way of transferring data on CDs and<br />
DVDs, which has faithfully served VLT<br />
operations since the beginning, was discontinued.<br />
As of December 006, VLT<br />
data are transferred to Garching in a<br />
novel and very efficient way, i.e. directly<br />
on NGAS (Next Generation Archiving<br />
System) discs, a technology developed<br />
at <strong>ESO</strong> and the foundation of the <strong>ESO</strong><br />
archive itself.<br />
Fundamentally, archive operations rely<br />
on a large number of hardware servers to<br />
store science data and their associated<br />
metadata in a reliable manner. We estimate<br />
that the archive data volume will exceed<br />
the petabyte limit by 011. Therefore,<br />
a petabyte-class archive has been<br />
designed to deal with the challenge<br />
of huge astronomical data volumes. This<br />
petabyte-class archive consists of <strong>ESO</strong>’s<br />
Primary and Secondary Archive, the<br />
Compute Stack and the Fast Cache.<br />
The Primary Archive is based on hard-<br />
disc technology, currently distributed on<br />
5 Linux servers with a storage capac-<br />
ity of 6.4 TB each, whereas the Secondary<br />
Archive is based on a petabyte tape<br />
library, currently equipped with over 300<br />
tapes, each with a storage capacity of<br />
0.5 TB. The Secondary Archive will store<br />
a second copy of the entire <strong>ESO</strong> archive<br />
contents at another physical location.<br />
The Compute Stack consists of blade<br />
Structure of the <strong>ESO</strong> archive and its main<br />
components. Scheme by R. Höllmüller.<br />
systems with a maximum capacity of<br />
13 CPUs. The Fast Cache provides 9<br />
TB of extendable Fibre Channel discbased<br />
storage. For the safe installation<br />
of the Primary Archive at different<br />
physical locations, <strong>ESO</strong> approved the<br />
plan to build an <strong>ESO</strong> Data, Computing<br />
and Operations Centre, to be completed<br />
in 007.<br />
Archive Database Content Management<br />
The <strong>ESO</strong> science archive contains two<br />
kinds of information: the actual science<br />
data generated by various <strong>ESO</strong> telescopes<br />
as well as the HST, and<br />
metadata which describe these science<br />
data, e.g. what objects were observed,<br />
when they were observed, and how they<br />
were observed. These important descriptions<br />
are necessary to allow users to find<br />
and retrieve science data and data<br />
products from the Archive. The DFO<br />
Database Content Management (DBCM)<br />
group has responsibility for maintaining<br />
these metadata. This is not an easy task,<br />
with the landmark of two billion database<br />
entries being reached and surpassed in<br />
006!<br />
In particular, DBCM implements metadata<br />
changes and updates following<br />
requests from various <strong>ESO</strong> operations<br />
groups or upon identification of erroneous<br />
entries. In addition, the DBCM<br />
group works closely with the DMO<br />
Virtual Observatory Systems (VOS)<br />
department to interface VOS services<br />
with the operational archive.
SN 006X in the spiral galaxy M 100.<br />
<strong>ESO</strong> Annual Report 006<br />
61
The European Virtual Observatory<br />
The Virtual Observatory (VO) aims to allow<br />
users easy and seamless access<br />
to the huge amount of astronomical data<br />
currently available, to facilitate its exploitation<br />
and foster new science. The VO initiative<br />
is a global collaboration of the<br />
world’s astronomical communities under<br />
the auspices of the International Virtual<br />
Observatory Alliance (IVOA). From the<br />
start, <strong>ESO</strong> has been very active in the VO<br />
arena, creating on 1 November 004 a<br />
Virtual Observatory Systems (VOS) Department<br />
in the <strong>ESO</strong> Data Management<br />
and Operations Division. VOS’ role is also<br />
to make the Science Archive Facility<br />
(SAF) a powerful scientific resource for<br />
the <strong>ESO</strong> community, and thereby ensure<br />
that <strong>ESO</strong> also plays a major role in the<br />
VO as a data provider.<br />
<strong>ESO</strong> is a founding member of the EURO-<br />
VO project, whose aim is to deploy an<br />
operational VO in Europe. Besides <strong>ESO</strong>,<br />
initial partners include the European<br />
Space Agency (ESA), and six national<br />
funding agencies, with their respective<br />
VO nodes: Istituto Nazionale di Astrofisica<br />
(INAF, Italy), Institut National des Sciences<br />
de l’Univers (INSU, France),<br />
Instituto Nacional de Técnica Aeroespacial<br />
(INTA, Spain), Nederlandse Onderzoeksschool<br />
voor Astronomie (NOVA,<br />
Netherlands), the Particle Physics and<br />
Astronomy Research Council (PPARC,<br />
UK), and Rat Deutscher Sternwarten<br />
(RDS, Germany). EURO-VO has established<br />
three interlinked structures:<br />
– the Data Centre Alliance (DCA), an alliance<br />
of European data centres which<br />
will populate the EURO-VO with data,<br />
provide the physical storage and computational<br />
fabric and which will publish<br />
data, metadata and services to the<br />
EURO-VO using VO technologies;<br />
– the Facility Centre (VOFC), an organisation<br />
that provides the EURO-VO with<br />
a centralised registry for resources,<br />
standards and certification mechanisms<br />
as well as community support for<br />
VO technology take-up and dissemination<br />
and scientific programme<br />
support using VO technologies and<br />
resources; the VOFC is located at <strong>ESO</strong><br />
and is managed by <strong>ESO</strong> and ESA;<br />
6<br />
<strong>ESO</strong> Annual Report 006<br />
– the Technology Centre (VOTC), a distributed<br />
organisation that coordinates a<br />
set of research and development projects<br />
on the advancement of VO technology,<br />
systems, and tools in response<br />
to scientific and community requirements.<br />
The EURO-VO Science Advisory Committee<br />
(SAC) was put together in March<br />
006 to provide overall scientific input<br />
to the project. Two SAC meetings were<br />
held in 006, the first on 7– 8 April<br />
at <strong>ESO</strong>, the second on November at<br />
ESRIN in Frascati, Italy. SAC members<br />
were introduced to the different aspects<br />
of the EURO-VO through various presentations<br />
and were updated on the latest<br />
EURO-VO developments and on the goals<br />
of the three EURO-VO substructures. The<br />
SAC then discussed some EURO-VO<br />
tools and a call for proposals to carry<br />
out astronomical research projects using<br />
VO tools.<br />
New EURO-VO Web pages (http://www.<br />
euro-vo.org) were presented to the SAC<br />
at its first meeting, and opened to the<br />
public a week or so later. They contain,<br />
among other things, concrete examples<br />
for astronomers of what the VO can and<br />
cannot do for them at present, and links<br />
to VO software applications.<br />
VOS was in charge of the organisation of<br />
the IVOA booth at the XXVIth General<br />
Assembly of the International Astronomical<br />
Union in Prague, on 14– 5 August.<br />
VOS also coordinated the EURO-VO presence<br />
and demonstration and the work on<br />
the EURO-VO flier.<br />
The first meeting of the board of the<br />
EURO-VO Data Centre Alliance (DCA)<br />
project, which has received funding of<br />
1.5 M€ from the Sixth Framework Programme<br />
(FP6; Coordination Actions) of<br />
the European Community, took place<br />
on –3 October in Strasbourg. The DCA,<br />
which is made up of eight European astronomical<br />
organisations including <strong>ESO</strong>,<br />
is vital for the EURO-VO goal of making<br />
the VO a reality in Europe. The DCA project<br />
is currently funded for two years,<br />
with expected completion by September<br />
008. <strong>ESO</strong>’s main role in the DCA is to<br />
organise, in collaboration with ESA, dedicated<br />
workshops to ensure the dissemination<br />
of technical knowledge necessary<br />
to implement VO-endorsed standards.<br />
The VOTech project is a design study,<br />
which aims to complete the technical<br />
preparation for the construction of the<br />
EURO-VO. The project is funded at<br />
the 6.6 M€ level by FP6 and by the part-<br />
ners, which include <strong>ESO</strong>, the Universi-<br />
ties of Edinburgh, Leicester, and Cambridge<br />
(UK), CNRS and Université Louis<br />
Pasteur (France), and INAF (Italy). The<br />
duration of the project is three years, with<br />
expected completion by the end of 008.<br />
<strong>ESO</strong> has a strong role in the VOTech<br />
project as leader of the Design Study 4<br />
on New User Tools, which aims to<br />
provide European astronomers with research<br />
tools integrated in, and fully<br />
compliant with, the VO. The project<br />
works in six-month cycles. Two planning<br />
meetings were held: on 6–9 March in<br />
Sorrento, Italy, and on 4–7 September<br />
in Strasbourg, France.<br />
VOS maintains the Euro-VO project web<br />
site, which in 006 served 77 GB of<br />
content resulting from 10 000 user sessions.<br />
VOS is also in charge of the IVOA<br />
project web site, which served 6 GB of<br />
web content resulting from 330 000 user<br />
sessions.
ST-ECF<br />
<strong>ESO</strong> and the European Space Agency<br />
continued their successful collaboration<br />
through the Space Telescope European<br />
Coordinating Facility (ST-ECF).<br />
The Hubble Space Telescope (HST) is<br />
currently in observing cycle 15, routine-<br />
ly achieving observing efficiencies between<br />
45 and 50 per cent. It is performing<br />
nominally in two-gyro mode. As a<br />
precautionary measure, plans have been<br />
designed to test the HST in one-gyro<br />
mode. Science highlights include the<br />
mapping of dark energy in space and<br />
time, the observation of the earliest<br />
galaxies in the Universe, and the discovery<br />
of many planets around nearby stars.<br />
European participation continued to be<br />
well above the nominal 15 %.<br />
Following directives from the ESA executive<br />
the ST-ECF reached a stable staffing<br />
level: seven ESA-funded positions and<br />
seven <strong>ESO</strong>-funded positions, corresponding<br />
exactly to the initial agreements between<br />
the two organisations, except that<br />
two of the staff members are now allocated<br />
to public outreach. The primary<br />
consequence of this staff rampdown was<br />
the discontinuation of the Advanced Calibration<br />
Project. It was possible to salvage<br />
some of the products of the group<br />
through an early partial delivery to the<br />
STScI. Moreover, two staff members of<br />
the former ST-ECF Advanced Calibration<br />
Group are now working for <strong>ESO</strong>, continuing<br />
this very successful effort, which,<br />
while initially developed for the HST spectrographs,<br />
works exceedingly well for<br />
the <strong>ESO</strong> ground-based instruments. In<br />
October, <strong>ESO</strong> and ESA decided to terminate<br />
the ST-ECF when the current Hubble<br />
ESA/NASA MoU expires at the end of<br />
010. The tasks of the group remain<br />
those agreed at the 006 Annual Review.<br />
The focus of the ST-ECF efforts was on<br />
Advanced Science Data Products: both<br />
the ACS and the NICMOS instruments on<br />
HST have integral-field spectroscopic<br />
capabilities. The data produced in these<br />
modes are complex to analyse and require<br />
techniques unfamiliar to most astronomers.<br />
ST-ECF has therefore begun<br />
to extract the spectra from the data<br />
frames and to calibrate them, with the<br />
aim of making them available to the community.<br />
This capability is also applica-<br />
ble to Wide Field Camera 3, one of the<br />
two new scientific instruments that will<br />
be installed on the HST during Servicing<br />
Mission 4.<br />
The proposed mode of operation for the<br />
other instrument to be installed, the Cosmic<br />
Origins Spectrograph, will put a<br />
higher demand on the usage of the wavelength<br />
calibration lamps. The ST-ECF<br />
coordinated a NASA/ESA funded project<br />
that involved <strong>ESO</strong>, NIST, STScI and the<br />
COS team to evaluate the spectral characteristics<br />
and the life expectancy under<br />
these operating conditions.<br />
The European HST Archive was migrated<br />
to the new <strong>ESO</strong> Archive infrastructure.<br />
The total holdings are now 547000 data<br />
sets. During 006, 414 6 data sets<br />
( .9 TB) were distributed to 40 users.<br />
ST-ECF staff also assisted the STScI<br />
in the final reprocessing of the FOC and<br />
GHRS archives. In collaboration with<br />
the STScI and the CADC the Hubble Legacy<br />
Archive was initiated. The goal is to<br />
collect and generate selected High Level<br />
Science Data Products and make them<br />
available to the community.<br />
User support continued through the<br />
Newsletter, the HST email hotline, and<br />
the production of technical documents.<br />
ST-ECF staff also monitored the TAC<br />
process and continued to support the<br />
<strong>ESO</strong> SAMPO Project. More recently,<br />
the editorship of the <strong>ESO</strong> Messenger was<br />
taken over by ST-ECF staff.<br />
For the ST-ECF’s task to disseminate the<br />
discoveries from Hubble to the public,<br />
006 has been the most successful year<br />
so far. Nineteen news and photo releases<br />
were produced (up 0 % from 005). The<br />
European Hubble website had .8 million<br />
visitors (up 90 %) and distributed 36 TB of<br />
multimedia materials (up 65 %).<br />
The ESA/<strong>ESO</strong>/NASA Photoshop FITS<br />
Liberator .1 was released. Several exhibitions<br />
were produced together with<br />
external organisations – perhaps most<br />
noteworthy was a part of the perma-<br />
nent exhibition in Armagh Planetarium.<br />
The Astronomy Visualisation Metadata<br />
standard (co-authored with Robert Hurt)<br />
was endorsed by the International Vir-<br />
tual Observatory Alliance.<br />
The third ESA-<strong>ESO</strong> Bilateral meeting took<br />
place in Garching at the end of Octo ber.<br />
The third working group report – on<br />
Fundamental Cosmology by Peacock,<br />
Schneider et al. – was finished and distributed.<br />
The meeting addressed the recommendations<br />
of all three working groups<br />
and decided to continue both the bilateral<br />
meetings, which are essential for the<br />
coordination of science planning, and the<br />
series of topical working groups.<br />
The former Instrument Advanced Calibration<br />
Group was selected by NASA to<br />
receive the “Group Achievement Award”<br />
for its work on high-fidelity calibration.<br />
The award, given at a ceremony at NASA<br />
Headquarters on 1 July to Paul Bristow,<br />
Florian Kerber and Michel Rosa, is<br />
shared with a three-member team from<br />
the US National Institute of Standards.<br />
Artist’s view of Servicing Mission 4 to<br />
Hubble. This Servicing Mission will<br />
not only ensure that Hubble can function<br />
for perhaps as much as another<br />
ten years, it will also increase its capabilities<br />
significantly in key areas. As<br />
part of the upgrade, two new scientific<br />
instruments will be installed: the<br />
Cosmic Origins Spectrograph and the<br />
Wide Field Camera 3.<br />
ESA/Hubble<br />
<strong>ESO</strong> Annual Report 006<br />
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64<br />
<strong>ESO</strong> Annual Report 006<br />
Open House at the <strong>ESO</strong> Headquarters on 15 October 006.
Public Outreach<br />
On all accounts, the year 006 marked<br />
a record year in terms of Public Outreach<br />
activities by <strong>ESO</strong>. This growth is motivated<br />
by several factors, including<br />
– the increase in the number of mem-<br />
ber states of <strong>ESO</strong>;<br />
– the current and planned project port-<br />
folio, which foresees investments in<br />
the range of several hundreds of millions<br />
of Euros;<br />
– the increased focus on the need to<br />
secure an adequate recruitment base,<br />
not just in the time to come, but also<br />
in today’s labour market, which is characterised<br />
by stiff competition for the<br />
best people.<br />
Furthermore the increased competition<br />
for public visibility and communication<br />
in general in today’s society places strong<br />
demands on the quality of the communication<br />
efforts, not just in terms of contents<br />
but also with respect to delivery mechanisms.<br />
Other aspects such as timing and<br />
timeliness are of course of crucial importance<br />
in today’s fast moving media world.<br />
This has led us to pursue a particular<br />
strategy, which builds on technical autonomy,<br />
short communication lines within<br />
the organisation and an elaborate system<br />
of partnerships. For example, <strong>ESO</strong> has<br />
established a Science Outreach Network<br />
with representatives in all <strong>ESO</strong> member<br />
states. These ‘ambassadors’ perform an<br />
important interface function between the<br />
national media and <strong>ESO</strong>.<br />
Of course, as in the previous years, many<br />
press releases are done in collaboration<br />
with national organisations (e.g. PPARC,<br />
MPE, CNRS, INAF), universities, the leading<br />
research journal Astronomy & Astrophysics,<br />
and other partners.<br />
Obviously, the Public Affairs Department<br />
(PAD) works in close consultation and<br />
coordination with <strong>ESO</strong>’s Santiago Representation,<br />
which conducts targeted outreach<br />
activities for Chile and provides<br />
logistical support to European media and<br />
high-level visitors.<br />
PAD also works with <strong>ESO</strong>’s sister organisation<br />
ESA, including the Hubble Europe<br />
Information Centre, sited in adjacent<br />
rooms to PAD. The cooperation involves<br />
sharing of information and technical facilities,<br />
wherever possible.<br />
In the field of education, the European<br />
Association for Astronomy Education<br />
(EAAE) is a long-standing partner of <strong>ESO</strong>.<br />
The EAAE members help by spreading<br />
information about <strong>ESO</strong> in the schools,<br />
while at the same time they often provide<br />
didactic advice to PAD as it formulates<br />
and prepares its education activities.<br />
The European Commission has become<br />
a major partner as well, not least in<br />
funding educational activities, which have<br />
come to be seen as representing substantial<br />
added value for Europe’s societies<br />
and therefore enjoy significant political<br />
attention and goodwill.<br />
Finally, the major education activities,<br />
such as Science on Stage and Science in<br />
School, are carried out within the framework<br />
of the EIROforum, the partnership<br />
of Europe’s seven intergovernmental research<br />
organisations. The partnership<br />
enables a very successful pooling of resources<br />
and expertise and allows undertaking<br />
activities on a scale that would<br />
have been impossible for the individual<br />
organisations alone.<br />
Media<br />
In 006, <strong>ESO</strong> issued a total number of<br />
51 releases to the media, or roughly one<br />
release per week.<br />
Press conference on exoplanets at <strong>ESO</strong>F, Munich.<br />
This number can be broken down into<br />
39 ‘standard’ press releases, including<br />
6 about scientific results from observations<br />
with <strong>ESO</strong> telescopes, and 13 press<br />
photos. The press photos enjoy great<br />
popularity among the media and ensure a<br />
much increased visibility of <strong>ESO</strong>. Seven<br />
<strong>ESO</strong> images were selected as the Astronomy<br />
Picture of the Day in 006 by the<br />
NASA website. This number is indicative<br />
of our potential for creating world-class<br />
astronomical images – a potential that<br />
with increased resources could be expanded<br />
significantly. The most appreciated<br />
image was certainly the new, stunning<br />
mosaic of the Tarantula Nebula (<strong>ESO</strong><br />
Press Photo 50a/06), a 56 million pixel<br />
image obtained with the Wide-Field Imager<br />
on the . -m telescope at La Silla.<br />
The image was voted amongst the ten<br />
best of 006 by a very popular web site.<br />
Other successes were encountered particularly<br />
with images of galaxies, such as<br />
the topsy-turvy one (<strong>ESO</strong> Press Photo<br />
43a/06) or the gigantic dusty potato crisp<br />
(<strong>ESO</strong> Press Photo 17/06), as well as those<br />
of the broken comet (<strong>ESO</strong> Press Photo<br />
15a/06).<br />
Among the most successful press releases,<br />
the prize goes without any doubt<br />
to the discovery through microlensing<br />
of a five-Earth-mass planet, a press release<br />
(<strong>ESO</strong> Science Release 03/06) that<br />
<strong>ESO</strong> Annual Report 006<br />
65
generated huge media attention worldwide.<br />
Other excellent results were obtained<br />
with the press releases on the VLT<br />
being equipped with a laser guide star<br />
(<strong>ESO</strong> Instrument Release 07/06), the discovery<br />
of a trio of Neptune-mass planets<br />
(<strong>ESO</strong> Science Release 18/06), the SIN-<br />
FONI observations of a very remote galaxy<br />
(<strong>ESO</strong> Science Release 31/06) and<br />
<strong>ESO</strong>’s Council decision to go ahead with<br />
a design study for the European Extremely<br />
Large Telescope (<strong>ESO</strong> Organisation<br />
Release 46/06).<br />
Other features which have been very<br />
much welcomed by the media are the<br />
increased use of captivating artistic<br />
imagery as an alternative way of explaining<br />
physical phenomena, and the provision<br />
of video footage that is directly<br />
linked to <strong>ESO</strong> press releases.<br />
With respect to broadcast support and<br />
video production, in 006 we delivered<br />
an average of 11 minutes/day of footage<br />
to TV Channels worldwide, produced<br />
1.5 seconds/day of high-end 3D animations<br />
on technical and scientific topics<br />
and 90 minutes of videos, including six<br />
video newsreels – the equivalent of a<br />
15-minute full film production every two<br />
months. This resulted in some 75 registered<br />
broadcasts about <strong>ESO</strong>. The real<br />
number is likely to be significantly higher,<br />
since the use of <strong>ESO</strong> footage is often not<br />
reported to us.<br />
Provision of high-quality material is clearly<br />
a prerequisite for winning the daily battle<br />
for visibility in the public sphere, but<br />
it is not enough. Exploiting a variety of<br />
diffusion channels and new communication<br />
tools are crucially important. Not<br />
surprisingly, much of this is linked to the<br />
world-wide web. For example, we now<br />
make broadcast material electronically<br />
available for download by TV channels,<br />
giving them the option of almost instant<br />
access to <strong>ESO</strong> news reels. Another aspect<br />
is the web-based public sphere.<br />
This has arguably emerged as one of the<br />
most important ways to reach young<br />
people in particular – beyond the classic<br />
media such as broadsheet newspapers<br />
and conventional TV. These new media<br />
include traditional web pages, blogs,<br />
pod-casts, vodcasts, and other emerging<br />
technologies sometimes described as<br />
‘Web .0’. PAD is taking steps to gain a<br />
66<br />
<strong>ESO</strong> Annual Report 006<br />
<strong>ESO</strong> stand in Paris, France.<br />
foothold in this virtual world. A first experiment<br />
was done for the press release<br />
about the discovery of a five-Earth-mass<br />
exoplanet, when a podcast and a vodcast<br />
was provided. Vodcasts are also<br />
done in connection with Video newsreels,<br />
whenever possible.<br />
The growing importance of the web and<br />
the speed with which it evolves, both<br />
technically and conceptually, creates new<br />
demands on web sites to remain up to<br />
date. Of course, <strong>ESO</strong> cannot turn its back<br />
on this development. Hence, a major effort<br />
has been undertaken during the year<br />
by PAD, in collaboration with other departments,<br />
to develop a new website for<br />
our organisation. This web site, which will<br />
serve as the point of entry into <strong>ESO</strong> for<br />
thousands of users every day will feature<br />
a much more attractive appearance, easier<br />
navigation and a major overhaul of<br />
the content. It is the intention to launch<br />
the new web site in the course of 007.<br />
The web is, of course, not just a diffusion<br />
channel, but also provides an important<br />
source of information regarding the public<br />
awareness of and interest in <strong>ESO</strong>’s activities.<br />
Hence, the increased visibility of<br />
<strong>ESO</strong> in media is mirrored by the growth in<br />
traffic on the <strong>ESO</strong> Outreach site, which<br />
in 006 has reached a mean number of<br />
almost 10 000 visitors/day, a factor of .3<br />
increase from three years ago.<br />
Exhibitions and Events<br />
In spite of the undisputed importance of<br />
new distribution methods and tools, faceto-face<br />
communication of course remains<br />
of crucial value, particularly from the perspective<br />
of a coordinated communication<br />
effort. Exhibitions and events clearly provide<br />
excellent forums for exchange and<br />
communication with key target groups,<br />
such as scientists, media, industry and<br />
policymakers. In 006, PAD organised or<br />
participated in more than 0 events,<br />
involving exhibitions, briefings and VIP<br />
visits – in other words roughly an event<br />
every ½ weeks. This constitutes a<br />
significant increase over the previous<br />
years, both illustrating the growing<br />
importance and visibility of <strong>ESO</strong>, but also<br />
the necessity to enlist wide support for<br />
<strong>ESO</strong>’s ambitious future projects. For<br />
example, on February, PAD in collaboration<br />
with PPARC organised a very<br />
successful press event in London in<br />
connection with this year’s AstroFest at<br />
Kensington Town Hall. The event was a<br />
briefing about <strong>ESO</strong> in general and also<br />
served as a ‘primer’ to a subsequent visit<br />
to <strong>ESO</strong>’s sites in Chile by a group of UK<br />
journalists. About 15 journalists attended<br />
this meeting. Just 11 days hence, a major<br />
press event took place in Madrid on the<br />
occasion of the signing of the agreement<br />
aimed at bringing Spain into <strong>ESO</strong>. Only<br />
10 days later, we took part at the AAAS<br />
meeting in Saint Louis, Missouri. The<br />
AAAS is the world’s largest forum for
science and media contacts, and our<br />
presence at such an event not only<br />
supports <strong>ESO</strong>’s visibility in the USA but<br />
also in Europe, since the meetings attract<br />
large numbers of European journalists.<br />
The AAAS exhibition stand was subsequently<br />
transferred to and assembled at<br />
the SPIE conference in Orlando, Florida,<br />
in May. <strong>ESO</strong> was very strongly represented<br />
at this meeting, illustrating that our<br />
organisation has become a global actor<br />
in the field of astronomy.<br />
Back in Europe, we had a major information<br />
stand at the year’s Salon de la Recherche<br />
et de l’Innovation in Paris in June<br />
and, in the context of the EIROforum<br />
partnership, at the <strong>ESO</strong>F 006 Conference<br />
in Munich. At <strong>ESO</strong>F we also held a<br />
press event about exoplanet research.<br />
In August, at the XXVIth General Assembly<br />
of the International Astronomical Union<br />
in Prague, PAD set up a 60 square<br />
metre exhibition for <strong>ESO</strong> and a somewhat<br />
smaller one, on behalf of ALMA.<br />
The last press event of the year took<br />
place in connection with the ELT conference<br />
in Marseille in late November.<br />
The event was co-organised by PAD and<br />
INSU, and resulted in many media reports,<br />
including ones in all major French<br />
newspapers – Libération devoting three<br />
full pages to the story – and also, for example,<br />
on German radio.<br />
The last exhibition took place in Dublin at<br />
the beginning of December. <strong>ESO</strong> participated<br />
as the ‘guest of honour’ at the<br />
Astro-Expo 006 event, organised at the<br />
Dublin City University (DCU) by the Irish<br />
Astronomy and Space magazine.<br />
Education<br />
One of <strong>ESO</strong>’s major education activities<br />
for pupils is the popular Catch a Star!<br />
contest, carried out in close collaboration<br />
with the EAAE. Students work in teams<br />
or individually, learning about an astronomical<br />
topic and writing a report. During<br />
006 we saw the conclusion of the fourth<br />
iteration of the competition. The contest<br />
is evolving, with its division into three categories.<br />
As an important aim is simply<br />
to encourage an interest in astronomy,<br />
and because we wish to avoid a sense of<br />
elitism, some of the winning projects<br />
were decided by lottery. Nevertheless, to<br />
cater for particularly talented students<br />
who may be budding astronomers, there<br />
were also major prizes to be won. These<br />
prizes, including a trip to the VLT on<br />
Paranal, were awarded by an international<br />
jury. Furthermore, a drawing competition<br />
category was introduced, following<br />
the success of a similar competition as<br />
part of the Venus Transit 004 activities.<br />
For the first time, the contest was also<br />
opened to countries beyond Europe and<br />
Chile. We received a total of 134 written<br />
projects and 60 pieces of artwork from<br />
4 countries across Europe and beyond,<br />
with about 400 students and teachers<br />
taking part.<br />
In November 006 Catch a Star! 2007,<br />
was launched (so named because this<br />
competition will conclude in 007). Building<br />
on lessons learned in the previous<br />
competition, its structure was streamlined<br />
to make it easier to enter, and the webbased<br />
infrastructure for administering it at<br />
<strong>ESO</strong> was greatly improved. The differentiation<br />
in categories has been retained<br />
with Catch a Star! Artists, Catch a Star!<br />
Adventurers and Catch a Star! Researchers.<br />
Over the years, <strong>ESO</strong> has supported<br />
the EAAE summer schools for astronomy<br />
teachers in a number of ways, e.g. by<br />
providing speakers and taking care of<br />
proceedings. This was also the case<br />
in 006, where the summer school took<br />
place on the island of La Palma. Next<br />
year, however, the summer school will<br />
change format and scope, and will be<br />
hosted by <strong>ESO</strong>. The intention is to foster<br />
a stronger interaction between teachers<br />
and active scientists and to bring real<br />
science into the classrooms. Towards the<br />
end of the year, preparations for this<br />
event were underway.<br />
Similar thoughts underpin the wider, targeted<br />
effort to stimulate original, attractive<br />
high-quality science teaching in Europe’s<br />
secondary schools, known as the<br />
EIROforum European Science Teachers’<br />
Initiative (ESTI), in which <strong>ESO</strong> is an active<br />
partner. With its twin pillars, Science on<br />
Stage and Science in School, ESTI is a<br />
unique activity in the world. In the teaching<br />
world it constitutes a completely<br />
innovative approach with a focus on excellence,<br />
market mechanisms, interdisciplinarity<br />
combined with direct links between<br />
teachers and active scientists and,<br />
finally, cross-border collaboration on a<br />
big scale. The most recent Science on<br />
Stage Festival, with about 500 participants<br />
from more than 5 countries, took<br />
place at CERN in November 005; the<br />
next one is scheduled for Easter 007.<br />
Throughout 006, staff members of the<br />
EIROforum organisations, including those<br />
at <strong>ESO</strong>, supported and participated in the<br />
many national events that took place in 9<br />
countries to select the participants to the<br />
European festival. In March 006 the first<br />
issue of Science in School was launched.<br />
Science in School is a new European<br />
science education journal for teachers,<br />
scientists, and others. Issues include<br />
teaching material, articles about cuttingedge<br />
science, interviews, and reviews.<br />
<strong>ESO</strong> is strongly involved with the journal,<br />
contributing astronomy-related articles<br />
and participating in the editorial board.<br />
Videoconference with Paranal on the main square of Munich, Marienplatz, Germany, during the<br />
annual German Wissenschaftssommer.<br />
<strong>ESO</strong> Annual Report 006<br />
67
<strong>ESO</strong> Press Releases<br />
<strong>ESO</strong> Press Photo 01/06 (3 January): <strong>ESO</strong> PR High-<br />
lights in 005<br />
<strong>ESO</strong> 0 /06 Science Release (4 January): Measuring<br />
the Size of a Small, Frost World<br />
<strong>ESO</strong> Science Release 03/06 ( 5 January): It’s Far,<br />
It’s Small, It’s Cool: It’s an Icy Exoplanet!<br />
<strong>ESO</strong> Press Photo 04/06 (7 February): How to Steal a<br />
Million Stars?<br />
<strong>ESO</strong> Organisation News 05/06 (13 February): Spain<br />
to Join <strong>ESO</strong><br />
<strong>ESO</strong> Science Release 06/06 (15 February): The Invis-<br />
ible Galaxies That Could Not Hide<br />
<strong>ESO</strong> Instrument Release 07/06 ( 3 February): Man-<br />
made Star Shines in the Southern Sky<br />
<strong>ESO</strong> Press Photo 08/06 ( 3 February): A Blast To<br />
Chase<br />
<strong>ESO</strong> Science release 09/06 ( 8 February): Cepheids<br />
and their ‘Cocoons’<br />
<strong>ESO</strong> Science release 10/06 (15 March): The Cosmic<br />
Dance of Distant Galaxies<br />
<strong>ESO</strong> Science release 11/06 ( March): The Sun’s<br />
New Exotic Neighbour<br />
<strong>ESO</strong> EIROforum release 1 /06 ( 8 March): Bringing<br />
Science out of the Lab into the Classroom<br />
<strong>ESO</strong> Press Photo 13/06 (7 April): Cosmic Spider is<br />
Good Mother<br />
<strong>ESO</strong> Press Photo 14/06 (14 April): The Great Easter<br />
Egg Hunt: The Void’s Incredible Richness<br />
<strong>ESO</strong> Press Photo 15/06 ( 5 April): The Comet With a<br />
Broken Heart<br />
<strong>ESO</strong> Science Release 16/06 (8 May): Physics in Uni-<br />
verse’s Youth<br />
<strong>ESO</strong> Press Photo 17/06 (11 May): Twin Explosions In<br />
Gigantic Dusty Potato Crisp<br />
<strong>ESO</strong> Science Release 18/06 (18 May): Trio of Nep-<br />
tunes and their Belt<br />
68<br />
<strong>ESO</strong> Annual Report 006<br />
<strong>ESO</strong> Science Release 19/06 (6 June): Do ‘Planemos’<br />
Have Progeny?<br />
<strong>ESO</strong> Press Photo 0/06 (8 June): The Toucan’s<br />
Diamond<br />
<strong>ESO</strong> Organisation News 1/06 (19 June): <strong>ESO</strong> and<br />
Chile: 10 Years of Productive Scientific<br />
Collaboration<br />
<strong>ESO</strong> Press Photo /06 ( 8 June): The Hooked<br />
Galaxy<br />
<strong>ESO</strong> Science Release 3/06 (3 July): Falling Onto the<br />
Dark<br />
<strong>ESO</strong> Instrument Release 4/06 (13 July): Sub-<br />
millimetre Astronomy in Full Swing on Southern<br />
Skies<br />
<strong>ESO</strong> Organisation Release 5/06 (18 July): Towards<br />
a European Extremely Large Telescope<br />
<strong>ESO</strong> Science Release 6/06 ( 1 July): Looking Deep<br />
with Infrared Eyes<br />
<strong>ESO</strong> Press Photo 7/06 ( 6 July): Island Universes<br />
with a Twist<br />
<strong>ESO</strong> Science Release 8/06 (3 August): A Sub-Stellar<br />
Jonah<br />
<strong>ESO</strong> Science Release 9/06 (4 August): The<br />
‘Planemo’ Twins<br />
<strong>ESO</strong> Science Release 30/06 (10 August): Stars Too<br />
Old to be Trusted?<br />
<strong>ESO</strong> Science Release 31/06 (17 August): Far Away<br />
Galaxy Under The Microscope<br />
<strong>ESO</strong> Organisation Release 3 /06 ( 4 August):<br />
Catherine Cesarsky elected President of the<br />
International Astronomical Union and Ian Corbett<br />
elected Assistant General Secretary<br />
<strong>ESO</strong> Science Release 33/06 (31 August): Long-<br />
lasting but Dim Brethren of Cosmic Flashes<br />
<strong>ESO</strong> Science Release 34/06 (1 September): A<br />
“Genetic Study” of the Galaxy<br />
<strong>ESO</strong> Science Release 35/06 ( 0 September): To Be<br />
or Not to Be: Is It All About Spinning?<br />
<strong>ESO</strong> Science Release 36/06 ( 8 September): Watch-<br />
ing How Planets Form<br />
<strong>ESO</strong> Science Release 37/06 ( October): Stellar<br />
Vampires Unmasked<br />
<strong>ESO</strong> Science Release 38/06 (4 October): Increasing<br />
the Odds of the Sweep<br />
<strong>ESO</strong> Science Release 39/06 (19 October): The Star,<br />
the Dwarf and the Planet<br />
<strong>ESO</strong> 40/06 ( October) - Organisation News: Ex-<br />
tremely Large Telescope Project Selected in<br />
ESFRI Roadmap<br />
<strong>ESO</strong> Science Release 41/06 (7 November): Cut from<br />
Different Cloth<br />
<strong>ESO</strong> Organisation News 4 /06 (1 November): Catch<br />
a Star!<br />
<strong>ESO</strong> Press Photo 43/06 (11 November): The Topsy-<br />
Turvy Galaxy<br />
<strong>ESO</strong> Science Release 44/06 (30 November): Asym-<br />
metric Ashes<br />
<strong>ESO</strong> Science Release 45/06 (6 December): Do<br />
Galaxies Follow Darwinian Evolution?<br />
<strong>ESO</strong> Organisation Release 46/06 (11 December):<br />
The Rise of a Giant<br />
<strong>ESO</strong> EIROforum Release 47/06 (14 December):<br />
Magna Carta for Researchers<br />
<strong>ESO</strong> Press Photo 48/06 ( 0 December): It Is Too<br />
Early To Be Santa’s Sleigh, Isn’t It?<br />
<strong>ESO</strong> Science Release 49/06 ( 0 December): The<br />
Dark Side of Nature: the Crime was Almost<br />
Perfect<br />
<strong>ESO</strong> Press Photo 50/06 ( 1 December): Portrait of a<br />
Dramatic Stellar Crib<br />
<strong>ESO</strong> Press Photo 51/06 ( December): Little<br />
Brother Joins the Large Family<br />
<strong>ESO</strong> Organisation Release 5 /06 ( December):<br />
Czech Republic to Become Member of <strong>ESO</strong><br />
<strong>ESO</strong> Press Photo 53/06 ( 4 December): Season’s<br />
Greetings!
The starburst galaxy NGC 908 (FORS/VLT).<br />
<strong>ESO</strong> Annual Report 006<br />
69
Relations with Chile<br />
The year 006 marked an important anniversary:<br />
a decade of the Supplementary<br />
Agreement between the Republic of Chile<br />
and <strong>ESO</strong>, which has allowed the successful<br />
installation of the VLT at Paranal<br />
and strengthened the cooperative<br />
relations between <strong>ESO</strong> and the Chilean<br />
scientific and local communities. To<br />
celebrate this, rectors of Chilean universities<br />
and representatives of the Chilean<br />
Ministry of Foreign Affairs gathered at the<br />
<strong>ESO</strong> offices in Santiago to launch a<br />
commemorative book, “10 Years Exploring<br />
the Universe”. This publication<br />
presented an external, independent overview<br />
of the broad impact of the <strong>ESO</strong>–<br />
Government of Chile Joint Committee,<br />
an annual fund for the development of<br />
astrophysics and scientific culture in the<br />
country, which was established by the<br />
Supplementary Agreement.<br />
In January 006, Dr. Michelle Bachelet<br />
became the first woman in the history of<br />
Chile to be elected President of the<br />
Republic. One of the first international<br />
events in which the new government<br />
participated was the opening of the 006<br />
International Air and Space Fair, held<br />
in Santiago in March. There, more than<br />
150 000 people visited the Space &<br />
Astronomy Pavilion, which presented realistic<br />
scale models of the VLT, ALMA<br />
and the E-ELT as well as a collection of<br />
most impressive astronomical pictures.<br />
The exhibition in the Pavilion was<br />
organised by <strong>ESO</strong> Santiago and the<br />
Planetario USACH.<br />
As a step forward in the well-established<br />
<strong>ESO</strong> astronomical outreach program-<br />
mes in Chile, a new strategic partnership<br />
was launched with the Chilean Ministry of<br />
Education to improve the teaching of<br />
astronomy in primary schools, within the<br />
framework of a national programme<br />
called “Science Education Based on Research”.<br />
<strong>ESO</strong> staff astronomers worked in<br />
collaboration with education specialists<br />
to design a learning module on basic<br />
astronomy, which is currently being<br />
tested by the Ministry of Education in pilot<br />
schools in Santiago and cities close<br />
to the observatory sites.<br />
70<br />
<strong>ESO</strong> Annual Report 006<br />
Another new initiative promoted by <strong>ESO</strong>,<br />
in a joint effort with the French Embassy<br />
in Chile, was the organisation of the first<br />
Cafés Scientifiques, in which adults and<br />
youngsters could freely ask questions of<br />
specialists while enjoying an informal café<br />
atmosphere. Inspirational issues like<br />
exoplanets and the possibility of life in the<br />
Universe attracted the interest of many in<br />
Santiago and Antofagasta.<br />
The Universidad Católica del Norte Astronomy<br />
Institute, in partnership with <strong>ESO</strong><br />
Vitacura, continued an extensive programme<br />
of public lectures and star parties<br />
in Antofagasta, Taltal and San Pedro<br />
de Atacama, the closest neighbours to<br />
Paranal and the ALMA site. Also in Chile’s<br />
Region II, <strong>ESO</strong> supported partial scholarships<br />
of 170 undergraduates studying<br />
at regional universities, in a joint programme<br />
with the Municipality of Taltal.<br />
Near La Silla, the educational agreement<br />
with the Municipality of La Higuera<br />
entered its second year of cooperative<br />
work to support local schools.<br />
<strong>ESO</strong> also played an active role in the<br />
Chilean National Science and Technology<br />
week, in partnership with the “Explora”<br />
Programme of CONICYT. Enthusiastic<br />
young students and teachers visited the<br />
<strong>ESO</strong> stand at the recently opened<br />
Biblioteca de Santiago, and more than<br />
300 schools received copies of a new<br />
documentary produced in-house about<br />
recent science highlights obtained at La<br />
Silla and Paranal.<br />
In the framework of ALMA, the regional<br />
fund financed by <strong>ESO</strong>, AUI and NAOJ<br />
supported several social and educational<br />
projects in San Pedro de Atacama and<br />
Toconao in 006. The only primary school<br />
in the village of San Pedro de Atacama<br />
has, in particular, increased its regular<br />
staff of teachers thanks to this fund.<br />
Besides this, ALMA is contributing to other<br />
areas of education and culture. A site<br />
museum located near the ALMA road was<br />
inaugurated in 006, in the presence<br />
of the Intendenta of Region II, the Mayor<br />
of San Pedro de Atacama, and members<br />
of the local communities. The site<br />
museum – in the form of a reconstruction<br />
of an abandoned estancia – provides<br />
physical evidence of the way of life of<br />
shepherds from the ancient Likan Antai<br />
culture. In order to support the understanding<br />
and protection of the archaeological<br />
heritage in the area, a book edited<br />
by <strong>ESO</strong>, “Footprints in the Desert”, was<br />
published and distributed among all<br />
schools of Region II, teachers, and regional<br />
authorities.<br />
In partnership with <strong>ESO</strong> and ALMA, the<br />
University of Antofagasta and University<br />
of Chile, in collaboration with the University<br />
of Copenhagen, launched a joint<br />
research programme on high-altitude<br />
medicine, taking advantage of the operations<br />
on the Chajnantor plateau at 5 050<br />
metres above sea level. For the very<br />
first time, scientists will have systematic,<br />
detailed statistics on the long-term<br />
reaction of the human body to regular<br />
commuting between sea level and<br />
high sites. This information will help to<br />
solve some intriguing, open questions of<br />
human physiology and high-altitude<br />
illness.<br />
Continuing our promotion of scientific<br />
interaction with the Chilean community,<br />
<strong>ESO</strong> held joint open houses with the<br />
Astronomy Department at the Pontificia<br />
Universidad Católica and Universidad de<br />
Chile with the participation of about 60<br />
young researchers in each of the events.<br />
<strong>ESO</strong> Santiago also sponsored the<br />
international conference on Globular<br />
Clusters organised by Universidad de<br />
Concepción in March, and the Fourth<br />
Advanced Chilean School of Astrophysics<br />
organised by the Pontificia Universidad<br />
Católica de Chile in December.<br />
Several delegations from Europe and all<br />
over the world were hosted in Santiago<br />
and the observatories, in particular three<br />
delegations from China, including that<br />
of the Vice-President of the Academy of<br />
Sciences. All scientific delegations gave<br />
informative seminars on science and<br />
technology in their countries.
Inaugurating the ALMA site museum.<br />
Launch of the “10 Years Exploring the Universe” book.<br />
<strong>ESO</strong> at the 006 International Air and Space Fair.<br />
<strong>ESO</strong> Annual Report 006<br />
71
European Affairs<br />
European Affairs at <strong>ESO</strong> is coordinated<br />
by the Public Affairs Department, but<br />
frequently involves several other departments<br />
within the organisation as well<br />
as external partners, notably the EIROforum.<br />
European Affairs focuses on EUrelated<br />
policy aspects of relevance to<br />
<strong>ESO</strong>. These can manifest themselves in<br />
many ways, which has increased the<br />
scope of <strong>ESO</strong>’s EU-related activities in recent<br />
years. This development is in line<br />
with the overall changes in Europe as<br />
European integration progresses. Hence,<br />
our activities are not necessarily limited<br />
to direct interaction with the primary institutions<br />
of the European Union, such as<br />
the European Commission and the European<br />
Parliament. The main conceptual<br />
frame within which this development<br />
follows is the European Research Area.<br />
The end of 006 marked the termina-<br />
tion of the EU Sixth R&D Framework<br />
Programme (FP6) and the new Seventh<br />
Framework Programme (FP7) was<br />
launched at the beginning of 007.<br />
<strong>ESO</strong>’s FP6 participation can be judged as<br />
very positive and successful, both because<br />
it has allowed us to carry out projects<br />
that could not have been funded<br />
otherwise, and as a vehicle for a more<br />
general interaction with the EU at a time<br />
when the Union is emerging as a new,<br />
but potentially important actor in the field<br />
of setting European science policy. In<br />
this sense, the activities deserve continuation<br />
in the context of FP7. Currently<br />
<strong>ESO</strong> still has 11 running FP6 projects,<br />
most of which will terminate in 008.<br />
From the running FP6 projects the E-ELT<br />
preparatory-phase, the ESTI project<br />
and the VO project are already aiming for<br />
continuation in FP7.<br />
Obviously, the preparation of the Seventh<br />
Framework Programme played an important<br />
role in 006. From <strong>ESO</strong>’s perspective,<br />
the challenge has been to be able to<br />
deal with the first FP7 calls, which were<br />
launched by the Commission in December<br />
006. The complications of this were<br />
linked to the preceding legislative process,<br />
which meant that many important<br />
details still remained unclear by the end<br />
of the year. Other issues were not subject<br />
to the direct political process, but nonetheless<br />
remained important. This was the<br />
case for the E-ELT project, which became<br />
7<br />
<strong>ESO</strong> Annual Report 006<br />
included in the so-called ESFRI-list that<br />
was published by the European Strate-<br />
gy Forum for Research Infrastructures<br />
(ESFRI) in October 006. The ESFRI-list<br />
is a ‘road-map’ describing 35 major research<br />
infrastructure projects that are<br />
deemed to be “Research Infrastructures<br />
of European interest” (from the Competitiveness<br />
Council Conclusions, 5– 6<br />
November 004), and thus pre-qualify for<br />
potential co-funding, however limited,<br />
from the Seventh Framework Programme.<br />
Furthermore, EU member states were<br />
encouraged to develop national roadmaps<br />
that are aligned with the ESFRI-list,<br />
in order to determine funding priorities.<br />
ESFRI was tasked with developing a longterm<br />
European view of the development<br />
of Research Infrastructures of pan-European<br />
interest, covering a wide range of<br />
sciences. In the meantime, another activity<br />
took place, focusing on Astronomy and<br />
Space Sciences. This occurred under<br />
the auspices of ASTRONET (http://www.<br />
astronet-eu.org/), a network comprising<br />
<strong>ESO</strong> Council member Jean-Pierre Swings at the Walloon Space Days.<br />
national funding agencies and <strong>ESO</strong> (with<br />
ESA as an observer), which was set up<br />
under the FP6 ERA-net scheme. <strong>ESO</strong>’s<br />
main responsibility in the ASTRO-NET<br />
programme is to coordinate the development<br />
of a common Science Vision for<br />
European Astronomy in the next 0<br />
years, with NWO in charge of collating<br />
the scientific content from the community.<br />
To prepare for this development and<br />
the follow-up construction in 007– 008<br />
of a prioritised Infrastructure Roadmap<br />
under the responsibility of PPARC, a<br />
web-based census tool has been<br />
developed by <strong>ESO</strong>. It currently contains<br />
all available European national prospectives<br />
and a comprehensive list of existing<br />
and planned medium- to large-scale<br />
infrastructures. The activity picked up<br />
much momentum in the autumn of 006<br />
with the preparation for a dedicated<br />
symposium scheduled to take place<br />
towards the end of January 007 in<br />
Poitiers to discuss and refine the draft<br />
Science Vision released by NWO by<br />
mid-December 006.
As mentioned, <strong>ESO</strong>’s European Affairs activities<br />
are linked to basic policy changes<br />
in Europe that have a bearing on many<br />
parts of society. Since these changes are<br />
a result of constant negotiation between<br />
stakeholders at the European and national<br />
levels, our activities must also be of<br />
a broad nature and involve contacts with<br />
decision-takers beyond the EU system.<br />
Thus, on 15 March, <strong>ESO</strong> was pleased to<br />
host the Education Committee of the<br />
Finnish Parliament, an event which created<br />
a fine opportunity for dialogue<br />
between <strong>ESO</strong> and national policy-makers<br />
as well as a chance to present <strong>ESO</strong>’s future<br />
plans. Further visits by diplomatic<br />
representatives of the UK and Switzerland<br />
occurred in the spring. On 8– 9 March,<br />
<strong>ESO</strong> played a major role in the First<br />
Walloon Space Days, organised by the<br />
Walloon Space Cluster and intended<br />
to become a recurring event focusing on<br />
technologies for astronomy and space sciences,<br />
including R&D policy issues. The<br />
event coincided with the delivery of the<br />
fourth Auxiliary Telescope for the VLTI<br />
and provided a forum for European<br />
companies to meet with <strong>ESO</strong> experts.<br />
Visit by the Education Committee of the Finnish<br />
Parliament.<br />
In November, we welcomed to Paranal<br />
a high-ranking delegation from the Academy<br />
of Sciences of the Czech Republic<br />
(CAS), led by its President, Václav Pačes,<br />
and Jan Palouš, responsible for international<br />
relations of the CAS. The visit was<br />
related to the negotiations regarding the<br />
Czech Republic’s membership of <strong>ESO</strong>.<br />
In December these negotiations were<br />
successfully concluded with the approval<br />
both of the <strong>ESO</strong> Council and the Czech<br />
government, paving the way for the signing<br />
of the agreement on December<br />
and enabling the parliamentary ratification<br />
procedure to be initiated. Whilst a<br />
Czech accession to the <strong>ESO</strong> Convention<br />
is not in itself of formal institutional EU<br />
relevance, it may open possibilities with<br />
respect to EU funding for national Czech<br />
activities that follow in the wake of the<br />
membership – illustrating the complexities,<br />
but also the importance, of <strong>ESO</strong>’s<br />
European Affairs activities.<br />
Finally, within the EIROforum partnership,<br />
three events deserve particular men-<br />
tion. On 15 November, a brainstorming<br />
session was organised between the<br />
EIROforum Directors General and key<br />
Commission officials to discuss long-<br />
term perspectives for the European Research<br />
Area.<br />
On November, EIROforum organised a<br />
‘Breakfast Event’ at the European Parliament<br />
on the topic “Fostering Scientific<br />
Understanding Among Young People –<br />
Reinforcing scientific education initiatives<br />
in Europe”. The event was hosted by<br />
Prof. Jerzy Buzek MEP, and attended by<br />
more than 10 MEPs and a further 0 people<br />
from the European Parliament.<br />
On 13 December, a get-together was organised<br />
between senior staff from the<br />
EIROforum partner organisations and research<br />
attachés of the permanent representations<br />
of the EU member states.<br />
The topic for discussion was how to<br />
achieve synergies between the activities<br />
of the intergovernmental research organisations<br />
and the EU-based actions as<br />
conducted through the Framework Programme.<br />
In 006, the Research Directorate General<br />
of the Commission established a<br />
dedicated unit to facilitate contacts with<br />
the European Intergovernmental Research<br />
Organisations. This is clearly an<br />
expression of the intensification of<br />
the interactions between the EC and the<br />
EIROforum in relation to both project<br />
funding and policy-related interactions.<br />
Delegation from the Czech Academy of Science visits Paranal.<br />
<strong>ESO</strong> Annual Report 006<br />
73
The <strong>ESO</strong> Council in session on 6 December 006.
Council<br />
The Council is <strong>ESO</strong>’s ruling body, which<br />
delegates day-to-day responsibility to<br />
the Executive under <strong>ESO</strong>’s Director General.<br />
In 006, Council held two ordinary<br />
meetings, both in Garching. Committee<br />
of Council met three times, in February in<br />
Berne, Switzerland, in September in Santiago,<br />
Chile, and in October in Munich.<br />
The President of Council, Prof. Richard<br />
Wade, chaired all the meetings.<br />
In 006, Council approved the extension<br />
of the agreement for APEX until 01 , the<br />
agreements for the instrument SPHERE,<br />
and the agreement for a fourth star-separator<br />
for the VLT, including the proposed<br />
guaranteed observing time, in accordance<br />
with the standing rules.<br />
Council received the usual VLT/VLTI, Instrumentation<br />
and ALMA biannual reports,<br />
and the reports from the Chairs of<br />
the Finance Committee, the Scientific<br />
Technical Committee, and Observing Programmes<br />
Committee. Council also endorsed<br />
the document “<strong>ESO</strong> Medium<br />
Range Implementation Plan, 006– 010”<br />
and examined the document “<strong>ESO</strong> Future<br />
Perspectives, 006– 03 ”.<br />
In December, Council adopted a resolution<br />
authorising the move of the E-ELT<br />
project, based on the innovative five-mirror<br />
design, to Phase B (detailed design)<br />
and requested the Executive to provide a<br />
detailed work plan by early 007.<br />
Council had been kept informed about<br />
the developments in the negotiations with<br />
the Czech Republic, and at its meeting<br />
in December adopted the necessary resolutions<br />
on the accession of the Czech<br />
Republic to <strong>ESO</strong> as the 13th member<br />
state from 1 January 007.<br />
The issue of a new Headquarters building<br />
in Garching was still of concern. However,<br />
progress in obtaining the necessary land<br />
could be reported, and Council agreed to<br />
give the Executive freedom to pursue the<br />
most cost-effective solution, including the<br />
option of purchasing the land.<br />
76<br />
<strong>ESO</strong> Annual Report 006<br />
Council dealt with various other issues<br />
and approved the schedule and terms of<br />
reference for the visiting committee.<br />
The visiting committee will come to the<br />
sites in Chile and the Headquarters<br />
in Garching in early 007. New terms of<br />
reference for the Finance Committee<br />
were also approved and the working<br />
group which had been chaired by Dr. Finn<br />
Karlsson was discharged. Council agreed<br />
on a new remit and membership of<br />
the Scientific Strategy Working Group.<br />
The Working Group will meet again in<br />
early 007.<br />
At the meeting in December, Prof.<br />
Richard Wade was re-elected President<br />
of Council for 007 and Dr. Monnik<br />
Desmeth was re-elected Vice-President.<br />
Ms. Rowena Sirey was re-appointed<br />
Chair of the Finance Committee for 007.<br />
Dr. Simon Morris was appointed Chair<br />
of the Observing Programmes Committee<br />
for 007 and Dr. Svetlana Berdyugina<br />
was appointed Vice-Chair.<br />
Dr. Monnik Desmeth was appointed Assessor<br />
to the ALMA Board for 007.<br />
The President of Council and the Director<br />
General are members ex officio.<br />
Council set up an ELT Standing Review<br />
Committee and appointed Prof. Roger<br />
Davies as its Chair. This Committee met<br />
twice in 006 and subsequently reported<br />
to Council.<br />
The Scientific Strategy Working Group<br />
met twice during 006. In January it<br />
met with three representatives of the<br />
European Square Kilometre Array (SKA)<br />
Consortium and the initial findings<br />
were reported on at the meeting of Committee<br />
of Council in February. The working<br />
group met again in April and presented<br />
an interim report to the Council at<br />
its meeting in June. Council requested<br />
the working group to elaborate on some<br />
of the scenarios included in the interim<br />
report and to look into related European<br />
Union issues. In addition, it was decided<br />
to organise a meeting of the Council<br />
members representing the funding agencies.<br />
Council and Committee of Council<br />
2006<br />
President Richard Wade<br />
Belgium Monnik Desmeth<br />
Jean-Pierre Swings<br />
Denmark Jens Viggo Clausen<br />
Henrik Grage<br />
Finland Kalevi Mattila<br />
Pentti Pulkkinen<br />
France Philippe Barré<br />
(until November 006)<br />
Julien Galabru<br />
(as of November 006)<br />
Laurent Vigroux<br />
Germany Ralf Bender<br />
Andreas Drechsler<br />
Italy Vicenzo Dovì<br />
Bruno Marano<br />
The Netherlands P. Tim De Zeeuw<br />
(until September 006)<br />
Piet C. van der Kruit<br />
(as of September 006)<br />
Jan A. C. van de Donk<br />
Portugal Fernando Bello<br />
Teresa Lago<br />
Sweden Claes Fransson<br />
Finn Karlsson<br />
Switzerland Michel Mayor<br />
Martin Steinacher<br />
United Kingdom Gerry Gilmore<br />
Rowena Sirey<br />
The <strong>ESO</strong> Tripartite Group, chaired by Dr.<br />
Ugo Sessi, met in Garching in April and in<br />
October. The issue of the CERN Pension<br />
Fund continued to be a very important<br />
topic. Among the other discussion points<br />
were the changes to the regulations regarding<br />
cost-of-living adjustment, expatriation<br />
allowance, and regarding family/<br />
spouse and related leave. The Tripartite<br />
Group received information concerning<br />
the and the collective bargaining for local<br />
staff in Chile.
The Scientific Technical Committee<br />
The Scientific Technical Committee<br />
2006<br />
José Afonso (P)<br />
Willy Benz (CH)<br />
Joris Blommaert (B)<br />
Jean-Gabriel Cuby (F)<br />
Raffaele Gratton (I)<br />
Lauri Haikala (FIN)<br />
Thomas Michael Herbst (D)<br />
Richard Hills (UK)<br />
Hans Kjeldsen (DK)<br />
Yannick Mellier (F)<br />
Dante Minniti (RCH)<br />
Goran Olofsson (SE)<br />
Patrick Roche (UK)<br />
(Chair for first meeting in 006)<br />
Linda Tacconi (D)<br />
(Chair as of second meeting in 006)<br />
Leonardo Testi (I)<br />
Huib Jan van Langevelde (NL)<br />
Dr. Artemio Herrero participated in the<br />
meetings as the representative of Spain,<br />
first as an observer, and then as the<br />
interim Spanish member of the committee.<br />
Due to personal reasons, Dr. Ikka<br />
Tuominen resigned from the committee<br />
and in the interim was replaced by<br />
Dr. Juhani Huovelin.<br />
006 was an extremely busy year for the<br />
Scientific Technical Committee (STC), in<br />
particular in relation to the European Extremely<br />
Large Telescope (E-ELT). In addition<br />
to the two regular meetings (6 nd<br />
and 64th) in April and October, STC met<br />
for two extra one-day sessions in May<br />
and November. In order to cope with the<br />
wide range of technical projects currently<br />
going on at <strong>ESO</strong>, STC appointed two<br />
additional sub-panels which, in addition<br />
to members of the committee, incorporate<br />
experts from the community. These<br />
are the ELT Science and Engineering<br />
(ESE) sub-panel and the Very Large Telescope<br />
Interferometer (VLTI) sub-panel.<br />
Together with the ALMA European Science<br />
Advisory Committee (ESAC), these<br />
three panels advise STC in all matters<br />
related to these important components of<br />
the <strong>ESO</strong> programme.<br />
STC 62nd Meeting<br />
At its 61st meeting, STC had encouraged<br />
<strong>ESO</strong> to explore ways of achieving the<br />
goal of a large, deep, multi-colour survey,<br />
which would be substantially deeper than<br />
the multipurpose Sloan Digital Sky Survey<br />
whilst also tackling the nature of dark<br />
energy. A detailed report about achieving<br />
this goal with the two VLT survey telescopes<br />
(VST and VISTA) was presented<br />
at the 6 nd meeting that took place on<br />
6 and 7 April. Recognising that VST and<br />
VISTA have the potential to play a leading<br />
role in investigating some of the major<br />
current astronomical questions such as<br />
the nature of dark energy, STC encouraged<br />
the Director General to find ways of<br />
maximising the fraction of time that these<br />
telescopes will dedicate to public surveys.<br />
In particular, STC suggested that<br />
the OPC should award only up to 15 % of<br />
the available <strong>ESO</strong> time with these telescopes<br />
to PI projects (down from the<br />
5 % foreseen originally), and that this<br />
fraction should be considered in scientific<br />
competition with the public surveys<br />
such that any unallocated time should be<br />
returned to public surveys.<br />
A full report by the Director of the La Silla<br />
Paranal Observatory on the activities of<br />
the Interferometry Task Force (ITF) was<br />
presented at the meeting. STC was “enormously<br />
impressed by the heroic efforts”<br />
of the ITF that found solutions to many of<br />
the issues which were limiting the performance<br />
of the VLTI. STC congratulated<br />
ITF and Paranal for these achievements,<br />
and in particular for demonstrating fringe<br />
tracking with FINITO and the Auxiliary<br />
Telescopes.<br />
Following the recommendations at the<br />
60th meeting of STC, proposals for<br />
Phase A studies for three second-generation<br />
VLTI instruments were presented<br />
to the committee: MATISSE, VSI (a merging<br />
of VITRUV and BOBCAT), and GRAVI-<br />
TY. Reassured by the progress in understanding<br />
the performance of the VLTI<br />
infrastructure reported at the meeting,<br />
STC made the following recommendations<br />
regarding second-generation VLTI<br />
instruments:<br />
1. The three consortia should proceed<br />
with Phase A studies for secondgeneration<br />
instruments.<br />
. <strong>ESO</strong> should issue a draft Interface<br />
Control Document (ICD) reflecting the<br />
current state of knowledge of the<br />
VLTI system, which should be updated<br />
during these Phase A studies as ITF<br />
further defines the VLTI performance.<br />
3. Phase A studies should proceed<br />
on timescales consistent with the ITF<br />
investigations. At the end of these<br />
studies, and following the review of the<br />
Phase A instrument studies, a new<br />
definition of the VLTI mission and a new<br />
ICD will be put in place.<br />
Extraordinary STC 63rd meeting<br />
Another STC meeting took place on<br />
11 May. The need for this extraordinary<br />
meeting was dictated by the fast pace<br />
of the E-ELT project established by Coun-<br />
cil in December 005. Extensive reports<br />
by the five ELT working groups and by<br />
the Core ELT Science and Engineering<br />
(Core-ESE) working group were presented<br />
at the meeting. STC welcomed<br />
these reports and congratulated the<br />
committees for the “admirable job of investigating<br />
potential telescope design<br />
and adaptive optics solutions”. STC recommended<br />
to develop an operational<br />
model for the E-ELT, which will inform<br />
telescope and instrument design options.<br />
The committee also recommended that<br />
the highest priority of the ESE should be<br />
to define, together with <strong>ESO</strong> and the community,<br />
“the key science and technology<br />
that Europe will want to pursue”. STC emphasised<br />
that the combination of the<br />
E-ELT and the VLT will be unparalleled in<br />
the world, and recommended <strong>ESO</strong> to devote<br />
a significant effort to identify the<br />
science cases that would uniquely utilise<br />
both the E-ELT and the VLT.<br />
A very important item of the agenda was<br />
the nomination of the ESE committee<br />
that would take over from the Core-ESE<br />
as a sub-panel advising STC in all matters<br />
related to the E-ELT project. The STC<br />
endorsed <strong>ESO</strong>’s proposal that the<br />
members of the Core-ESE continue to<br />
serve in the ESE, and thus formally<br />
nominated Daniel Enard (France), Roland<br />
Gredel (Germany), Colin Cunningham<br />
(UK), Gerard Rousset (France), Marijn<br />
Franx (the Netherlands), and Isobel Hook<br />
<strong>ESO</strong> Annual Report 006<br />
77
(UK) as members of the ESE. As STC<br />
members of the ESE, STC nominated<br />
Jean-Gabriel Cuby (France), Raffaele<br />
Gratton (Italy), Thomas Herbst (Germany),<br />
and Göran Olofsson (Sweden). To<br />
complete the committee, STC proposed<br />
names of experienced astronomers<br />
from the community at large. STC also<br />
appointed Daniel Enard as Chair and<br />
Thomas Herbst as co-Chair.<br />
STC 64th meeting<br />
<strong>ESO</strong> received a partnership offer to participate<br />
in the Large Synoptic Survey<br />
Telescope (LSST) project, which was presented<br />
to STC for advice at its 64th meeting<br />
on 3 and 4 October. While STC<br />
recognised the enormous scientific potential<br />
of LSST, it also recognised that<br />
the financial impact of such partnership<br />
would stress <strong>ESO</strong>, given the on-going<br />
developments for the E-ELT, ALMA, VLTI,<br />
and the VLT. Therefore STC recommended<br />
the creation of a small working<br />
group of <strong>ESO</strong> and STC members to<br />
further explore and identify viable options<br />
for an <strong>ESO</strong> LSST collaboration, and indicated<br />
the terms of reference for this<br />
group. STC proposed Yannick Mellier and<br />
Artemio Herrero as members of the<br />
group with Dante Minniti as an alternative.<br />
For <strong>ESO</strong> the members are Bruno Leibundgut<br />
and Paolo Padovani.<br />
Following a presentation of the status of<br />
the APEX project, and the request of the<br />
partners to extend the APEX agreement<br />
until the end of 01 , STC, encouraged<br />
by the recent progress on commissioning<br />
APEX instruments, and recognising the<br />
potential unique nature of this facility<br />
in the Southern Hemisphere, unanimous-<br />
ly agreed that <strong>ESO</strong> should extend the<br />
APEX agreement as proposed. STC also<br />
strongly supported the development and<br />
expansion of APEX/ALMA synergies,<br />
and in particular, the development of surveys<br />
using the APEX instruments to provide<br />
targets for ALMA (as well as for the<br />
VLT and even the E-ELT).<br />
78<br />
<strong>ESO</strong> Annual Report 006<br />
The STC endorsed the ESAC recommendations<br />
concerning the enhanced capabilities<br />
for Early Science operations of<br />
ALMA, and the optimisation of the time<br />
allocation process by having a single<br />
international Time Allocation Committee.<br />
The ESAC also recommended names<br />
to replace two of its members whose<br />
terms expire at the end of 006 and early<br />
007. STC also recommended that, given<br />
their expertise in sub-millimetric systems,<br />
the ESAC should also be the forum where<br />
APEX matters could be discussed.<br />
Concerning the E-ELT development, STC<br />
fully endorsed the recommendations of<br />
the ESE concerning the importance of retaining<br />
nine science cases for the Design<br />
Reference Mission (DRM) and that three<br />
demonstrator science cases be selected<br />
in the early evaluation by <strong>ESO</strong>. The ESE<br />
also made a number of technical and organisational<br />
recommendations including<br />
a request for a detailed plan for instrument<br />
development and selection, and an<br />
organisation chart of the E-ELT effort<br />
within <strong>ESO</strong>. The ESE lauded the efforts of<br />
the E-ELT Project Office in rapidly advancing<br />
in the study of both the five-mirror<br />
and the Gregorian optical designs,<br />
and recommended that the project office<br />
continue contacts to understand the<br />
potential of segmented secondaries.<br />
The VLTI sub-committee met for the first<br />
time in September 006. While recognising<br />
the progress made in some areas,<br />
especially by the ITF, and that the resources<br />
required for VLTI are both adequate<br />
and necessary, the sub-panel<br />
recommended that the ITF be maintained<br />
and even strengthened with the addition<br />
of one or two persons. The sub-panel<br />
considered that the development of an<br />
AMBER data reduction package within<br />
the framework of the SAMPO project<br />
in the Data Management Division (DMD)<br />
is an asset to the VLTI that should be extended<br />
to all VLTI instruments. The members<br />
of the sub-committee were impressed<br />
by the progress on PRIMA and,<br />
while recognising that PRIMA is well<br />
on track, recommended that the project<br />
establishes contacts with the VLBI community<br />
since they have experience in<br />
solving similar technical problems. These<br />
and other technical recommendations<br />
made by the sub-panel were endorsed by<br />
STC, especially the recommendation of<br />
maintaining the ITF effort.<br />
Extraordinary STC 65th meeting<br />
Developments of the E-ELT and their related<br />
impact on <strong>ESO</strong>’s Medium Range<br />
Implementation Plan (MRIP) prompted a<br />
special meeting of the STC, on 3 November,<br />
to discuss these developments<br />
and make related recommendations<br />
prior to the December meeting of Council.<br />
Noting that the highest priority components<br />
of the <strong>ESO</strong> programme, and especially<br />
the Phase B of the E-ELT project,<br />
are included in the document, STC endorsed<br />
the MRIP presented by <strong>ESO</strong>. It<br />
took note of the fact that the MRIP does<br />
not include initiatives for a next-generation<br />
deep-sky survey. STC also discussed<br />
the document on Long Term Perspectives<br />
(LTP) and noted that it does not include<br />
funding for the La Silla Observatory<br />
beyond 010, indicating that the scientific<br />
impact of this will be evaluated in 007.<br />
STC emphasised the requirement to<br />
deliver the E-ELT on a competitive timescale,<br />
and encouraged Council to seek<br />
extra funds to make this a reality. STC<br />
reaffirmed that the scientific importance<br />
of the VLT and ALMA will not wane in<br />
the era of the E-ELT, and stressed that it<br />
will be critical to maintain these facilities<br />
as world-class even then.<br />
At the meeting, the E-ELT Project Office<br />
presented STC with comprehensive information<br />
on the E-ELT Basic Reference<br />
Design, including a detailed analysis of<br />
the pros and cons of the Gregorian and<br />
five-mirror designs. On the basis of the<br />
evidence acquired from within <strong>ESO</strong> and<br />
from industry so far, STC was convinced<br />
that there are no showstoppers for the
five-mirror option, which they considered<br />
would be the most ambitious project<br />
that <strong>ESO</strong> had thus far endeavoured to<br />
undertake.<br />
The ESE held a special meeting after the<br />
E-ELT conference in Marseille, France,<br />
during which it essentially confirmed the<br />
statements made by STC. In particular,<br />
the ESE considered that a 4 -m aperture<br />
is a good balance between very ambitious<br />
scientific goals, risks, cost, and<br />
schedule, and recommended to adopt<br />
the nominal 4 -m aperture for the E-ELT.<br />
Considering that the Gregorian design<br />
bears as a single high-risk item the large<br />
secondary mirror, for which there is no<br />
mitigation, the ESE recommended that<br />
<strong>ESO</strong> and its governing bodies adopt the<br />
4 -m five-mirror concept as the E-ELT<br />
project baseline and that the project proceeds<br />
to Phase B as soon as possible.<br />
STC fully endorsed the recommendations<br />
of the ESE.<br />
A report on the status of the VST was<br />
presented at the meeting. Gianpaolo<br />
Vettolani, representing INAF, assured STC<br />
that INAF was working together with<br />
<strong>ESO</strong> to enable as quickly as possible the<br />
start of scientific operations of VST on<br />
Paranal. STC recommended that <strong>ESO</strong> engage<br />
fully in the critical design review<br />
of the primary and secondary mirror supports<br />
that will take place in early 007,<br />
and requested that STC be represented<br />
at the review. Noting that the delay in VST<br />
is impacting key components of <strong>ESO</strong>’s<br />
scientific programme, and that completion<br />
of the project is very urgent, STC<br />
urged <strong>ESO</strong> to start immediately a study<br />
of alternative plans or possible back-up<br />
solutions.<br />
Finally, STC endorsed the recommendation<br />
of ESAC concerning the implementation<br />
of a sub-reflector tilt capability for<br />
the European ALMA antennas, noting this<br />
enhancement is a cost-effective means<br />
to regain some of the sensitivity lost by<br />
descoping the project to 50 antennas.<br />
NGC 5917, the ‘Hooked’ Galaxy and its companion<br />
(FORS/VLT).<br />
<strong>ESO</strong> Annual Report 006<br />
79
Finance Committee<br />
80<br />
Finance Committee<br />
2006<br />
Chair Rowena Sirey<br />
Belgium Alain Heyen<br />
Denmark Cecilie Tornøe<br />
Finland Jaana Aalto<br />
France Patricia Laplaud<br />
Germany Marlene Lohkamp-<br />
Himmighofen<br />
Italy Ugo Sessi<br />
The Netherlands Coen J. van Riel<br />
Portugal Fernando Bello<br />
Sweden Sofie Björling<br />
Switzerland Jean-Pierre Ruder<br />
United Kingdom Colin Vincent<br />
In 006 the Finance Committee held two<br />
ordinary meetings. It met in addition<br />
twice in extraordinary sessions. All the<br />
meetings were chaired by Ms. Rowena<br />
Sirey and took place in Garching.<br />
The committee dealt with various financial<br />
issues (annual accounts, budget,<br />
cash-flow situation, financial projections,<br />
member state contributions) and with<br />
personnel issues concerning international<br />
as well as local staff. These subjects were<br />
discussed in detail and recommendations<br />
were made to Council.<br />
Finance Committee approved the awarding<br />
of 15 contracts exceeding 300 000 €<br />
and 31 single-source procurements exceeding<br />
150 000 €. Conditions governing<br />
forthcoming ALMA production contracts<br />
were also approved and information was<br />
received concerning procurement statistics,<br />
forthcoming calls for tenders and<br />
price inquiries.<br />
A major item was the approval of a contract<br />
for the construction of the technical<br />
facilities at the Operation Support Facility<br />
(OSF) site of the ALMA Observatory in<br />
Chile.<br />
The committee received regular progress<br />
reports on the implementation of the ERP<br />
system, and appreciated the outcome of<br />
the external ERP review.<br />
<strong>ESO</strong> Annual Report 006<br />
The Users’ Committee<br />
The Users’ Committee<br />
2006<br />
Belgium Griet Van de Steene<br />
Denmark Uffe Gråe Jørgensen<br />
Finland Merja Tornikoski<br />
France Pascale Jablonka<br />
(Chairwoman)<br />
Germany Jochen Heidt<br />
Italy Bianca Maria Poggianti<br />
The Netherlands Walter Jaffe<br />
Portugal Nuno Cardoso Santos<br />
Sweden Sofia Feltzing<br />
Vice-Chairwoman)<br />
Switzerland Fréderic Courbin<br />
United Kingdom Malcolm Bremer<br />
Chile Wolfgang Gieren<br />
The Users’ Committee (UC) held its annual<br />
meeting on 3 and 4 April. The meeting<br />
was chaired by Pascale Jablonka.<br />
Representatives from <strong>ESO</strong> gave presentations<br />
to the Committee about the<br />
La Silla Paranal Observatory, ALMA, the<br />
proposal submission and time allocation<br />
processes and the revised OPC procedures,<br />
the forthcoming User Portal,<br />
and the SAMPO project for data reduction.<br />
The UC in turn provided feedback<br />
from the users on the usage of <strong>ESO</strong> facilities,<br />
based in part on the outcome of<br />
a survey designed and distributed by the<br />
Committee. The level of satisfaction of the<br />
users with respect to observations carried<br />
out both at the La Silla and Paranal<br />
sites is in general high. Most of the expressed<br />
concerns are related to the diffusion<br />
of information from <strong>ESO</strong> to its<br />
community, in particular about the current<br />
and future status of available instrumentation,<br />
and to the transparency of<br />
the OPC processes. This is reflected in<br />
a number of action items and recommendations<br />
assigned by the UC to <strong>ESO</strong> following<br />
the open and constructive discussion<br />
of these topics. The number of such<br />
action items and recommendations from<br />
005 that could be closed at the 006<br />
meeting, or on which significant progress<br />
had been achieved following corresponding<br />
action by <strong>ESO</strong>, is a testimony to efficiency<br />
of the UC process for improvement<br />
of <strong>ESO</strong>’s service to its user<br />
community in the direction expected by<br />
the latter.<br />
As usual, half a day was devoted to a<br />
‘special topic’, this time the VLT secondgeneration<br />
instruments. Given the nature<br />
of this topic, exceptionally, no frequent<br />
users were invited to contribute. Instead,<br />
presentations were given by <strong>ESO</strong> representatives,<br />
starting with an overview of<br />
the instrumentation under development,<br />
followed by specific talks on the individual<br />
instruments HAWK-I, X-Shooter, KMOS,<br />
MUSE and SPHERE. The subsequent discussion<br />
featured a first exchange of views<br />
about possible additional candidates<br />
for developments to start around 010.<br />
Finally, <strong>ESO</strong> presented a report on the<br />
status of the E-ELT project.<br />
The globular cluster 47Tuc (FORS/VLT).
<strong>ESO</strong> Annual Report 006<br />
81
The Observing Programmes Committee<br />
8<br />
The Observing Programmes Committee<br />
2006<br />
Xavier Barcons<br />
Svetlana Berdyugina (Period 79)<br />
Eric F. Bell<br />
Hermann Böhnhardt<br />
Sven de Rijcke<br />
Hans de Ruiter<br />
Gösta Gahm (Period 79)<br />
Martin Groenewegen (Period78)<br />
Michiel Hogerheijde<br />
Jari Kotilainen<br />
Donald W. Kurtz (Period 79)<br />
Rafael Rebolo Lopez (Period 78)<br />
André Moitinho de Almeida (Vice-chairman)<br />
Simon Morris<br />
Tom Richtler<br />
Daniel Rouan (Period 78)<br />
María Teresa Ruíz (Period 78)<br />
Monica Tosi<br />
Lutz Wisotzki (Chairman)<br />
Sebastian Wolf (Period 79)<br />
In 006, the Observing Programmes<br />
Committee (OPC) held its two annual<br />
meetings in May/June and in November.<br />
While the number of proposals received<br />
for Observing Period 78 (P78: 1 Octo-<br />
ber 006 to 31 March 007), at 8 7, was<br />
somewhat lower than in recent periods,<br />
a new all-time record was hit for Observing<br />
Period 79 (P79: 1 April to 30 September<br />
007), with the submission of 913<br />
proposals. This corresponds primarily<br />
to an increased demand in the ‘Galactic’<br />
scientific areas: interstellar medium, star<br />
formation and planetary systems (OPC<br />
category C ), and stellar evolution (OPC<br />
category D). Indeed, since the introduction<br />
of the current OPC categories for<br />
Period 66 (starting in October 000), the<br />
number of proposals submitted in<br />
categories C and D has nearly doubled,<br />
while this number has remained approximately<br />
constant for the ‘extragalactic’<br />
proposals of categories A (cosmology)<br />
and B (galaxies and galactic nuclei).<br />
In Period 78, the ratio between the requested<br />
time and the available time (the<br />
‘pressure factor’) has risen above 6 on<br />
some of the Unit Telescopes (Antu and<br />
Kueyen) for the first time since the start of<br />
science operations of the VLT in April<br />
1999, while demand for the La Silla telescopes<br />
has decreased by about 10 %<br />
from 005 to 006. The workhorse instrument<br />
FORS , which has been in operation<br />
since early 000, remains extremely<br />
popular: the amount of time that is re-<br />
<strong>ESO</strong> Annual Report 006<br />
quested on it is considerably higher than<br />
on any other VLT instruments. Most<br />
of the latter experience similar demand,<br />
within about 0 % of one another. The<br />
only exception is VISIR: the significantly<br />
lower demand on this instrument can<br />
be attributed to the specific nature of<br />
the science for which it is designed. The<br />
last first-generation VLT instrument,<br />
CRIRES, which was offered to the community<br />
for the first time in Period 79,<br />
was immediately on a par with more established<br />
instruments in terms of the<br />
amount of requested time. Visitor Instruments<br />
were also scheduled at the VLT<br />
in both P78 (DAZLE on Melipal) and P79<br />
(ULTRACAM on Melipal and DAZLE on<br />
Yepun).<br />
As in P75 and P77, joint telescope time<br />
applications for coordinated observations<br />
with the VLT and with the XMM-Newton<br />
X-ray observatory have been invited in<br />
P79. These proposals fall within the framework<br />
of an agreement between <strong>ESO</strong><br />
and ESA for a joint telescope time application<br />
scheme, which aims to take full<br />
advantage of the complementary nature<br />
of ground-based and space-borne observing<br />
facilities. Of the four joint applications<br />
evaluated by <strong>ESO</strong>’s OPC in P79,<br />
one was allocated time on both the VLT<br />
and XMM-Newton telescopes; one of<br />
the nine proposals evaluated by the XMM<br />
Time Allocation Committee was also successful.<br />
In 006, the field of gamma-ray bursts<br />
(GRBs) continued to account for about<br />
half of the successful Target of Opportunity<br />
(ToO) proposals. A large fraction of<br />
the GRB proposals make use of the<br />
Rapid Response Mode (RRM) of the VLT,<br />
with which observation of a transient<br />
event can be automatically started within<br />
minutes of its triggering. The unique<br />
performance of the VLT in this mode,<br />
combined with <strong>ESO</strong>’s policy to allow it to<br />
override both Visitor and Service Mode<br />
observations, have positioned the VLT<br />
and the GRB community of the <strong>ESO</strong><br />
member states at the forefront of this<br />
field of research. We further support the<br />
optimisation of the scientific return of the<br />
GRB programmes carried out at its<br />
observatory sites by inviting the Principal<br />
Investigators (PIs) of the successful<br />
GRB proposals to observational strategy<br />
meetings in Garching twice a year.<br />
Large Programmes<br />
Large Programmes (LPs) are projects requiring<br />
more than 100 hours of observing<br />
time per year over no more than two<br />
years, and that have the potential to lead<br />
to a major advance or breakthrough in<br />
the considered field of study. In P78, the<br />
OPC evaluated 0 LP proposals, and<br />
recommended five of them for implementation.<br />
A sixth proposal, submitted as a<br />
preliminary step towards the construction<br />
of a Visitor Instrument for the NTT, was<br />
also supported. In P79, four of the 15 LP<br />
proposals that had been submitted were<br />
approved. In total, between the start of<br />
VLT science operations in 1999 and 006<br />
(P79), 7 LP proposals that received<br />
favourable evaluation from the OPC were<br />
allocated time on the La Silla Paranal<br />
Observatory telescopes. They cover almost<br />
all current astronomical topics,<br />
from the Solar System to cosmological<br />
studies.
Public Surveys<br />
Surveys provide large, homogeneous<br />
data sets covering a variety of combinations<br />
in the parameter space of wavelength,<br />
depth and sky area. Often surveys<br />
span longer time intervals and have<br />
a broader scope than LPs. From their<br />
databases, large uniformly-treated products<br />
can be generated, which can be<br />
used for a variety of scientific purposes.<br />
For optimal exploitation of the wide-field<br />
telescopes VST and VISTA, <strong>ESO</strong>, recognising<br />
that it does not have the resources<br />
to conduct public surveys on behalf of<br />
its user community, has put in place in<br />
005 a new scheme for the implementation<br />
of such surveys, allowing them to<br />
be treated as a separate category of LPs.<br />
Within this framework, a Public Survey<br />
is understood to be an observing programme<br />
in which the investigators commit<br />
to produce and to make publicly<br />
available, within a defined time, a fully<br />
reduced and scientifically usable data<br />
set that is likely to be of general use to a<br />
broader community of astronomers. Following<br />
recommendations by the STC and<br />
the OPC, 75 % of the <strong>ESO</strong> time on both<br />
VST and VISTA will be devoted to Public<br />
Surveys.<br />
For evaluation of Public Survey proposals,<br />
<strong>ESO</strong> established a Public Survey Panel<br />
(PSP), comprising scientists with expertise<br />
in a broad range of current astronomical<br />
research, with particular emphasis on<br />
the areas that can profit from Public Surveys.<br />
The PSP prime mandate is to review<br />
the proposals and to elaborate a scientifically<br />
and observationally well-coordinated<br />
set of Public Surveys.<br />
Similarly to what had been done in 004<br />
for the VST, a call for VISTA Public Survey<br />
proposals was issued at the beginning<br />
of 006. In response to this call, 15 proposals<br />
were received. The PSP held a<br />
first meeting in Garching on –3 May, at<br />
which it identified those proposals that<br />
indeed qualified as scientifically valid public<br />
surveys. A second meeting took place<br />
in Edinburgh in June, with participation<br />
of the PIs of the selected projects. At this<br />
meeting, possible revisions of these proposals<br />
and the merging of some of them<br />
with the aim of enhancement of the scientific<br />
value of the coordinated set were<br />
discussed, and corresponding recommendations<br />
were issued. This resulted in<br />
the submission of six revised proposals<br />
by the P79 OPC deadline. Following their<br />
evaluation by the PSP at a final meet-<br />
ing in Garching on 31 October, and formal<br />
endorsement of the conclusions of the<br />
PSP by the OPC at its November meeting,<br />
these six programmes were recommended<br />
for execution.<br />
OPC procedures<br />
Starting with P78, the revised OPC procedures<br />
that had been worked out in<br />
005 were implemented. The most significant<br />
changes took place in the areas<br />
of the nomination of the members of the<br />
OPC and of its Panels, and of the duration<br />
of their terms of service. As a result,<br />
as of P78, OPC members are no longer<br />
proposed by the member states. Instead,<br />
members of the OPC and of its panels<br />
are selected on scientific excellence. They<br />
are appointed by <strong>ESO</strong>’s Director Gener-<br />
al based on the recomendations of the<br />
Nominating Committee for the OPC. This<br />
Nominating Committee, which was constituted<br />
and held its first two meetings<br />
in 006, comprises three astronomers<br />
from the community and two <strong>ESO</strong> astronomers.<br />
In order to reduce the burden<br />
of the commitment required from astronomers<br />
who serve on the OPC or on its<br />
panels, and to allow a greater fraction of<br />
the community to participate more actively<br />
in the selection of the observing<br />
programmes, and hence in the definition<br />
of the orientation of European astronomy,<br />
the term of service was reduced to two<br />
years for OPC members (compared to<br />
four years previously) and to one year for<br />
panel members (from two years).<br />
On the other hand, in order to face the<br />
increasing number of proposals in scientific<br />
categories C and D, new sub-<br />
panels were created for each of these<br />
categories. Thus as of P78, the OPC<br />
consisted of a total of 10 sub-panels: two<br />
for each of categories A and B (unchanged)<br />
and three for each of categories<br />
C and D (instead of two until P77).<br />
The beneficial effect of this change on the<br />
workload of the referees of categories C<br />
and D was already offset by P79, where<br />
due to the unexpectedly steep increase in<br />
the numbers of proposals submitted in<br />
these categories, the amount of work of<br />
the members of the corresponding subpanels<br />
was back to its P77 level. Further<br />
steps to be taken to address this extremely<br />
fast evolution were discussed<br />
at the P79 OPC meeting, for implementation<br />
in 007.<br />
<strong>ESO</strong> Annual Report 006<br />
83
Summary of Use of Telescopes by Discipline<br />
The scientific categories referred to in<br />
the following tables correspond to the<br />
OPC classifications given below:<br />
OPC Categories and Sub-Categories<br />
A: Cosmology<br />
A1 Surveys of AGNs and high-z<br />
galaxies<br />
A Identification studies of extragalactic<br />
surveys<br />
A3 Large-scale structure and evolution<br />
A4 Distance scale<br />
A5 Groups and clusters of galaxies<br />
A6 Gravitational lensing<br />
A7 Intervening absorption-line systems<br />
A8 High-redshift galaxies (star formation<br />
and ISM)<br />
B: Galaxies and Galactic Nuclei<br />
B1 Morphology and galactic structure<br />
B Stellar populations<br />
B3 Chemical evolution<br />
B4 Galaxy dynamics<br />
B5 Peculiar/interacting galaxies<br />
84<br />
<strong>ESO</strong> Annual Report 006<br />
B6 Non-thermal processes in galactic<br />
nuclei (incl. QSRs, QSOs, blazars,<br />
Seyfert galaxies, BALs, radio galaxies,<br />
and LINERS)<br />
B7 Thermal processes in galactic nuclei<br />
and starburst galaxies (incl. ultraluminous<br />
IR galaxies, outflows,<br />
emission lines, and spectral energy<br />
distributions)<br />
B8 Central supermassive objects<br />
B9 AGN host galaxies<br />
C: Interstellar Medium, Star Formation<br />
and Planetary Systems<br />
C1 Gas and dust, giant molecular<br />
clouds, cool and hot gas, diffuse<br />
and translucent clouds<br />
C Chemical processes in the interstellar<br />
medium<br />
C3 Star-forming regions, globules,<br />
protostars, H ii regions<br />
C4 Pre-main-sequence stars (massive<br />
PMS stars, Herbig Ae/Be stars and<br />
T Tauri stars)<br />
C5 Outflows, stellar jets, HH objects<br />
C6 Main-sequence stars with circumstellar<br />
matter, early evolution<br />
C7 Young binaries, brown dwarfs,<br />
exosolar planet searches<br />
C8 Solar system (planets, comets,<br />
small bodies)<br />
D: Stellar Evolution<br />
D1 Main-sequence stars<br />
D Post-main-sequence stars, giants,<br />
supergiants, AGB stars, post-AGB<br />
stars<br />
D3 Pulsating stars and stellar activity<br />
D4 Mass loss and winds<br />
D5 Supernovae, pulsars<br />
D6 Planetary nebulae, nova remnants<br />
and supernova remnants<br />
D7 Pre-white dwarfs and white dwarfs,<br />
neutron stars<br />
D8 Evolved binaries, black-hole<br />
candidates, novae, X-ray binaries,<br />
CVs<br />
D9 Gamma-ray and X-ray bursters<br />
D10 OB associations, open and globular<br />
clusters, extragalactic star clusters<br />
D11 Individual stars in external galaxies
85<br />
<strong>ESO</strong> Annual Report 006<br />
Percentage of scheduled observing time/telescope/instrument/discipline<br />
Telescope<br />
. -m<br />
Total<br />
Instrument<br />
FEROS<br />
WFI<br />
B<br />
3<br />
5<br />
8<br />
C<br />
14<br />
6<br />
20<br />
D<br />
45<br />
3<br />
48<br />
Total<br />
66<br />
34<br />
100<br />
A<br />
4<br />
0<br />
24<br />
Scientific Categories<br />
Telescope<br />
3.6-m<br />
Total<br />
Instrument<br />
EFOSC<br />
HARPS<br />
Special3.6<br />
TIMMI<br />
B<br />
7<br />
0<br />
0<br />
9<br />
C<br />
1<br />
51<br />
1<br />
7<br />
60<br />
D<br />
6<br />
1<br />
0<br />
1<br />
19<br />
Total<br />
6<br />
63<br />
1<br />
10<br />
100<br />
A<br />
1<br />
0<br />
0<br />
0<br />
12<br />
Scientific Categories<br />
Telescope<br />
APEX<br />
Total<br />
Instrument<br />
APEX- A<br />
FLASH<br />
B<br />
1<br />
14<br />
C<br />
35<br />
57<br />
D<br />
14<br />
13<br />
27<br />
Total<br />
63<br />
37<br />
100<br />
A<br />
0<br />
2<br />
Scientific Categories<br />
Telescope<br />
NTT<br />
Total<br />
Instrument<br />
EMMI<br />
SOFI<br />
SUSI<br />
SpecialNTT<br />
B<br />
8<br />
5<br />
5<br />
0<br />
18<br />
C<br />
9<br />
4<br />
37<br />
D<br />
1<br />
9<br />
1<br />
1<br />
23<br />
Total<br />
46<br />
43<br />
8<br />
3<br />
100<br />
A<br />
17<br />
5<br />
0<br />
0<br />
22<br />
Scientific Categories<br />
Telescope<br />
UT1<br />
Total<br />
Instrument<br />
FORS<br />
ISAAC<br />
B<br />
17<br />
5<br />
22<br />
C<br />
3<br />
11<br />
14<br />
D<br />
14<br />
1<br />
26<br />
Total<br />
64<br />
36<br />
100<br />
A<br />
30<br />
8<br />
38<br />
Scientific Categories<br />
Telescope<br />
UT3<br />
Total<br />
Instrument<br />
DAZLE<br />
VIMOS<br />
VISIR<br />
B<br />
0<br />
5<br />
27<br />
C<br />
0<br />
4<br />
19<br />
23<br />
D<br />
0<br />
4<br />
4<br />
8<br />
Total<br />
4<br />
68<br />
8<br />
100<br />
A<br />
4<br />
38<br />
0<br />
42<br />
Scientific Categories<br />
Telescope<br />
UT<br />
Total<br />
Instrument<br />
FLAMES<br />
FORS1<br />
UVES<br />
B<br />
8<br />
5<br />
5<br />
18<br />
C<br />
10<br />
5<br />
5<br />
20<br />
D<br />
7<br />
15<br />
17<br />
39<br />
Total<br />
5<br />
41<br />
34<br />
100<br />
A<br />
0<br />
16<br />
7<br />
23<br />
Scientific Categories<br />
Telescope<br />
UT4<br />
Total<br />
Instrument<br />
NACO<br />
SINFONI<br />
B<br />
11<br />
1<br />
32<br />
C<br />
9<br />
31<br />
D<br />
1<br />
4<br />
16<br />
Total<br />
45<br />
55<br />
100<br />
A<br />
0<br />
1<br />
21<br />
Scientific Categories<br />
Telescope<br />
VLTI<br />
Total<br />
Instrument<br />
AMBER<br />
MIDI<br />
B<br />
0<br />
1<br />
1<br />
C<br />
10<br />
13<br />
23<br />
D<br />
11<br />
65<br />
76<br />
Total<br />
1<br />
79<br />
100<br />
A<br />
0<br />
0<br />
0<br />
Scientific Categories
Publications<br />
Publications in refereed journals based on <strong>ESO</strong> data<br />
Ábrahám, P.; Mosoni, L.; Henning, T.; Kóspál, Á.;<br />
Leinert, C.; Quanz, S. P.; Ratzka, T.; First AU-scale<br />
observations of V1647 Orionis with VLTI/MIDI;<br />
A&A 449, L13–L16<br />
Acke, B.; van den Ancker, M. E.; Resolving the disk<br />
rotation of HD 97048 and HD 100546 in the [O i]<br />
6300 Å line: evidence for a giant planet orbiting<br />
HD 100546; A&A 449, 67– 79<br />
Acke, B.; van den Ancker, M. E.; A survey for nano-<br />
diamond features in the 3 micron spectra<br />
of Herbig Ae/Be stars; A&A 457, 171–181<br />
Ádámkovics, M.; de Pater, I.; Hartung, M.;<br />
Eisenhauer, F.; Genzel, R.; Griffith, C. A.; Titan’s<br />
bright spots: Multiband spectroscopic measurement<br />
of surface diversity and hazes; JGRE 111<br />
Aerts, C.; de Cat, P.; de Ridder, J.; van Winckel, H.;<br />
Raskin, G.; Davignon, G.; Uytterhoeven, K.; Multiperiodicity<br />
in the large-amplitude rapidly-rotating<br />
b Cephei star HD 03664; A&A 449, 305–311<br />
Afonso, C.; Glicenstein, J. F.; Gould, A.; Smith, M. C.;<br />
Wagner, R. M.; Albert, J. N.; Andersen, J.; Ansari,<br />
R.; Aubourg, É.; Bareyre, P.; Beaulieu, J. P.; Blanc,<br />
G.; Charlot, X.; Coutures, C.; Ferlet, R.; Fouqué,<br />
P.; Goldman, B.; Graff, D.; Gros, M.; Haissinski, J.;<br />
Hamadache, C.; de Kat, J.; Leguillou, L.; Lesquoy,<br />
É.; Loup, C.; Magneville, C.; Marquette, J. B.;<br />
Maurice, É.; Maury, A.; Milsztajn, A.; Moniez, M.;<br />
Palanque-Delabrouille, N.; Perdereau, O.; Prévot,<br />
L.; Rahal, Y. R.; Rich, J.; Spiro, M.; Tisserand, P.;<br />
Vidal-Madjar, A.; Vigroux, L.; Zylberajch, S.;<br />
The OGLE-II event sc5 859: a classical nova outburst?;<br />
A&A 450, 33– 39<br />
Alcalá, J. M.; Spezzi, L.; Frasca, A.; Covino, E.;<br />
Porras, A.; Merín, B.; Persi, P.; The first brown<br />
dwarf with a disk in Chamaeleon II; A&A 453,<br />
L1–L4<br />
Allen, D. M.; Barbuy, B.; Analysis of 6 barium stars.<br />
II. Contributions of s-, r-, and p-processes in the<br />
production of heavy elements; A&A 454, 917–931<br />
Allen, D. M.; Barbuy, B.; Analysis of 6 barium stars.<br />
I. Abundances; A&A 454, 895–915<br />
Allen, P. D.; Driver, S. P.; Graham, A. W.; Cameron,<br />
E.; Liske, J.; de Propris, R.; The Millennium Galaxy<br />
Catalogue: bulge-disc decomposition of 10095<br />
nearby galaxies; MNRAS 371, –18<br />
Alvarez-Candal, A.; Duffard, R.; Lazzaro, D.;<br />
Michtchenko, T.; The inner region of the asteroid<br />
Main Belt: a spectroscopic and dynamic analysis;<br />
A&A 459, 969–976<br />
Alves-Brito, A.; Barbuy, B.; Zoccali, M.; Minniti, D.;<br />
Ortolani, S.; Hill, V.; Renzini, A.; Pasquini, L.; Bica,<br />
E.; Rich, R. M.; Meléndez, J.; Momany, Y.;<br />
VLT-UVES abundance analysis of four giants in<br />
NGC 6553; A&A 460, 69– 76<br />
Andreon, S.; Quintana, H.; Tajer, M.; Galaz, G.;<br />
Surdej, J.; The Butcher-Oemler effect at z ~ 0.35:<br />
a change in perspective; MNRAS 365, 915–9 8<br />
Annibali, F.; Bressan, A.; Rampazzo, R.; Zeilinger, W.<br />
W.; Nearby early-type galaxies with ionized gas.<br />
II. Line-strength indices for 18 additional galaxies;<br />
A&A 445, 79–91<br />
Antonello, E.; Mantegazza, L.; Rainer, M.; Miglio, A.;<br />
Probable nonradial g-mode pulsation in early<br />
A-type stars; A&A 445, L15–L18<br />
Antonello, E.; Fossati, L.; Fugazza, D.; Mantegazza,<br />
L.; Gieren, W.; Variable stars in nearby galaxies.<br />
VII. P-L relation in the BVRI bands of Cepheids in<br />
IC 1613; A&A 445, 901–906<br />
86<br />
<strong>ESO</strong> Annual Report 006<br />
Antonelli, L. A.; Testa, V.; Romano, P.; Guetta, D.;<br />
Torii, K.; D’Elia, V.; Malesani, D.; Chincarini, G.;<br />
Covino, S.; D’Avanzo, P.; Della Valle, M.; Fiore, F.;<br />
Fugazza, D.; Moretti, A.; Stella, L.; Tagliaferri, G.;<br />
Barthelmy, S.; Burrows, D.; Campana, S.; Capalbi,<br />
M.; Cusumano, G.; Gehrels, N.; Giommi, P.;<br />
Lazzati, D.; La Parola, V.; Mangano, V.; Mineo, T.;<br />
Nousek, J.; O’Brien, P. T.; Perri, M.; The multiwavelength<br />
afterglow of GRB 0507 1: a puzzling<br />
rebrightening seen in the optical but not in the<br />
X-ray; A&A 456, 509–515<br />
Argiroffi, C.; Favata, F.; Flaccomio, E.; Maggio, A.;<br />
Micela, G.; Peres, G.; Sciortino, S.; XMM-Newton<br />
survey of two upper Scorpius regions; A&A 459,<br />
199– 13<br />
Arias, J. I.; Barbá, R. H.; Maíz Apellániz, J.; Morrell,<br />
N. I.; Rubio, M.; The infrared Hourglass cluster in<br />
M8; MNRAS 366, 739–757<br />
Asplund, M.; Lambert, D. L.; Nissen, P. E.; Primas, F.;<br />
Smith, V. V.; Lithium Isotopic Abundances in<br />
Metal-poor Halo Stars; ApJ 644, 9– 59<br />
Astier, P.; Guy, J.; Regnault, N.; Pain, R.; Aubourg,<br />
E.; Balam, D.; Basa, S.; Carlberg, R. G.; Fabbro,<br />
S.; Fouchez, D.; Hook, I. M.; Howell, D. A.; Lafoux,<br />
H.; Neill, J. D.; Palanque-Delabrouille, N.; Perrett,<br />
K.; Pritchet, C. J.; Rich, J.; Sullivan, M.; Taillet, R.;<br />
Aldering, G.; Antilogus, P.; Arsenijevic, V.; Balland,<br />
C.; Baumont, S.; Bronder, J.; Courtois, H.; Ellis, R.<br />
S.; Filiol, M.; Gonçalves, A. C.; Goobar, A.; Guide,<br />
D.; Hardin, D.; Lusset, V.; Lidman, C.; McMahon,<br />
R.; Mouchet, M.; Mourao, A.; Perlmutter, S.;<br />
Ripoche, P.; Tao, C.; Walton, N.; The Supernova<br />
Legacy Survey: measurement of ΩM, Ω∆ and w<br />
from the first year data set; A&A 447, 31–48<br />
Ausseloos, M.; Aerts, C.; Lefever, K.; Davis, J.;<br />
Harmanec, P.; High-precision elements of doublelined<br />
spectroscopic binaries from combined interferometry<br />
and spectroscopy. Application to the b<br />
Cephei star b Centauri; A&A 455, 59– 69<br />
Bagnulo, S.; Landstreet, J. D.; Mason, E.; Andretta,<br />
V.; Silaj, J.; Wade, G. A.; Searching for links between<br />
magnetic fields and stellar evolution.<br />
I. A survey of magnetic fields in open cluster A-<br />
and B-type stars with FORS1; A&A 450, 777–791<br />
Bagnulo, S.; Boehnhardt, H.; Muinonen, K.;<br />
Kolokolova, L.; Belskaya, I.; Barucci, M. A.;<br />
Exploring the surface properties of transneptunian<br />
objects and Centaurs with polarimetric FORS1/<br />
VLT observations; A&A 450, 1 39–1 48<br />
Bains, I.; Wong, T.; Cunningham, M.; Sparks, P.;<br />
Brisbin, D.; Calisse, P.; Dempsey, J. T.; Deragopian,<br />
G.; Ellingsen, S.; Fulton, B.; Herpin, F.; Jones, P.;<br />
Kouba, Y.; Kramer, C.; Ladd, E. F.; Longmore, S.<br />
N.; McEvoy, J.; Maller, M.; Minier, V.; Mookerjea,<br />
B.; Phillips, C.; Purcell, C. R.; Walsh, A.; Voronkov,<br />
M. A.; Burton, M. G.; Molecular line mapping of<br />
the giant molecular cloud associated with RCW<br />
106 – I. 13CO; MNRAS 367, 1609–16 8<br />
Bamford, S. P.; Aragón-Salamanca, A.; Milvang-<br />
Jensen, B.; The Tully-Fisher relation of distant field<br />
galaxies; MNRAS 366, 308–3 0<br />
Barbuy, B.; Zoccali, M.; Ortolani, S.; Momany, Y.;<br />
Minniti, D.; Hill, V.; Renzini, A.; Rich, R. M.; Bica,<br />
E.; Pasquini, L.; Yadav, R. K. S.; VLT-UVES analysis<br />
of two giants in the bulge metal-poor globular<br />
cluster HP-1. Analysis of two giants in HP-1; A&A<br />
449, 349–358<br />
Barucci, M. A.; Merlin, F.; Dotto, E.; Doressoundiram,<br />
A.; de Bergh, C.; TNO surface ices. Observations<br />
of the TNO 55638 ( 00 VE95; A&A 455, 7 5–730<br />
Bassa, C. G.; Jonker, P. G.; in’t Zand, J. J. M.;<br />
Verbunt, F.; Two new candidate ultra-compact Xray<br />
binaries; A&A 446, L17–L 0<br />
Bassa, C. G.; van Kerkwijk, M. H.; Koester, D.;<br />
Verbunt, F.; The masses of PSR J1911-5958A and<br />
its white dwarf companion; A&A 456, 95–304<br />
Bastian, N.; Emsellem, E.; Kissler-Patig, M.;<br />
Maraston, C.; Young star cluster complexes in<br />
NGC 4038/39. Integral field spectroscopy using<br />
VIMOS-VLT; A&A 445, 471–483<br />
Bastian, N.; Saglia, R. P.; Goudfrooij, P.; Kissler-<br />
Patig, M.; Maraston, C.; Schweizer, F.; Zoccali, M.;<br />
Dynamical mass estimates for two luminous star<br />
clusters in galactic merger remnants; A&A 448,<br />
88–891<br />
Battaglia, G.; Tolstoy, E.; Helmi, A.; Irwin, M. J.;<br />
Letarte, B.; Jablonka, P.; Hill, V.; Venn, K. A.;<br />
Shetrone, M. D.; Arimoto, N.; Primas, F.; Kaufer, A.;<br />
Francois, P.; Szeifert, T.; Abel, T.; Sadakane, K.;<br />
The DART imaging and CaT survey of the Fornax<br />
dwarf spheroidal galaxy; A&A 459, 4 3–440<br />
Baume, G.; Moitinho, A.; Vázquez, R. A.; Solivella,<br />
G.; Carraro, G.; Villanova, S.; NGC 401: a template<br />
of the young population of the Norma-<br />
Cygnus arm in the Third Galactic Quadrant;<br />
MNRAS 367, 1441–1449<br />
Beaulieu, J.-P.; Bennett, D. P.; Fouqué, P.; Williams,<br />
A.; Dominik, M.; Jorgensen, U. G.; Kubas, D.;<br />
Cassan, A.; Coutures, C.; Greenhill, J.; Hill, K.;<br />
Menzies, J.; Sackett, P. D.; Albrow, M.; Brillant, S.;<br />
Caldwell, J. A. R.; Calitz, J. J.; Cook, K. H.;<br />
Corrales, E.; Desort, M.; Dieters, S.; Dominis, D.;<br />
Donatowicz, J.; Hoffman, M.; Kane, S.; Marquette,<br />
J.-B.; Martin, R.; Meintjes, P.; Pollard, K.; Sahu,<br />
K.; Vinter, C.; Wambsganss, J.; Woller, K.; Horne,<br />
K.; Steele, I.; Bramich, D. M.; Burgdorf, M.;<br />
Snodgrass, C.; Bode, M.; Udalski, A.; Szymański,<br />
M. K.; Kubiak, M.; Wie¸ ckowski, T.; Pietrzyński, G.;<br />
Soszyński, I.; Szewczyk, O.; Wyrzykowski, Ł.;<br />
Paczyński, B.; Abe, F.; Bond, I. A.; Britton, T. R.;<br />
Gilmore, A. C.; Hearnshaw, J. B.; Itow, Y.; Kamiya,<br />
K.; Kilmartin, P. M.; Korpela, A. V.; Masuda, K.;<br />
Matsubara, Y.; Motomura, M.; Muraki, Y.;<br />
Nakamura, S.; Okada, C.; Ohnishi, K.; Rattenbury,<br />
N. J.; Sako, T.; Sato, S.; Sasaki, M.; Sekiguchi, T.;<br />
Sullivan, D. J.; Tristram, P. J.; Yock, P. C. M.;<br />
Yoshioka, T.; Discovery of a cool planet of 5.5<br />
Earth masses through gravitational microlensing;<br />
Nature 439, 437–440<br />
Beccari, G.; Ferraro, F. R.; Possenti, A.; Valenti, E.;<br />
Origlia, L.; Rood, R. T.; The Dynamical State and<br />
Blue Straggler Population of the Globular Cluster<br />
NGC 6 66 (M6 ); AJ 131, 551– 560<br />
Beccari, G.; Ferraro, F. R.; Lanzoni, B.; Bellazzini, M.;<br />
A Population of Binaries in the Asymptotic Giant<br />
Branch of 47 Tucanae?; ApJ 65 , L1 1–L1 4<br />
Becker, W.; Kramer, M.; Jessner, A.; Taam, R. E.; Jia,<br />
J. J.; Cheng, K. S.; Mignani, R.; Pellizzoni, A.; de<br />
Luca, A.; Słowikowska, A.; Caraveo, P. A.; A Multiwavelength<br />
Study of the Pulsar PSR B19 9+10<br />
and Its X-Ray Trail; ApJ 645, 14 1–1435
Bedding, T. R.; Butler, R. P.; Carrier, F.; Bouchy, F.;<br />
Brewer, B. J.; Eggenberger, P.; Grundahl, F.;<br />
Kjeldsen, H.; McCarthy, C.; Nielsen, T. B.; Retter,<br />
A.; Tinney, C. G.; Solar-like Oscillations in the<br />
Metal-poor Subgiant b Indi: Constraining the<br />
Mass and Age Using Asteroseismology; ApJ 647,<br />
558–563<br />
Bedregal, A. G.; Aragón-Salamanca, A.; Merrifield,<br />
M. R.; Milvang-Jensen, B.; S0 galaxies in Fornax:<br />
data and kinematics; MNRAS 371, 191 –19 4<br />
Behrend, R.; Bernasconi, L.; Roy, R.; Klotz, A.; Colas,<br />
F.; Antonini, P.; Aoun, R.; Augustesen, K.; Barbotin,<br />
E.; Berger, N.; Berrouachdi, H.; Brochard, E.;<br />
Cazenave, A.; Cavadore, C.; Coloma, J.; Cotrez, V.;<br />
Deconihout, S.; Demeautis, C.; Dorseuil, J.; Dubos,<br />
G.; Durkee, R.; Frappa, E.; Hormuth, F.; Itkonen, T.;<br />
Jacques, C.; Kurtze, L.; Laffont, A.; Lavayssière,<br />
M.; Lecacheux, J.; Leroy, A.; Manzini, F.; Masi, G.;<br />
Matter, D.; Michelsen, R.; Nomen, J.; Oksanen, A.;<br />
Pääkkönen, P.; Peyrot, A.; Pimentel, E.; Pray, D.;<br />
Rinner, C.; Sanchez, S.; Sonnenberg, K.; Sposetti,<br />
S.; Starkey, D.; Stoss, R.; Teng, J.-P.; Vignand, M.;<br />
Waelchli, N.; Four new binary minor planets: (854)<br />
Frostia, (1089) Tama, (1313) Berna, (449 ) Debussy;<br />
A&A 446, 1177–1184<br />
Bellazzini, M.; Correnti, M.; Ferraro, F. R.; Monaco, L.;<br />
Montegriffo, P.; The age of the main population of<br />
the Sagittarius dwarf spheroidal galaxy. Solving<br />
the “M giant conundrum”; A&A 446, L1–L4<br />
Belloche, A.; Parise, B.; van der Tak, F. F. S.; Schilke,<br />
P.; Leurini, S.; Güsten, R.; Nyman, L.-Å.; The evolutionary<br />
state of the southern dense core Chamaeleon-MMS1;<br />
A&A 454, L51–L54<br />
Bellazzini, M.; Newberg, H. J.; Correnti, M.; Ferraro,<br />
F. R.; Monaco, L.; Detection of a population gradient<br />
in the Sagittarius stream; A&A 457, L 1–L 4<br />
Beltrán, M. T.; Brand, J.; Cesaroni, R.; Fontani, F.;<br />
Pezzuto, S.; Testi, L.; Molinari, S.; Search for<br />
massive protostar candidates in the southern<br />
hemisphere. II. Dust continuum emission; A&A<br />
447, 1– 33<br />
Benetti, S.; Cappellaro, E.; Turatto, M.; Taubenberger,<br />
S.; Harutyunyan, A.; Valenti, S.; Supernova 00 ic:<br />
The Collapse of a Stripped-Envelope, Massive<br />
Star in a Dense Medium?; ApJ 653, L1 9–L13<br />
Bennert, N.; Jungwiert, B.; Komossa, S.; Haas, M.;<br />
Chini, R.; Size and properties of the NLR in the<br />
Seyfert- galaxy NGC 1386; A&A 446, 919–93<br />
Bennert, N.; Jungwiert, B.; Komossa, S.; Haas, M.;<br />
Chini, R.; Size and properties of the narrow-line<br />
region in Seyfert- galaxies from spatially-resolved<br />
optical spectroscopy; A&A 456, 953–966<br />
Bennert, N.; Jungwiert, B.; Komossa, S.; Haas, M.;<br />
Chini, R.; Size and properties of the narrow-line<br />
region in Seyfert-1 galaxies from spatially-resolved<br />
optical spectroscopy; A&A 459, 55–69<br />
Bensby, T.; Feltzing, S.; The origin and chemical<br />
evolution of carbon in the Galactic thin and thick<br />
discs; MNRAS 367, 1181–1193<br />
Bergond, G.; Zepf, S. E.; Romanowsky, A. J.;<br />
Sharples, R. M.; Rhode, K. L.; Wide-field kinematics<br />
of globular clusters in the Leo I group; A&A<br />
448, 155–164<br />
Berta, S.; Rubele, S.; Franceschini, A.; Held, E. V.;<br />
Rizzi, L.; Lonsdale, C. J.; Jarrett, T. H.; Rodighiero,<br />
G.; Oliver, S. J.; Dias, J. E.; Buttery, H. J.; Fiore, F.;<br />
La Franca, F.; Puccetti, S.; Fang, F.; Shupe, D.;<br />
Surace, J.; Gruppioni, C.; The <strong>ESO</strong>-Spitzer Imaging<br />
extragalactic Survey (ESIS). I. WFIB, V, R<br />
deep observations of ELAIS-S1 and comparison<br />
to Spitzer and GALEX data; A&A 451, 881–900<br />
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Lyra, W.; Moitinho, A.; van der Bliek, N. S.; Alves, J.;<br />
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Wilkinson, M. I.; Halliday, C.; Bridges, T. J.; A<br />
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A&A 459, 31–4<br />
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Starck, J.-L.; Valtchanov, I.; Read, A. M.; Altieri,<br />
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Geissler, K.; Masciadri, E.; Meteorological Parameter<br />
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PASP 118, 1048–1065<br />
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Mozurkewich, D.; Schmitt, H.; Resolving the<br />
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Kotak, R.; Meikle, P.; Pozzo, M.; van Dyk, S. D.;<br />
Farrah, D.; Fesen, R.; Filippenko, A. V.; Foley, R.<br />
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ApJ 651, L117–L1 0<br />
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Bacon, R.; Bureau, M.; Cappellari, M.; Davies, R.<br />
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SAURON project – VIII. OASIS/CFHT integral-field<br />
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Colless, M.; Central stellar populations of earlytype<br />
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Zdanavičius, K.; Korakitis, R.; Malkov, O.; Smette,<br />
A.; The design and performance of the Gaia<br />
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Claeskens, J.-F.; Smette, A.; Vandenbulcke, L.;<br />
Surdej, J.; Identification and redshift determination<br />
of quasi-stellar objects with medium-band<br />
photometry: application to Gaia; MNRAS 367,<br />
879–904<br />
Kriek, M.; van Dokkum, P. G.; Franx, M.; Quadri, R.;<br />
Gawiser, E.; Herrera, D.; Illingworth, G. D.; Labbé,<br />
I.; Lira, P.; Marchesini, D.; Rix, H.-W.; Rudnick, G.;<br />
Taylor, E. N.; Toft, S.; Urry, C. M.; Wuyts, S.; Spectroscopic<br />
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649, L71–L74<br />
Treister, E.; Urry, C. M.; The Evolution of Obscuration<br />
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van Dokkum, P. G.; Quadri, R.; Marchesini, D.;<br />
Rudnick, G.; Franx, M.; Gawiser, E.; Herrera, D.;<br />
Wuyts, S.; Lira, P.; Labbé, I.; Maza, J.; Illingworth,<br />
G. D.; Förster Schreiber, N. M.; Kriek, M.; Rix, H.-<br />
W.; Taylor, E. N.; Toft, S.; Webb, T.; Yi, S. K.; The<br />
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Sauer, D. N.; Mazzali, P. A.; Deng, J.; Valenti, S.;<br />
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Thompson, R. I.; Sauvage, M.; Kennicutt, R. C., Jr.;<br />
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Fruchter, A. S.; Levan, A. J.; Strolger, L.; Vreeswijk,<br />
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Financial Statement<br />
Financial Statements 2006<br />
(in € 1000)<br />
Balance Sheet<br />
Assets<br />
Cash and short-term deposits<br />
Claims, advances, refundable taxes and other assets<br />
Total assets<br />
Liabilities and equity<br />
Dues<br />
Advance payments received and other liabilities<br />
Total liabilities<br />
Cumulated result previous years<br />
Annual result<br />
Total equity<br />
Total liabilities and equity<br />
Statement of Income and Expenditure<br />
Income<br />
Contributions from member states<br />
Contributions from third parties and partners<br />
Income from sales and other income<br />
Total income<br />
Expenditure<br />
Expenditure for staff<br />
Operating and other expenditure<br />
Total expenditure<br />
2006 Result<br />
Statement of Cash flow<br />
Cash flow from operating activities<br />
Receipts<br />
Income<br />
Net movements on accounts receivable<br />
Total<br />
Payments<br />
Expenditure<br />
Net movements on accounts payable<br />
Total<br />
Net cash flow from operating activities<br />
Cash flow from financing activities<br />
Net cash flow from financing activities<br />
Net cash flow = Net increase/decrease in cash<br />
and short-term deposits<br />
31.12.2006<br />
89<br />
60 40<br />
149 624<br />
6803<br />
0 616<br />
27419<br />
46 675<br />
75 530<br />
122205<br />
149 624<br />
31.12.2005<br />
76 880<br />
4 958<br />
81838<br />
18 438<br />
16 7 5<br />
35163<br />
1 977<br />
33 698<br />
46 675<br />
81838<br />
01.01.2006–31.12.2006<br />
179 089<br />
5 00<br />
4 6 3<br />
188 912<br />
49 734<br />
63 648<br />
113 382<br />
75 530<br />
01.01.2006–31.12.2006<br />
188 91<br />
–55 443<br />
133469<br />
–113 38<br />
–14140<br />
–127522<br />
5 947<br />
6 395<br />
12 342<br />
Budget for 2007<br />
(in € 1000)<br />
Income budget<br />
Contributions from member states<br />
Other income from member states<br />
Income from third parties<br />
Various income<br />
Total income budget<br />
Payment budget<br />
Personnel cost<br />
Other cost<br />
Total payment budget<br />
Commitment budget<br />
Personnel cost<br />
Projects commitments without personnel<br />
Operations commitments without personnel<br />
Total commitment budget<br />
<strong>ESO</strong> Annual Report 006<br />
2007<br />
117 73<br />
4 388<br />
1 014<br />
4 000<br />
138134<br />
2007<br />
51170<br />
149 7 8<br />
200 898<br />
2007<br />
51170<br />
158 09<br />
37 61<br />
246 640<br />
Since 003, the <strong>ESO</strong> annual accounts have shown a positive cash flow<br />
development, which is reflected in the amount of cash and short-term deposits at<br />
end of year. In 006, the positive cash flow amounted to 1 ,3 M€ and the cash<br />
and short-term deposits as of 31 December 006 amounted to 89, M€.<br />
The net result of the statement of income and expenditure for 006 was<br />
+ 75,5 M€. The high income figure of 188,9 M€ included in particular the amount<br />
of the entrance fee due by Spain following the country’s accession as a new<br />
<strong>ESO</strong> member state as of 1 July 006.<br />
The budget for 007 was approved by the <strong>ESO</strong> Council in December 006.<br />
The budget comprises three sections: the income budget, the payment budget<br />
and the commitment budget.<br />
With 00,9 M€, the 007 payment budget is driven by the payment profile of<br />
the ALMA project. It also includes a provision for the detail design phase of the<br />
European ELT. In total, it is expected to be significantly higher than the 007<br />
income budget, which amounts to 138,1 M€.<br />
The commitment budget for 007 is 46,6 M€.<br />
105
Four Seasons at a Glance<br />
January<br />
First Light for the Laser Guide Star on<br />
UT4 of the VLT.<br />
Astronomers find 5 Earth-mass exoplanet<br />
with microlensing technique, using a<br />
worldwide network of telescopes, including<br />
the 1.5-m telescope at La Silla.<br />
Meeting of the Scientific Strategy Working<br />
Group.<br />
15th release of the VLT Software.<br />
Workshop on ALMA (From Z-Machines<br />
to ALMA: (Sub)millimeter Spectroscopy of<br />
Galaxies), NRAO Charlottesville.<br />
ALMA European Science Advisory Committee<br />
meeting, Garching.<br />
ALMA Science Advisory Committee<br />
meets in Washington, US.<br />
February<br />
Signing of the agreement between Spain<br />
and <strong>ESO</strong> about membership.<br />
Committee of Council meets in Berne,<br />
Switzerland.<br />
Breakfast press briefing for the UK media<br />
in connection with the yearly Astrofest<br />
in London, organised by <strong>ESO</strong> and PPARC.<br />
<strong>ESO</strong> is also present at the Astrofest<br />
with a scale model of the VLT and display<br />
panels.<br />
<strong>ESO</strong> is present at the annual AAAS meeting<br />
in St. Louis, Missouri.<br />
Yearly <strong>ESO</strong> Status Overwiew held in<br />
Garching.<br />
106<br />
<strong>ESO</strong> Annual Report 006<br />
March<br />
Visit to the <strong>ESO</strong> HQ by the Education<br />
Committee of the Finnish Parliament.<br />
Walloon Space Days in Liège and delivery<br />
ceremony for the 4th VLT Auxiliary Telescope<br />
at AMOS, Belgium.<br />
Launch of the first international, multidisciplinary<br />
journal for innovative science<br />
teaching, “Science in School”, by<br />
EIROforum at EMBL in Heidelberg.<br />
Joint <strong>ESO</strong>-FONDAP Workshop on Globular<br />
Clusters, Concepción, Chile.<br />
European ALMA Board meets in Garching.<br />
ALMA Board meeting, Kyoto, Japan.<br />
Extraordinary Finance Committee in<br />
Garching.<br />
Danish Minister of Education, Bertel<br />
Haarder, visits Paranel.<br />
April<br />
Preliminary Acceptance Europe review of<br />
CRIRES.<br />
8 7 proposals are received in answer<br />
to the Call for Proposals for observing in<br />
Period 78.<br />
CRIRES AO system (MACAO) installed<br />
and commissioned at UT1.<br />
An image made of about 300 million pixels<br />
is released by <strong>ESO</strong>, based on more<br />
than 64 hours of observations with the<br />
Wide-Field Imager on the . -m telescope<br />
at La Silla.<br />
VLT observes fragment B of the comet<br />
Schwassmann-Wachmann 3, that had<br />
split a few days earlier.<br />
Meeting of the Scientific Strategy Working<br />
Group.<br />
6 nd Meeting of the Scientific Technical<br />
Committee.<br />
The Users’ Committee meets in Garching.<br />
Meeting of the <strong>ESO</strong> Tripartite Group.<br />
Opening of the IPP/<strong>ESO</strong> Crèche.<br />
May<br />
HARPS helps discover a nearby star<br />
hosting three Neptune-mass planets.<br />
Strong <strong>ESO</strong> participation at the SPIE<br />
Astronomical Telescopes and Instrumentation<br />
Symposium in Orlando, Florida.<br />
First recoating of M of UT1 successfully<br />
completed.<br />
114th Finance Committee Meeting in<br />
Garching.<br />
Extraordinary 63rd meeting of the<br />
Scientific Technical Committee.<br />
European ALMA Board meeting, Garching.<br />
Public Survey Panel meets in Garching.<br />
Workshop on “Complex Molecules<br />
in Space: Present status and prospects<br />
with ALMA”, Fuglsøcentret, Denmark.
June<br />
First spectra on-sky obtained by CRIRES<br />
on the VLT.<br />
<strong>ESO</strong> establishes a dedicated E-ELT<br />
Project Office.<br />
X-shooter passes Final Design Review in<br />
Europe.<br />
The <strong>ESO</strong> Council meets in Garching.<br />
ALMA Board meeting, Santiago, Chile.<br />
Signing of the ALMA agreement with<br />
Japan.<br />
Observing Programmes Committee<br />
meeting in Garching.<br />
<strong>ESO</strong> and the Government of Chile launch<br />
the book “10 Years Exploring the Universe”,<br />
written by the beneficiaries of the<br />
<strong>ESO</strong>-Government of Chile Joint Committee.<br />
Public Survey Panel meets in Edinburgh,<br />
UK.<br />
<strong>ESO</strong> participates with a major information<br />
stand at the nd Salon Européen de<br />
la Recherche & de l’Innovation in Paris,<br />
France.<br />
EuroSummer School, Observation and<br />
data reduction with the Very Large<br />
Telescope Interferometer, Château de<br />
Goutelas, France.<br />
Conference “Library and Information<br />
Services in Astronomy V: Common Challenges,<br />
Uncommon Solutions”, Cambridge,<br />
Mass., USA.<br />
July<br />
6 articles based on early science<br />
with APEX are published in the research<br />
journal Astronomy & Astrophysics.<br />
The first of seven years of data of<br />
the UKIRT Infrared Deep Sky Survey<br />
(UKIDSS) enters <strong>ESO</strong>’s archive.<br />
The Fifth NEON Observing School,<br />
Observatoire de Haute-Provence, France.<br />
EIROforum takes part in the Euroscience<br />
Open Forum 006 Conference in<br />
Munich with a major information stand,<br />
press conferences and a reception.<br />
<strong>ESO</strong> is also visible in the German Science<br />
Festival with an on-stage show at<br />
Munich’s Marienplatz, involving a live<br />
videoconference with Paranal.<br />
August<br />
The new SINFONI spectrograph scrutinises<br />
a distant protodisc galaxy with a<br />
record-breaking resolution of a mere 0.15<br />
arcseconds.<br />
Provisional Design Review for the ALMA<br />
Transporter.<br />
“Heating vs. Cooling in Galaxies and<br />
Clusters of Galaxies”, MPA/<strong>ESO</strong>/MPE/<br />
USM Joint Astronomy Conference,<br />
Garching, Germany.<br />
The Second NEON Archive Observing<br />
School takes place at <strong>ESO</strong>.<br />
<strong>ESO</strong> is present at the IAU XXVIth General<br />
Assembly in Prague with presentations<br />
and information stands. <strong>ESO</strong>’s<br />
Director General Catherine Cesarsky<br />
is elected President of the International<br />
Astronomical Union while <strong>ESO</strong>’s<br />
Deputy Director General Ian Corbett is<br />
elected Assistant General Secretary<br />
September<br />
Thomas Wilson is appointed as <strong>ESO</strong>’s<br />
Associate Director.<br />
Committee of Council meets in Santiago,<br />
Chile.<br />
ALMA European Science Advisory Committee<br />
meeting, Garching.<br />
ALMA Science Advisory Committee<br />
meets in Florence, Italy.<br />
Joint <strong>ESO</strong>-Lisbon-Aveiro University<br />
Conference on Precision Spectroscopy in<br />
Astrophysics, Aveiro, Portugal.<br />
October<br />
KMOS passes Preliminary Design Review.<br />
913 proposals are received in answer<br />
to the Call for Proposals for observing in<br />
Period 79, a new all-time record.<br />
DAZLE visitor instrument successfully<br />
commissioned on UT3.<br />
UT4 recoating of M1/M3 completed.<br />
<strong>ESO</strong> Annual Report 006<br />
107
Visit to the <strong>ESO</strong> Headquarters by a group<br />
of university rectors from Chile.<br />
Committee of Council meets in Munich.<br />
<strong>ESO</strong> exhibition at major astronomy festival<br />
in Vaulx-en-Velin, France.<br />
<strong>ESO</strong> exhibition in Montpellier, France.<br />
64th Meeting of the Scientific Technical<br />
Committee.<br />
Extraordinary Finance Committee in<br />
Garching.<br />
Public Survey Panel meets in Garching.<br />
ALMA Commissioning meeting.<br />
Meeting of the <strong>ESO</strong> Tripartite Group.<br />
UNAWE Workshop in Leiden, the<br />
Netherlands.<br />
Almost 3000 people visit the <strong>ESO</strong> HQ<br />
at the Open House. On that occasion<br />
<strong>ESO</strong> together with other institutes on the<br />
Garching campus, receives the “Deutschland<br />
– Land der Ideen” Trophy for its<br />
public communication activities.<br />
<strong>ESO</strong> releases its 007 Calendar.<br />
November<br />
Visit to Paranal by a delegation from the<br />
Academy of Sciences of the Czech<br />
Republic.<br />
More than 50 European astronomers<br />
gather at the ‘Towards the European ELT’<br />
conference in Marseille, France.<br />
International ALMA Conference on<br />
“Science with ALMA: a new era for Astrophysics”,<br />
held in Madrid, Spain.<br />
108<br />
<strong>ESO</strong> Annual Report 006<br />
European Extremely Large Telescope is<br />
selected in the European Strategy Forum<br />
on Research Infrastructures (ESFRI)<br />
Roadmap.<br />
EIROforum breakfast meeting at the<br />
European Parliament discusses science<br />
education issues in Europe.<br />
<strong>ESO</strong> and the European Association<br />
for Astronomy Education launch the 007<br />
edition of ‘Catch a Star!’, their international<br />
astronomy competition for school<br />
students.<br />
The Finance Committee (116th) meets in<br />
Garching.<br />
ALMA board meets in Madrid, Spain.<br />
Extraordinary 65th meeting of the<br />
Scientific Technical Committee.<br />
Observing Programmes Committee<br />
meeting in Garching.<br />
EIROforum Assembly in Grenoble,<br />
France.<br />
A top-level meeting on exoplanets takes<br />
place in Washington D.C. between <strong>ESO</strong>,<br />
ESA and NASA.<br />
December<br />
<strong>ESO</strong> participates at major astronomy and<br />
space exhibition, Astro-expo, in Dublin,<br />
Ireland.<br />
The <strong>ESO</strong> Council meets in Garching.<br />
Council decides to proceed with Phase B<br />
studies for the European Extremely<br />
Large Telescope. Council also approves<br />
the Agreement with the Czech Republic<br />
about membership.<br />
Fourth and last-to-be-installed VLTI Auxiliary<br />
Telescope (AT4) obtains its ‘First<br />
Light’.<br />
EIROforum issues statement of support<br />
for the European Charter for Researchers<br />
and the Code of Conduct for the Recruitment<br />
of Researchers.<br />
<strong>ESO</strong> releases 56 million pixel image of<br />
30 Doradus.<br />
UT recoating of M1/M3 completed.<br />
Laser Guide Star Facility on VLT successfully<br />
commissioned.<br />
The Multi-conjugate Adaptive optics<br />
Demonstrator (MAD) passes its PAE<br />
(Preliminary Acceptance Europe).<br />
Fourth Advanced Chilean School of Astrophysics<br />
(co-sponsored by <strong>ESO</strong>),<br />
“Interferometry in the Epoch of ALMA and<br />
VLTI”, P. Universidad Católica de Chile,<br />
Santiago, Chile.<br />
Signing Ceremony in Prague of the<br />
Agreement between <strong>ESO</strong> and the Czech<br />
Republic regarding Czech membership of<br />
<strong>ESO</strong>.
Glossary of Frequently Used Acronyms<br />
4LGSF Four-Laser Guide Star Facility<br />
AAAS American Association for the<br />
Advancement of Science<br />
A&A Journal “Astronomy & Astrophysics”<br />
ACS Advanced Camera for Surveys (HST)<br />
ACS ALMA Common Software<br />
ADP Advanced Data Products (VOS)<br />
AEM Alcatel Alenia Space France, Alcatel<br />
Alenia Space Italy, European Industrial<br />
Engineering s.r.L., MT<br />
Aerospace Consortium (ALMA)<br />
ALMA Atacama Large Millimeter/Submilli-<br />
meter Array<br />
ALMA ARC ALMA Regional Centre<br />
AMBER Astronomical Multi-BEam combineR<br />
(VLTI Instrument)<br />
ANSYS ANSYS Multiphysics, general-<br />
purpose finite element analysis<br />
software<br />
AO Adaptive Optics<br />
AOF Adaptive Optics Facility<br />
AOS Array Operations Site<br />
APEX Atacama Pathfinder Experiment<br />
ASAC ALMA Science Advisory Committee<br />
ASI Italian Space Agency (Agenzia<br />
Spaziale Italiana)<br />
ASSIST Adaptive Secondary Setup and<br />
Instrument Simulator<br />
AT Auxiliary Telescope for the VLTI<br />
AVO Astrophysical Virtual Observatory<br />
BMBF German Federal Ministry for Education<br />
and Research<br />
CADC Canadian Astronomy Data Centre<br />
CAS Academy of Sciences of the Czech<br />
Republic<br />
CCD Charge-Coupled Device<br />
CES Coudé Echelle Spectrometer (3.6-m)<br />
CERN European Organisation for Nuclear<br />
Research (Conseil Européen pour la<br />
Recherche Nucléaire, Switzerland)<br />
CDR Conceptual Design Review<br />
CFD Computational Fluid Dynamics<br />
CI corporate identity<br />
CMMS computerised maintenance management<br />
system<br />
CNRS Centre National de la Recherche<br />
Scientifique (France)<br />
CRIRES Cryogenic InfraRed Echelle Spectrometer<br />
(VLT)<br />
CSIC Spanish National Research Council<br />
(Consejo Superior de Investigaciones<br />
Científicas)<br />
darkCAM dark energy camera for VISTA<br />
DAZLE Dark Age ‘Z’ Lyman-alpha Explorer<br />
DBCM Database Content Management<br />
DCA EURO-VO Data Centre Alliance<br />
DCU Dublin City University<br />
DFO Data Flow Operations<br />
DMD Data Management Division<br />
DMO Data Management and Operations<br />
Division<br />
DRM Design Reference Mission<br />
DSM Deformable Secondary Mirror<br />
EAAE European Association for Astronomy<br />
Education<br />
EFOSC <strong>ESO</strong> Faint Object Spectrograph and<br />
Camera (3.6-m)<br />
EIS <strong>ESO</strong> Imaging Survey<br />
ELT Extremely Large Telescope<br />
E-ELT European Extremely Large Telescope<br />
EMC Electromagnetic Compatibility<br />
EMMI <strong>ESO</strong> Multi-Mode Instrument (NTT)<br />
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<strong>ESO</strong> Annual Report 006<br />
ERA-net European Research Area Network<br />
ESA European Space Agency<br />
ESAC European Science Advisory Committee<br />
(for ALMA)<br />
ESE ELT Science and Engineering<br />
ESFRI European Strategy Forum on/for<br />
Research Infrastructures<br />
ESRC ELT Standing Review Committee<br />
ESRIN ESA Centre for Earth Observations<br />
ESTI EIROforum European Science<br />
Teachers’ Initiative<br />
EURO-VO European Virtual Observatory<br />
FDR Final Design Review<br />
FE Front End<br />
FEIC Front End Integration Centres<br />
FEM Finite Element Method<br />
FEROS Fibre-fed, Extended Range, Échelle<br />
Spectrograph ( . -m)<br />
FINITO Fringe Tracking Instrument Nice<br />
Torino (VLTI)<br />
FLAMES Fibre Large Array Multi Element<br />
Spectrograph (VLT)<br />
FOC Faint Object Camera<br />
FORS FOcal Reducer/low dispersion<br />
Spectrograph<br />
FP Framework Programme<br />
FP6 Sixth Framework Programme<br />
FP7 Seventh Framework Programme<br />
GALACSI Ground Atmospheric Layer Adaptive<br />
Optics for Spectroscopic Imaging<br />
GENIE Ground based European Nulling<br />
Interferometer Experiment (VLTI)<br />
GHRS Goddard High-Resolution Spectrograph<br />
GRAAL GRound-layer Adaptive opctics<br />
Assisted by Lasers<br />
GRAVITY AO assisted, two-object, multiplebeam-combiner<br />
(VLTI)<br />
GRB Gamma-Ray Burst<br />
GROND Gamma-Ray burst Optical/Nearinfrared<br />
Detector<br />
HARPS High Accuracy Radial Velocity<br />
Planetary Searcher (3.6-m)<br />
HAWK-I High Acuity Wide field K-band<br />
Imager (VLT)<br />
HLA Hubble Legacy Archive<br />
HOT High Order Test-bench<br />
HST Hubble Space Telescope<br />
IAU International Astronomical Union<br />
ICD Interface Control Document<br />
IEM Instituto de Estructura de la Materia<br />
(Madrid, Spain)<br />
INAF Istituto Nazionale di Astrofisica (Italy)<br />
INSU Institut National des Sciences de<br />
l’Univers (France)<br />
INTA Instituto Nacional de Tecnica Aeroespacial<br />
(Spain)<br />
IPP Max-Planck-Institut für Plasmaphysik<br />
IPT Integrated Project Team (ALMA)<br />
IR InfraRed<br />
IRAM Institut de Radioastronomie Millimétrique<br />
(France)<br />
ISAAC Infrared Spectrometer And Array<br />
Camera (VLT)<br />
IT Information Technology<br />
ITF Interferometry Task Force<br />
ITRE European Parliament’s Committee<br />
on Industry, Research and Energy<br />
IVOA International Virtual Observatory<br />
Alliance<br />
JBO Jodrell Bank Observatory (UK)<br />
KMOS K-band multi-object spectrograph<br />
(VLT)<br />
LABOCA Large APEX Bolometer CAmera<br />
LAOG Laboratoire d’Astrophysique de<br />
Grenoble<br />
LERMA Laboratoire d’Étude du Rayonnement<br />
et de la Matière en Astrophysique<br />
(France)<br />
LGS Laser Guide Star<br />
LGSF Laser Guide Star Facility<br />
LP Large Programme<br />
LTP Long Term Perspectives<br />
MACAO Multi-Application Curvature Adaptive<br />
Optics (VLT/VLTI)<br />
MAD Multi-Conjugate Adaptive Optics<br />
Demonstrator<br />
MATISSE Multi AperTure mid-Infrared<br />
SpectroScopic Experiment (VLTI)<br />
MEC Minsitry of Education and Science<br />
(Ministerio de Educación y Ciencia,<br />
Spain)<br />
MIDI Mid-Infrared Interferometric<br />
Instrument (VLTI Instrument)<br />
MoU Memorandum of Understanding<br />
MPE Max Planck Institute for Extraterrestrial<br />
Physics (Germany)<br />
MPIfR Max Planck Institute for Radioastronomy<br />
(Germany)<br />
MRIP Medium Range Implementation Plan<br />
MUSE Multi Unit Spectroscopic Explorer<br />
(VLT)<br />
MVM Image processing library<br />
NACO NAOS-CONICA (VLT)<br />
NAOJ National Astronomical Observatory<br />
of Japan<br />
NAOS Nasmyth Adaptive Optics System<br />
(VLT)<br />
NASA National Air and Space Administration<br />
(US)<br />
NGAS Next Generation Archiving System<br />
NGC New General detector Controller<br />
NICMOS Near Infrared Camera and<br />
Multi-Object Spectrograph (HST)<br />
NIST National Institute of STandards<br />
NOTSA Nordic Optical Telescope Scientific<br />
Association<br />
NOVA Dutch Research School for Astronomy<br />
(Nederlandse Onderzoekschool<br />
voor Astronomie)<br />
NSF National Science Foundation<br />
NTT New Technology Telescope<br />
OmegaCAM Optical Camera for the VST<br />
OPC Observing Programmes Committee<br />
OPD Optical Path Differences<br />
OPTICON Optical Infrared Coordination<br />
Network for Astronomy<br />
OSF Operations Support Facility (ALMA)<br />
OSO Onsala Space Observatory<br />
OWL OverWhelmingly Large Telescope<br />
P PP Phase Preparation Tool<br />
P75 Period 75<br />
P76 Period 76<br />
P77 Period 77<br />
P78 Period 78<br />
P79 Period 79<br />
PAD Public Affairs Department<br />
PAE Preliminary Acceptance Europe<br />
PARSEC Sodium line laser for VLT AO<br />
PDM Product Data Management<br />
PDR Preliminary Design Review<br />
PI Principal Investigator<br />
PPARC Particle Physics and Astronomy<br />
Research Council (UK)
PRIMA Phase-Referenced Imaging and<br />
Micro-arcsecond Astrometry facility<br />
(VLTI)<br />
PSP Public Survey Panel<br />
QC Quality Control<br />
R&D Research and Development<br />
RADIONET Radio Astronomy Network in Europe<br />
RDS Rat Deutscher Sternwarten<br />
(Germany)<br />
RoHS Restriction on the use of Hazardous<br />
Substances<br />
RRM Rapid-Response Mode<br />
SAC EURO-VO Science Advisory Committee<br />
SAF Science Archive Facility<br />
SAO Science Archive Operation<br />
SEI System Engineering and Integration<br />
SINFONI Spectrograph for INtegral Field<br />
Observations in the Near Infrared<br />
SMI Structural Modelling Interface<br />
SMA SubilliMeter Array<br />
SOCHIAS Chilean Astronomical Society<br />
SOFI SOn oF Isaac (NTT)<br />
SPHERE Spectro-Polarimetric High-contrast<br />
Exoplanet Research instrument<br />
SPIE International Society for Optical<br />
Engineering<br />
SSWG Scientific Strategy Planning Working<br />
Group<br />
STC Scientific Technical Committee<br />
ST-ECF Space Telescope European<br />
Coordination Facility<br />
STIS Slit spectrograph (HST)<br />
STScI Space Telescope Science Institute<br />
(USA)<br />
SUSI SUperb Seeing Imager (NTT)<br />
TAC Time Allocation Committee<br />
TB TeraBytes<br />
TFB Turnable Filter Bank<br />
TIMMI Thermal Infrared MultiMode<br />
Instrument (3.6-m)<br />
TMT Thirty Meter Telescope<br />
ToO Target of Opportunity<br />
UC Users’ Committee<br />
UK United Kingdom<br />
UKIDSS UKIRT Infrared Deep Sky Survey<br />
UKIRT UK Infrared Telescope<br />
ULTRACAM ULTRA-fast, triple-beam CCD<br />
CAMera<br />
USD User Support Department<br />
UT1–4 VLT Unit Telescope 1–4: Antu,<br />
Kueyen, Melipal and Yepun<br />
UVES UV-Visual Echelle Spectrograph<br />
(VLT)<br />
VCM Variable Curvature Mirrors<br />
VIMOS VIsible MultiObject Spectrograph<br />
(VLT)<br />
VINCI VLT INterferometer Commissionning<br />
Instrument<br />
VIRCAM VISTA IR Camera<br />
VISA VLTI Sub-Array<br />
VISIR VLT Mid-Infrared Imager Spectrometer<br />
VISTA Visible and Infrared Survey<br />
Telescope for Astronomy<br />
VITRUV Near-IR spectro-imager using fibre<br />
(VLTI)<br />
VLT Very Large Telescope<br />
VLTI Very Large Telescope Interferometer<br />
VO Virtual Observatory<br />
VOFC EURO-VO Facility Centre<br />
VOS Virtual Observatory System<br />
VOTC EURO-VO Technology Centre<br />
VSI VLTI Spectro Imager<br />
VST VLT Survey Telescope<br />
VTK Vibration Tracking<br />
VVDS VIMOS VLT Deep Survey<br />
WFCAM Wide-Field Camera (UKIDSS)<br />
WFI Wide Field Imager ( . -m)<br />
X-Shooter Wideband UV-IR single target<br />
spectrograph (VLT)<br />
<strong>ESO</strong> Annual Report 006<br />
111
<strong>ESO</strong> Europe<br />
Headquarters<br />
Karl-Schwarzschild-Straße<br />
85748 Garching bei München<br />
Germany<br />
Phone +49 89 3 0 06 -0<br />
Direct lines<br />
Director General - 6<br />
Visiting Astronomers -553/473<br />
Science Office - 9/ 86<br />
Technology Division - 58<br />
Data Management Division -69<br />
Public Affairs Department - 76<br />
Instrumentation Division -506<br />
Telescope Division -347<br />
Administration - 38<br />
Fax +49 89 3 0 3 6<br />
www.eso.org<br />
<strong>ESO</strong> Chile<br />
La Silla Paranal Observatory<br />
La Silla Site<br />
IV Región<br />
Chile<br />
Phone +56 464 4100<br />
Fax +56 464 4101<br />
La Silla Paranal Observatory<br />
Paranal Site<br />
II Región<br />
Chile<br />
Phone +56 55 43 5100<br />
Fax +56 55 43 5101<br />
APEX Radio Observatory<br />
Séquitor<br />
II Región<br />
Chile<br />
Phone +56 55 44 8 00<br />
Fax +56 55 44 8 1<br />
Santiago Office<br />
Alonso de Córdova 3107<br />
Vitacura<br />
Casilla 19001<br />
Santiago de Chile 19<br />
Chile<br />
Phone +5 6 463 3100<br />
Fax +5 6 463 3101<br />
11<br />
<strong>ESO</strong> Annual Report 006<br />
La Serena Office<br />
Avenida El Santo 1538<br />
Casilla 567<br />
La Serena<br />
Chile<br />
Phone +56 51 53 87<br />
Fax +56 51 15175<br />
Guest House<br />
Rey Gustavo Adolfo 4634<br />
Las Condes<br />
Santiago de Chile<br />
Chile<br />
Phone +56 08 4 54<br />
Fax +56 8 93 33<br />
Antofagasta Office<br />
Avenida Balmaceda 536<br />
Office 504<br />
Edificio ‘Don Guillermo’<br />
Antofagasta<br />
Chile<br />
Phone +56 55 6 00 3<br />
Fax +56 55 6 00 81<br />
<strong>ESO</strong> is a partner in the international<br />
ALMA project<br />
ALMA Office San Pedro de Atacama<br />
Kilómetro 1 1 CH 3<br />
II Región<br />
Chile<br />
Phone +56 55 44 8416<br />
Fax +56 55 44 84 81<br />
ALMA Office Santiago<br />
El Golf 40, Piso 18<br />
Las Condes<br />
Santiago de Chile<br />
Chile<br />
Phone +56 4676100<br />
Fax +56 4676101<br />
DVD (Mac/PC and DVD Player)<br />
The <strong>ESO</strong> Annual Report 006 DVD<br />
contains two parts. It should play<br />
automatically when inserted in any DVD<br />
player, featuring a set of videos made by<br />
<strong>ESO</strong>.<br />
In addition, on a Mac or a PC, it is<br />
possible to open it to access additional<br />
content:<br />
– All the <strong>ESO</strong> Press Releases and Press<br />
Photos having been published in 006.<br />
– The four Messenger issues of 006.<br />
– The list of all publications based on <strong>ESO</strong><br />
telescopes that appeared in 006.<br />
– A gallery of photos.<br />
To access these features, simply view the<br />
index.html file in your favourite browser.<br />
All images are copyright <strong>ESO</strong> except<br />
where otherwise indicated.<br />
Produced by the<br />
Public Affairs Department<br />
© <strong>ESO</strong> 007<br />
ISSN 0531-4496<br />
Back cover photo:<br />
The Laser Guide Stars System at Paranal.
<strong>ESO</strong> Annual Report 006<br />
113