Untitled - ESO

ESO 

European Organisation 

for Astronomical 

Research in the 

Southern Hemisphere 

Annual Report 2006 

presented to the Council by the 

Director General 

Dr. Catherine Cesarsky

About ESO 

ESO is the foremost intergovernmental 

European Science and Technology organisation 

in the field of ground-based 

astrophysics. It is supported by 1 countries: 

Belgium, Denmark, France, Finland, 

Germany, Italy, the Netherlands, Portugal, 

Spain, Sweden, Switzerland and the 

United Kingdom. The Czech Republic is 

currently in the process of joining ESO 

(Status as of 31.1 . 006). Further 

countries have expressed interest in 

membership. 

Created in 196 , ESO provides state-ofthe-art 

research facilities to European 

astronomers and astrophysicists. In pursuit 

of this task, ESO’s activities cover 

a wide spectrum including the design 

and construction of world-class groundbased 

observational facilities for the 

member-state scientists, large telescope 

projects, design of innovative scientific 

instruments, developing new and advanced 

technologies, furthering European 

cooperation and carrying out European 

educational programmes. 

ESO operates the La Silla Paranal Observatory 

at several sites in the Atacama Desert 

region of Chile. The first site is at 

La Silla, a 400 m high mountain 600 km 

north of Santiago de Chile. It is equipped 

with several optical telescopes with mirror 

diameters of up to 3.6 metres. The 

3.5-m New Technology Telescope (NTT) 

was the first in the world to have a computer-controlled 

main mirror. 

Whilst La Silla remains one of the scientifically 

most productive observing sites in 

the world, the 600 m high Paranal site 

with the Very Large Telescope array (VLT) 

is the flagship facility of European astronomy. 

Paranal is situated about 130 km 

south of Antofagasta in Chile, 1 km inland 

from the Pacific Coast in what is 

probably the driest area in the world. Scientific 

operations began in 1999 and have 

resulted in a high number of extremely 

successful research programmes. The 

VLT is a most unusual telescope, based 

on the latest technology. It is not just 

one, but an array of four telescopes, each 

with a main mirror of 8. -m diameter. 

With one such telescope, images of celestial 

objects as faint as magnitude 30 

have been obtained in a one-hour exposure. 

This corresponds to seeing objects 

that are four billion times fainter than 

what can be seen with the naked eye. 

ESO Annual Report 006 

One of the most exciting features of the 

VLT is the possibility to use it as a giant 

optical interferometer (VLT Interferometer 

or VLTI). This is done by combining the 

light from several of the telescopes, including 

one or more of four 1.8-m moveable 

Auxiliary Telescopes. In the interferometric 

mode, one can reach the resolution on 

the sky that would be obtained with a 

telescope of the size of the separation 

between the most distant of the combined 

mirrors. 

Artist’s impression 

of a part of ALMA 

on Chajnantor. 

The . -m, the 3.5-m 

NTT and the 3.6-m 

telescopes at La Silla. 

In 006, over 1700 proposals were made 

for the use of ESO telescopes. They 

have resulted in a large number of peerreviewed 

publications. In 006, 630 refereed 

papers based on data from ESO 

telescopes were published. 

ESO is also a major partner in the Atacama 

Large Millimeter/Submillimeter Array 

(ALMA), one of the largest ground-based 

astronomy projects of the next decade.

ALMA will be comprised of a main array 

of fifty 1 -m submillimetre quality antennas, 

with baselines of several kilometres. 

An additional compact array of four 1 -m 

and twelve 7-m antennas complements 

the main array. Construction of ALMA 

started in 003 and will be completed in 

01 ; it will become incrementally operational 

from 010 on. ALMA is located on 

the high-altitude Llano de Chajnantor 

(5 000 m elevation), east of the village of 

San Pedro de Atacama in Chile. The 

ALMA project is a partnership between 

Europe, Japan and North America in 

cooperation with the Republic of Chile. 

ALMA is funded in Europe by ESO, in 

Japan by the National Institutes of Natural 

Sciences in cooperation with the 

Academia Sinica in Taiwan and in North 

America by the U.S. National Science 

Foundation in cooperation with the National 

Research Council of Canada. 

ALMA construction and operations are 

led on behalf of Europe by ESO, on behalf 

of Japan by the National Astronomical 

Observatory of Japan and on be- 

half of North America by the National 

Radio Astronomy Observatory, which is 

managed by Associated Universities, Inc. 

The Chajnantor site is also home of the 

1 -m APEX submillimetre/millimetre-wavelength 

telescope, operated by ESO on 

behalf of the Onsala Space Observatory, 

the Max-Planck Institute for Radio Astronomy 

and ESO itself. 

ESO has built up considerable expertise 

in developing, integrating and operat- 

ing large astronomical telescopes at remote 

sites. Together with the ideas developed 

in the framework of the OWL 

Conceptual Study and the EC co-funded 

Extremely Large Telescope Design Study, 

this expertise forms the backbone of 

the effort to develop a next-generation 

extremely large ground-based optical/infrared 

telescope for Europe’s astronomers. 

For this project, currently known as 

the European Extremely Large Telescope 

(E-ELT), ESO has developed a basic reference 

design for a 4 -m telescope with 

a novel five-mirror optical concept. The 

current detailed design phase is scheduled 

to be completed by the end of 009. 

The ESO headquarters are located in 

Garching, near Munich, Germany. This is 

the scientific, technical and administrative 

centre of ESO where technical development 

programmes are carried out to provide 

the observatories with the most 

advanced instruments. It is also home for 

the Space Telescope – European Coordinating 

Facility (ST-ECF), operated jointly 

by ESO and the European Space Agency 

(ESA). 

Artist’s impression 

of the E-ELT. 

The VLT Array 

at Paranal. 


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Contents 

Foreword 6 

Introduction 7 

Research Highlights 10 

La Silla Paranal Observatory 30 

Atacama Large Millimeter/Submillimeter Array 38 

The European Extremely Large Telescope 45 

Organisation and Personnel 

Organigramme 49 

List of Personnel 50 

Personnel Services 5 

Instrumentation 53 

Technical Developments 57 

Science Archive Operation 60 

The European Virtual Observatory 6 

ST-ECF 63 

Public Outreach 65 

ESO Press Releases 68 

Relations with Chile 70 

European Affairs 7 

Committees 

Council 76 

The Scientific Technical Committee 77 

Finance Committee 80 

The Users’ Committee 80 

The Observing Programmes Commitee 8 

Summary of Use of Telescopes by Discipline 84 

Publications 86 

Financial Statement 105 

Four Seasons at a Glance 106 

Glossary of Frequently Used Acronyms 110 

DVD 113 


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6 


Foreword 

It would be evident even to the most casual 

observer that ESO is as vibrant and 

dynamic as ever with a strong track record 

of excellence and ambitious projects. 

Some of these projects are now operational 

facilities, some are under construction 

and others are in the design phase. 

The task of Council is to provide the overall 

strategy and a framework for the further 

evolution of the organisation and it is 

this forward-looking task that makes the 

work of Council members so rewarding. 

Arguably, the most important issue 

regarding the future that Council had to 

address in 006 was the decision to 

endorse the proposal to embark on the 

detailed design study for a European 

Extremely Large Telescope (E-ELT). The 

study, scheduled to last for three years, 

will lead to a proposal for construction for 

Council to consider in due course. Council 

was able to take this decision not 

least because of the impressive preparatory 

work by ESO and the various working 

groups with strong involvement by the 

scientific community across Europe. In 

taking this important step Council recognised 

that the E-ELT is crucial to the further 

development of European astronomy 

and its ability to retain a competitive edge 

on a global stage. 

Building the E-ELT is as big a challenge 

to all of us as any of the preceding projects 

in ESO’s already impressive project 

portfolio. We can succeed only if we 

manage to harness the necessary resources 

– financial, technological and 

human. It is therefore gratifying that more 

potential member countries continue to 

express interest in joining. I was delighted 

that the entry of Spain as the 1 th member 

state of ESO was becoming a reality 

at the end of the year, with just the final 

formalities pending. Spain plays an important 

role in European astronomy and 

its membership of ESO is a very welcome. 

At its December meeting Council 

also approved the entry of the Czech 

Republic, the first of the Central European 

countries to join. 

The expansion of ESO’s membership 

base is clearly important in the context of 

the E-ELT. It also strengthens ESO as 

the focal point for Europe’s astronomers 

and thus reinforces the significance of 

the organisation as an important actor in 

the European Research Area. 

ESO’s overall role in the European research 

landscape is an important question 

that warrants serious consideration. 

At the June meeting of Council, the 

Science Strategy Working Group presented 

several scenarios that are now 

subject to further debate. 

Entrusting the management of the organisation 

to the most competent leader 

is clearly most important to all of us. With 

the term of the current Director Gener- 

al coming to its end by September 007, 

Council set up a search committee for 

the next DG, leading to the selection 

of Prof. Tim de Zeeuw as successor to 

Dr. Catherine Cesarsky. With this decision, 

Council has provided the base 

for a smooth transition of the management 

of ESO. 

In conclusion I am pleased to note that by 

the end of the year, Council, working with 

the Executive, had acted to set ESO on 

a track towards a very exciting future and 

I wish to express my sincere thanks to 

all involved in this important endeavour. 

Richard Wade 

President of the ESO Council

Introduction 

In my introduction to the 005 Annual 

Report, I described that year as a pivotal 

year for ESO. This was not least on the 

basis of the progress regarding the ALMA 

project. Looking at 006, however, it is 

impossible not to use similar vocabulary 

again. Shortly before Christmas 005 I 

had launched a very ambitious plan aiming 

to move quickly and decisively towards 

the realisation of the European 

Extremely Large Telescope (E-ELT). The 

task was daunting: the plan foresaw 

the establishment of five mixed Community-ESO 

topical Working Groups with- 

in the shortest space of time to lay the 

groundwork for a set of extremely intense 

activities to be conducted within a ‘core’ 

Working Group, the ELT Science and Engineering 

Working Group, supplemented 

by an ELT Standing Advisory Committee. 

Before the end of 006, and with broad 

involvement of the scientific community, 

we wanted to be able to present a basic 

reference design and ask Council for approval 

of a Phase B for the project. 

The way the scientific community and the 

ESO staff embraced the plan was truly 

encouraging, with 85 out of 88 invitees 

enthusiastically agreeing to board the 

‘ELT-train’. Now, 1 months later, the train 

has arrived – precisely on schedule. 

At the 7 November–1 December conference 

in Marseille, which was attended by 

more than 50 scientists, the results were 

presented to and discussed by the 

scientific community. Only a week later, 

Council gave the green light to embark 

on Phase B, a three-year long detailed 

design study that should allow us to present 

a proposal for construction to the 

ESO Council in the 009– 010 time frame. 

The basis for the design study is a 4 -m 

telescope with a unique five-mirror design. 

It constitutes an innovative design 

solution that takes account of all the concerns 

raised with previous design proposals. 

Yet, while pursuing the detailed 

studies, we retain the option of the classical 

Gregorian telescope as a fallback 

possibility. 

These twelve months have seen a remarkable 

coming together of people, 

ideas, policy decisions and much hard 

work. The outcome is a tribute to the 

ability of Europe’s astronomers to set ambitious 

goals but also to forge tenable 

compromises – to set their sights on the 

sky, while keeping their feet on the 

ground. 

Aside from the impressive mobilisation 

of the scientific community, two other elements 

in the jigsaw puzzle should be 

mentioned: the inclusion of the ELT in the 

so-called ESFRI-list of large future research 

infrastructures deemed to be of 

European interest, and the setting up at 

ESO of a dedicated E-ELT project office 

with cross-divisional parts in a matrix 

structure. The former embeds the E-ELT 

decision process in the wider European 

science policy scene, a necessary step in 

the age of the European Research Area. 

The latter is part of preparing ESO for 

the challenges arising from the fact that 

we have become a multi-project organisation. 

A new step in the matrix structure 

foreseen to cope with this new situation 

is the creation of the Software Development 

Division, encompassing software 

developers from the previous Data Management 

Division, the Technological 

Division, and ALMA. Meanwhile, the new 

Data Management Operations division 

serves the VLT/VLTI and the ALMA ARC, 

ensuring continued attention to our running 

operations. 

At Paranal, we introduced in January the 

Laser Guide Star (LGS) system on Yepun. 

At ESO, as elsewhere, success requires 

hard work, and indeed it became evident 

that the LGS launch-telescope needed 


Photo: Volker Steger 

modifications in order to perform as required. 

However, with the improvements 

carried out, the LGS commissioning 

could resume by October, and the facility 

will be fully used in scientific observations 

early in 007. 

Also this year, the fourth Auxiliary Telescope 

saw First Light, completing the 

suite of ATs for the Very Large Telescope 

Interferometer (VLTI) and we thank 

the Belgians, the Swiss and the Italians 

for providing the additional resources 

needed for this significant improvement. 

Progress was also achieved with respect 

to VISTA, the 4-m survey telescope that 

forms a part of the UK entrance fee to 

ESO. In May 006 most of the structural 

parts were shipped to Chile. The telescope 

enclosure was accepted in Chile, 

while the camera was ready to leave 

the UK for Chile at the end of the year. 

The coating plant that comes with VISTA 

was also being installed. This facility 

will prove a useful resource as it will allow 

mirrors to be silver rather than alumin- 

ium coated. Public Surveys for VISTA 

have been selected and I am glad to see 

that there were so many proposals, with 

the result that a very good set of surveys 

have been chosen. 

The other survey telescope, the .5-m 

VST, remains on the other hand a matter 

of concern due to serious, continued 

delay. Nonetheless, following a visit by 

ESO engineers to Naples, plans were 

made for shipping of the telescope struc- 

7

ture early in 007. The 3 -CCD-mosaic 

OmegaCAM wide-field optical camera for 

the VST, which was developed by ESO, 

was, however, finished. The primary 

mirror of the telescope is also now ready, 

in Moscow. 

In June the VLT cryogenic high-resolution 

infrared echelle spectrograph CRIRES 

was commissioned at the Nasmyth focus 

of Antu, marking the completion of the 

first-generation VLT instrumentation. First 

steps of Science Verification also took 

place during the year and work was progressing 

very well on developing a de- 

dicated pipeline for the CRIRES data reduction. 

At the same time, the near-infrared imager 

HAWK-I, often described as a VLT 

‘generation 1.5’ instrument, was in an 

advanced stage, undergoing Assembly 

and Integration at ESO Garching, paving 

the way for a shipment to Chile in 007. 

Important progress was also achieved 

with respect to the second-generation 

instrumentation. In September, an agreement 

was signed with an extended 

consortium led by LAOG in Grenoble to 

develop SPHERE. The revised design 

fulfils all the requirements set by the ESO 

Scientific Technical Committee (STC) for 

the planet-finder instrument. 

Meanwhile, the multi-conjugate adap- 

tive optics demonstrator (MAD) was successfully 

tested in the laboratory in 

Garching, passing its PAE (Preliminary 

Acceptance Europe) in December and 

thus being ready to go to Chile. 

All of these instruments constitute technological 

marvels; we are thrilled by their 

ingenious design and capabilities, for 

they allow us to do science at the cuttingedge. 

This is undoubtedly also the case 

for AMBER, the interferometric beam 

combiner for the VLTI, which was offered 

to the scientific community from P 76, and 

it is gratifying to see a string of truly impressive 

scientific results, scheduled to 

appear in a special issue of A&A in March 

007. 

AMBER is not the only facility to have this 

honour, as in July 006 the submillimetric 

telescope APEX was also the topic of 

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a special A&A issue, with no fewer than 

6 articles based on early science being 

published. 

Although some of the great scientific 

achievements made with ESO’s telescopes 

are published in the Research 

Highlights, I cannot resist mentioning 

a few. In January, the discovery of the 

smallest exoplanet found so far, a five- 

Earth-mass planet, was announced. 

The planet was discovered by microlensing, 

with the help of a worldwide network 

of telescopes, among which the 1.5-m 

Danish telescope at La Silla was the one 

that could pick up the signal due to the 

planet. This discovery heralds a new era 

in the search for exoplanets. The identification, 

also at La Silla but with the 3.6-m 

telescope this time, of a planetary system 

containing three Neptune-mass planets 

and an asteroid belt, is also of crucial 

importance in this very hot research area. 

With the VLT, astronomers have found 

possible proofs of stellar vampirism in the 

globular cluster 47 Tucanae. Indeed, 

some hot, bright, and apparently young 

stars in the cluster present less carbon 

and oxygen than the majority of their sisters, 

indicating that these few stars likely 

formed by taking their material from another 

star. Farther away, the combination 

of adaptive optics techniques with the 

new SINFONI integral-field spectrograph 

allowed astronomers to study a very distant 

galaxy with a record-breaking resolution 

of a mere 0.15 arcseconds, giving 

an unprecedented detailed view of the 

anatomy of such a distant proto-disc galaxy. 

The observations imply that large 

disc galaxies akin to our Milky Way must 

have formed on a rapid timescale, only 

three billion years after the Big Bang. 

With the VISIR instrument, astronomers 

have mapped the disc around a star 

more massive than the Sun. The very extended 

and flared disc most likely contains 

enough gas and dust to spawn planets. 

It appears as a precursor of debris 

discs such as those around Vega-like 

stars and thus provides the rare opportunity 

to witness the conditions prevailing 

prior to or during planet formation. The 

huge gain in resolving power offered 

by the VLTI also made a difference. VINCI 

and MIDI were used to discover envelopes 

around three Cepheids, massive 

pulsating stars that play a crucial role 

in cosmology, being one of the first steps 

on the cosmic distance ladder. 

Of course, these are but a few examples 

of the science that is based on observations 

with ESO telescopes. In fact, on 

average, our user community produces 

close to two papers with ESO data a day 

all year round, more than any other 

ground-based observatory in the world. 

ESO telescopes generate a large quantity 

of data, which are kept for reuse in the 

Science Archive. With the coming online 

of VISTA, and later of the VST, the flow 

of data will considerably increase, reaching 

100 TB of data per year. To anticipate 

this, ESO is preparing a Petabyte-class 

archive that will be ready next year. 

In July, the first data release of the UKIRT 

Infrared Deep Sky Survey (UKIDSS) 

was available, providing a year of data to 

the ESO community of users. The full survey 

is expected to take seven years. But 

this first set of observations already 

shows how powerful the full survey will 

be at finding rare objects that hold vital 

clues to how stars and galaxies in our 

Universe formed. Indeed, the new data 

on young galaxies is already challenging 

current thinking on galaxy formation, 

revealing galaxies that are massive at a 

much earlier stage of development than 

anticipated. 

In 005, the ALMA project was set on 

track with major industrial contracts 

being awarded. The year 006 was a year 

of construction: the road from the highway 

to the high site, the AOS, was completed 

at its full width, and construction 

of the buildings at the OSF, at 900 m 

altitude, began at full speed. The road 

and the OSF buildings are deliverables for 

which ESO is responsible. 

In Europe, the first cryostats and receivers 

for two frequency bands were delivered. 

By now, prototypes are available 

for all four ALMA frequencies (0.6, 0.9, 

1.3 and 3 mm), fulfilling specifications. For 

the cryostats, a first series of eight was

manufactured and delivered. The first cartridge 

for Band 7 exceeded the specifications, 

being much more sensitive than 

initially planned. This, in effect, is equivalent 

to having many more antennas. 

First tests on the SMA on Mauna Kea of 

the water vapour radiometers proved 

the technology to be highly successful. It 

was thus decided to implement these 

in ALMA, thereby further increasing the 

output of this unique facility. 

Another important milestone for the 

ALMA project was reached in June with 

the signing of the agreement with Japan 

(and Taiwan), bringing a Compact Ar- 

ray and other wavebands to the project. 

According to the agreement, the ALMA 

array will thus initially comprise 66 antennas, 

54 of them with 1 -m diameter 

and 1 7-m antennas. 

ALMA is the first quasi-global project in 

ground-based astronomy, and it is fitting 

that ESO, with its international orientation, 

plays its part in it. That ESO plays an 

important role on the international scene 

was also visible during the 006 SPIE 

conference, with a large involvement in 

the organisation and numerous presentations 

by ESO staff. The SPIE meeting 

also allowed for starting most fruitful discussions 

with other ELT groups, especially 

the TMT, that have since been ongoing. 

Equally, in November, a top-level meeting 

on exoplanets took place in Washington 

D.C. between ESO, ESA, NSF and NASA. 

Back in Europe, the IAU General Assembly 

was held in Prague. These triennial 

events always provide a unique opportunity 

to experience first-hand the progress 

across the entire range of astronomy, 

as well as to meet friends and colleagues 

from one’s own and other sub-fields, and 

this General Assembly certainly lived 

up to expectation. Some 800 participants 

from around the world attended the 

event. Again, ESO was well presented, 

in the various sessions and also with a 

major information stand – fitting in the 

context of our ongoing talks with the 

Czech Republic. 

We continued our collaboration with ESA, 

with the publication of two joint reports 

on Herschel/ALMA synergies and fundamental 

cosmology, respectively, as visible 

signs of the coordination efforts in this 

field on our continent. 

In June, with our Chilean colleagues we 

celebrated the 10th anniversary of the 

supplementary agreement with Chile, 

which not only paved the way for ESO’s 

operations in Chile in the VLT era, but 

also provided strong impulses to Chilean 

astronomy. Some of the results are described 

in the book “10 Years Exploring 

the Universe” that was published on this 

occasion. We are pleased that our relations 

with Chile, its scientific community 

and its people, remain strong and positive. 

Moving from international relations in general 

to the issue of new member states, 

we were happy when, in February, Spain 

took a decisive step towards full membership 

with the signing in Madrid of a 

statement aiming at accession to the 

ESO Convention effective from 1 July. 

As it turned out, the ratification process 

needed more time and the last steps remained 

to be completed by the end of 

the year. Nonetheless, we were assured 

by the Spanish authorities of the intent 

to respect the accession date, as set out 

in the February statement. 

In parallel, negotiations with the Czech 

Republic progressed rapidly. At the 

December meeting, Council approved 

the agreement, which foresaw Czech 

membership as of 1 January 007. A few 

days later, the agreement was also approved 

by the Czech Government, and 

on December the agreement was 

signed at a ceremony in Prague. As in the 

case of Spain, however, the parliamentary 

approval and the subsequent deposition 

of the instrument of ratification remained 

to be completed. 

ESO is a high-tech research organisation 

with a global perspective. As such it must 

meet the challenges of the dynamic, international 

labour market, competing for 

the best and most talented staff. With the 

opening of the IPP/ESO crèche for our 

staff in Garching, we have taken further 

steps to create a working climate that 

is also amenable to family needs. In Chile, 

we entered collective bargaining, concluding 

collective arrangements valid for 

three years. 

Having physical surroundings that foster 

human and intellectual exchange is another 

important element. It is therefore 

good that the long-awaited expansion of 

our Headquarters building moved clos- 

er as, with the help of the German authorities, 

we made progress towards securing 

the land to the south of the existing 

premises. 

In its 45th year, ESO remains a strong 

and dynamic organisation, not just full of 

ideas and initiatives but with a clear will 

to harness these into projects that can 

serve our users. An important tool in this 

process is the Medium Range Implementation 

Plan, which was endorsed by 

Council at its December meeting. This 

plan provides a clear path for ESO’s development 

over the next four years; now 

it is for us to turn it into reality. 

Catherine Cesarsky 

Director General, ESO 


9

Research Highlights 

In 006 ESO again proved that it has 

the telescopes and instruments to maintain 

its lead position in the quest for 

exoplanets, that is, planets that orbit a 

star other than the Sun. Using a variety 

of telescopes, at La Silla and Paranal, 

astronomers were able to find the smallest 

exoplanet yet discovered — a five- 

Earth-mass icy world — as well as a complete 

planetary system composed of 3 

Neptune-mass planets. Also noteworthy 

is the study of free-floating planets that 

appear to harbour discs and even form as 

twins, thereby sharing many properties 

of stars. 

The Comet With a Broken Heart 

On the night of 3/ 4 April, ESO’s Very 

Large Telescope observed fragment B of 

the comet Schwassmann-Wachmann 

3 that had split a few days earlier. To their 

great surprise, the ESO astronomers 

discovered that the piece just ejected by 

fragment B was splitting again! Five 

other mini-comets are also visible on the 

image. The comet seems thus doomed 

to disintegrate but the question remains in 

how much time. 

Comet 73P/Schwassmann-Wachmann 3 

(SW 3) is a body with a very tormented 

past. This comet revolves around the Sun 

in about 5.4 years, in a very elongated 

orbit that brings it from inwards of the 

Earth’s orbit to the neighbourhood of giant 

planet Jupiter. In 1995, when it was 

coming ‘close’ to the Earth, it underwent 

a dramatic and completely unexpected, 

thousandfold brightening. Observations 

in 1996, with ESO’s New Technology 

Telescope and 3.6-m telescope, at La 

Silla, showed that this was due to the fact 

that the comet had split into three distinct 

pieces. Later, in December 1996, two 

more fragments were discovered. At the 

last comeback, in 001, of these five 

10 


Talking about discs, the VISIR instrument 

allowed astronomers to map a disc 

around a very young star, possibly witnessing 

the precursor of a planetary system. 

But it is not all about stars and planets. 

In 006, astronomers provided unique 

insights into two classes of important 

objects in cosmology, Cepheids and 

Type Ia supernovae. 

They also have revealed several cases of 

stellar vampirism, including one on a 

very big scale. In other studies, they have 

provided important clues on the past 

of our own Galaxy. Looking farther away, 

SINFONI on the VLT made a record 

fragments only three were still seen, the 

fragments C (the largest one), B and E. 

No new fragmentations happened during 

this approach, apparently. 

Things were different this time, when the 

comet moved again towards its closest 

approach to the Sun – and to the Earth. 

Early in March, seven fragments were 

observed, the brightest (fragment C) 

being of magnitude 1 , i.e. 50 times 

fainter than what the unaided eye can 

see, while fragment B was 10 times fainter 

still. In the course of March, 6 new 

fragments were seen. 

Early in April, fragment B went into outburst, 

brightening by a factor 10 and 

on 7 April, six new fragments were discovered, 

confirming the high degree of 

fragmentation of the comet. On 1 April, 

fragment B was as bright as the main 

fragment C, with a magnitude around 9 

(16 times fainter than what a keen 

observer can see with unaided eyes). 

Fragment B seems to have fragmented 

again, bringing the total of fragments 

close to 40, some being most probably 

very small, boulder-sized objects with 

irregular and short-lived activity. 

observation of a very young galaxy, showing 

that it formed very quickly, contrarily 

to previous beliefs. The VLT also helped 

discover a ‘blob’ twice as large as the 

Milky Way and emitting as much as 

several billion suns, yet it is invisible in 

normal light! In another bout of magic, the 

VLT also studied an invisible galaxy, from 

the imprint it leaves on the spectrum of a 

distant quasar acting as a beacon. 

One cannot doubt that the Universe has 

still many surprises in store but it seems 

also evident from the few Research 

Highlights presented here that ESO 

telescopes are revealing more and more 

of them every day! 

The new observations reveal that this 

new small fragment has split again! The 

image clearly reveals that below the 

main B fragment, there is a small fragment 

that is divided into two and a 

careful analysis reveals five more tiny fragments 

almost aligned. Thus, this image 

alone shows at least 7 fragments. The 

comet has thus produced a whole set of 

mini-comets! 

Mini-comets coming off comet SW 3.

An Icy 5 Earth-mass Exoplanet 

Driven by the need for increasing efficiency 

to address current frontline research 

topics, astronomy is moving more and 

more in the direction of huge international 

teams working together, not unlike what 

has been the rule for many years in particle 

physics. Nothing can better illustrate 

this trend than the discovery of the 

smallest exoplanet. This incredible result 

is a joint effort of three independent 

campaigns: PLANET/RoboNet, OGLE, 

and MOA, involving a total of 73 collaborators 

affiliated with 3 institutions in 1 

countries. 

Designated by the unglamorous identifier 

of OGLE- 005-BLG-390Lb, the alien 

world is a five Earth-mass object located 

0 000 lightyears away, not far from the 

centre of our Milky Way galaxy. 

Contrary to most of the more than 00 

exoplanets discovered until now, 

OGLE- 005-BLG-390Lb was found using 

the ‘microlensing’ technique. This method 

is based on the fact that the gravity of 

a dim, intervening star can act as a giant 

natural telescope, magnifying a more 

distant star, which then temporarily looks 

brighter. A small ‘glitch’ in the brightening 

reveals the existence of a planet around 

the lens star. Neither the planet nor the 

star that it is orbiting can be seen, only 

the effect of their gravity. Such an 

intervening star causes a characteristic 

brightening that lasts about a month. 

Any planets orbiting this star can produce 

an additional signal, lasting from days for 

giant planets down to hours for Earthmass 

planets. 

In order to be able to catch and characterise 

these planets, nearly-continuous 

round-the-clock high-precision monitoring 

of ongoing microlensing events is 

required. This is the goal of the PLANET 

network of 1-m-class telescopes consisting 

of the ESO 1.54-m Danish at La 

Silla (Chile), the Canopus Observatory 

1.0-m (Hobart, Tasmania, Australia), 

the Perth 0.6-m (Bickley, Western Australia), 

the Boyden 1.5-m (South Africa), 

and the SAAO 1.0-m (Sutherland, South 

Africa). Since 005, PLANET has 

operated a common campaign with 

RoboNet, a UK-operated network of -m 

fully robotic telescopes currently comprising 

the Liverpool Telescope (Roque 

de Los Muchachos, La Palma, Spain) and 

the Faulkes Telescope North (Haleakala, 

Hawaii, USA). 

The OGLE (Optical Gravitational Lensing 

Experiment) search team discovered 

the event OGLE- 005-BLG-390 on 11 

July 005, triggering the PLANET telescopes 

to start taking data. A light curve 

consistent with a single lens star peaking 

at an amplification of about 3 on 31 July 

005 was observed, until 10 August 

when a PLANET member, observing at 

the Danish 1.54-m at ESO La Silla, noticed 

a planetary deviation. An OGLE 

point from the same night showed the 

same trend, while the last half of the planetary 

deviation, lasting about a day, had 

been covered by images from Perth 

Observatory. The MOA (Microlensing 

Observations in Astrophysics) collaboration 

was later able to identify the source 

star on its images and confirmed the 

deviation. 

The new planet orbits a red star five times 

less massive than the Sun in about 

10 years. It is the least massive exoplanet 

around an ordinary star detected so far, 

and also the coolest: its relatively cool 

parent star and large orbit implies that 

the likely surface temperature of the 

planet is 0 degrees Celsius below zero, 

too cold for liquid water. It is likely to have 

a thin atmosphere, like the Earth, but its 

rocky surface is probably deeply buried 

beneath frozen oceans. It may therefore 

more closely resemble a more massive 

version of Pluto, rather than the rocky 

inner planets like Earth and Venus. 

Astronomers claim that this planet is 

actually the first and only planet that 

has been discovered so far that is in 

agreement with the theories for how 

our Solar System formed. The favoured 

theoretical explanation for the formation 

of planetary systems proposes that solid 

‘planetesimals’ accumulate to build up 

planetary cores, which then accrete 

nebular gas – to form giant planets – if 

they are sufficiently massive. Around red 

dwarfs, the most common stars of our 

Galaxy, this model favours the formation 

of Earth- to Neptunemass planets being 

between 1 and 10 times the Earth-Sun 

distance away from their host. 

OGLE- 005-BLG-390Lb is only the third 

extrasolar planet discovered so far 

through microlensing searches. While the 

other two microlensing planets have 

masses of a few times that of Jupiter, the 

discovery of a 5 Earth-mass planet – 

despite being much harder to detect than 

more massive ones – is a strong hint 

that these lower-mass objects are very 

common. In particular, astronomers now 

think that such frozen worlds are much 

more common than their larger, Jupiterlike 

brethren, as otherwise the microlensing 

method should have found dozens of 

them by now. 

There is no doubt that the discovery of 

this planet marks a groundbreaking result 

in the search for planets that support life. 

J.-P. Beaulieu, D. P. Bennett, P. Fouqué, A. Williams, 

M. Dominik, U. G. Jørgensen, D. Kubas et al., Nature, 

6 January 006. 

Artist’s Impression of the Icy Exoplanet. 

Light Curve of OGLE- 005-BLG-390. 


11

Trio of Neptunes and their Belt 

A most unusual planetary system has 

been found, in which a nearby star is hosting 

three Neptune-mass planets. The 

innermost planet is most probably rocky, 

while the outermost is the first known 

Neptune-mass planet to reside in the habitable 

zone. This unique system is likely 

further enriched by an asteroid belt. 

A planet in orbit around a star will manifest 

its presence by pulling the star in 

different directions, thereby changing its 

measured velocity by very small amounts. 

Astronomers therefore measure the 

velocity of a star with very high precision 

to detect the signature of one or more 

planets. Certainly the best instrument to 

do this kind of work is the High Accuracy 

Radial velocity Planet Searcher (HARPS) 

at the ESO La Silla 3.6-m telescope, a 

fibre-fed high-resolution echelle spectrograph 

that has demonstrated a longterm 

precision of about 1 m/s. 

During more than two years, a team of 

astronomers used HARPS to monitor the 

velocity of HD 69830, a rather inconspicuous 

nearby star slightly less massive 

than the Sun. Located 41 light-years 

away towards the constellation of Puppis 

(the Stern), it is, with a visual magnitude 

of 5.95, just visible with the unaided eye. 

Precise measurements allowed the 

astronomers to discover the presence of 

three tiny companions orbiting their 

parent star in 8.67, 31.6 and 197 days. 

The detected velocity variations are between 

and 3 metres per second, 

Increasing the Odds of the Sweep 

The VLT has confirmed the extrasolar 

planet status of two of the 16 candidates 

discovered by the NASA/ESA Hubble 

Space Telescope. 

The 16 candidates were uncovered 

during an international HST survey, called 

the ‘Sagittarius Window Eclipsing 

Extrasolar Planet Search’, or SWEEPS. 

HST couldn’t see the 16 newly found planet 

candidates directly. Instead, astronomers 

used HST to search for planets by 

measuring the slight dimming of a star 

due to the passage of a planet in front of 

it. This event is called a transit. The 

1 


Impression of the planetary system around HD 69830. 

corresponding to about 9 km/h! That’s 

the speed of a person walking briskly. 

Such tiny signals could not have been 

distinguished from ‘simple noise’ by most 

of today’s available spectrographs. 

The newly found planets have minimum 

masses between 10 and 18 times the 

mass of the Earth. Extensive the oretical 

simulations favour an essentially rocky 

composition for the inner planet, and a 

rocky/gas structure for the middle one. 

The outer planet has probably accreted 

some ice during its formation, and is likely 

to be made of a rocky/icy core surrounded 

by a quite massive envelope. Further 

calculations have also shown that the 

system is in a dynamically stable configuration. 

The outer planet also appears to be located 

near the inner edge of the habitable 

zone, where liquid water can exist 

planet would have to be about the size of 

Jupiter to block enough starlight, about 

1 to 10 per cent, to be measurable by 

HST. These objects are called planetary 

‘candidates’ because astronomers 

cannot be sure of their mass, and hence 

of their status, without further spectroscopic 

measurements. 

For two of the stars, the SWEEPS team 

could use the UVES and FLAMES 

instruments on the VLT to make an independent 

confirmation of a planet’s 

presence by spectroscopically measuring 

a slight wobble in the star’s motion 

due to the gravitational pull of an unseen 

at the surface of rocky/icy bodies. 

Although this planet is probably not Earthlike 

due to its heavy mass, its discovery 

opens the way to exciting possibilities. 

This alone would make this system already 

exceptional. But the recent discovery 

by the Spitzer Space Telescope 

that the star most likely hosts an asteroid 

belt adds the cherry to the cake. With 

three roughly equal-mass planets, one 

being in the habitable zone, and an asteroid 

belt, this planetary system shares 

many properties with our own Solar System. 

The planetary system around HD 

69830 clearly represents a ‘Rosetta 

stone’ for our understanding of how 

planets form. No doubt it will help us 

better understand the huge diversity we 

have observed since the first extrasolar 

planet was found in 1995. 

Christophe Lovis et al., Nature, 18 May 006. 

companion. One of the planetary 

candidates has a mass below 3.8 Jupiter 

masses. It orbits its host star, which 

is 5% more massive than the Sun, in 4. 

days. The other candidate’s mass is 

9.7 Jupiter masses. 

These are the faintest stars with planets 

that have been confirmed by radial 

velocities so far. To confirm the other planet 

candidates one would need a much 

bigger telescope on Earth, such as 

the European Extremely Large Telescope. 

Kailash Sahu et al., Nature, 5 October 006.

Do ‘Planemos’ Have Progeny? 

Two new studies show that objects only a 

few times more massive than Jupiter are 

born with discs of dust and gas, the raw 

material for planet-making. This suggests 

that miniature versions of the Solar 

System may circle objects that are some 

100 times less massive than our Sun. 

What’s more, such objects appear also to 

be able to form as twins: an approximately 

seven-Jupiter-mass companion 

was found orbiting an object that is itself 

only twice as hefty. The existence of such 

a double system puts strong constraints 

on formation theories of free-floating 

planetary-mass objects. 

Since a few years ago, it has been known 

that many young brown dwarfs — 

‘failed stars’ that weigh less than 8 per 

cent the mass of the Sun — are surrounded 

by a disc of material. This may 

indicate these objects form in the same 

way as our Sun. The new findings confirm 

that the same appears to be true for their 

even punier cousins, sometimes called 

free-floating planetary mass objects or 

‘planemos’. These objects have masses 

similar to those of extrasolar planets, but 

they are not in orbit around stars – 

instead, they float freely. 

In a way, the new discoveries are not too 

surprising – after all, Jupiter must have 

been born with its own disc, out of which 

its bigger moons formed. Still they may 

lead to a revision of our understanding of 

planetary formation as, unlike Jupiter, 

these planemos are not circling stars. 

The first study used two of ESO’s telescopes 

– Antu, the 8. -metre Unit Telescope 

no. 1 of the Very Large Telescope, 

and the 3.5-metre New Technology 

Telescope – to obtain optical spectra of 

six candidates identified recently by 

researchers at the University of Texas at 

Austin. Two of the six turned out to 

have masses between five and 10 times 

that of Jupiter while two others are 

a tad heftier, at 10 to 15 times Jupiter’s 

mass. All four of these objects are 

‘newborns’, just a few million years old, 

and are located in star-forming regions 

about 450 light years from Earth. The 

planemos show infrared emission from 

dusty discs that may evolve into miniature 

planetary systems over time. 

The other study also used the Very Large 

Telescope, but this time with its adaptive 

optics system and infrared camera 

NACO, to obtain images and spectra of 

a planetary-mass companion discovered 

two years ago at ESO around a young 

brown dwarf that is itself about 5 times 

the mass of Jupiter. 

This planetary-mass companion is the 

first-ever exoplanet to have been imaged. 

The brown dwarf, dubbed M1 07 for 

short and located 170 light years from 

Earth, was known to be surrounded by a 

disc. Now, evidence has been found for 

a disc around the eight-Jupiter-mass 

companion as well. 

The pair probably formed together, like a 

petite stellar binary, instead of the 

companion forming in the disc around the 

brown dwarf like a star-planet system. 

It is also possible that smaller planets or 

asteroids could now form in the disc 

around each one. 

Astronomers have in fact found a double 

system composed of even smaller 

objects. Oph 16 5- 40515, or Oph 

16 for short, is the first planemo found 

to be a double. Researchers discovered 

the companion candidate in an optical 

image taken with the NTT, then took 

optical spectra and infrared images of the 

pair with the VLT to make sure that it is a 

true companion, instead of a foreground 

or background star that happens to be in 

the same line of sight. These follow-up 

observations indeed confirmed that both 

objects are young, at the same distance, 

and much too cool to be stars. This 

suggests the two are physically associated. 

By comparing to widely used theoretical 

models, the astronomers estimate 

that the companion is about seven times 

the mass of Jupiter, while the more 

massive object comes in at about 14 

times Jupiter’s mass. The newborn pair, 

barely a million years old, is separated 

by about six times the distance between 

the Sun and Pluto, and is located in 

the Ophiuchus star-forming region approximately 

400 light years away. 

Planets are thought to form out of discs 

of gas and dust that surround stars, 

brown dwarfs, and even some free-floating 

planetary mass objects, as described 

above. But, it is likely that these planemo 

twins formed together out of a contracting 

gas cloud that fragmented, like a 

miniature stellar binary. 

Oph 16 B is only the second or third 

directly-imaged planetary-mass companion 

to be confirmed spectroscopically, 

and the first one around a primary that is 

itself a planetary-mass object. Its existence 

poses a challenge to a popular 

theoretical scenario, which suggests that 

brown dwarfs and free-floating planetary- 

mass objects are embryos ejected from 

multiple protostar systems. 

Since the two objects in Oph16 are so 

far apart, and only weakly bound to each 

other by gravity, they would not have 

survived such a chaotic birth. 

Recent discoveries have revealed an 

amazing diversity of worlds out there. 

Still, the Oph16 pair stands out as one 

of the most intriguing. Now, the as- 

tronomers are curious to find out whether 

such pairs are common or rare. The 

answer could shed light on how free- 

floating planetary-mass objects form. 

Ray Jayawardhana & Valentin Ivanov, American 

Astronomical Society, June 006, Calgary, Canada. 

Ray Jayawardhana & Valentin D. Ivanov, Science, 3 

August 006. 

Subhanjoy Mohanty et al., American Astronomical 

Society, June 006, Calgary, Canada. 

Spectra of candidate ‘planemos’. 


13

Watching How Planets Form 

The disc around a star more massive 

than the Sun has been mapped, revealing 

a very extended and flared disc that most 

likely contains enough gas and dust to 

spawn planets. It appears as a precursor 

of debris discs such as the one around 

Vega-like stars and so provides the rare 

opportunity to witness the conditions 

prevailing prior to or during planet 

formation. 

Planets form in massive, gaseous and 

dusty protoplanetary discs that surround 

nascent stars. This process must be 

rather ubiquitous given the many exoplanets 

already known. However, very little 

is known about these discs, especially 

those around stars more massive than the 

Sun. Such stars are much more luminous 

and could have a large influence on their 

disc, possibly quickly destroying the inner 

part. 

Astronomers used the VISIR instrument 

on the VLT to map the disc surrounding 

the young star HD 97048 in the infrared. 

HD97048 has an age of a few million 

years – a blink of an eye compared to the 

age of the Sun (4.6 billion years) – and 

belongs to the Chameleon I dark cloud, 

a stellar nursery 600 lightyears away. 

14 


Sketch of a flared proto-planetary disc such as the one around the young star HD 97048. 

The star is 40 times more luminous than 

our Sun and is .5 times as massive. 

The astronomers could only have 

achieved such a detailed view due to the 

high angular resolution offered by an 8metre-size 

telescope in the infrared, 

reaching a resolution of 0.33 arcsecond. 

They discovered a very large disc, at 

least 1 times more extended than the 

or-bit of the farthest planet in the Solar 

System, Neptune. The observations suggest 

that the disc is flared, the first time 

such a structure, predicted by some 

theoretical models, has been imaged 

around a massive star. 

Such geometry can only be explained 

if the disc contains a large amount of 

gas, in this case, at least as much as 10 

times the mass of Jupiter. It should also 

contain more than 50 Earth masses in 

dust. 

The dust mass derived here is more 

than thousand times larger than what is 

observed in debris discs and Kuiper- 

belt-like structures found around older, 

‘Vega-like’ stars, such as Beta Pictoris, 

Vega, Fomalhaut and HR 4796, and 

which is thought to be produced by 

collisions of larger bodies. 

The dust mass observed around HD 

97048 is similar to the mass invoked for 

the (undetected) parent bodies in the 

more evolved systems. HD 97048’s disc 

is thus most likely a precursor of debris 

discs observed around older stars. 

From the structure of the disc, the astronomers 

gather that planetary embryos 

may be present in the inner part of the 

disc. Follow-up observations at higher 

angular resolution with the VLT interferometer 

(VLTI) should allow them to probe 

these regions. 

Pierre-Olivier Lagage et al., Science, 8 September 

006.

A Substellar Jonah 

Astronomers have discovered a rather unusual 

system, in which two planet-size 

stars, of different colours, orbit each other. 

One is a rather hot white dwarf, weighing 

a little bit less than half as much as the 

Sun. The other is a much cooler, 55 

Jupiter-masses brown dwarf. 

The low-mass companion to the white 

dwarf (named WD0137-349) was found 

using spectra taken with EMMI at the New 

Technology Telescope at La Silla. The 

astronomers then used the UVES spectrograph 

on the VLT to record 0 spectra 

and so measure the period and the mass 

ratio. 

Numerical simulations of a brown dwarf being swallowed by a red giant. 

The two objects, separated by less than 

/3 of the radius of the Sun, or only a 

few thousandths of the distance between 

the Earth and the Sun, rotate around 

each other in about hours. The brown 

dwarf moves on its orbit at the amazing 

speed of 800 000 km/h! 

The two stars were not so close in their 

past. Only when the solar-like star 

that has now become a white dwarf was 

a red giant did the separation between 

the two objects diminish drastically. During 

this fleeting moment, the giant engulfed 

its companion. The latter, feeling a 

large drag similar to trying to swim in 

a bath full of oil, spiralled in towards the 

core of the giant. The envelope of the 

giant was finally ejected, leaving a binary 

system in which the companion is in a 

close orbit around a white dwarf. 

Image: Los Alamos National Laboratory 

The existence of the system proves that 

the brown dwarf came out almost 

unaltered from an episode in which it was 

swallowed by a red giant. Models show 

that had the companion been less than 

0 Jupiter masses, it would have 

evaporated during this phase. The brown 

dwarf shouldn’t rejoice too quickly to 

have escaped this doom, however. 

Einstein’s General Theory of Relativity 

predicts that the separation between the 

two stars will slowly decrease. In about 

1.4 billion years, the orbital period will 

have decreased to slightly more than one 

hour. At that stage, the two objects will 

be so close that the white dwarf will work 

as a giant ‘vacuum cleaner’, drawing gas 

off its companion, in a cosmic cannibal 

act. 

Pierre Maxted et al., Nature, 3 August 006. 


15

Stellar Vampires Unmasked 

Some hot, bright, and apparently young 

stars – known as ‘blue stragglers’ – in the 

globular cluster 47 Tucanae contain less 

carbon and oxygen than the majority of 

their sisters. This indicates that these few 

stars likely formed by taking their material 

from another star, acting as stellar 

vampires. 

Blue stragglers are unexpectedly younglooking 

stars found in stellar aggregates, 

such as globular clusters, which are 

known to be made up of old stars. 

These enigmatic objects are thought to be 

created in either direct stellar collisions 

or through the evolution and coalescence 

of a binary star system in which one 

star ‘sucks’ material off the other, rejuvenating 

itself. As such, they provide 

interesting constraints on both binary stellar 

evolution and star-cluster dynamics. 

To date, the unambiguous signatures of 

either stellar traffic accidents or stellar 

vampirism have not been observed, and 

the formation mechanisms of blue stragglers 

are still a mystery. 

16 


Oxygen Abundance 

Abundances in blue straggler stars. 

The VLT was used to measure the abundance 

of chemical elements at the 

surface of 43 blue straggler stars in the 

globular cluster 47 Tucanae, an impressive 

globular cluster that has a total 

mass of about 1 million times the mass of 

the Sun and is 1 0 light years across. 

Measurements of so many faint stars are 

only possible since the advent of 8-m- 

class telescopes equipped with spectrographs 

which have multiplexing capability. 

In this case, the astronomers used 

the FLAMES/GIRAFFE instrument, that 

allows the simultaneous observation of 

up to 130 targets at a time, making it 

ideally suited for surveying individual stars 

in closely populated fields. 

Six of these blue straggler stars were 

found to contain less carbon and oxygen 

than the majority of these peculiar 

objects. Such an anomaly indicates that 

the material at the surface of the blue 

stragglers comes from the deep interiors 

of a parent star. Such deep material can 

reach the surface of the blue straggler 

only during the mass transfer process 

occurring between two stars in a binary 

system. Numerical simulations indeed 

show that the coalescence of stars should 

not result in anomalous abundances. 

Carbon Abundance 

In the core of a globular cluster, stars are 

packed extremely close to each other: 

more than 4 000 stars are found in the innermost 

lightyear-sized cube of 47 

Tucanae. Thus, stellar collisions are 

thought to be very frequent and the collision 

channel for the formation of blue 

stragglers should be extremely efficient. 

The chemical signature detected by these 

observations demonstrates that the 

binary mass-transfer scenario is also fully 

active, even in a high-density cluster like 

47 Tucanae. 

This is the first detection of a chemical signature 

clearly pointing to a specific 

scenario to form blue straggler stars and 

therefore a fundamental step toward the 

solution of the long-standing mystery of 

blue-straggler formation in globular 

clusters. 

Francesco R. Ferraro et al. 006, Astrophys. Journal 

Lett., 647, L53.

Cepheids and their ‘Cocoons’ 

Combining data from the Very Large 

Telescope Interferometer (VLTI) and the 

CHARA Interferometer at Mount Wilson, 

California, astronomers have discovered 

envelopes around three Cepheids, including 

the Pole Star. This is the first time 

that matter has been found surrounding 

members of this important class of rare 

and very luminous stars whose luminosity 

varies in a very regular way. 

Cepheids are commonly used as distance 

indicators, thanks to the existence 

of a basic relation between their intrinsic 

brightness and their pulsation period. By 

measuring the period of a Cepheid star, 

its intrinsic brightness can be deduced, 

and from the observed apparent brightness 

the distance may then be calculated. 

As they are intrinsically very bright 

stars, and can be observed in distant 

galaxies, this remarkable property has 

turned these yellow supergiant stars into 

primary ‘standard candles’ for extragalactic 

distance estimations. Cepheids 

thus play a crucial role in cosmology, 

being one of the first ‘steps’ on the 

cosmic distance ladder. 

The southern Cepheid L Carinae was observed 

with the VINCI and MIDI instrument 

at the VLTI, while Polaris (the Pole 

Star) and Delta Cephei were scrutinised 

with FLUOR on CHARA, located on the 

other side of the equator. FLUOR is the 

prototype instrument of VINCI, both being 

built by the Paris Observatory (France). 

L Carinae is the brightest Cepheid in the 

sky, and also the one that presents 

the largest apparent angular diameter. 

It is a massive supergiant star, having 

about 10 times the mass of the Sun and 

approximately 180 times its radius. 

Polaris is a peculiar star located very close 

to the north celestial pole (hence its 

name). It is classified as a Cepheid, but it 

shows very weak pulsations compared 

to the other stars of its class. Delta 

Cephei is the prototype of the Cepheids. 

It was discovered to be a variable star in 

the 18th century by the English amateur 

John Goodricke, and it is still one of the 

brightest members of the Cepheid class. 

Its short period is characteristic of a 

relatively small supergiant, with a radius 

of ‘only’ 43 times that of the Sun. 

Although such stars are thus rather large, 

they are so far away that they cannot 

be resolved by single telescopes. Indeed, 

even the largest Cepheids in the sky 

subtend an angle of only 0.003 arc second. 

To resolve this would be similar to 

viewing a two-storey house on the Moon. 

Astronomers therefore have to rely on the 

interferometric technique, which combines 

the light of two or more distant telescopes, 

providing the angular resolution 

of a single telescope as large as the 

separation between them. With the VLTI, 

it is possible to achieve a resolution of 

0.001 arcsecond or less. 

For most stars, the observations made 

with interferometers follow the theoretical 

stellar models very closely. However, for 

these three stars a tiny deviation was 

detected, revealing the presence of an 

envelope. The envelopes were found to 

be to 3 times as large as the star itself. 

The fact that such deviations were found 

for all three stars, which have very 

different properties, seems to imply that 

envelopes surrounding Cepheids are 

a widespread phenomenon. The physical 

processes that have created these 

envelopes are still uncertain, but, in analogy 

to what happens around other 

classes of stars, it is most probable that 

the environments were created by matter 

ejected by the star itself. Cepheids 

pulsate with periods of a few days. 

As a consequence, the star goes regularly 

through large-amplitude oscillations 

that create very rapid motions of its 

apparent surface (the photosphere) with 

velocities up to 30 km/s, or 108 000 km/ 

h! While this remains to be established, 

there could be a link between the 

pulsation, the mass loss and the formation 

of the envelopes. 

P. Kervella et al. 006, Astronomy and Astrophysics, 

448, 6 3. 

Antoine Mérand et al. 006, Astronomy and 

Astrophysics, 453, 155. 

Model image of the Cepheid L Carinae. 


17

To Be or Not to Be: Is It All About Spinning? 

A study of the active hot star Alpha Arae 

solves a 140-year-old mystery. 

Lying about 300 light years away from the 

Sun, Alpha Arae is the closest member of 

the class of active stars known as ‘Be 

stars’. Be stars are very luminous, 

massive and hot stars that rotate rapidly. 

They are losing mass along the poles 

through a strong stellar wind and are 

surrounded at the equator by a disc of 

matter. Alpha Arae has ten times the mass 

of the Sun, is three times hotter and 6 000 

times as luminous. 

With AMBER on the VLTI, the team of astronomers 

were able to examine the 

structure of the disc surrounding Alpha 

Arae in detail. Moreover, because AMBER 

also provides spectra, the astronomers 

could study the motion of the gas in the 

disc and so understand how it rotates. 

The disc surrounding Alpha Arae was 

found to be in ‘Keplerian rotation’, that is, 

obeying the same rules as discovered by 

Johannes Kepler for the planets circling 

the Sun: the velocity of the material 

decreases with the square root of the 

distance from the star. The new result 

rules out the possibility of the disc 

rotating with a uniform velocity, as would 

be the case if a strong magnetic field 

were present which forced the matter to 

spin at the same rate as the star. 

Combining the new data with previous 

studies, the astronomers also show that 

the star Alpha Arae rotates 50 times 

faster than our Sun. In fact, with a speed 

at the equator of 470 km/s, it is spinning 

so quickly that it is near its break-up 

velocity. Matter having such a critical 

velocity would be able to freely escape 

from the star, in the same way that we 

would be ejected from a merry-go-round 

that has gone out of control. This could 

be the clue to the ‘Be phenomenon’. 

A. Meilland et al., 007, Astronomy and Astrophysics, 

464, 549. 

18 


Artist’s rendering of the Be star Alpha Arae.

Asymmetric Ashes 

Astronomers are reporting remarkable 

new findings that shed light on a decadelong 

debate about one type of the 

supernova explosions that mark a star’s 

final demise: does the star die in a slow 

burn or with a fast bang? From their 

observations, the scientists find that the 

matter ejected by the explosion shows 

significant peripheral asymmetry but a 

nearly spherical interior, most likely implying 

that the explosion finally propagates 

at supersonic speed. 

Using observations of 17 supernovae 

made over more than 10 years with the 

VLT for one part and the McDonald 

Observatory’s Otto Struve Telescope for 

another, astronomers inferred the shape 

and structure of the debris cloud thrown 

out from Type Ia supernovae. Such 

supernovae are thought to be the result 

of the explosion of a small and dense star 

– a white dwarf – inside a binary system. 

As its companion continuously spills 

matter onto the white dwarf, the white 

dwarf reaches a critical mass, leading to 

a fatal instability and the supernova. But 

what sparks the initial explosion, and how 

the blast travels through the star have 

long been thorny issues. 

Artist’s impression of a clumpy SN Ia explosion. 

The supernovae that were observed occurred 

in distant galaxies, and because 

of the vast cosmic distances could not be 

studied in detail using conventional 

imaging techniques, including interferometry. 

Instead, the team of researchers 

determined the shape of the exploding 

cocoons by recording the polarisation 

of the light from the dying stars. 

Polarimetry relies on the fact that light is 

composed of electromagnetic waves that 

oscillate in certain directions. Reflection 

or scattering of light favours certain orientations 

of the electric and magnetic 

fields over others. This is why polarising 

sunglasses can filter out the glint of 

sunlight reflected off a pond. When light 

scatters through the expanding debris of 

a supernova, it retains information about 

the orientation of the scattering layers. If 

the supernova is spherically symmetric, all 

orientations will be present equally and 

will average out, so there will be no net 

polarisation. If, however, the gas shell is 

not round, a slight net polarisation will be 

imprinted on the light. 

This is what broadband polarimetry can 

accomplish. If additional spectral in- 

formation is available (‘spectropolarimetry’), 

one can determine whether the 

asymmetry is in the continuum light or in 

some spectral lines. In the case of the 

Type Ia supernovae, the astronomers 

found that the continuum polarisation is 

very small, implying that the overall shape 

of the explosion is crudely spherical. But 

the much larger polarisation in strongly 

blue-shifted spectral lines shows the 

presence, in the outer regions, of fast- 

moving clumps with peculiar chemical 

composition. 

The study reveals that explosions of Type 

Ia supernovae are truly three-dimensional 

phenomena. The outer regions of the 

blast cloud are asymmetric, with different 

materials found in ‘clumps’, while the 

inner regions are smooth. 

The research team first spotted this 

asymmetry in 003, as part of the same 

observational campaign. The new, more 

extensive results show that the degree of 

polarisation, and hence the asphericity, 

correlates with the intrinsic brightness of 

the explosion. The brighter the supernova, 

the smoother, or less clumpy, it is. 

This has some impact on the use of Type 

Ia supernovae as standard candles. 

This kind of supernovae is used to measure 

the rate of acceleration of the expansion 

of the Universe, assuming these 

objects behave in a uniform way. But 

asymmetries can introduce dispersions in 

the quantities observed. 

The discovery also puts strong constraints 

on any successful models of 

thermonuclear supernova explosions. 

Models have suggested that the clumpiness 

is caused by a slow-burn process, 

called ‘deflagration’, and leaves an irregular 

trail of ashes. The smoothness of 

the inner regions of the exploding star 

implies that at a given stage, the deflagration 

gives way to a more violent process, 

a ‘detonation’, which travels at supersonic 

speeds – so fast that it erases all 

the asymmetries in the ashes left behind 

by the slower burning of the first stage, 

resulting in a smoother, more homogeneous 

residue. 

Lifan Wang, Dietrich Baade and Ferdinando Patat, 

Science Express, 30 November 006. 


19

How to Steal a Million Stars? 

In another bout of stellar vampirism, but 

on a grand scale, astronomers found that 

the stellar cluster Messier 1 must have 

lost close to one million low-mass stars to 

the rest of the Milky Way galaxy. 

The astronomers measured the brightness 

and colours of more than 16 000 

stars within the globular cluster Messier 

1 with the FORS1 multimode instrument 

attached to one of the Unit Telescopes of 

ESO’s VLT at Cerro Paranal (Chile). The 

astronomers could study stars that are 

40 million times fainter than what the 

unaided eye can see. 

Messier 1 is one of about 00 globular 

clusters known in our Galaxy. These are 

large groupings of from 10 000 to more 

than a million stars that were formed 

together in the youth of the Milky Way, 

about 1 to 13 billion years ago. Globular 

clusters are a key tool for astronomers, 

because all the stars in a globular cluster 

share a common history. They were 

all born together, at the same time and 

place, and only differ from one another in 

their mass. By accurately measuring 

the brightness of the stars, astronomers 

can determine their relative sizes and 

stage of evolution precisely. Globular 

clusters are thus very helpful for testing 

theories of how stars evolve. 

Located at a distance of 3 000 light 

years in the constellation Ophiuchus 

(The Serpent-holder), Messier 1 got its 

name by being the 1 th entry in the catalogue 

of nebulous objects compiled in 

1774 by French astronomer and comet 

chaser Charles Messier. It is also known 

to astronomers as NGC 6 18 and 

contains about 00 000 stars, most 

of them having a mass between 0 and 

80 per cent of the mass of the Sun. 

It is however clear that Messier 1 is 

surprisingly devoid of low-mass stars. 

For each solar-like star, we would expect 

roughly four times as many stars with half 

that mass. The VLT observations only 

show an equal number of stars of different 

masses. 

In the solar neighbourhood and in 

most stellar clusters, the least massive 

0 


The Central Part of Messier 1 . 

stars are by far the most common. 

The new observations show this is not 

the case for Messier 1 . 

Globular clusters move in extended 

elliptical orbits that periodically take them 

through the densely populated plane 

of our Galaxy, then high above and below, 

in the ‘halo’. When venturing too 

close to the innermost and denser ‘bulge’ 

of the Milky Way a globular cluster can be 

perturbed, with the smallest stars being 

ripped away. 

The astronomers estimate that Messier 

1 lost four times as many stars as it still 

has. That is, roughly one million stars 

must have been ejected into the halo of 

our Milky Way. 

The total remaining lifetime of Messier 1 

is predicted to be about 4.5 billion years, 

i.e. about a third of its present age. This 

is very short compared to the typical 

expected globular cluster’s lifetime, which 

is about 0 billion years. 

The scientists now hope to discover and 

study many more clusters like this, since 

catching clusters while they are being 

disrupted should clarify the dynamics of 

the process that shaped the halo of our 

home galaxy, the Milky Way. 

Guido de Marchi, Luigi Pulone, and Francesco 

Paresce, 006, Astronomy and Astrophysics, 449, 

161.

A ‘Genetic Study’ of the Galaxy 

Looking in detail at the composition of 

stars with the VLT, astronomers are 

providing a fresh look at the history of 

the Milky Way. They reveal that the 

central part of our Galaxy formed not 

only very quickly but also independently 

of the rest. 

For the first time, it has been possible 

to clearly establish a ‘genetic difference’ 

between stars in the disc and the bulge 

of our Galaxy. From this one can infer 

that the bulge must have formed more 

rapidly than the disc, probably in less 

than a billion years and when the 

Universe was still very young. 

The Milky Way is a spiral galaxy, having 

a pinwheel shape with arms of gas, dust, 

and stars lying in a flattened disc, and 

extending directly out from a spherical 

nucleus of stars in the central region, the 

bulge. While the disc of our Galaxy is 

made up of stars of all ages, the bulge 

contains old stars dating from the time 

the galaxy formed, more than 10 billion 

years ago. Thus, studying the bulge 

allows astronomers to know more about 

how our Galaxy formed. 

The Oxygen abundance in the bulge of our Galaxy. 

To do this, an international team of 

astronomers analysed in detail the chemical 

composition of 50 giant stars in four 

different areas of the sky towards the 

Galactic bulge. They made use of the 

FLAMES/UVES spectrograph on the VLT 

to obtain high-resolution spectra. 

The chemical composition of stars carries 

the signature of the enrichment processes 

undergone by the interstellar matter 

up to the moment of their formation. 

It depends on the previous history of star 

formation and can thus be used to infer 

whether there is a ‘genetic link’ between 

different stellar groups. In particular, 

comparison between the abundance of 

oxygen and iron in stars is very illustrative. 

Oxygen is predominantly produced 

in the explosion of massive, short-lived 

stars (so-called Type II supernovae), while 

iron instead originates mostly in Type Ia 

supernovae, which can take much longer 

to develop. Comparing oxygen with iron 

abundances therefore gives insight into 

the star-birth rate in the Milky Way’s past. 

The larger size and iron-content coverage 

of the new sample allowed the astronomers 

to draw much more robust conclusions 

than were possible until then. 

They clearly established that, for a given 

iron content, stars in the bulge possess 

more oxygen than their disc counterparts. 

This highlights a systematic, hereditary 

difference between bulge and disc stars. 

In other words, bulge stars did not originate 

in the disc and then migrate inward 

to build up the bulge but rather formed 

independently of the disc. Moreover, the 

chemical enrichment of the bulge, and 

hence its formation timescale, was faster 

than that of the disc. Comparisons with 

theoretical models indicate that the 

Galactic bulge must have formed in less 

than a billion years, most likely through a 

series of starbursts when the Universe 

was still very young. 

Manuela Zoccali et al. 006, Astronomy and 

Astrophysics, 457, L1. 


1

Cut from Different Cloth 

A large survey has shed light on our Galaxy’s 

ancestry. After determining the 

chemical composition of over 000 stars 

in four of the nearest dwarf galaxies 

to our own, astronomers have demonstrated 

fundamental differences in their 

make-up, casting doubt on the theory 

that these diminutive galaxies could ever 

have formed the building blocks of our 

Milky Way Galaxy. 

Our Milky Way Galaxy is surrounded by 

a number of dwarf satellite galaxies, 

which because of their loosely rounded 

shape are referred to as ‘dwarf spheroidal’ 

galaxies. Faint and diffuse, these 

dwarf galaxies are a thousand times 

fainter than the Milky Way itself, making 

them the least luminous galaxies known. 

Modern cosmological models predict 

that small galaxies form first, and later 

assemble into larger systems like our Galaxy. 

Since the Universe initially only 

The Topsy-Turvy Galaxy 

This FORS image of the central parts of 

NGC 1313 shows a stunning natural 

beauty. The galaxy bears some resemblance 

to some of the Milky Way’s closest 

neighbours, the Magellanic Clouds. 

NGC 1313 has a barred spiral shape, 

with the arms emanating outwards in a 

loose twist from the ends of the bar. 

The galaxy lies just 15 million light years 

away from the Milky Way – a mere skip 

on cosmological scales. The spiral arms 

are a hotbed of star-forming activity, with 

numerous young clusters of hot stars 

being born continuously at a staggering 

rate out of the dense clouds of gas and 

dust. Their light blasts through the 

surrounding gas, creating an intricately 

beautiful pattern of light and dark 

nebulosity. 


contained hydrogen and helium (most of 

all other chemical elements being 

synthesized inside stars), dwarf galaxies 

should have the lowest heavy element 

content. Not so, reveal the observations. 

As part of a large observational programme, 

called the Dwarf galaxies Abundances 

and Radial-velocities Team 

(DART), astronomers from institutes in 9 

different countries used FLAMES on the 

VLT to measure the amount of iron in over 

000 individual giant stars in the Fornax, 

Sculptor, Sextans and Carina dwarf 

spheroidals. 

Their data unearthed fundamental differences 

in the dwarf galaxy stars’ chemical 

composition compared with those 

in our galactic halo, calling into question 

the merger theory as the origin of large 

galaxies’ haloes. Whilst the average 

abundances of elements in the dwarf 

spheroidals is comparable with that seen 

NGC 1313’s appearance suggests it 

has seen troubled times: its spiral arms 

look lop-sided and gas globules are 

spread out widely around them. Moreover, 

observations with ESO’s 3.6-m 

telescope at La Silla have revealed that 

its ‘real’ centre, around which it rotates, 

does not coincide with the central bar. 

Its rotation is therefore also out of kilter. 

Strangely enough, NGC 1313 seems to 

be an isolated galaxy. It is not part of a 

group and has no neighbour, and it is not 

clear whether it may have swallowed a 

small companion in its past. So what 

caused its asymmetry and stellar baby 

boom? 

Chemical abundance in several dwarf galaxies. 

in the Galactic halo, the former are 

lacking the very metal-poor stars that are 

seen in the Milky Way – the two types 

of systems, contrary to theoretical predictions, 

are essentially of different descent. 

Amina Helmi et al. 006, Astrophysical Journal 

Letters, 651, L1 1-L1 4. 

The Topsy-Turvy Galaxy NGC 1313.


3

Long-lasting but Dim Brethren of Cosmic Flashes 

For the first time, it has been possible to 

make the link between an X-ray flash 

and a supernova. Such flashes are the little 

siblings of gamma-ray bursts (GRB) 

and this discovery suggests the existence 

of a population of events less luminous 

than ‘classical’ GRBs, but possibly much 

more numerous. This also implies a 

common origin for these two classes of 

events. 

The event began on 18 February 006: 

the NASA/PPARC/ASI Swift satellite 

detected an unusual gamma-ray burst, 

about 5 times closer and 100 times 

longer than the typical gamma-ray burst. 

GRBs release in a few seconds more 

energy than that of the Sun during its entire 

lifetime of more than 10 000 million 

years. The GRBs are thus the most powerful 

events known in the Universe since 

the Big Bang. 

The explosion, called GRB 060 18 

after the date it was discovered, originated 

in a star-forming galaxy about 440 

million light years away toward the 

constellation Aries. This is the secondclosest 

gamma-ray burst ever detected. 

Moreover, the burst of gamma rays lasted 

for nearly 000 seconds; most bursts 

last a few milliseconds to tens of seconds. 

The explosion was surprisingly 

dim, however. 

Using several telescopes, among them the 

VLT, the scientists watched the afterglow 

of this burst grow brighter in optical light. 

This brightening, along with other telltale 

spectral characteristics in the light, 

strongly suggests that a supernova was 

unfolding. Within days, the supernova 

became apparent. 

The observations with the VLT started on 

1 February 006, just three days after 

the discovery. Spectroscopy was then 

performed nearly daily for seventeen 

days, providing the astronomers with a 

large data set to document this new class 

of events. 

4 


The field around SN 006aj. 

The astronomers could finally confirm that 

the event was tied to a supernova called 

SN 006aj which was observed a few 

days later. The newly discovered supernova 

is dimmer by about a factor of two 

than the hypernovae associated with 

normal long gamma-ray bursts, but it is 

still a factor of -3 times more luminous 

than regular core-collapse supernovae. 

All together, these facts point to a 

substantial diversity between supernovae 

associated with GRBs and supernovae 

associated with X-ray flashes. This 

diversity may be related to the masses 

of the exploding stars. 

Whereas gamma-ray bursts probably 

mark the birth of a black hole, X-ray 

flashes appear to signal the type of star 

explosion that leaves behind a neutron 

star. Based on the VLT data, another 

team of astronomers postulate that the 

18 February event might have led to a 

highly magnetic type of neutron star 

called a magnetar. 

They find indeed that the star that 

exploded had an initial mass of ‘only’ 0 

times the mass of the Sun. This is 

smaller, by about a factor of two at least, 

than those estimated for the typical GRBsupernovae. 

The properties of GRB 060 18 suggest 

the existence of a population of events 

less luminous than ‘classical’ GRBs, but 

possibly much more numerous. Indeed, 

these events may be the most abundant 

form of X- or gamma-ray bursts in the 

Universe, but instrumental limits allow us 

to detect them only locally. The astronomers 

find that the number of such events 

could be about 100 times more numerous 

than typical gamma-ray bursts. 

Elena Pian et al., Nature, 31 August 006. 

Paolo Mazzali et al., Nature, 31 August 006.

Faraway Galaxy Under the Microscope 

Some large-disc galaxies akin to our 

Milky Way have formed on a rapid time- 

scale, only 3 billion years after the 

Big Bang, reveals a study made with the 

new SINFONI spectrograph on VLT. 

Over the past decade astronomers have 

established an overall model of how 

galaxies formed and evolved when the 

Universe was only a few billion years old. 

Gas made of ordinary matter cooled and 

collected in concentrations of the 

mysterious ‘dark’ matter (so-called dark- 

matter halos). Since that time, and up to 

the present epoch, collisions and 

mergers of galaxies subsequently led to 

the hierarchical build-up of galaxy mass. 

This general picture leaves open, 

however, on what timescales galaxies 

were assembled and when and how 

bulges and discs, the primary components 

of present-day galaxies, were 

formed. 

A major study of distant, luminous starforming 

galaxies at the VLT, the ‘SINS’ 

(Spectroscopic Imaging survey in the 

Near-infrared with SINFONI) survey, has 

now resulted in a major breakthrough on 

these questions. This study exploited 

SINFONI, a novel infrared ‘integral-field 

spectrometer’ that simultaneously 

delivers sharp images, with adaptive 

optics, and highly resolved spectra of an 

object on the sky. 

In one case, studying the galaxy 

BzK155043 at cosmological redshift of 

.4, the SINFONI observations achieved 

an angular resolution of 0.15 arcsecond, 

a mere 4 000 light years at the distance 

of this high-redshift galaxy. With this 

superior angular resolution the data 

reveal the physical and dynamical 

properties in unprecedented detail. 

Surprisingly, instead of showing mostly 

irregular and perhaps even chaotic 

motions caused by the frequent merger 

activity in the young Universe, the 

observations reveal a large and massive 

rotating protodisc that is channelling gas 

toward a growing central stellar bulge. 

The high gas surface densities, the large 

star-formation rate and the moderately 

young stellar ages derived from these 

observations suggest that the system 

was assembled rapidly, by fragmentation 

and star formation in an initially very gas 

rich protodisc. SINS observations of 

several other massive, high-redshift 

galaxies give similar results. 

The fact that these galaxies are so large 

and rotate rapidly indicates that the gas 

has a similar amount of rotation as the 

dark matter halo from which it cooled, 

thus empirically solving an important 

question of galaxy formation. 

The SINFONI data suggest that the protodiscs 

may have eventually been transformed 

to dense elliptical galaxies, either 

by internal processes, such as the 

spectacular gas inflows observed in BzK- 

15504, or by collisions and mergers with 

other galaxies, which were frequent in the 

dense environments in which the highredshift 

luminous star-forming galaxies 

appear to reside. 

Another important aspect of the work is 

the deduction of very high star-formation 

rates for many of the luminous starforming 

high-redshift galaxies, about one 

hundred times greater than in the 

present-day Milky Way. 

Astronomers have a growing body of 

evidence that massive galaxies formed 

much more rapidly in the redshift range 

-3 than originally anticipated. The new 

SINFONI data give us a first glimpse of 

what processes might be involved. 

SINFONI maps of emission in BzK-15504. 

In fact, the SINS programme on the VLT 

is a stunning demonstration of what is 

going to be possible in the next few years 

with the combination of integral-field 

spec-troscopy and adaptive optics. 

N.M. Förster Schreiber et al. 006, Astrophys. 

Journal 645, 106 . 

R. Genzel et al., Nature, 17 August 006. 

X. Kong et al. 006, Astrophys.J. 638, 7 . 

Emission of the galaxy BzK-15504. 


5

The Invisible Galaxies That Could Not Hide 

Astronomers have found a metal-rich hydrogen 

cloud in the distant universe. 

The result may help to solve the missing 

metal problem and provides insight on 

how galaxies form. This discovery shows 

that significant quantities of metals are to 

be found in very remote galaxies that are 

too faint to be directly seen. 

Metal shouldn’t however be taken too literally 

as, for astronomers, metals are all 

chemical elements heavier than helium. 

The Sun, for example, is made mostly of 

hydrogen (73%) and helium ( 5%), and 

% of ‘metals’. 

Almost all of the elements present in the 

Universe were formed in stars, which 

themselves are members of galaxies. By 

estimating how many stars formed over 

the history of the Universe, it is possible 

to estimate how much of the metals 

should have been produced. However, 

this apparently straightforward reasoning 

has been confronted for several years 

with an apparent contradiction: adding 

up the amount of metals observable 

today in distant astronomical objects falls 

Falling Onto the Dark 

Using the FORS1 instrument on the VLT, 

an international team of astronomers 

have discovered a new ‘blob’ located at a 

distance of 11.6 billion light years (redshift 

3.16). It is thus seen as it was when 

the Universe was only billion years old, 

or less than 15% its present age. The 

newly discovered object is located in the 

well-studied GOODS South field. 

With a diameter of 00 000 light years, 

the blob is twice as big as our Milky Way 

and the total energy emitted is equivalent 

to that of about billion suns. Despite 

this, the object is invisible in images taken 

with various telescopes observing from 

the infrared to the X-ray wavebands, 

making it a very peculiar object indeed. 

This is because the object emits most of 

its light in the Lyman-alpha hydrogen line, 

while its continuum emission is too low to 

be detected. It is also the only such 

object found by the astronomers in their 

survey. 

6 


short of the predicted value. When the 

contribution of galaxies now observed at 

cosmological distances is added to that 

of the intergalactic medium, the total 

amounts for no more than a tenth of the 

metals expected. 

Studying distant galaxies is however a 

difficult task. The further a galaxy, the 

fainter it is, and the smallest or intrinsically 

faintest ones will not be observed. 

This may introduce severe biases in the 

observations as only the largest and most 

active galaxies are picked up. 

Astronomers therefore came up with 

other ways to study distant galaxies: they 

use quasars, most probably the brightest 

distant objects known, as beacons in the 

Universe. 

Interstellar clouds of gas in galaxies, located 

between the quasars and us on the 

same line of sight, absorb parts of the 

light emitted by the quasars. The 

resulting spectrum consequently presents 

dark ‘valleys’ that can be attributed to 

well-known elements. Thus, astronomers 

Trying to explain this blob by invoking 

a powerful galaxy as the cause for the 

object to emit so much radiation proved 

impossible. The astronomers are instead 

led to the conclusion that the observed 

hydrogen emission comes from primordial 

gas falling onto a clump of dark 

HST Image Narrow-band 

A Rare Blob. 

can measure the amount of metals 

present in these galaxies – that are otherwise 

invisible – at various epochs. 

This can best be done by high-resolution 

spectrographs on the largest telescopes, 

such as UVES on the VLT. 

Astronomers thus studied, with the 

UVES spectrograph on the VLT, the light 

emitted by the quasar SDSS J13 3-00 1. 

Located 9 billion light years away, its 

light is partially absorbed by an otherwise 

invisible galaxy sitting 6.3 billion light years 

away along the line of sight. 

The analysis of the spectrum shows that 

this galaxy has four times more metals 

than the Sun. This is the first time one 

finds such a large amount of ‘metals’ 

in a very distant object, giving encouragement 

to astronomers. If a large number of 

such ‘invisible’ galaxies with high metal 

content were to be discovered, they 

might well alleviate the missing metals 

problem considerably. 

C. Péroux et al., 006, Astronomy and Astrophysics, 

450, 53. 

matter. They could thus be literally seeing 

the building up of a massive galaxy, like 

our own, the Milky Way. 

K.K. Nilsson et al. 006, Astronomy and Astrophysics, 

45 , 3. 

Red Blue

A 1.8-m Auxiliary Telescope at Paranal. 


7

8 

ESO Annual Report 006

Venus and the Moon setting over Paranal. 


9

La Silla Paranal Observatory 

In 006 the La Silla Paranal Observatory 

has been routinely operating a total of 

10 telescopes with 19 optical, near-infrared 

and mid-infrared instruments. On 

Paranal these are nine VLT instruments at 

the four 8. -m Unit Telescopes (UTs). 

There are also two instruments at the VLT 

Interferometer (VLTI), which coherently 

combine the light of the UTs or the 1.8-m 

Auxiliary Telescopes (ATs). On La Silla, a 

total of eight instruments are operated on 

the 3.5-m NTT, the 3.6-m, and the MPG/ 

ESO . -m telescopes. 

The observatory has also supported the 

operation of the Atacama Pathfinder 

Experiment (APEX). The 1 -m APEX 

antenna is located on the high plateau 

of Chajnantor at an altitude of 5100 m. 

APEX and its two workhorse instruments, 

APEX a and FLASH, have been 

operated from the base camp in the village 

of Sequitor near San Pedro de 

Atacama. During this first year of regular 

operation about 10 nights of mostly 

Service Mode observations were carried 

out at APEX with an average observing 

time of 13 hours per night. 

In 006 more than 630 peer-reviewed articles 

and papers were published in scientific 

journals in which the authors have 

made use of astronomical data collected 

with telescopes and instruments available 

at the three sites of the La Silla Paranal 

Observatory. This number translates into 

an impressive publication rate of nearly 

two refereed papers for every day of the 

year. APEX alone in its very first year of 

routine operations has produced the respectable 

number of 1 publications – all 

contained in a special edition of the Astronomy 

& Astrophysics journal. 

One of the important ingredients for such 

a high productivity of the observatory is 

the high availability of its telescopes and 

instruments to carry out scientific observations. 

In this respect the observatory 

had another excellent year, with a total of 

410 nights scheduled for scientific 

observations with the four UTs at the VLT 

and with the three major telescopes at 

La Silla. In addition, the VLTI was oper- 

30 


ated for about 140 nights, executing scientific 

observations with its MIDI and 

AMBER instruments. This total number of 

nights scheduled for scientific observations 

is equivalent to about 90% of the 

theoretically available total time. 

The remaining 10 % were scheduled 

for planned engineering and maintenance 

activities to guarantee the continuous 

performance of the telescopes and instruments. 

Technical time further includes 

the time slots required to commission 

the new instruments and facilities, which 

keep arriving in particular on Paranal for 

the VLT. 

Of the available science time on Paranal, 

only .3% was lost due to technical problems 

and about 6% due to bad weather. 

On La Silla bad weather accounted for a 

loss of about 11%, and technical 

problems for 5.4%. This comparatively 

high figure for the technical downtime in 

La Silla was solely due to a major problem 

of the aged dome rotation system of 

the 3.6-m telescope, which required extended 

periods of corrective maintenance 

during which no operation of the 

telescope was possible. Otherwise, the 

downtime figure would have been reduced 

to an excellent .6 %. 

One of the great technical achievements 

of the year has been the first-ever recoating 

of a secondary mirror (M ) of the 

VLT with a few-nanometre-thick layer of 

fresh aluminium (Al). The M of the VLT is 

a lightweight 1. -m hyperbolic mirror, 

made of beryllium in order to minimise its 

mass to allow precise and fast tilt motions 

(‘field stabilisation’) and chopping 

with frequencies of up to several hertz. 

The optical surface of the M is protected 

by a thin layer of nickel (Ni) onto which 

the reflective layer of Al is superimposed. 

The challenges are first to develop and 

define the M recoating procedure, then 

to actually remove the old Al layer without 

affecting the Ni layer, and finally to recoat 

the surface with fresh Al. The engineering 

department mastered these 

challenges for the M of Antu (UT1), in 

May 006. Recoating of the secondary 

mirrors of the UTs has now become part 

of the regular maintenance of the VLT 

to ensure the optimal long-term performance 

of the telescope optics. The scheduled 

recoating of the primary and tertiary 

mirrors of Kueyen (UT ) and Yepun (UT4) 

were also successfully performed. 

Cleaning a mirror at La Silla.

New Instruments and Facilities 

With the installation and commissioning 

of the CRIRES instrument on the Nasmyth 

A focus of Antu (UT1) a major milestone 

of the VLT programme was 

reached this year: the completion of the 

first generation of VLT instruments. 

CRIRES is a cryogenic high-resolution 

infrared échelle spectrograph, that provides 

a resolving power of up to 10 5 in the 

spectral range from 1 to 5 μm when used 

with a narrow slit of 0. arcseconds. After 

its successful commissioning in 006, 

CRIRES was offered for the first time to 

the astronomical community for Period 

79, which starts in April 007. 

The sixth ESO standard adaptive optics 

system, Multi-Applications Curvature 

Adaptive Optics (MACAO), was deployed 

on Paranal to feed the narrow CRIRES 

slit, and to optimise the achievable signalto-noise 

ratio and spatial resolution. Four 

MACAO systems were already installed 

in the Coudé feeds to VLTI, and a similar 

system has been installed in the Cassegrain 

focus of UT4 feeding the SINFONI 

instrument. 

Maximum concentration during the CRIRES Commissioning. 

The Laser Guide Star Facility (LGSF) 

achieved its ‘First Light’ in early 006 and 

created the first artificial star in the Paranal 

sky. The LGSF provides the adaptive 

optics (AO) systems of instruments like 

SINFONI and NACO with bright reference 

stars in regions of the sky where sufficiently 

bright natural stars cannot be 

found close enough to the scientific targets 

for the AO system to perform. The 

path from having seen the first artificial 

laser star to regular operations turned out 

to be longer and harder than expected 

after the initial success. Several modifications 

and improvements of the LGSF 

were required over the course of the year 

until the facility was successfully commissioned 

by the end of the year. The 

very first observations with SINFONI and 

NACO in the new LGS mode immediately 

gave a taste of the exciting new possibilities 

this facility will provide to the observatory 

in early 007 when the LGSF 

will be fully commissioned together with 

the AO instruments. 

The VLT welcomed its second Visitor 

Instrument, DAZLE (Dark Age ‘Z’ Lymanalpha 

Explorer). DAZLE is an innovative 

narrowband imaging instrument, specifically 

developed by the Institute of Astronomy 

(Cambridge, UK) and the Anglo- 

Australian Observatory for use on the 

Visitor focus of UT3 (Melipal) in order to 

detect the most distant objects in the 

Universe. Nine nights of data were taken 

with the VLT and first results from this 

ambitious search project are eagerly expected. 

On La Silla the mid-infrared instrument 

TIMMI was decommissioned after the 

corresponding mid-infrared instrument 

VISIR at the VLT had begun full operation. 

A new telescope has joined the suite of 

gamma-ray burst (GRB) hunters on 

La Silla: the very fast moving and robotic 

TAROT-S telescope has been installed 

by a consortium led by Observatoire de 

Haute-Provence to follow-up GRBs within 

seconds of their detection by dedicated 

satellites in the Earth’s orbit. The new 

telescope delivered first results on newlydetected 

GRBs only a few days after its 

installation. 

The . -m telescope on La Silla was prepared 

over the year to receive the GRB 

follow-up instrument GROND, which 

is being built by the Max-Planck-Institut 

für Extraterrestrische Physik and will be 

commissioned in early 007. 

GRBs also triggered several fast followup 

observations with the VLT using 

the novel Rapid-Response Mode (RRM), 

which allows authorised VLT users 

to interrupt ongoing observations and to 

point the UTs to a transient target of 

interest. On 7 June 006, the Rapid-Response 

Mode triggered UVES observations 

of the quickly fading afterglow of 

a distant gamma-ray source. Integrations 

with the high-resolution spectrograph 

started a mere 7.5 minutes after the detection 

of the GRB by the SWIFT satellite 

– to date, still a record for the spectroscopic 

follow-up of any GRB. 

APEX is expecting its final suite of facility 

instruments, including new heterodyne 

receivers from the Onsala Space Observatory 

to cover all atmospheric windows 

from 00 to 1000 GHz, and the Large 


31

APEX Bolometer Camera (LABOCA) developed 

by the Max-Planck-Institut für 

Radioastronomie. LABOCA, a detector 

array with 95 pixels operating at a wavelength 

of 870 μm, has been extensively 

tested during the year at Chajnantor. We 

expect regular science operation for all 

new instruments to start in 007. 

In addition to these workhorse instruments, 

several experimental receivers 

covering selected windows above 1 THz 

are under development. This frequency 

regime has so far been considered to 

be only accessible from space. However, 

the exceptional site of Chajnantor at 

an altitude of 5100 m, and the excellent 

quality of the APEX antenna, will allow 

us soon to explore the sky at the shortest 

radio wavelengths from the ground. 

The VLT Interferometer 

In 006 the VLT Interferometer (VLTI) executed 

about 140 nights of scientific 

observations with MIDI and AMBER using 

both UT and AT baselines. The other 

nights were used for intensive engineering 

and commissioning activities to 

complete and improve the interferometer 

infrastructure and to fully exploit the 

capabilities of the VLTI Sub-Array (VISA). 

The VISA feeds the VLTI infrastructure 

and instruments with the light from the 

1.8-m Auxiliary Telescopes (AT) when the 

individual UTs are used for stand-alone 

VLT observations. By the end of 006, 

VISA was completed with the arrival 

of the fourth AT and has become integral 

part of the VLTI science operation. Because 

it is now possible to choose between 

any six baselines and switch from 

one to another during the same night, 

AT4 provides the VLTI operations with 

ad-ditional flexibility in the selection of different 

and complementary AT baselines 

without having to physically reconfigure 

the array of telescopes. This capability, in 

combination with AMBER phase-closure 

on three telescopes, is an important step 

toward imaging with the VLTI. 

3 


The AMBER instrument allows the interferometric 

combination of up to three 

beams, and could be offered to the community 

for the first time with three ATs 

starting in Period 79 after first fringes 

were obtained on 3 August 006. The 

VLTI infrastructure was prepared accordingly 

and the three delay lines numbered 

4, 5 and 6 were equipped with 

Variable Curvature Mirrors (VCM) to control 

the longitudinal position of the pupil 

of the individual interferometric beams. 

The delay lines themselves were put under 

an intensive preventive maintenance 

plan in order to keep them literally in the 

best possible shape. 

These were all necessary steps towards 

the VLTI team’s ambitious goal of offering 

AMBER on three ATs with FINITO 

fringe-tracking for the call for proposals 

for Period 80, and to eventually bring 

AMBER close to the expected sensitivities 

in its different spectroscopic modes. 

A major milestone in this direction was 

reached when, for the first time, FINITO 

fringe-tracking with AMBER and three 

ATs was achieved on 1 December 006 

on the bright star b Ceti. 

The investigation and improvement of 

the stability of the interferometric beams, 

and in particular of the vibration-induced 

variations in the optical path differences 

(OPD) of the interferometric beams 

delivered by the 8. -m UTs, continued in 

parallel to the implementation of new VLTI 

observing modes with the VISA and the 

ATs. 

Working on APEX. 

Beam instabilities and vibrations of the 

UTs transmitted to the VLTI were identified 

as the primary reasons that prevented 

fringe-tracking with the UTs in the 

past. While the beam stability was recently 

improved dramatically through the 

introduction of fast beam control with the 

VLTI Infrared Image Sensor IRIS, the 

elimination of vibrations or their compensation 

remained the primary goal of the 

VLTI team during 006. Active suppression 

of the OPD variations as introduced 

by the vibrating optical surfaces of the 

Unit Telescopes was achieved through a 

novel Vibration Tracking (VTK) system. 

The performance of this vibration-suppression 

system was further enhanced by 

the installation of accelerometers close to 

the vibrating optical surfaces of the UTs.

User Support 

The User Support Department (USD) of the 

ESO Data Management and Operations 

Division, based in Garching, represents the 

primary link between the ESO community and 

the Observatory and its operation groups. It 

provides support primarily to Service Mode 

users of ESO facilities and to the operations 

teams of the La Silla Paranal Observatory. In 

006, Service Mode continued to be the most 

requested observing mode at the VLT (a 

factor of .5 higher than the time requested 

for Visitor Mode during Period 77 and 78). 

This clearly shows that the community has 

recognised the advantages of this observing 

mode for many different types of projects. 

Period 77 also marked the beginning of 

Service Mode observing at the APEX facility, 

the ESO Project Scientist of which is a 

member of the User Support Department. 

A total of 1054 Service Mode runs were 

supported by USD at the VLT, VLTI, and 

MPG/ESO . -m telescope during 006, 

which includes all runs approved during 

Period 77 and 78, including those that were 

granted telescope time via the Director’s 

Discretionary Time channel. 

Data Processing and Quality Control 

Ensuring that data taken on Paranal are of 

certified and predictable quality, and 

continuously monitoring the ‘health’ of the 

instruments, are cornerstone concepts in the 

ESO end-to-end data flow model. The DFO 

Quality Control (QC) group is responsible 

primarily for the monitoring and reporting of 

basic instrument performance for all VLT/VLTI 

instruments as well as the creation of various 

calibration and science data products for 

these instruments. Raw calibration data are 

processed into master calibration products 

that are used not only to monitor instrument 

performance but also to process science 

data. These master calibration products are 

stored in the ESO archive and are available to 

the scientific community at large. 

For Service Mode users, the QC group 

provides two additional services. First, 

Service Mode science data are processed 

into science products using standard 

pipelines which, by now, cover virtually 100 % 

of the Paranal data stream. Second, QC 

creates data packages that include all raw 

data, resultant products, and associated 

information for each and every Service Mode 

observing run. These packages are burned 

onto DVDs and shipped to users by the DFO 

SAO group. 

During 006 QC processed 5 TB of raw data 

in 156 500 processing jobs to create 1014 

service mode packages – an increase of 13 % 

compared to 005 – which were distributed 

to their respective Principal Investigators on 

100 DVDs. The quality control processing of 

the expected 150 TB/year of VISTA/VIRCAM 

data will certainly be challenging. New 

concepts and tools were developed and 

tested in 006 both to cope with the 

computing challenges posed by the high data 

rate itself and to efficiently monitor the quality 

of a large number of images. 

The Data Flow System 

The Data Flow System Department is responsible 

for the design, the implementation 

and the maintenance of the Data Flow System 

software components, that are critical for the 

end-to-end operation of the VLT, VLTI, VST, 

VISTA and some of the La Silla telescopes. 

The Data Flow System consists of two kinds 

of modules or tools. Some of them (e.g. 

P PP) are generic and provide a uniform 

interface to all instruments, while others, e.g. 

pipelines, are instrument specific. The 

department delivers its tools to a variety of 

customers: the astronomical community (e.g. 

P PP, Exposure Time Calculators, Archive 

Interface), VISAS and OPC, User Support 

Department (P PP, Observing Tool), and 

Science Operations and Data Flow Operation 

(Instrument Pipelines, data packing tools). 

The Data Flow System Department is also 

responsible for the installation and the 

commissioning of its software modules 

on-site. 

The front-end and back-end teams continued 

to concentrate their efforts on the design and 

implementation of software components 

required to support survey facilities. This 

includes an upgrade of the Observation 

Preparation Tools to introduce new scheduling 

concepts such as groups and links of 

Observation Blocks. The development of the 

User Portal, which will provide the user 

community with one registration system for all 

services provided by the Observatory, is 

progressing well. The pipeline team released 

three instrument pipelines to the community: 

the ISAAC, VISIR and GIRAFFE packages, 

based on the Common Pipeline Library. At the 

same time, the CRIRES pipeline was verified 

and validated during the commissioning 

phases of the instrument. The pipeline team 

developed an innovative algorithm based on 

pattern-matching for the wavelength calibration 

of spectroscopic data. This algorithm was 

implemented in the new FORS pipeline, which 

is now fully operational and will become 

publicly available in the first quarter of 007. 

During 006 the SAMPO work has focused on 

addressing the requirements within the ESO 

community for more flexible access to the 

ESO reduction pipeline recipes. Following a 

review of the available options an open source 

graphical workflow system (Taverna) was 

selected and extensively extended to interface 

to ESO software components. This workflow 

system has been named ESO Reflex (ESO 

Recipe Flexible Execution Workbench). The 

FORS spectroscopy and AMBER recipes have 

been integrated in a beta-test version of 

Reflex. 

The Reflex scientific workflow allows users to run 

instrument recipes as a sequence of reduction steps 

while inspecting intermediate products and calling 

external applications. 


33

The accelerometers enable the feeding of 

direct measurements of the actual vibration 

signals to the VTK system. Through 

this effort the original residual OPD variations 

of 480 nm were reduced by the end 

of the year to 30 nm. The VLTI team is 

confident that, with a robust implementation 

of these new vibration-suppression 

techniques and further elimination of the 

major vibration sources, fringe-tracking 

with three UTs and AMBER can be delivered 

to science operations by the end 

of 007 – just in time for the observatory 

to receive PRIMA, the next VLTI facility, 

which is expected to further push the 

sensitivity of the VLTI and provide relative 

astrometric measurements of the highest 

precision. 

VST and VISTA Survey Telescopes 

The construction, integration and test- 

ing of the .4-m optical VLT Survey Telescope 

(VST) and its subsystems con- 

tinued in Naples during 006 by the 

Osservatorio di Capodimonte. The disassembly 

of the main telescope structure 

started in collaboration with ESO at the 

end of the year, to prepare for the shipment 

to Paranal where the reintegration 

of the telescope is planned during the 

second half of 007. 

34 


The primary mirror cell and the secondary 

mirror unit, however, remain in Naples for 

their completion. The VST secondary 

mirror optics were completed and shipped 

to Paranal early this year while the .4-m 

primary mirror remained at the manufacturer’s 

premises for its completion. 

The 4. -m infrared survey telescope 

VISTA is currently under construction by 

the VISTA project office on its own peak 

about 1500 m from the Paranal summit. 

The enclosure was essentially completed 

and accepted before the telescope 

structure arrived on 11 May 006. Since 

then, the telescope assembly progressed 

rapidly and the VISTA telescope had 

entered a phase of intensive testing and 

tuning by the end of the year. At the same 

time, the VISTA facility was integrated 

into the power and computer networks of 

the Paranal site to prepare for its future 

operation. VISTA – as all telescopes on 

Paranal – will eventually be operated from 

the same common control room as the 

VLT and the VLTI. 

A dedicated coating unit arrived in September 

and was successfully commissioned 

in the following months. The 

VISTA coating unit is the only facility 

on Paranal that allows the coating of 

mirror surfaces with a layer of silver (instead 

of aluminium as used for the 

VLT mirrors) to provide highest reflectivity 

of the optical surfaces in the near-infrared 

wavelengths where VISTA is going to 

survey the sky. 

The VISTA telescope is now awaiting the 

arrival of its optics and its instrument. 

The primary and secondary mirrors are 

still in the phase of final polishing in Europe, 

and are now only expected to arrive 

on Paranal in the second quarter of 007. 

Commissioning of the telescope and the 

formal handover to ESO are planned to 

take place in the second half of 007. 

In December, the IR Camera that was 

developed at the Rutherford Appleton 

Laboratory in the UK was also shipped to 

Paranal for arrival in mid-January 007. 

VISTA enclosure. The VISTA telescope.


35

36 

Llano de Chajnantor 



37

Atacama Large Millimeter/submillimeter Array 

The Atacama Large Millimeter/submillimeter 

Array (ALMA) is a very sensitive, 

high-resolution aperture-synthesis array 

telescope, which will work at millimetre 

and submillimetre wavelengths. It is an 

international facility, constructed and 

operated as a partnership between 

Europe (through ESO), North America 

(through the National Radio Astronomy 

Observatory, NRAO) and Japan (through 

the National Astronomical Observatory of 

Japan, NAOJ), in cooperation with the 

Republic of Chile. 

The initial plan was to install and operate 

64 antennas of 1 metres diameter, but 

detailed design studies and prototype 

research showed that this project could 

not be realised with the funds foreseen 

by the agreement between the North 

American and European partners. During 

005, in-depth studies were made to 

redefine the ALMA baseline project with 

acceptable cost, while still maintaining 

the prime scientific objectives. By the 

middle of 006, the North American 

partners received approval from their 

Funding Agency (the US National Science 

Foundation, NSF) for the rebaselined 

ALMA project, which had already been 

approved by ESO Council towards the 

end of 005. 

In parallel, Japanese scientists, through 

the NAOJ, continued to define their 

participation in the ALMA project. The 

European and North American partners 

in ALMA spent a considerable amount of 

time with their Japanese partners in 

identifying the Japanese participation and 

reviewed various subsystems, in particular 

the correlator, receivers and antennas. 

Details of the partnerships were defined 

and a trilateral agreement between ESO, 

the NSF, and the National Institute for 

Natural Sciences (NINS, Japan) was 

signed in summer 006. In addition to the 

equipment that NAOJ will provide for the 

bilateral ALMA configuration of 50 

antennas, NAOJ will provide four antennas 

of 1 metre diameter, twelve antennas 

of 7 metre diameter, and two receiver 

bands for all 66 antennas of ALMA. 

Approval of funds required for the 

Japanese participation in ALMA is 

38 


expected by spring 007. With the 

inclusion of the Japanese partners, 

ALMA becomes a truly global astronomy 

facility, involving scientists from four 

different continents. 

Construction Work 

The ALMA Array Operations Site (AOS) 

will be located at a truly unique and 

unusual place: the Altiplano de Chajnantor, 

a plateau at an altitude of 5 000 

metres above sea level, in the Atacama 

Desert in Chile. This location was 

selected for scientific reasons, particularly 

dryness and altitude. Considering 

these aspects, the ALMA Observatory 

will not only be unique because of its 

ambitious scientific goals and the 

unprecedented technical requirements. 

It will also be unique because of the 

harsh environment and living conditions 

in which the array has to operate with 

high efficiency and accuracy. 

A second site, the ALMA Operations 

Support Facilities (OSF), will be the base 

camp for the day-to-day operation of the 

observatory. It is located at an altitude of 

about 900 metres, quite high compared 

to standard living conditions, but still 

acceptable for scientific projects in 

astronomy of similar scope. However, the 

OSF will not only serve as the location for 

operating the ALMA Observatory: it will 

also be the site for Assembly, Integration 

and Verification (AIV) of all the hightechnology 

equipment before this is 

moved to the Array Operations Site. 

The AOS Technical Building. 

Both the AOS and OSF are remote 

locations. The 900-metre OSF site is 

about 15 kilometres away from the 

closest public road, the Chilean highway 

No. 3. The AOS is another 8 kilometres 

away from the OSF site. Thus, one of the 

first ALMA projects was to construct an 

access road not only to the OSF but also 

to the AOS. This road, 43 kilometres long 

and at high altitude, with sufficient width 

for the regular transport of many large 

radio telescopes with diameters of 1 

metres, was completed in the course of 

006. 

The OSF is in many ways the centre of 

activities of the ALMA project, and will 

remain so in the future. The focus there 

will, however, change as ALMA moves 

through the different phases of construction 

and operations. 

Presently, the OSF site is the area where 

all ALMA Site contractors and their staff 

are accommodated – the base camp for 

work on the OSF and AOS infrastructure. 

Local contractors’ staff live there and 

start their work either at the OSF, the 

road construction (between the Chilean 

Highway No. 3 and the AOS) or at the 

AOS itself. Work is organised in 0 days 

working/10 days rest periods. Special 

facilities for board and lodging have had 

to be organised for such a large activity. 

Camps have been erected and by now 

can accommodate the maximum 

required capacity of 500 workers.

Construction of the OSF Technical Buildings. 

The construction of the multi-purpose 

OSF, intended to serve over the lifetime of 

the observatory, is a challenging task. It 

requires taking into account many 

aspects of the functionality of these 

facilities over a period of 30 years. During 

the years 005 and 006 the Technical 

Specifications and Statements of Work 

for the OSF construction were defined, 

refined and adapted to the requirements 

and resources of ALMA. ESO signed a 

very important contract for the construction 

of the OSF Technical Facilities in 

August 006. Construction work has 

started, and during the first five months of 

this unique endeavour no major problems 

or delays occurred. As specified in the 

construction schedule, foundations have 

been prepared and the erection of the 

first walls started in November 006. 

Provisional Acceptance of all facilities is 

foreseen for the first quarter of 008. 

The construction of the AOS Technical 

Building, a project to be delivered by the 

North American partner in ALMA, started 

in October 005 and the outer shell was 

completed by mid- 006. After this date 

installation of the interior infrastructure 

started. 

Antennas 

The four antennas of 1 metre diameter 

to be provided by Japan have been 

ordered from Mitsubishi Electrical 

Company by NAOJ. The twelve remaining 

antennas of 7 metre diameter will be 

ordered during the year 007. 

The Preliminary Production Design 

Review for antennas to be produced by 

Vertex SRL was held in September 006. 

The corresponding review for the AEM 

antennas contracted by ESO is scheduled 

for the end of January 007. 

The design of the antenna transporter 

vehicle has progressed well. Some 

delays, due to long delivery time for 

materials, have arisen. The first transporter 

is expected to be delivered to the 

OSF in October 007, about three 

months later than originally foreseen. 

Front End 

The ALMA Front End system is the first 

element in a complex chain of signal 

reception, conversion, processing and 

recording. The Front End is designed to 

receive signals in ten different frequency 

bands. In the initial phase of operation 

the antennas will be equipped with six 

bands. These are Bands 3, 4, 6, 7, 8 and 

9. ESO is in charge of providing Bands 7 

and 9. It is planned to equip the antennas 

with the missing bands at a later stage of 

ALMA operation. 

The ALMA Front Ends are superior to 

almost all existing systems. Indeed, 

development work for the ALMA prototypes 

has also led to improved receivers 

for existing millimetre and submillimetre 

observatories. 

The Front End units are comprised of 

numerous elements, produced at 

different locations in Europe, North America 

and East Asia. In the initial phase of 

construction after the prototyping and 

developing stage, it was decided to build 

a set of eight pre-production units before 

moving to mass production. This initial 

phase started in the years 00 and 

003. The pre-production phase has 

advanced well and 006 was an especially 

important year, because it marked 

the start of the transition from this preproduction 

to the final series production 

phase. 


39

ALMA FE No. 1 rear view (chassis covers removed) 

with receiver cartridges for Bands 3, 6, 7 and 9 

installed. 

In 006, the European groups made 

essential contributions to the integration 

of the first ALMA front end. In early 006, 

the Band 7 Cartridge delivered by IRAM 

(Grenoble, France) was the first of all the 

cartridges to be accepted by the North 

American Front End Integration Centre 

(NAFEIC), which is based at NRAO 

(Charlottesville, Virginia, USA). The first 

Band 9 Cartridge, manufactured by 

NOVA (Groningen, the Netherlands), was 

successfully delivered and accepted by 

the NAFEIC at the end of 006. 

Receiver noise performance for three Band 9 Cartridge (pre-production) units. 

40 


In 003, ESO and the Rutherford 

Appleton Laboratory (RAL, UK) launched 

a development and pre-production 

programme for the manufacture of eight 

operational cryostats. By the end of 

006, six cryostats had been fully 

assembled. The remaining two units are 

in manufacture and will be completed in 

early 007. 

With the end of the pre-production phase 

of these cryostats in sight, efforts were 

made to prepare the final series production 

phase. This resulted in the approval 

by ESO Finance Committee at its 

November 006 meeting of a proposal to 

place a contract for 45 production units 

to cover the needs of the ALMA Baseline. 

With the ongoing production of ALMA 

receiver cartridges, more insight was also 

obtained into the repeatability of their 

performance. Collecting this information 

was one of the main goals of the preproduction 

phase, and is essential for 

increasing the accuracy of the series 

production schedule. The graph below 

shows the receiver noise performance for 

three Band 9 Cartridges, each having 

two independent polarisation channels. 

Besides the exceptionally good noise 

performance for reach of the cartridges – 

well within the specified project requirements 

– the repeatability is very good. 

Pre-production 4-8 GHz cryogenic low-noise amplifier. 

In the framework of an EC FP6 programme, 

ESO is leading a group of 

European institutes to develop and build 

six Band-5 receiver cartridges and to 

develop associated software. This 

project, “Enhancement of ALMA Early 

Science”, was approved by the European 

Commission at the end of 005 and 

actual work started in January 006. The 

Band 5 receiver design is being developed 

by the Onsala Space Observatory 

(OSO, Sweden). By the end of 006, 

most of the receiver design concept had 

been finalised. 

Discussions have been initiated between 

ESO, OSO, and RAL to provide the local 

oscillator as needed in this Band 5 

receiver. An initial plan for this activity has 

been provided by RAL and it is planned 

to include them as a participant in the 

FP6 programme. 

The pre-production phase of the cryogenic 

low-noise amplifiers used in the IF 

of the Band 7, 4-8 GHz bandwidth, and 

Band 9, 4-1 GHz bandwidth receivers 

has been successfully completed by 

Centro Astronómico de Yebes (CAY, 

Spain). Amplifier production for the Band 

7 cartridges (198 units) by industry will 

commence in early 007. A proposal was 

received and approved by the ESO 

Finance Committee at its meeting in 

November 006. 

Production of the more complex 4-1 

GHz cryogenic amplifiers will remain at 

CAY. It is planned to start this series 

production phase in early 007.

Water Vapour Radiometers (WVRs) 

operating at 183 GHz are essential for 

ALMA to improve the fidelity of highresolution 

radio maps when using 

baselines longer than 300 metres. These 

radiometers provide a correction of the 

signal phase due to atmospheric water 

vapour fluctuations. The development of 

two prototype WVRs, a joint undertaking 

by the University of Cambridge and OSO, 

has been completed and they are 

undergoing intensive tests at the Submillimeter 

Array (SMA) on Mauna Kea 

(Hawaii). This field test of the WVRs has 

shown that it is feasible to do this 

correction of the atmospheric phase 

fluctuations with the necessary accuracy. 

The performance of both prototypes 

meets the requirements, and a simpler, 

more cost-effective, single-channel Dicke 

switched radiometer design has been 

adopted as the baseline for production. 

By the end of 006 a Call for Tender had 

been prepared for the final detailed 

design phase and production phase of 

53 units. This Call will be issued to 

industry in early 007. 

Back End 

The ALMA Back End systems deliver 

signals generated by Front End units 

installed in each antenna to the central 

Correlator at the AOS Technical Building. 

At any time, 8 GHz of signal bandwidth in 

each of two orthogonal linear polarisations 

can be processed and recorded. 

Analogue data, produced by the Front 

End electronics, are processed and 

digitised before entering first the data 

encoder, and then the optical transmitter 

Pre-production ALMA cryostat lined up for delivery 

at the Rutherford Appleton Laboratory. 

units and multiplexers. All these elements 

are installed in the receiver cabins of 

each antenna. Optical signals are then 

transmitted by fibres to the AOS Technical 

Building. The total distance in the 

most extended antenna configuration is 

about 15 kilometres. At the AOS Technical 

Building the incoming optical signals 

are de-multiplexed and de-formatted 

before entering the Correlator. 

The European deliverables in the ALMA 

Back End project are various components, 

which are produced by several 

European institutes, working closely with 

ESO and NRAO. These deliverables are: 

– digitiser chip production 

– digitiser chip assembly, 

– digitiser clock and assembly, 

– optical data transmission system 

design, 

– fibre patch panel, 

– optical multiplexers (MUX), amplifiers 

(EDFA), and de-multiplexers (De-MUX), 

and 

– photonic local oscillator photomixers. 

Development and pre-production of 

these components has either been 

successfully completed or is so far 

advanced that completion will happen in 

the first few months of 007. The components 

will be integrated at the Back End 

Integration Center at Socorro (New 

Mexico) and installed in the European 

and North American prototype antennas 

for tests at the ALMA Test Facility. 

Correlator 

The ALMA Correlator, to be installed in 

the AOS Technical Building, is the last 

component in the receiving end of the 

data transmission. It takes as input the 

digitised signals from the individual 

antennas, and outputs amplitude and 

phase on all of the interferometer 

baselines in each of a large number of 

spectral channels. It is a very large data- 

processing system, composed of four 

quadrants, each of which can process 

data coming from up to 16 different 

antennas. The complete correlator will 

have 91 printed circuit boards, 5 00 

interface cables, and more than 0 

million solder joints. The first quadrant 

was completed at NRAO in the third 

quarter of 006. Work on the second 

quadrant is progressing on schedule. 

Integral parts of the Correlator are 

Tunable Filter Bank (TFB) cards, which 

allow a major increase in the flexibility by 

subdividing the frequency range into 3 

independently configurable sub-channels. 

The layout is such that four TFB 

cards are needed for the data coming 

from a single antenna. The TFB cards 

have been developed and optimised by 

the University of Bordeaux over the last 

few years. Prototypes and pre-production 

units have been extensively tested and 

their performance was critically reviewed 

in the first half of 006. In the meantime, 

series production has started and the first 

batch of 36 cards has been produced. 

Software Development 

The ALMA software is planned from the 

beginning as an end-to-end software 

system, which goes from proposal 

preparation to data reduction, including 

all the necessary control software for 

antennas and correlator. The computing 

work in Europe is organised through 

ESO. Many developments are done 

directly by ESO; others are done in 

collaboration with European institutes in 

Spain, France, Italy, Germany and the 

United Kingdom. 

In 006, the ALMA software was tested 

end-to-end in different observing modes, 

starting from proposals consisting of 

Scheduling Blocks up to reducing data 

obtained with the ALMA prototype 

antennas at the ALMA Test Facility (ATF) 

located at the site o the Very Large Array 

(VLA) in Socorro. ESO and its associated 

institutes not only provided their software 

for this, but also actively participated in 

the testing campaigns. 

The next goal is to perform interferometry 

tests with the two prototype antennas at 

the ATF, while preparing to support 

integration and tests of the first European 

ALMA antenna to be delivered to Chile in 

the second part of 007. 


41

System Engineering (SE) 

Substantial progress was achieved on 

project-wide requirements and Interface 

Control Document (ICD) completion, 

which are now 93% and 80% completed, 

respectively. The ALMA system requirement 

version B was released, and is now 

consistent with the refined science 

requirements document and much more 

complete. Progress was also made on 

the Front End and Back End requirements 

and these will be formally released 

at the beginning of 007. The requirements 

database DOORS was updated 

and enhanced, and more requirements 

were added. 

The 3-dimensional models of the AEM 

and Vertex Antenna receiver cabins with 

their interiors have been developed and 

documented. The Antenna cabling 

designs for these antennas were done 

and released. Support was given to all 

Integrated Project Teams (IPTs) for their 

technical activities, e.g. for the ridges 

procurement and for the design and 

manufacturing of the ridges alignment 

tool. The mechanical tolerance budget 

was refined. Master Frequency Standard 

specification was prepared and the 

procurement process was initiated. 

ALMA system block diagrams have been 

updated, refined and distributed. The 

sensitivity budget was further refined and 

used for system design trade-offs and 

analysis tasks. 

System Engineering participated in 

several review meetings, such as maser 

laser review, and organised and chaired 

the Antenna Transporter PDR, Band 7 

Cartridge CDR, 1st Local Oscillator CDR, 

System Requirement review, Vertex 

antenna Pre-production review (PPDR), 

and the ACA correlator CDR. 

4 


The ALMA optical analysis led by SE 

started. The goal is to perform a detailed 

analysis of the antenna optical performance 

including polarisation, sidelobe 

patterns, and subreflector scattering 

cone under load conditions to predict 

antenna performance and the science 

case of polarisation mosaicing. 

A new ALMA Product Assurance (PA) 

manager was hired in mid- 006. His main 

task was to organise PA to be ready for 

the production contracts. This was 

achieved through close cooperation and 

meeting with all IPTs. Also, Statements of 

Work, verification plans and PA plans 

were reviewed and updated. 

System prototyping in the laboratory 

continued until November. A lot of 

detailed technical work was done to 

finally achieve continuity of the signal 

chain in the laboratory. Millimetrewavelength 

cross-correlation was 

achieved in the lab using both the AEM 

and Vertex antenna racks. For this a 

signal at 86 GHz was injected into each 

leg of the RF simulator. Then, system 

level testing, leading to phase tracking 

and delay switching interferometry, was 

achieved in the lab. 

After that the Back End antenna racks 

were removed from the lab in November, 

moved onto the antennas, and installed. 

The Evaluation Front Ends were also 

installed on both antennas, on which the 

signal path through the Front End to the 

Correlator is functional; the evaluation 

Front Ends were cooled down; and 

monitoring and control is functional via 

control software. The Central Local 

Oscillator racks and Correlator were 

installed, populated, powered up, and 

monitoring and control was established. 

First on-the-sky fringes are expected in 

the first quarter of 007. 

Other activities of PSI staff were the 

support of the holography system at the 

ATF and the support of the photogrammetry 

mission. 

System integration planning in Chile 

progressed well. Discussions with all IPTs 

about deliveries and acceptance of 

equipment for Chilean Assembly, 

Integration and Verification (AIV) were 

held and documented. The Japanese AIV 

involvement, deliverable and schedule 

were agreed. The interface between the 

ALMA Back End engineers at work. 

IPTs delivering the equipment and the 

commissioning team receiving the system 

from AIVS was agreed and documented. 

The AIV Interim Lab construction, needed 

because the OSF technical building will 

only be ready at the beginning of 008, 

was completed. The Holography Tower 

construction was completed. In total 11 

AIV engineers have been employed. All 

are posted at the executives (Socorro, 

Charlottesville, Garching) for training. 

Science Activities 

One of the main roles of the Science IPT 

is to define the top-level science requirements 

for ALMA and, in close collaboration 

with the System Engineering team, to 

ensure that they can be met by the 

hardware and software. The year 006 

saw the completion of a comprehensive 

System Requirements Review, covering 

all aspects of the specification. The major 

conclusion was that the current design 

would indeed meet (and in several areas 

such as receiver sensitivity even exceed) 

the demanding specification.

The calibration of ALMA is a challenging 

problem. The Science IPT has produced 

a comprehensive series of examples 

which demonstrate how key quantities 

such as amplitude, phase, antenna 

location and instrumental polarisation can 

be calibrated in practice. Even on the 

excellent Chajnantor site, water vapour in 

the atmosphere both absorbs and 

refracts millimetre waves from astronomical 

sources. To correct the fast fluctuations 

of phase which would otherwise 

limit imaging, ALMA will use a combination 

of two methods: fast switching 

between the object of interest and a 

nearby point calibrator, and water vapour 

radiometry. The latter technique measures 

emission from the 183-GHz atmospheric 

water line, using receivers 

mounted on each antenna and infers the 

resulting phase differences on all 

baselines. 

ALMA Regional Centre 

The European ALMA Regional Centre 

(ARC) is part of ESO’s Data Management 

Operations Division and started its activities 

on 1 June 006. The ARC’s mission 

is to provide the science and technical 

support services necessary for 

the European user community to exploit 

ALMA to its full scientific potential. The 

ARC will form the interface between 

the ALMA Observatory in Chile and the 

European user community. Similar ARCs 

are currently being established in North 

America and East Asia, ESO’s partners in 

the trilateral ALMA project. For Europe- 

an users, the ARC is being set up as a 

cluster of nodes located throughout Europe, 

with the main coordinating centre at 

the ESO Headquarters in Garching. In 

this distributed network, user support 

and operations experience at ESO can 

be mixed with millimetre-wave astronomy 

experience that exists in the communi- 

ty to create optimal science support services. 

The European ARC will be the point of 

contact for European ALMA users 

from the moment of proposal submission 

to the actual distribution of calibrated 

data and consequent analysis. The core 

of the ARC activities will consist of running 

a help desk for the proposal submission 

and submission of observing programmes, 

the delivery of data to principal 

investigators, the maintenance and refinement 

of the ALMA data archive, and 

the feedback to the data reduction pipeline 

and the off-line reduction software 

systems that surround it. 

Among the tasks of the ARC Manager is 

the contribution to the preparation of 

the ALMA Operations Plan (AOP), which 

describes both the science operations 

and the technical services provided by 

the technical staff when ALMA becomes 

operational, and its implementation within 

ESO. 

Fundamental to ALMA’s success in Europe 

are the enhanced services provided 

by the network of ARC nodes. These are 

required to fully realise the potential of 

ALMA and to maximise the scientific return 

for the European community. Fostering 

community development and guid- 

ing the future evolution of ALMA’s use 

are among the primary tasks for the 

nodes. The nodes will provide face-toface 

help and additional support, beyond 

what are called the ARC core functions. 

This help includes, for example, 

advanced user support for special projects, 

and refinement in the data reduction 

process. To achieve these goals, 

the nodes will conduct fellowship, user 

grant, student and postdoctoral programmes, 

as well as promote the organisation 

of workshops, schools, and any 

other support facilities for users. 

The ARC Manager coordinates this network 

of nodes. Activities have been 

started with a face-to-face meeting with 

representatives of the ARC nodes, held 

at ESO on 9 August. Most of these activities 

are described on the ARC web 

page (www.eso.org/projects/alma/ARC), 

whereas internal information is shared 

and exchanged via a ‘wiki’. 


Organisational structure 

of the European 

ALMA Regional Centre. 

43

44 


The European Extremely Large Telescope 

Extremely Large Telescopes – telescopes 

with a diameter of 30 m or more – are 

seen worldwide as one of the highest priorities 

in ground-based astronomy. They 

will vastly advance astrophysical knowledge, 

allowing detailed studies of, inter 

alia, planets around other stars, the first 

objects in the Universe, supermassive 

black holes, and the nature and distribution 

of the dark matter and dark energy 

which dominate the Universe. The European 

Extremely Large Telescope project 

will maintain and reinforce Europe’s position 

at the forefront of astrophysical research 

and, as such, it is no surprise that 

it was included in the European Strate- 

gy Forum on Research Infrastructures 

(ESFRI) Roadmap in October 006. This 

European Roadmap, defined at the 

request of the European Union Council, 

identifies new Research Infrastructures 

of pan-European interest corresponding 

to the long-term needs of the European 

research communities which are likely to 

be realised in the next 10 to 0 years, 

covering all scientific areas and regardless 

of possible location. 

The European Extremely Large Telescope 

(E-ELT) project made large strides in 

006. In the first half of the year, five working 

groups composed of over 100 scientists 

and engineers from ESO and its 

community of users elaborated a new 

vision for the project. These ELT Science 

and Engineering (ESE) working groups 

focused on the scientific case, telescope 

design, site, adaptive optics and instrumentation. 

Chaired by members of the 

community, the working groups produced 

their reports, which were collected into 

a ‘tool box’ to guide the further design activities. 

The chairs of the working groups, augmented 

by members of the ESO Scientific 

Technical Committee (STC), formed a 

subcommittee of the STC naturally 

named ESE to monitor the project and 

advise both the STC and ESO on the 

work. In parallel to this community-wide 

consultation, the ESO Council established 

an ELT Standing Review Committee 

(ESRC) composed of external experts 

to advise on a broad variety of aspects to 

do with the project. 

With the tool box in place, ESO formed a 

telescope project office in the middle 

of the year and tasked it with absorbing 

the recommendations of the ESE working 

groups and developing a coherent 

proposal for a telescope – a baseline reference 

design – and associated instrumentation 

to be elaborated upon in the 

coming years. The ESO ELT programme 

is in fact split into three parallel activities 

on telescope, instrumentation and operations, 

each with its own office within the 

respective divisions at ESO: Telescope 

Systems, Instrumentation, and Data Management 

and Operations. 

Innovative Design 

The baseline reference design of the telescope 

is to have adaptive optics as 

an integral part of the system, to provide 

instrumentation with gravity-invariant 

foci, to have an instrumentation-friendly 

focal plane and to avoid the areas considered 

high-risk by the OWL review undertaken 

in late 005. The telescope 

design working group activities focused 

on establishing the viability and relative 

merits of the two front-runners in the designs 

that could address these basic 

requirements. The first design was a classical 

Gregorian telescope and the second 

a novel five-mirror design. The activities 

at ESO focused on establishing the 

viability of a mechanical structure to support 

a mirror diameter of 4 metres and 

the rest of the optics required to relay the 

beam back to a focal station. Sophisticated 

finite-element modelling and analysis, 

as well as preliminary control engineering 

work, were used to develop a 

mechanical structure that could host 

either of the two designs with comparable 

performance. The size of 4 metres 

was considered by the ESE as a good 

compromise between ambition and technical 

feasibility. 

In parallel, ESO contracted European industrial 

firms to develop conceptual designs 

for the adaptive optics systems that 

are going to be built into the telescope. 

External consultants worked on developing 

concepts for the dome to house the 

telescope and within ESO a great deal of 

attention has been placed on the interfaces 

of the telescope and its infrastructure 

with instrumentation. Industrial firms 

were contacted to establish a first topdown 

cost estimate for the telescope. 

The two optical designs considered during the Basic Reference Design development: five-mirror (left) and 

Gregorian (right). 


45

The activities within the EU FP6-supported 

ELT Design Studies programme, 

led by ESO but largely executed in 

industry and academia outside the 

organisation, are aligned with the 

activities of the E-ELT programme and in 

all areas much progress is being made. 

Actuator prototypes, edge sensors, phasing 

techniques, wind evaluation systems, 

dome designs, site testing and many 

other such activities are all contributing to 

the knowledge we require to advance the 

project into the next phase. Integral to 

this planning is the membership of Spain 

in ESO and the expertise that the Spanish 

community will bring. Spain has just 

completed the segmented 10.4-m Gran 

Telescopio Canarias (GTC) telescope 

and, with Spain’s membership, ESO 

engineers will gain technical access to 

that system. 

Participants to the E-ELT conference in Marseille. 

46 


The baseline reference design selected 

and approved by the ESO Council to 

move into the Phase B of the project is 

the five-mirror design. While the Gregorian 

design had advantages in a better 

theoretical performance in adaptive optics, 

a smaller mirror count and smaller 

central obstruction, the five-mirror design 

was considered to have advantages in 

the image quality across the focal plane, 

the control of the wavefront using laser 

guide stars, the flexibility of the focal stations, 

the deployment of atmospheric 

dispersion compensators, the smaller 

dome and the relative ease with which it 

could be upgraded to follow the development 

of technology in the future. Most 

critically however, the five-mirror design 

was considered to have much lower risk 

in the area of adaptive optics by virtue 

of the separation of the field-stabilisation 

and adaptive-optics functions, a key recommendation 

of the OWL review. 

Into Phase B 

The results of this burst of activity came 

together during November 006 in preparation 

for a series of presentations of 

the Project Office conclusions to ESE, 

ESRC, STC, to 50 astronomers at the 

Marseilles meeting on the E-ELT and, finally, 

to the ESO Council. The endorsement 

of the Project Office proposal by 

this broad spectrum of the community 

and decision makers reflects not only the 

good progress ESO made during 006 

in the elaboration of the design but also 

the clear scientific need to advance 

rapidly and effectively in the area of E- 

ELTs and the commitment of the user 

community.

The baseline reference design selected and 

approved by the ESO Council to move into 

the Phase B of the project is the five-mirror 

design. While the Gregorian design had 

advantages in a better theoretical performance 

in adaptive optics, a smaller mirror 

count and smaller central obstruction, the 

five-mirror design was considered to have 

advantages in the image quality across the 

focal plane, the control of the wavefront 

using laser guide stars, the flexibility of the 

focal stations, the deployment of atmospheric 

dispersion compensators, the 

smaller dome and the relative ease with 

which it could be upgraded to follow the 

development of technology in the future. 

Most critically however, the five-mirror 

design was considered to have much lower 

risk in the area of adaptive optics by virtue 

of the separation of the field-stabilisation 

and adaptive optics functions, a key recommendation 

of the OWL review. 

The E-ELT is now in Phase B, a period 

during which the design will be elaborated 

further. Together with academic and 

industrial partners, and with continuous 

consultation with its user community, 

ESO expects that a proposal for the 

construction of this ambitious project can 

be ready by the end of this decade. 

A Revolutionary Concept 

The present concept features as a 

base-line a 4 -m diameter mirror 

telescope, and is revolutionary. The 

primary mirror is composed of 906 

segments, each 1.45 m wide, while the 

secondary mirror is as large as 6 m in 

diameter. In order to overcome the 

fuzziness of stellar images due to 

atmospheric turbulence the telescope 

needs to incorporate adaptive mirrors 

into its optics, and a tertiary mirror, 4. 

m in diameter, relays the light to the 

adaptive optics system, composed of 

two mirrors: a .5-m mirror supported 

by 5 000 or more actuators so as to be 

able to distort its own shape a 

thousand times per second, and one 

.7 m in diameter that allows for the 

final image corrections. This five-mirror 

approach results in an exceptional 

image quality, with no significant 

aberrations in the field of view. 


47

48 


Organisation and Personnel 

The main organisational and managerial 

units of ESO are the Divisions which 

currently include: the Office of the 

Director-General, the Administration, the 

Space Telescope/European Coordinating 

Facility, the La Silla Paranal Observatory, 

and the Instrumentation, Telescope 

Systems, Technology, Data Management 

and Operations, Software Development, 

and ALMA Divisions. Most divisions are 

organised in Departments, some of which 

consist of two or more Groups. 


49

List of Personnel 

Office of the Director 

General 1 

Catherine Cesarsky 

Fatme Allouche 

Catarina Alves de 

Oliveira 

Gonzalo Argandoña 

Lazo 

Mustafa Basbilir 

Mary Bauerle Blandford 

Luigi Bedin 

Yuri Beletsky 

Angelika Beller 

Adrianus Bik 

Michael Böcker 

Henri Boffin 

Konstantina Boutsia 

Jutta Boxheimer 

Pamela Bristow 

Benoît Carry 

Mary Cesetti 

Gaël Chauvin 

Lise Bech Christensen 

Blair Campbell Conn 

Silvia Cristiani 

Itziar De Gregorio 

Monsalvo 

Gayandhi Manomala 

De Silva 

Eric Depagne 

Jörg Dietrich 

Michelle Doherty 

Michaela Döllinger 

Brigitta Eder 

Christopher Erdmann 

Davide Fedele 

Cedric Foellmi 

Audrey Galametz 

Emmanuel Galliano 

Kerstin Geissler 

Mark Gieles 

Carla Gil 

Rachel Emily Gilmour 

Raphael Gobat 

María Eugenia 

Gómez Carrasco 

Luis Goncalves Calçada 

Claudio Grillo 

Uta Grothkopf 

Karin Hansen 

Markus Hartung 

Hans Hermann Heyer 

Renate Hoppe-Lentner 

Hannes Horst 

Gaël James 

Edmund Janssen 

Paulina Jiron Planella 

Andres Jordan 

Eric Jullo 

Georg Junker 

Jouni Kainulainen 

Katarina Kiupel 

Karina Kjær 

Rubina Kotak 

Isolde Kreutle 

Daniel Kubas 

Jean Baptiste 

Le Bouquin 

Bruno Leibundgut 

Silvia Leurini 

Cristian Lopez 

Paul Lynam 

1 Including all the 

Fellows and Students 

under the Studentship 

programme. 

50 


Mariya Lyubenova 

Claus Madsen 

Vincenzo Mainieri 

Gautier Mathys 

Jorge Melnick 

Maria Messineo 

Steffen Mieske 

Igor-Felix Mirabel 

Lorenzo Monaco 

Marcelo Mora 

Dominique Naef 

Thomas Naets 

Kim Nilsson 

Pasquier Noterdaeme 

Christina Papadaki 

Laura Catherine Parker 

Enikö Patkos 

Silvia Pedicelli 

Douglas Pierce-Price 

Olga Pinto Moreira 

Farid Rahoui 

Suzanna Randall 

Jaroslaw P. Rzepecki 

Francesco Saitta 

Hugues Sana 

Julia Scharwächter 

Andreas Seifahrt 

Zhixia Shen 

Rodolfo Silva Smiljanic 

Colin Snodgrass 

Veronica Sommariva 

Thomas Stanke 

Christina Stoffer 

Gabriel Szasz 

Svea Teupke 

Sune Toft 

Ezequiel Treister 

Stefan Uttenthaler 

Stefano Valenti 

Elena Valenti 

Gerrit van der Plas 

Martin Vannier 

Stefan Vehoff 

Daniela Villegas Mansilla 

Elisabeth Völk 

Rein Warmels 

Michael Weigand 

Thomas Wilson 

Gabriele Zech 

Administration Division 

Hans Jahreiss 

Hugo Freddy Aguilera 

Eduardo Arenas 

Paredes 

Andres Arias 

Angela Arndt 

Roland Block 

Jean-Michel Bonneau 

Renate Brunner 

Cecilia Carrasco Cruz 

Laura Comendador 

Frutos 

Walter Demartis 

Tommaso Di Dio 

Günther Dremel 

Willem Arie Dirk Eng 

Robert Fischer 

Nicolás Fischman Rajii 

Sonia Gárnica Plaza 

Rebonto Guha 

Priya Nirmala Hein 

Charlotte Hermant 

Hans Jahreiss 

Nathalie Kastelyn 

Elizabeth Kerk 

Hans-Jürgen Kraus 

Katjuscha Lockhart 

Ignacio Lopez Gil 

Maria Madrazo 

Silvia Madrid Pariente 

Jorge Moreno González 

María Angélica Moya 

Helene Neuville 

Christine Nieuwenkamp 

Mauricio Quintana 

Ipinza 

Rolando Quintana 

Ipinza 

André Louis Ritz Solari 

Rosa Ivonne Riveros 

Cárdenas 

Francky Rombout 

Nadja Sababa 

María Soledad Silva 

Castán 

Erich Siml 

Beatrice Sivertsen 

Roswitha Slater 

Albert Triat Saurat 

Ullrich Urban 

Lone Vedsø Marschollek 

Sabine Weiser 

Yves Wesse 

Gerd Wieland 

La Silla Paranal 

Observatory 

Andreas Kaufer 

Nancy Ageorges 

Luis Águila Vargas 

Claudio Agurto 

Bernardo Ahumada 

Héctor Alarcón Ramírez 

Mario Alfaro Varela 

Jaime Alonso Torrini 

Nilso Alquinta Espejo 

Jose Luis Alvarez 

Paola Amico 

Michel Anciaux 

Andreas Andersson 

Lundgren 

Gaetano Andreoni 

Ernesto Araya Troncoso 

Juan Carlos Arcos 

Álvarez 

Javier Argomedo 

Karla Aubel 

Francisco Azagra 

Jose Baez 

Stefano Bagnulo 

Pedro Baksai 

Emilio Barrios Rojas 

Rogelio Bascunan 

Bertrand Bauvir 

Eduardo Bendek 

Per Mikael Bergman 

Guillame Blanchard 

Carlos Bolados 

Henri Bonnet 

Stephane Brillant 

Armando Bruna Bruna 

Erich Bugueño 

Blanca Camucet Ortiz 

Massimiliano Camuri 

Luis Alejandro 

Caniguante 

Michael Cantzler 

Ruben Carcamo 

Cesar Cardenas 

Johan Carstens 

Fabio Caruso 

Duncan Castex 

Roberto Castillo Ladrón 

De Guevara 

Mónica Castillo Cortés 

Jorge Castizaga 

Cáceres 

Susana Cerda 

Hernández 

Cecilia Cerón Canelo 

Claudia Cid Fuentes 

Florentino Contreras 

Alex Correa Gutiérrez 

José Ignacio Cortés 

Mandiola 

Ángela Cortés Carvallo 

Jaime Costa Abarca 

Claudio De Figueiredo 

Melo 

Reinaldo Donoso Marín 

Javier Duk Díaz 

Christophe Dumas 

Michael Dumke 

Domingo Durán Cortés 

Carlos Durán Urrutia 

Yves Durand 

Carlos Ebensperger Eliz 

Cristian Esparza 

Morales 

Loreno Esparza Morales 

Erito Flores Arias 

Juan Carlos Fluxá 

Nadeau 

Patrick Francois 

Sergio Gaete Román 

Enrique Garcia 

José Gardiazabal 

Schilling 

Gordon Gillet 

Alain Gilliotte 

Percy Glaves Peters 

Leonardo González 

Hernández 

Domingo González 

Leyton 

Andrés González López 

Sergio Gonzalez Burgus 

Víctor González Toro 

Charlotte Groothuis 

Patricia Guajardo 

Obando 

Carlos Guerra Escobar 

Stephane Guisard 

Serge Guniat 

Flavio Gutiérrez Willer 

Fernando Gutierrez 

Nicolas Haddad 

Salcedo 

Juan Pablo Haddad 

Ferretto 

Pierre Haguenauer 

Olivier Hainaut 

George Harding 

Juan Pablo Henriquez 

León 

Cristian Herrera 

González 

Leonardo Herrera 

González 

Herrera Mena, Leonardo 

Swetlana Hubrig 

Gerhard Hüdepohl 

Rodrigo Huerta 

Ramón Huidobro 

Nordenflycht 

Christian Hummel 

Gerardo Ihle 

Valentin Ivanov 

Emmanuel Jehin 

Jorge Jiménez Rojas 

Nestor Jiménez Odgers 

Ismo Kastinen 

Andreas Kaufer 

Nicholas Charles 

Kornweibel 

Carlos La Fuente Peña 

Francisco Labraña 

Zamorano 

Octavio Lavín Catril 

Paul Le Saux 

Cedric Ledoux 

Alfredo Leiva Becerra 

Ramón Leyton Muñoz 

Christopher Lidman 

Gaspare Lo Curto 

Ignacio López Vilches 

Ariel Lopez Ortega 

Fernando Luco 

Meneses 

Javier Luhrs Middleton 

Felipe Mac-Auliffe Prieto 

Agustín Macchino Farías 

Massimiliano Marchesi 

Gianni Marconi 

Pedro Mardones Ojeda 

Pedro Marín Fuentes 

Kiriako Markar Aros 

Mauricio Martinez 

Parada 

Elena Mason 

Eduardo Matamoros 

Pastén 

Rolando Medina Zanetta 

Juan Alberto Mella 

Angel Mellado González 

Alejandra Mena Briceño 

Jorge Miranda Mery 

Juan Molina Watanabe 

Nelson Montano Ortiz 

Alex Morales Agurto 

Sebastien Morel 

Merilio Morell Rodríguez 

Manfred Mornhinweg 

Krohmer 

Ivan Muñoz Máximo 

Julio Navarrete Lavín 

Jean-Luc Nicoud 

Hernan Nievas 

Fernández 

Dieter Nürnberger 

Herman Nuñez Portilla 

Lars A. Nyman 

Kieran O’Brien 

Rodrigo Olivares Álvarez 

Francisco Olivares 

González 

Ernesto Orrego 

Cisternas 

Óscar Orrego Sandoval 

Juan Osorio Escrich 

Juan Carlos Palacio 

Valenzuela 

Ricardo Parra Paz 

José Parra Ortiz 

Andrés Parraguez 

Cárcamo 

Marcus Pavez Hubner 

Eduardo Peña 

Juan Pineda Hernández 

Andres Pino 

Manuel Pizarro López 

De Maturana 

Aldo Pizarro Hess 

Andrés Pizarro Pavez 

Emanuela Pompei 

Hugo Quijón Duarte 

Andrés Ramírez Molina 

Fredrik Rantakyrö 

Johnny Reveco Arias 

Vincent Reveret 

Miguel Riquelme Oyarce 

Christophe Risacher 

Thomas Rivinius 

Luis Roa Figueroa 

Pascal Robert 

William Robinson 

Chester Rojas 

Gorky Román Delgado 

José Rosas Ávalos 

Felix Alberto Rozas 

Francisco G. Ruseler 

Claudio Sagüez García 

Daniel Salazar Barrera 

Fernando Salgado 

Ibarra 

Alejandro Salinas 

Fenero 

Ariel Sánchez Peñailillo 

Stefan Sandrock 

Roberto Sanhueza 

Slater

Pierre Sansgasset 

Jorge Santana 

Marambio 

Ivo Saviane 

Linda Schmidtobreic 

Ricardo Schmutzer Von 

Oldershausen 

Markus Schöller 

Oliver Schuetz 

Fernando Selman 

Jorge Sepúlveda Ortega 

Tzu Chiang Shen 

Waldo Siclari Bordones 

Peter Sinclaire Aguirre 

Alain Smette 

Fabio Somboli 

Rubén Soto Troncoso 

Mauro Stefanon 

Stanislav Stefl 

Michael Fritz Sterzik 

Sandra Strunk 

Thomas Szeifert 

Roberto Tamai 

Mario Tapia Gonzáles 

Manuel Torres 

Zamorano 

Soraya Torres López 

Guillermo Valdés 

José Javier Valenzuela 

Soto 

Karen Vallejo Cerda 

Leonardo Vanzi 

Oscar Varas Mella 

Enrique Vera Diaz 

Jorge Vilaza Méndez 

Stefan Wehner 

Ueli Weilenmann 

Luis Wendegass 

Mellado 

Andrew Wright 

Juan Christóbal Zagal 

ALMA Division 

Hans Rykaczewski 

Gareth Aspinall 

Fabio Biancat Marchet 

Claus Dierksmeier 

Jörg Eschwey 

Preben Grosbøl 

Christoph Haupt 

Jorge Ibsen 

Andreas Kempf 

Hervé Kurlandczyk 

Robert Alexander Laing 

Pascal Lapeyre 

Pascal Martinez 

Angel Otárola Medel 

Eric Pangole 

Ferdinand Patt 

Gianni Raffi 

Silvio Rossi 

Hans Rudolf 

Joseph Schwarz 

Stefano Stanghellini 

Donald Tait 

Gie Han Tan 

Nathalie Thebaud 

Eugenio Ureta Bravo 

Elena Zuffanelli 

Jennifer Hewitson 

Manuel de Menezes 

Telescope System 

Division 

Roberto Gilmozzi 

Constanza Araujo 

Hauck 

Robin Arsenault 

Domenico Bonaccini 

Calia 

Jeroen de Jong 

Françoise Delplancke 

Frédéric Derie 

Philippe Dierickx 

Robert Donaldson 

Enrico Fedrigo 

Yan Feng 

Andreas Glindemann 

Wolfgang Hackenberg 

Ronald Holzlöhner 

Norbert Hubin 

Markus Kasper 

Bertrand Koehler 

Johann Kolb 

Visa Korkiakoski 

Miska Kristian Le Louarn 

Samuel Leveque 

Jochen Liske 

Enrico Marchetti 

Patrice Martinez 

Serge Menardi 

Samantha Milligan 

Guy Monnet 

Riccardo Muradore 

Sylvain Oberti 

Jérôme Paufique 

Duc Thanh Phan 

Florence Puech 

Mark Robinson 

Tatyana Sadibekova 

Marc Sarazin 

Kevin Scales 

Nicolas Schuhler 

Christian Soenke 

Jason Spyromilio 

Josef Strasser 

Stefan Ströbele 

Isabelle Surdej 

Arkadiusz Swat 

Luke Taylor 

Gautam Vasisht 

Christophe Verinaud 

Elise Vernet 

Anders Wallander 

Nataliya Yaitskova 

Davide Zil 

Data Management and 

Operations Division 

Fernando Comerón 

Paola Andreani 

Fabien Chereau 

Fernando Comeron 

Carlos De Breuck 

Nausicaa Delmotte 

Danuta Dobrzycka 

Adam Dobrzycki 

Markus Dolensky 

Nina Felber 

Nathalie Fourniol 

Monika Gotzens 

Reinhard Hanuschik 

Paul Harrison 

Evanthia Hatziminaoglou 

Michael Hilker 

Wolfgang Hummel 

John Lockhart 

Jean-Christophe 

Malapert 

Stephane Marteau 

Sabine Mengel 

Sabine Moehler 

Palle Møller 

Petra Nass 

Mark Neeser 

Paolo Padovani 

Ferdinando Patat 

Isabelle Percheron 

Francesca Primas 

John Pritchard 

Marina Rejkuba 

Jörg Retzlaff 

Bruno Rino 

Charles Rite 

Jesus Rodriguez Ulloa 

Martino Romaniello 

Piero Rosati 

Remco Slijkhuis 

Dieter Suchar 

Lowell Tacconi-Garman 

Mario Van Den Ancker 

Benoît Vandame 

Andreas Wicenec 

Markus Wittkowski 

Burkhard Wolff 

Martin A. Zwaan 

Space Telescope – 

European Coodination 

Facility 

Lars Lindberg 

Christensen 

Wolfram Freudling 

Francesca Granato 

Jonas Haase 

Richard Hook 

Martin Kornmesser 

Martin Kümmel 

Harald Kuntschner 

Marco Lombardi 

Paola Popesso 

Britt Sjöberg 

Aitana Vargas 

Jeremy Walsh 

Software Development 

Division 

Michele Peron 

Roberto Abuter 

Eric Allaert 

Luigi Andolfato 

Pascal Ballester 

Klaus Banse 

Peter Biereichel 

Alessandro Caproni 

Sandra Maria Castro 

Maurizio Chavan 

Gianluca Chiozzi 

Mauro Comin 

Livio Condorelli 

Stéphane Di Cesare 

Gabriele Donino 

Dario Dorigo 

Philippe Duhoux 

Sylvie Feyrin 

Robert Frahm 

Bruno Gilli 

Carlos Guirao Sanchez 

Birger Gustafsson 

Karim Haggouchi 

Carlo Izzo 

Bogdan Jeram 

Yves Jung 

Robert Karban 

Mario Kiekebusch 

Maurice Klein Gebbinck 

Jens Knudstrup 

Antonio Longinotti 

Henning Lorch 

Lars Kristian Lundin 

Holger Meuss 

Andrea Modigliani 

Christophe Moins 

Ralf Palsa 

Moreno Pasquato 

Martine Peltzer 

Werther Pirani 

Dan Popovic 

Eszter Pozna 

Marcus Schilling 

Diego Sforna 

Paola Sivera 

Fabio Sogni 

Heiko Andreas Sommer 

Stefano Turolla 

Jakob Vinther 

Krister Wirenstrand 

Michele Zamparelli 

Stefano Zampieri 

Instrumentation 

Division 

Alan Moorwood 

Matteo Accardo 

Gerardo Avila 

Dietrich Baade 

Andrea Balestra 

Paul Bristow 

Iris Bronnert 

Mark Casali 

Claudio Cumani 

Sebastian Deiries 

Klaas Johannes Dekker 

Sandro D’Odorico 

Reinhold Dorn 

Mark Desmond 

Downing 

Christophe Dupuy 

Siegfried Eschbaumer 

Gert Finger 

Christoph Geimer 

Stefan Hötzl 

Olaf Iwert 

Hans-Ulrich Käufl 

Florian Kerber 

Jean Paul Kirchbauer 

Jean-Louis Lizon à 

L’Allemand 

Antonio Ramon 

Manescau Hernandez 

Leander H. Mehrgan 

Manfred Meyer 

Luca Pasquini 

Markus Patig 

Jean-François Pirard 

Roland Reiss 

Javier Reyes 

Andrea Richichi 

Gero Rupprecht 

Ralf Siebenmorgen 

Armin Silber 

Jörg Stegmeier 

Sebastien Tordo 

Joel Daniel Roger Vernet 

Technology Division 

Martin Cullum 


Roland Brast 

Enzo Brunetto 

Bernard Buzzoni 

Ralf Dieter Conzelmann 

Bernard-Alexis Delabre 

Nicola Di Lieto 

Canio Dichirico 

Martin Dimmler 

Michel Duchateau 

Toomas Erm 

Raul Esteves 

Giorgio Filippi 

Gerhard Fischer 

Christoph Frank 

Philippe Gitton 

Domingo Gojak 

Frederic Yves Joseph 

Gonté 

Ivan Maria Guidolin 

Volker Heinz 

Florian Heissenhuber 

Guy Hess 

Georgette Hubert 

Gotthard Huster 

Georg Igl 

Andreas Jost 

Franz Koch 

Heinz E. Kotzlowski 

Maximilian Kraus 

Simon Lowery 

Christian Lucuix 

Ruben Mazzoleni 

Jean-Michel Moresmau 

Michael Müller 

Michael Naumann 

Lothar Noethe 

Edouard Pomaroli 

Marco Quattri 

Jutta Quentin 

Michael Schneermann 

Babak Sedghi 

Barbara Sokar 

Jesper Thillerup 

Arno Van Kesteren 

Véronique Ziegler 

Seconded Staff 

Members 

Joint ALMA Office 

Massimo Tarenghi 

Alejandra Araya 

Ann Edmunds 

Jacques Lassalle 

Russell Smeback 

51

Personnel Services 

The ‘Five-Yearly Review’ of the conditions 

of employment for International Staff 

Members was completed, in close interaction 

with CERN. The results of the 

study led to further reviews and amendments, 

in particular regarding: the definition 

of family, now recognising same-sex 

marriages and same-sex or opposite- 

sex partnerships; maternity leave, parental 

leave and further options to facilitate 

and increase the harmonisation of family 

and professional career; education grants 

and expatriation allowances. 

The Personnel Department in Garching 

and Vitacura prepared and concluded the 

collective bargaining with the representatives 

of the Unions of La Silla and Paranal 

as well as with the representatives of the 

Administration in Santiago. The new Collective 

Contracts are effective as of 1 December 

006 for a period of three years. 

The process of the creation and implementation 

of the Software Development 

Division and reorganisation of the Data 

Management and Operations Division 

was accomplished. Personnel also participated 

in the review and restructur- 

ing of the Administration Division, all the 

related decisions being implemented by 

1 July 006. 

5 

Others 

9.4 % 

Sweden 

.3 % 

Portugal 

0.3 % 

The Netherlands 

3.7 % 

Italy 

18.9 % 

United Kingdom 

5.7 % 


Personnel Services was greatly involved 

in matters regarding the ALMA project. 

We participated in the recruitment of key 

positions of the Joint ALMA Observatory, 

in the foundation of the ALMA Human 

Resource Advisory Group, and in the 

completion of the Internal Regulations as 

well as the Compensation and Benefits 

for ALMA Local Staff. 

The ‘leave module’ was implemented for 

Garching on 1 July 006 in the ERP system. 

To make this process smooth, training 

was provided for all the Staff. 

To make new staff members in Garching 

more used to all the aspects of the organisation, 

from an overview of its different 

activities to very practical questions, 

an induction day was established with 

support from all Divisions at ESO. Conditions 

in Garching have also been improved 

for young parents with the opening 

of the IPP/ESO Crèche on 1 April 

006. 

Other activities included participating in 

the recruitment of key management 

positions in Garching and Chile, making 

regular visits to the sites in Chile in or- 

der to keep close contact with the International 

and Local Staff Members and 

their representatives, organising common 

training in ‘managing people’ for about 

Belgium 

4.9 % 

Switzerland 

1.4 % 

Germany 

3 .6 % 

Denmark 

3.1% 

France 

17.7% 

5 team leaders of the La Silla Paranal 

Observatory during the month of November 

006, and providing short-term and 

long-term office accommodation in 

Garching. 

The employment conditions and further 

guidelines for International Staff Members 

and Local Staff in Chile were revised, particularly 

with respect to: 

– The calculation and adjustment of 

the Cost of Living for International Staff 

Members in Chile; 

– Contract Policy for International Staff 

Members; 

– Regular medical examinations for Staff 

in Chile and Garching; 

– Equal Opportunity Statement; 

– Recruitment Policy Statement and its 

guidelines; 

– The application of the Social Activity 

Day; 

– Limitation of claims; 

– Home leave regulation; 

– The application of official holidays 

during duty travels. 

In the course of the year, 9 Local Staff 

and 34 International Staff Members were 

recruited. In addition, 101 Students, Fellows, 

and Paid and Unpaid Associates 

joined ESO. The diagramme below shows 

the International Staff Members of ESO, 

by nationality, as of December 006. 

Distribution of International 

Staff Members 

by Nationality as of 

31 December 006.

Instrumentation 

Highlights of the year were the installation 

and commissioning on Antu (UT1) of the 

Cryogenic Infrared Spectrometer (CRI- 

RES), the last of the first-generation VLT 

instruments, and the successful commissioning 

of the laser guide-star facility 

on Yepun (UT4), which will substantial- 

ly increase the sky coverage achievable 

with the adaptive optics assisted instruments 

NACO and SINFONI. The Omega- 

CAM camera was completed in advance 

of the VLT Survey Telescope for which it 

has been built; integration of the HAWK-I 

infrared camera for the VLT started in 

Garching; work on PRIMA continued; 

the approved second-generation VLT 

instruments X-Shooter, KMOS, MUSE 

and SPHERE, plus the Adaptive Optics 

Facil-ity (AOF) and the new NGC detector 

con-troller all progressed well, and Phase 

A studies were launched of three 

potential second-generation VLT interferometric 

instruments to eventually 

replace MIDI and AMBER. In addition, 

work ramped up on defining the ELT 

instrument interfaces and the design of 

possble instruments both within the ESO 

E-ELT Instrument Project Office and the 

FP6 ELT Design Study. 

The leadership and know-how in astronomical 

instrumentation of ESO and 

its partners was very visible at the 006 

SPIE Astronomical Telescopes and 

Instrumentation Symposium that took 

place in Orlando, Florida, bringing together 

1700 astronomy, technology, and 

engineering experts from all over the 

world. ESO staff played a key role in the 

numerous meetings, either as organisers 

or speakers, and many ESO projects 

were discussed. 

CRIRES, the infrared (1–5 μm), high resolution 

(R = 10 5 ), adaptive optics assisted 

spectrograph built for the VLT by ESO 

was integrated, extensively tested and 

formally passed its Preliminary Acceptance 

Europe (PAE) review in Garching on 

13 April. In order to optimise the installation 

and commissioning process the 

adaptive optics part was reviewed first, 

and released for shipment to Chile by the 

end of February. First light was achieved 

with an infrared test camera on 6 April 

when the adaptive optics control loop 

was closed on the star b Muscae. Although 

packing of the cryogenic spectrograph 

only started on 5 April, first astro- 

nomical spectra were already obtained 

together with the adaptive optics feed on 

4 June. We believe that this constitutes 

a record time for such a complex installation. 

By year’s end, commissioning was 

almost complete and the first scientific 

results had already been obtained through 

a highly successful set of science verification 

observations conducted to test the 

end-to-end system including the proposal 

preparation, instrument operation, and 

data handling and analysis tools and procedures. 

Following final commissioning 

and calibration in early 007, CRIRES will 

officially enter full science operations at 

the start of Period 79 on 1 April. 

The Laser Guide Star Facility (LGSF) had 

first light on 8 January. During the first 

commissioning a degradation of the image 

quality of the projected artificial star 

was detected. This was found to be due 

to the deformation of the flange at the 

interface between the launch telescope 

and the secondary mirror of UT4. The 

flange was redesigned and replaced in 

April. This solved much of the image quality 

problem although a second problem 

appeared: at low temperatures the 

supports of the launch telescope’s primary 

mirror caused an aberration that 

also affected the image quality of the artificial 

star. The launch telescope was 

dismounted, tested and shipped back to 

Garching for repairs. A task force was 

created to manage the recovery actions. 

A new mirror support was designed 

and mounted in the launch telescope. A 

more advanced focusing mechanism 

was also developed and mounted. A comprehensive 

set of realistic tests was then 

performed in a controlled environment 

to check the quality of the refurbishment 

before sending the launch telescope 

back to Paranal in October. All recovery 

activities were done in collaboration 

with the telescope provider. The LGSF 

went back ‘on sky’ in October, and 

commissioning resumed together with 

the NACO and SINFONI instruments. 

Although not yet fully within specifications, 

the LGSF was starting to produce 

scientific results at the end of the year. 

The OmegaCAM wide-field optical camera 

for the VST was finished and passed 

its PAE. The camera itself has been 

built by a German/Dutch/Italian consortium 

and the detector system, compris- 

ing a mosaic of 3 CCDs, by ESO. The 

instrument is now being stored in Garching, 

awaiting the installation and commissioning 

on Paranal in 007 of the 

.6-m VST, being supplied by INAF in 

Italy. 

Manufacturing and procurement of essentially 

all the components of the 

HAWK-I infrared camera for the VLT proceeded 

well. In particular, all four of its 

k × k Hawaii RG infrared detectors 

were delivered and fully tested with excellent 

results. They were mounted together 

to form a mosaic similar to that planned 

for the James Webb Space Telescope. 

The radiation shield was installed in the 

vacuum vessel in Garching, resulting in a 

rather large camera system. The reflecting 

optics were also mounted and found 

to exhibit excellent optical quality at room 

temperature. The first cool-down and 

test of the complete system at cryogenic 

temperatures is expected in January 

007 and, if all goes well in the following 

few months, HAWK-I will be commissioned 

in the period June–September 

007 at one of the Nasmyth foci of Yepun 

(UT4). After around three years use for 

direct imaging it is planned to install four 

wavefront sensors to exploit the possibility 

of ground layer adaptive optics correction 

with the AOF. 

Installation of the radiation shield in the HAWK-I 

vacuum vessel in Garching. 


53

The Adaptive Optics Facility 

The AOF is a project to upgrade one of 

the VLT 8. -m telescopes, Yepun (UT4), 

with an adaptive secondary mirror, multiple 

Laser Guide Stars and two adaptive 

optics modules: GRAAL for HAWK-I and 

GALACSI for MUSE. The aim is to provide 

both instruments with ‘enhanced seeing’ 

performance in a large field of view and 

to achieve diffraction-limited performance 

in a small field of view for MUSE. An optical 

test-bench, ASSIST, built by a Dutch 

partner, will be used to test the complete 

system in Europe before sending it to the 

observatory. 

Substantial progress was achieved in the 

design of the various subsystems during 

the year. The Deformable Secondary 

Mirror (DSM) preliminary design has advanced 

well and major design difficulties 

– such as procedures for safe handling of 

the thin mirror shell, design of a stiff hexapod 

structure with sophisticated flexible 

joints, manufacture of a light-weight 

reference body – have been solved. The 

end of the year has been used to write 

the documentation for the DSM Preliminary 

Design Review (PDR) planned for 

early 007. A complete design for GRAAL 

has been produced, including the large 

bearing which allows rotation of the 

wavefront sensors. Preliminary inquiries 

have taken place for specifications and 

cost-estimate of such a device, opening 

the way for the GRAAL PDR in early 

007. GALACSI and 4LGSF preliminary 

designs are in line for reviews planned 

in autumn 007. The synergy between 

GRAAL and GALACSI (e.g. their similar 

real-time computer and wavefront sensor) 

allows GALACSI to benefit from the 

GRAAL progress. Moreover, the results 

and lessons learned from the LGSF commissioning 

in Paranal are retrofitted to 

the actual 4LGSF design. The ASSIST 

test-bench has undergone Optical PDR in 

October 006 and a reliable optical design 

is on hand for the ‘DSM main tower’. 

The mirror blank for the Thin Shell prototype 

has been prepared by a contractor 

and is ready to undergo aspherical polishing. 

Concerning the Very Large Telescope 

Interferometer (VLTI), several parts of the 

PRIMA (Phase-Referenced Imaging and 

Micro-arcsecond Astrometry facility) 

54 


CRIRES installed at a Nasmyth focus of Antu. The large vacuum vessel houses the cryogenically 

cooled, high-resolution infrared spectrometer, and the enclosure between it and the 

telescope contains adaptive optics and calibration systems. 

hardware have been delivered and are 

undergoing intensive tests in the Garching 

laboratories. The PRIMA facility is a 

sys-tem designed to enable simultaneous 

interferometric observations of two objects 

– each with size of at most arcseconds 

– that are separated by up to 

1 arcminute. PRIMA can be used to increase 

the sensitivity of the VLTI, to image 

faint objects with a high angular resolution 

and to perform high-precision 

astrometry, mainly for planet detection. 

The principal components of PRIMA 

are: a Star Separator per telescope, a 

system of laser metrology, two Fringe- 

Sensor Units, and four Differential Delay 

Lines. 

One Star Separator for the Auxiliary Telescopes 

and one for the Unit Telescopes 

have been delivered within specifications. 

The second of each type will be delivered 

in early 007. Two additional Star Separators 

for the Unit Telescopes are under 

manufacturing and should be delivered in 

008. The Fringe Sensor Units (FSU) are 

under intensive tests at a laboratory in 

the Max-Planck-Institut für Extraterrestrische 

Physik. Some specifications are not 

yet met but several solutions are being 

worked out and implemented in collaboration 

with the contractor. The laser metrology, 

the system measuring the phase 

and delay that is at the basis of the 

PRIMA concept, is regularly used in the 

testing of the FSU. Its interface with 

the Star Separators has also been proven 

adequate. Continuous improvement of 

this essential device is ongoing as the 

lessons learned from the Interferomet- 

ric Task Force in Paranal are taken into 

account and used to improve the PRIMA 

reliability. The Differential Delay Lines are 

under manufacturing and currently no 

problem has been encountered. Finally, 

the PRIMA Astrometric Software, a detailed 

data analysis software and calibration 

package needed to reach the ambitious 

10 micro-arcsecond accuracy, is 

under development. A first version of the 

software will be available for the integration 

and commissioning of PRIMA during 

008. 

Second-generation Instruments 

Design work advanced well on the four 

approved second-generation VLT in- 

struments. X-Shooter, the wideband UV- 

IR spectrograph being developed by a 

Danish/Dutch/French/Italian consortium 

led by ESO, is the most advanced. It 

passed its Final Design Review (FDR) in 

June 006 and its optical CCDs and 

infrared array detector have already been 

successfully tested. KMOS, the multiple, 

deployable integral-field infrared spectrometer 

being developed by a UK/German 

consortium (with ESO providing the 

detector system) passed its PDR in Sep-

Assembling the Hawk-I 4K x 4K detector mosaic. 


55

tember following successful tests of a 

prototype cryogenic pick-off arm – one of 

4 to be installed in the final instrument – 

and of diamond machined optical components 

representative of those needed 

for its image slicer systems. The agreement 

between ESO and the French/ 

Swiss/German MUSE consortium was 

signed and the instrument itself continued 

in its preliminary design phase. 

MUSE is an integral-field optical spectrograph 

– actually 4 spectrographs – 

with ESO again responsible for the design 

and procurement of the detector 

systems. An important milestone in 006 

was the optical PDR, which paved the 

way for the production of a prototype of 

one of the 4 spectrographs. MUSE is 

also designed to be used together with 

the AOF described above in order to 

enhance the delivered image quality and 

hence sensitivity and resolution. 

The aim of SPHERE is to directly detect 

extrasolar planets, possibly down to 

Jupiter masses, achieving a contrast of at 

least 1/100 000 at 0.1 arcsecond from a 

bright central star. This will be made possible 

by an ‘extreme’ adaptive optics system 

to correct atmospheric turbulence 

effects, by suppression of the diffraction 

pattern using state-of-the-art coronagraphs, 

and by advanced differential techniques 

aimed at reducing the speckle 

noise. The corrected beam will feed three 

scientific instruments which will work 

at optical and near-infrared wavelengths. 

The SPHERE consortium comprises partners 

from France, Germany, Switzerland, 

Italy, and the Netherlands. ESO is a full 

partner in the project, which also includes 

significant support by the OPTICON FP6 

network. During 006, the preliminary 

design of systems and subsystems has 

advanced well at the various institutes. 

The PDR of the Optics is planned for 

March 007, with the overall PDR planned 

for July 007. The development of the 

extreme AO deformable mirror, its drive 

electronics and the digital detectors necessary 

to analyse the wavefront is proceeding. 

The delivery of these critical 

components is expected in autumn 007. 

The High Order Test-bench (HOT), supported 

by OPTICON and dedicated to the 

verification of high-contrast imaging concepts, 

has been set up at ESO and first 

closure of the AO loop has been achieved. 

56 


A formal call for second-generation VLT 

interferometric instruments yielded three 

Proposals in January: for GRAVITY, 

MATISSE and VSI (down from nine possible 

concepts at the start of the selection 

process in 005). Following a recommendation 

of the STC committee, Phase A 

study contracts were let for all of them 

with final study reports being due in summer 

007. 

In addition to specific instrumentation 

projects, detector and other development 

work was undertaken to ensure that 

ESO remains at the forefront in this critical 

area. Most visibly, development of 

the Next General detector Controller 

(NGC) continued to advance. The NGC is 

designed to meet the needs of all foreseeable 

visible and infrared detector systems 

for the coming years – both to 

achieve the noise, speed and other performance 

requirements and also to provide 

the maintenance benefits of a single 

type of system at the La Silla Paranal 

Observatory. Furthermore, detector developments 

and characterisation together 

with industry continued in various areas 

aimed at improving the quantum efficiency, 

noise, speed and other properties 

of both visible and infrared detectors. In 

addition to the science detectors themselves, 

new drivers for these improvements 

have come from the requirements 

for adaptive optics wavefront sensors 

and fringe-tracking systems needed for 

interferometric applications. 

MAD, the Multi-Conjugate Adaptive Optics 

Demonstrator, is a bench instrument 

to demonstrate and study, both in the 

Laboratory and on-sky, many of the new 

AO approaches proposed in the last 

years, which are needed for some second-generation 

VLT instruments and 

which are crucial for the future European 

Extremely Large Telescope. The most 

important approaches to be demonstrated 

by MAD are the Multi-Conjugate 

AO and the Ground Layer AO, both aiming 

at enlarging the field of view of the 

correction, which is typically very small in 

traditional AO systems. During the year 

MAD completed its test and characterisation 

phase in the laboratory for both the 

‘classical’ wavefront-sensing mode developed 

at ESO and the layer-oriented mode 

developed by an Italian consortium. 

The laboratory results have shown that 

Multi-Conjugate AO has diffractionlimited 

capabilities and good correction 

uniformity across a field of view up to 

arcminutes, under Paranal median seeing 

conditions. Ground Layer AO has shown 

its great potential in increasing the energy 

concentration on similar fields of view. 

On-sky demonstration will be extremely 

helpful in understanding how the two 

correction approaches will perform under 

real atmospheric conditions. MAD 

achieved Preliminary Acceptance in 

Europe (PAE) in December. The infrared 

camera produced by the Portuguese 

partner also achieved PAE, in September. 

MAD has been sent to Paranal to be 

reintegrated and should perform first onsky 

runs in March/April 007.

Technical Developments 

The Technology Division provided engineering 

support to over 150 different ESO 

projects and workpackages in 006 – 

a 50 % increase over 005. The increase 

has been largely due to the start of the 

production phases of major on-going 

projects like ALMA, second-generation 

VLT instrumentation, and VLTI instruments, 

as well as the demands of new 

workpackages related to the E-ELT and 

FP6. Support for VLT operations at 

Paranal also continues as an important 

background activity for the Division. 

Electronic Engineering 

The introduction of the EU RoHS Directive 

(Restriction on the use of Hazardous 

Substances) has had an impact not only 

on internal electronic developments at 

ESO but also on the availability of many 

commercial electronic units. This relates, 

in particular, to the requirement for leadfree 

soldering. In some cases compatible 

alternative commercial units that conform 

to RoHS are available, but others, like 

the ESO-standard Maccon motor control 

units that are used within all VLT instruments, 

are now no longer available. The 

Electronics Department has therefore ordered 

a sufficient stock of these and 

other operations-critical modules to provide 

for long-term maintenance sup- 

port for the VLT and its instrumentation. 

A new standard motor-control suite for 

instrumentation based on the CAN-bus 

standard has been developed and, in 

006, a pre-production series of the DC 

motor controllers and prototypes of the 

stepper motor controllers were produced 

and tested in Garching. These will complement 

the existing Maccon boards and 

will be particularly suitable for new applications 

where distributed motors are to 

be controlled. 

In order to be able to assure reliable operation 

of electronic systems over the entire 

range of operational temperatures, 

the Electronics Department has acquired 

a new climatically controlled enclosure to 

allow thermal stress-testing all new electronics 

designs as well as commercially 

bought equipment. Although electronic 

reliability has not been a serious problem 

in the past, the new equipment will contribute 

to our goal of improving quality assurance 

procedures throughout the organisation. 

Systems Engineering 

Computer modelling of opto-mechanical 

systems is an important aspect of ESO’s 

systems engineering work. To enable increasingly 

complex systems such as the 

E-ELT to be modelled, the analysis tools 

used at ESO have to be continually extended 

to keep pace with project requirements. 

A particular example in 006 is 

the Structural Modelling Interface (SMI) 

tool developed jointly at ESO and the 

Technical University in Munich. The SMI 

Test chassis with multiple units of the ESO-developed CAN-bus DC motor drive module. 

can reduce the complexity of large FEM 

models produced in ANSYS to levels 

that permit control simulations using Matlab/Simulink 

to be carried out, but without 

significant losses in model fidelity. 

Another analysis tool that has been developed 

over a number of years at ESO, together 

with Astrium, is Beam Warrior. A 

limitation of classical optical design tools 

like Code-V and Zemax is that they produce 

optical models but these are not 

linked to the mechanical and other perturbations 

of the complete system. By combining 

optical design parameters from 

these programs with flexure information 

obtained from a FE Analysis, Beam Warrior 

can calculate parameters like the 

point-spread functions or Zernike coefficients 

for a variety of telescope orientations 

and load conditions. It allows optical 

models to be integrated into control-loop 

simulations and can also handle segmented-mirror 

telescopes. Beam Warrior 

will thus be an important element of the 

E-ELT integrated model. 

Systems Engineering is an important discipline 

for all complex projects, and for 

major projects like ALMA and the E-ELT it 

is indispensable. Keeping track of the 

continually evolving projects requirements 

throughout the development cycle is a 

challenging task and is an area where 

a Requirement Management Tool can be 

very useful. DOORS is such a tool that 

has been successfully used within the 

Software Department for several years for 

the ALMA software documentation and 

requirement management. Requirement 

Management promotes a formal approach 

to the definition of project requirements 

at different levels (stakeholder 

requirements, systems requirements, 

operational requirements, etc.), and links 

these to subsystems requirements, 

design documentation, verification procedures, 

and so on. It allows transparent 

requirement traceability for change control 

and helps with the early identifica- 

tion of errors that can be expensive to 

correct later on in the project. 

In 006, a pilot project has been started 

to apply DOORS to the E-ELT project. 

The Level 1 project requirements have 

been identified and integrated into the 

DOORS requirements management process 

framework, and linking has started. 


57

Opto-Mechanics 

During 006, several background developments 

have been pursued in technologies 

that could be of potential interest 

for future ESO projects. One area of key 

importance for an ELT project is fine mirror-shape 

control and, with this in mind, 

two parallel development projects have 

been undertaken to evaluate piezoelectric 

actuators. The first project used piezo 

fibres attached to a bar. The test results 

obtained showed bending that was in 

good agreement with a FE analysis and, 

in particular, showed no significant hysteresis. 

The second development, which 

is still ongoing, uses piezo stack actuators 

attached to a dummy mirror blank. 

Both these techniques show good potential 

for a precise and economic means of 

mirror deformation control. 

A design challenge for any large exposed 

structure like the ELT is wind buffeting 

control. Although wind tunnel testing and 

CFD (Computational Fluid Dynamics) 

models are both valuable techniques, 

there always remains a problem of validating 

these models, both in terms of scaling 

and understanding the correct disturbance 

spectra to apply. In order to 

obtain realistic test data for an extremely 

large telescope, an experiment has been 

undertaken with the support of the University 

of Manchester to attach some 00 

pressure sensors on the surface of the 

Jodrell Bank 70-m Lovell radio telescope 

in the UK. These allow not only the absolute 

pressure variations to be determined 

over a period of one year, but also enable 

us to gain a good understanding of the 

pressure correlations across the reflector 

surface, that have an important impact 

on the overall telescope design. During 

the course of 006, the sensors and their 

readout electronics were installed on the 

telescope by ESO’s partner firm GBF, and 

analysis of the initial data is already underway. 

58 


Software Engineering 

The 15th release of the VLT Software, i.e. 

the January 006 release, was the last to 

support HP-UX and Sun Solaris operating 

systems. The next planned release, in 

February 007, will support Linux only. 

This change will considerably reduce the 

amount of software testing to be carried 

out and contribute to improved reliability. 

ESO Videoconferences from 000 to 006 

3 000 

500 

000 

1500 

1000 

500 

0 

TBytes 

70 

60 

50 

40 

30 

0 

10 

0 

Software updates are needed primarily to 

meet the specific requirements of new 

VLT instruments as well to cater for various 

hardware configuration changes. 

For real-time control environments, ESO 

has now moved from WindRiver VxWorks 

release 5.5 to release 6.0. This step 

was necessary, not only to be able to use 

the latest real-time processor boards, 

but also because release 6, unlike its predecessors, 

supports Linux as a development 

platform. 

110 141 44 363 496 1 06 568 

000 001 00 003 004 005 006 

003 

004 005 006 

Above: The total number of yearly ESO 

videoconferences since the year 000. 

TBytes transmitted 

TBytes received 

Growth of Garching Internet traffic in 

Terabytes over the last four years. 

The dark blue bars show outgoing 

data and the light blue incoming data.

In December 006, an internal reorganisation 

in Garching led to the transfer 

of staff of the Software Department from 

the Technology Division to the newly 

formed Software Development Division. 

There they join software engineers who 

were previously in the software development 

group of the former Data Management 

Division. This move is intend- 

ed to consolidate software developers 

within the organisation and provide improved 

synergy. 

IT Services 

A major event for IT services was the 

change of outsource service provider in 

April 006. The new contractor has 

taken over responsibility for providing IT 

support not only in Garching but also 

in Santiago, La Silla and Paranal. Previously, 

three separate contractors were 

responsible for providing IT support in 

Garching, Paranal and Santiago respectively, 

with La Silla being supported by 

ESO staff. This change will greatly assist 

inter-site coordination and the rationalisation 

of IT services. 

The use of ESO communications systems 

continues to rise rapidly. Since videoconference 

systems were first introduced at 

ESO in 000, their usage has increased 

dramatically. Today, videoconferencing is 

an indispensable part of ESO’s activities, 

not only for internal ESO meetings between 

Europe and Chile, but also for regular 

contacts with our project partners 

in Europe and beyond. Videoconferences 

not only facilitate closer contact between 

staff in Europe and Chile but also lead to 

reduced travel costs. In 006, an average 

of 10 videoconferences took place each 

working day. 

Similarly, network traffic has also increased 

steadily over the last few years, 

fuelled by higher available bandwidths 

and cheaper access costs. In 006, the 

total incoming and outgoing traffic 

through the Garching Internet portal was 

about 90 Terabyte/year. 

The Spiral Galaxy NGC 3190 (FORS/ESO). 


59

Science Archive Operation 

The Science Archive Operation (SAO) 

group is responsible for receiving, storing 

and redistributing ESO and Hubble 

Space Telescope (HST) data, as well as 

providing front-line archive user sup- 

port. The current total archive holding is 

53. terabytes (TB) of ESO data and 

in excess of TB of HST data. Roughly 

13 TB of new data were archived during 

006, a 10 % increase over 005. While 

the volume of HST data is rather small 

compared to that of ESO data, the number 

of files archived for the two observatories 

is comparable: 6 million ESO files 

and 4 million from HST, for a grand total 

holding in excess of 10 million files hosted 

in the ESO Archive. Users around the 

world can access the ESO archive via a 

web-based data request submission 

system. In addition to the general archive 

web interface, all current VLT instruments, 

the VLTI MIDI instrument, the 

HARPS instrument on La Silla, and APEX 

on Chajnantor have dedicated instrumentspecific 

forms to query the data. More 

than 16 600 unique archive requests were 

served in 006, totalling 4 TB of data 

(a 4 % increase with respect to 005). Of 

those requests, 14 900 were for ESO 

data, while the remaining 1700 were for 

HST data. In addition we have prepared 

1 11 data packages that were delivered 

to Principal Investigators on 733 CDs 

or DVDs. Finally, 140 calibrated pre-imaging 

data sets from the two FORS instruments, 

VIMOS, VISIR and, as of the third 

quarter of 006, ISAAC, NACO and SIN- 

FONI were delivered automatically within 

48 hours of acquisition at the telescope. 

Raw data from the UKIRT Infrared Deep 

Sky Survey (UKIDSS) executed with the 

WFCAM instrument at the UK Infrared 

Telescope (UKIRT) have kept flowing into 

the ESO archive. During 006 we have 

received .5 TB worth of UKIDSS data, 

mostly concentrated in the first part of 

the year. 

The year 006 marked the beginning of 

operations of the APEX submillimetre 

antenna on the Llano de Chajnantor. The 

data belonging to two out of the three 

APEX partners – ESO itself and the 

Onsala Space Observatory in Sweden – 

are stored in the ESO archive. As with 

any other ESO data, APEX files will also 

be made public to the community at 

large, once the usual proprietary period 

has expired. The ESO archive currently 

60 


holds 75 GB of APEX data, as produced 

by the Science Verification runs and 

the first round of ESO and Onsala General 

Observer programmes. 

A major milestone for 007 will be the 

archiving of data from VISTA/VIRCAM, 

the new wide-field infrared imager scheduled 

to start operating in the course 

of the year. With an expected data rate of 

150 TB a year, this instrument alone 

will produce a tenfold increase of data 

volume compared to all other instruments 

combined! 

In order to cope with this massive flow of 

data, the way data themselves are transferred 

from Paranal to Garching was 

overhauled in 006. In fact, the traditional 

way of transferring data on CDs and 

DVDs, which has faithfully served VLT 

operations since the beginning, was discontinued. 

As of December 006, VLT 

data are transferred to Garching in a 

novel and very efficient way, i.e. directly 

on NGAS (Next Generation Archiving 

System) discs, a technology developed 

at ESO and the foundation of the ESO 

archive itself. 

Fundamentally, archive operations rely 

on a large number of hardware servers to 

store science data and their associated 

metadata in a reliable manner. We estimate 

that the archive data volume will exceed 

the petabyte limit by 011. Therefore, 

a petabyte-class archive has been 

designed to deal with the challenge 

of huge astronomical data volumes. This 

petabyte-class archive consists of ESO’s 

Primary and Secondary Archive, the 

Compute Stack and the Fast Cache. 

The Primary Archive is based on hard- 

disc technology, currently distributed on 

5 Linux servers with a storage capac- 

ity of 6.4 TB each, whereas the Secondary 

Archive is based on a petabyte tape 

library, currently equipped with over 300 

tapes, each with a storage capacity of 

0.5 TB. The Secondary Archive will store 

a second copy of the entire ESO archive 

contents at another physical location. 

The Compute Stack consists of blade 

Structure of the ESO archive and its main 

components. Scheme by R. Höllmüller. 

systems with a maximum capacity of 

13 CPUs. The Fast Cache provides 9 

TB of extendable Fibre Channel discbased 

storage. For the safe installation 

of the Primary Archive at different 

physical locations, ESO approved the 

plan to build an ESO Data, Computing 

and Operations Centre, to be completed 

in 007. 

Archive Database Content Management 

The ESO science archive contains two 

kinds of information: the actual science 

data generated by various ESO telescopes 

as well as the HST, and 

metadata which describe these science 

data, e.g. what objects were observed, 

when they were observed, and how they 

were observed. These important descriptions 

are necessary to allow users to find 

and retrieve science data and data 

products from the Archive. The DFO 

Database Content Management (DBCM) 

group has responsibility for maintaining 

these metadata. This is not an easy task, 

with the landmark of two billion database 

entries being reached and surpassed in 

006! 

In particular, DBCM implements metadata 

changes and updates following 

requests from various ESO operations 

groups or upon identification of erroneous 

entries. In addition, the DBCM 

group works closely with the DMO 

Virtual Observatory Systems (VOS) 

department to interface VOS services 

with the operational archive.

SN 006X in the spiral galaxy M 100. 


61

The European Virtual Observatory 

The Virtual Observatory (VO) aims to allow 

users easy and seamless access 

to the huge amount of astronomical data 

currently available, to facilitate its exploitation 

and foster new science. The VO initiative 

is a global collaboration of the 

world’s astronomical communities under 

the auspices of the International Virtual 

Observatory Alliance (IVOA). From the 

start, ESO has been very active in the VO 

arena, creating on 1 November 004 a 

Virtual Observatory Systems (VOS) Department 

in the ESO Data Management 

and Operations Division. VOS’ role is also 

to make the Science Archive Facility 

(SAF) a powerful scientific resource for 

the ESO community, and thereby ensure 

that ESO also plays a major role in the 

VO as a data provider. 

ESO is a founding member of the EURO- 

VO project, whose aim is to deploy an 

operational VO in Europe. Besides ESO, 

initial partners include the European 

Space Agency (ESA), and six national 

funding agencies, with their respective 

VO nodes: Istituto Nazionale di Astrofisica 

(INAF, Italy), Institut National des Sciences 

de l’Univers (INSU, France), 

Instituto Nacional de Técnica Aeroespacial 

(INTA, Spain), Nederlandse Onderzoeksschool 

voor Astronomie (NOVA, 

Netherlands), the Particle Physics and 

Astronomy Research Council (PPARC, 

UK), and Rat Deutscher Sternwarten 

(RDS, Germany). EURO-VO has established 

three interlinked structures: 

– the Data Centre Alliance (DCA), an alliance 

of European data centres which 

will populate the EURO-VO with data, 

provide the physical storage and computational 

fabric and which will publish 

data, metadata and services to the 

EURO-VO using VO technologies; 

– the Facility Centre (VOFC), an organisation 

that provides the EURO-VO with 

a centralised registry for resources, 

standards and certification mechanisms 

as well as community support for 

VO technology take-up and dissemination 

and scientific programme 

support using VO technologies and 

resources; the VOFC is located at ESO 

and is managed by ESO and ESA; 

6 


– the Technology Centre (VOTC), a distributed 

organisation that coordinates a 

set of research and development projects 

on the advancement of VO technology, 

systems, and tools in response 

to scientific and community requirements. 

The EURO-VO Science Advisory Committee 

(SAC) was put together in March 

006 to provide overall scientific input 

to the project. Two SAC meetings were 

held in 006, the first on 7– 8 April 

at ESO, the second on November at 

ESRIN in Frascati, Italy. SAC members 

were introduced to the different aspects 

of the EURO-VO through various presentations 

and were updated on the latest 

EURO-VO developments and on the goals 

of the three EURO-VO substructures. The 

SAC then discussed some EURO-VO 

tools and a call for proposals to carry 

out astronomical research projects using 

VO tools. 

New EURO-VO Web pages (http://www. 

euro-vo.org) were presented to the SAC 

at its first meeting, and opened to the 

public a week or so later. They contain, 

among other things, concrete examples 

for astronomers of what the VO can and 

cannot do for them at present, and links 

to VO software applications. 

VOS was in charge of the organisation of 

the IVOA booth at the XXVIth General 

Assembly of the International Astronomical 

Union in Prague, on 14– 5 August. 

VOS also coordinated the EURO-VO presence 

and demonstration and the work on 

the EURO-VO flier. 

The first meeting of the board of the 

EURO-VO Data Centre Alliance (DCA) 

project, which has received funding of 

1.5 M€ from the Sixth Framework Programme 

(FP6; Coordination Actions) of 

the European Community, took place 

on –3 October in Strasbourg. The DCA, 

which is made up of eight European astronomical 

organisations including ESO, 

is vital for the EURO-VO goal of making 

the VO a reality in Europe. The DCA project 

is currently funded for two years, 

with expected completion by September 

008. ESO’s main role in the DCA is to 

organise, in collaboration with ESA, dedicated 

workshops to ensure the dissemination 

of technical knowledge necessary 

to implement VO-endorsed standards. 

The VOTech project is a design study, 

which aims to complete the technical 

preparation for the construction of the 

EURO-VO. The project is funded at 

the 6.6 M€ level by FP6 and by the part- 

ners, which include ESO, the Universi- 

ties of Edinburgh, Leicester, and Cambridge 

(UK), CNRS and Université Louis 

Pasteur (France), and INAF (Italy). The 

duration of the project is three years, with 

expected completion by the end of 008. 

ESO has a strong role in the VOTech 

project as leader of the Design Study 4 

on New User Tools, which aims to 

provide European astronomers with research 

tools integrated in, and fully 

compliant with, the VO. The project 

works in six-month cycles. Two planning 

meetings were held: on 6–9 March in 

Sorrento, Italy, and on 4–7 September 

in Strasbourg, France. 

VOS maintains the Euro-VO project web 

site, which in 006 served 77 GB of 

content resulting from 10 000 user sessions. 

VOS is also in charge of the IVOA 

project web site, which served 6 GB of 

web content resulting from 330 000 user 

sessions.

ST-ECF 

ESO and the European Space Agency 

continued their successful collaboration 

through the Space Telescope European 

Coordinating Facility (ST-ECF). 

The Hubble Space Telescope (HST) is 

currently in observing cycle 15, routine- 

ly achieving observing efficiencies between 

45 and 50 per cent. It is performing 

nominally in two-gyro mode. As a 

precautionary measure, plans have been 

designed to test the HST in one-gyro 

mode. Science highlights include the 

mapping of dark energy in space and 

time, the observation of the earliest 

galaxies in the Universe, and the discovery 

of many planets around nearby stars. 

European participation continued to be 

well above the nominal 15 %. 

Following directives from the ESA executive 

the ST-ECF reached a stable staffing 

level: seven ESA-funded positions and 

seven ESO-funded positions, corresponding 

exactly to the initial agreements between 

the two organisations, except that 

two of the staff members are now allocated 

to public outreach. The primary 

consequence of this staff rampdown was 

the discontinuation of the Advanced Calibration 

Project. It was possible to salvage 

some of the products of the group 

through an early partial delivery to the 

STScI. Moreover, two staff members of 

the former ST-ECF Advanced Calibration 

Group are now working for ESO, continuing 

this very successful effort, which, 

while initially developed for the HST spectrographs, 

works exceedingly well for 

the ESO ground-based instruments. In 

October, ESO and ESA decided to terminate 

the ST-ECF when the current Hubble 

ESA/NASA MoU expires at the end of 

010. The tasks of the group remain 

those agreed at the 006 Annual Review. 

The focus of the ST-ECF efforts was on 

Advanced Science Data Products: both 

the ACS and the NICMOS instruments on 

HST have integral-field spectroscopic 

capabilities. The data produced in these 

modes are complex to analyse and require 

techniques unfamiliar to most astronomers. 

ST-ECF has therefore begun 

to extract the spectra from the data 

frames and to calibrate them, with the 

aim of making them available to the community. 

This capability is also applica- 

ble to Wide Field Camera 3, one of the 

two new scientific instruments that will 

be installed on the HST during Servicing 

Mission 4. 

The proposed mode of operation for the 

other instrument to be installed, the Cosmic 

Origins Spectrograph, will put a 

higher demand on the usage of the wavelength 

calibration lamps. The ST-ECF 

coordinated a NASA/ESA funded project 

that involved ESO, NIST, STScI and the 

COS team to evaluate the spectral characteristics 

and the life expectancy under 

these operating conditions. 

The European HST Archive was migrated 

to the new ESO Archive infrastructure. 

The total holdings are now 547000 data 

sets. During 006, 414 6 data sets 

( .9 TB) were distributed to 40 users. 

ST-ECF staff also assisted the STScI 

in the final reprocessing of the FOC and 

GHRS archives. In collaboration with 

the STScI and the CADC the Hubble Legacy 

Archive was initiated. The goal is to 

collect and generate selected High Level 

Science Data Products and make them 

available to the community. 

User support continued through the 

Newsletter, the HST email hotline, and 

the production of technical documents. 

ST-ECF staff also monitored the TAC 

process and continued to support the 

ESO SAMPO Project. More recently, 

the editorship of the ESO Messenger was 

taken over by ST-ECF staff. 

For the ST-ECF’s task to disseminate the 

discoveries from Hubble to the public, 

006 has been the most successful year 

so far. Nineteen news and photo releases 

were produced (up 0 % from 005). The 

European Hubble website had .8 million 

visitors (up 90 %) and distributed 36 TB of 

multimedia materials (up 65 %). 

The ESA/ESO/NASA Photoshop FITS 

Liberator .1 was released. Several exhibitions 

were produced together with 

external organisations – perhaps most 

noteworthy was a part of the perma- 

nent exhibition in Armagh Planetarium. 

The Astronomy Visualisation Metadata 

standard (co-authored with Robert Hurt) 

was endorsed by the International Vir- 

tual Observatory Alliance. 

The third ESA-ESO Bilateral meeting took 

place in Garching at the end of Octo ber. 

The third working group report – on 

Fundamental Cosmology by Peacock, 

Schneider et al. – was finished and distributed. 

The meeting addressed the recommendations 

of all three working groups 

and decided to continue both the bilateral 

meetings, which are essential for the 

coordination of science planning, and the 

series of topical working groups. 

The former Instrument Advanced Calibration 

Group was selected by NASA to 

receive the “Group Achievement Award” 

for its work on high-fidelity calibration. 

The award, given at a ceremony at NASA 

Headquarters on 1 July to Paul Bristow, 

Florian Kerber and Michel Rosa, is 

shared with a three-member team from 

the US National Institute of Standards. 

Artist’s view of Servicing Mission 4 to 

Hubble. This Servicing Mission will 

not only ensure that Hubble can function 

for perhaps as much as another 

ten years, it will also increase its capabilities 

significantly in key areas. As 

part of the upgrade, two new scientific 

instruments will be installed: the 

Cosmic Origins Spectrograph and the 

Wide Field Camera 3. 

ESA/Hubble 


63

64 


Open House at the ESO Headquarters on 15 October 006.

Public Outreach 

On all accounts, the year 006 marked 

a record year in terms of Public Outreach 

activities by ESO. This growth is motivated 

by several factors, including 

– the increase in the number of mem- 

ber states of ESO; 

– the current and planned project port- 

folio, which foresees investments in 

the range of several hundreds of millions 

of Euros; 

– the increased focus on the need to 

secure an adequate recruitment base, 

not just in the time to come, but also 

in today’s labour market, which is characterised 

by stiff competition for the 

best people. 

Furthermore the increased competition 

for public visibility and communication 

in general in today’s society places strong 

demands on the quality of the communication 

efforts, not just in terms of contents 

but also with respect to delivery mechanisms. 

Other aspects such as timing and 

timeliness are of course of crucial importance 

in today’s fast moving media world. 

This has led us to pursue a particular 

strategy, which builds on technical autonomy, 

short communication lines within 

the organisation and an elaborate system 

of partnerships. For example, ESO has 

established a Science Outreach Network 

with representatives in all ESO member 

states. These ‘ambassadors’ perform an 

important interface function between the 

national media and ESO. 

Of course, as in the previous years, many 

press releases are done in collaboration 

with national organisations (e.g. PPARC, 

MPE, CNRS, INAF), universities, the leading 

research journal Astronomy & Astrophysics, 

and other partners. 

Obviously, the Public Affairs Department 

(PAD) works in close consultation and 

coordination with ESO’s Santiago Representation, 

which conducts targeted outreach 

activities for Chile and provides 

logistical support to European media and 

high-level visitors. 

PAD also works with ESO’s sister organisation 

ESA, including the Hubble Europe 

Information Centre, sited in adjacent 

rooms to PAD. The cooperation involves 

sharing of information and technical facilities, 

wherever possible. 

In the field of education, the European 

Association for Astronomy Education 

(EAAE) is a long-standing partner of ESO. 

The EAAE members help by spreading 

information about ESO in the schools, 

while at the same time they often provide 

didactic advice to PAD as it formulates 

and prepares its education activities. 

The European Commission has become 

a major partner as well, not least in 

funding educational activities, which have 

come to be seen as representing substantial 

added value for Europe’s societies 

and therefore enjoy significant political 

attention and goodwill. 

Finally, the major education activities, 

such as Science on Stage and Science in 

School, are carried out within the framework 

of the EIROforum, the partnership 

of Europe’s seven intergovernmental research 

organisations. The partnership 

enables a very successful pooling of resources 

and expertise and allows undertaking 

activities on a scale that would 

have been impossible for the individual 

organisations alone. 

Media 

In 006, ESO issued a total number of 

51 releases to the media, or roughly one 

release per week. 

Press conference on exoplanets at ESOF, Munich. 

This number can be broken down into 

39 ‘standard’ press releases, including 

6 about scientific results from observations 

with ESO telescopes, and 13 press 

photos. The press photos enjoy great 

popularity among the media and ensure a 

much increased visibility of ESO. Seven 

ESO images were selected as the Astronomy 

Picture of the Day in 006 by the 

NASA website. This number is indicative 

of our potential for creating world-class 

astronomical images – a potential that 

with increased resources could be expanded 

significantly. The most appreciated 

image was certainly the new, stunning 

mosaic of the Tarantula Nebula (ESO 

Press Photo 50a/06), a 56 million pixel 

image obtained with the Wide-Field Imager 

on the . -m telescope at La Silla. 

The image was voted amongst the ten 

best of 006 by a very popular web site. 

Other successes were encountered particularly 

with images of galaxies, such as 

the topsy-turvy one (ESO Press Photo 

43a/06) or the gigantic dusty potato crisp 

(ESO Press Photo 17/06), as well as those 

of the broken comet (ESO Press Photo 

15a/06). 

Among the most successful press releases, 

the prize goes without any doubt 

to the discovery through microlensing 

of a five-Earth-mass planet, a press release 

(ESO Science Release 03/06) that 


65

generated huge media attention worldwide. 

Other excellent results were obtained 

with the press releases on the VLT 

being equipped with a laser guide star 

(ESO Instrument Release 07/06), the discovery 

of a trio of Neptune-mass planets 

(ESO Science Release 18/06), the SIN- 

FONI observations of a very remote galaxy 

(ESO Science Release 31/06) and 

ESO’s Council decision to go ahead with 

a design study for the European Extremely 

Large Telescope (ESO Organisation 

Release 46/06). 

Other features which have been very 

much welcomed by the media are the 

increased use of captivating artistic 

imagery as an alternative way of explaining 

physical phenomena, and the provision 

of video footage that is directly 

linked to ESO press releases. 

With respect to broadcast support and 

video production, in 006 we delivered 

an average of 11 minutes/day of footage 

to TV Channels worldwide, produced 

1.5 seconds/day of high-end 3D animations 

on technical and scientific topics 

and 90 minutes of videos, including six 

video newsreels – the equivalent of a 

15-minute full film production every two 

months. This resulted in some 75 registered 

broadcasts about ESO. The real 

number is likely to be significantly higher, 

since the use of ESO footage is often not 

reported to us. 

Provision of high-quality material is clearly 

a prerequisite for winning the daily battle 

for visibility in the public sphere, but 

it is not enough. Exploiting a variety of 

diffusion channels and new communication 

tools are crucially important. Not 

surprisingly, much of this is linked to the 

world-wide web. For example, we now 

make broadcast material electronically 

available for download by TV channels, 

giving them the option of almost instant 

access to ESO news reels. Another aspect 

is the web-based public sphere. 

This has arguably emerged as one of the 

most important ways to reach young 

people in particular – beyond the classic 

media such as broadsheet newspapers 

and conventional TV. These new media 

include traditional web pages, blogs, 

pod-casts, vodcasts, and other emerging 

technologies sometimes described as 

‘Web .0’. PAD is taking steps to gain a 

66 


ESO stand in Paris, France. 

foothold in this virtual world. A first experiment 

was done for the press release 

about the discovery of a five-Earth-mass 

exoplanet, when a podcast and a vodcast 

was provided. Vodcasts are also 

done in connection with Video newsreels, 

whenever possible. 

The growing importance of the web and 

the speed with which it evolves, both 

technically and conceptually, creates new 

demands on web sites to remain up to 

date. Of course, ESO cannot turn its back 

on this development. Hence, a major effort 

has been undertaken during the year 

by PAD, in collaboration with other departments, 

to develop a new website for 

our organisation. This web site, which will 

serve as the point of entry into ESO for 

thousands of users every day will feature 

a much more attractive appearance, easier 

navigation and a major overhaul of 

the content. It is the intention to launch 

the new web site in the course of 007. 

The web is, of course, not just a diffusion 

channel, but also provides an important 

source of information regarding the public 

awareness of and interest in ESO’s activities. 

Hence, the increased visibility of 

ESO in media is mirrored by the growth in 

traffic on the ESO Outreach site, which 

in 006 has reached a mean number of 

almost 10 000 visitors/day, a factor of .3 

increase from three years ago. 

Exhibitions and Events 

In spite of the undisputed importance of 

new distribution methods and tools, faceto-face 

communication of course remains 

of crucial value, particularly from the perspective 

of a coordinated communication 

effort. Exhibitions and events clearly provide 

excellent forums for exchange and 

communication with key target groups, 

such as scientists, media, industry and 

policymakers. In 006, PAD organised or 

participated in more than 0 events, 

involving exhibitions, briefings and VIP 

visits – in other words roughly an event 

every ½ weeks. This constitutes a 

significant increase over the previous 

years, both illustrating the growing 

importance and visibility of ESO, but also 

the necessity to enlist wide support for 

ESO’s ambitious future projects. For 

example, on February, PAD in collaboration 

with PPARC organised a very 

successful press event in London in 

connection with this year’s AstroFest at 

Kensington Town Hall. The event was a 

briefing about ESO in general and also 

served as a ‘primer’ to a subsequent visit 

to ESO’s sites in Chile by a group of UK 

journalists. About 15 journalists attended 

this meeting. Just 11 days hence, a major 

press event took place in Madrid on the 

occasion of the signing of the agreement 

aimed at bringing Spain into ESO. Only 

10 days later, we took part at the AAAS 

meeting in Saint Louis, Missouri. The 

AAAS is the world’s largest forum for

science and media contacts, and our 

presence at such an event not only 

supports ESO’s visibility in the USA but 

also in Europe, since the meetings attract 

large numbers of European journalists. 

The AAAS exhibition stand was subsequently 

transferred to and assembled at 

the SPIE conference in Orlando, Florida, 

in May. ESO was very strongly represented 

at this meeting, illustrating that our 

organisation has become a global actor 

in the field of astronomy. 

Back in Europe, we had a major information 

stand at the year’s Salon de la Recherche 

et de l’Innovation in Paris in June 

and, in the context of the EIROforum 

partnership, at the ESOF 006 Conference 

in Munich. At ESOF we also held a 

press event about exoplanet research. 

In August, at the XXVIth General Assembly 

of the International Astronomical Union 

in Prague, PAD set up a 60 square 

metre exhibition for ESO and a somewhat 

smaller one, on behalf of ALMA. 

The last press event of the year took 

place in connection with the ELT conference 

in Marseille in late November. 

The event was co-organised by PAD and 

INSU, and resulted in many media reports, 

including ones in all major French 

newspapers – Libération devoting three 

full pages to the story – and also, for example, 

on German radio. 

The last exhibition took place in Dublin at 

the beginning of December. ESO participated 

as the ‘guest of honour’ at the 

Astro-Expo 006 event, organised at the 

Dublin City University (DCU) by the Irish 

Astronomy and Space magazine. 

Education 

One of ESO’s major education activities 

for pupils is the popular Catch a Star! 

contest, carried out in close collaboration 

with the EAAE. Students work in teams 

or individually, learning about an astronomical 

topic and writing a report. During 

006 we saw the conclusion of the fourth 

iteration of the competition. The contest 

is evolving, with its division into three categories. 

As an important aim is simply 

to encourage an interest in astronomy, 

and because we wish to avoid a sense of 

elitism, some of the winning projects 

were decided by lottery. Nevertheless, to 

cater for particularly talented students 

who may be budding astronomers, there 

were also major prizes to be won. These 

prizes, including a trip to the VLT on 

Paranal, were awarded by an international 

jury. Furthermore, a drawing competition 

category was introduced, following 

the success of a similar competition as 

part of the Venus Transit 004 activities. 

For the first time, the contest was also 

opened to countries beyond Europe and 

Chile. We received a total of 134 written 

projects and 60 pieces of artwork from 

4 countries across Europe and beyond, 

with about 400 students and teachers 

taking part. 

In November 006 Catch a Star! 2007, 

was launched (so named because this 

competition will conclude in 007). Building 

on lessons learned in the previous 

competition, its structure was streamlined 

to make it easier to enter, and the webbased 

infrastructure for administering it at 

ESO was greatly improved. The differentiation 

in categories has been retained 

with Catch a Star! Artists, Catch a Star! 

Adventurers and Catch a Star! Researchers. 

Over the years, ESO has supported 

the EAAE summer schools for astronomy 

teachers in a number of ways, e.g. by 

providing speakers and taking care of 

proceedings. This was also the case 

in 006, where the summer school took 

place on the island of La Palma. Next 

year, however, the summer school will 

change format and scope, and will be 

hosted by ESO. The intention is to foster 

a stronger interaction between teachers 

and active scientists and to bring real 

science into the classrooms. Towards the 

end of the year, preparations for this 

event were underway. 

Similar thoughts underpin the wider, targeted 

effort to stimulate original, attractive 

high-quality science teaching in Europe’s 

secondary schools, known as the 

EIROforum European Science Teachers’ 

Initiative (ESTI), in which ESO is an active 

partner. With its twin pillars, Science on 

Stage and Science in School, ESTI is a 

unique activity in the world. In the teaching 

world it constitutes a completely 

innovative approach with a focus on excellence, 

market mechanisms, interdisciplinarity 

combined with direct links between 

teachers and active scientists and, 

finally, cross-border collaboration on a 

big scale. The most recent Science on 

Stage Festival, with about 500 participants 

from more than 5 countries, took 

place at CERN in November 005; the 

next one is scheduled for Easter 007. 

Throughout 006, staff members of the 

EIROforum organisations, including those 

at ESO, supported and participated in the 

many national events that took place in 9 

countries to select the participants to the 

European festival. In March 006 the first 

issue of Science in School was launched. 

Science in School is a new European 

science education journal for teachers, 

scientists, and others. Issues include 

teaching material, articles about cuttingedge 

science, interviews, and reviews. 

ESO is strongly involved with the journal, 

contributing astronomy-related articles 

and participating in the editorial board. 

Videoconference with Paranal on the main square of Munich, Marienplatz, Germany, during the 

annual German Wissenschaftssommer. 


67

ESO Press Releases 

ESO Press Photo 01/06 (3 January): ESO PR High- 

lights in 005 

ESO 0 /06 Science Release (4 January): Measuring 

the Size of a Small, Frost World 

ESO Science Release 03/06 ( 5 January): It’s Far, 

It’s Small, It’s Cool: It’s an Icy Exoplanet! 

ESO Press Photo 04/06 (7 February): How to Steal a 

Million Stars? 

ESO Organisation News 05/06 (13 February): Spain 

to Join ESO 

ESO Science Release 06/06 (15 February): The Invis- 

ible Galaxies That Could Not Hide 

ESO Instrument Release 07/06 ( 3 February): Man- 

made Star Shines in the Southern Sky 

ESO Press Photo 08/06 ( 3 February): A Blast To 

Chase 

ESO Science release 09/06 ( 8 February): Cepheids 

and their ‘Cocoons’ 

ESO Science release 10/06 (15 March): The Cosmic 

Dance of Distant Galaxies 

ESO Science release 11/06 ( March): The Sun’s 

New Exotic Neighbour 

ESO EIROforum release 1 /06 ( 8 March): Bringing 

Science out of the Lab into the Classroom 

ESO Press Photo 13/06 (7 April): Cosmic Spider is 

Good Mother 

ESO Press Photo 14/06 (14 April): The Great Easter 

Egg Hunt: The Void’s Incredible Richness 

ESO Press Photo 15/06 ( 5 April): The Comet With a 

Broken Heart 

ESO Science Release 16/06 (8 May): Physics in Uni- 

verse’s Youth 

ESO Press Photo 17/06 (11 May): Twin Explosions In 

Gigantic Dusty Potato Crisp 

ESO Science Release 18/06 (18 May): Trio of Nep- 

tunes and their Belt 

68 


ESO Science Release 19/06 (6 June): Do ‘Planemos’ 

Have Progeny? 

ESO Press Photo 0/06 (8 June): The Toucan’s 

Diamond 

ESO Organisation News 1/06 (19 June): ESO and 

Chile: 10 Years of Productive Scientific 

Collaboration 

ESO Press Photo /06 ( 8 June): The Hooked 

Galaxy 

ESO Science Release 3/06 (3 July): Falling Onto the 

Dark 

ESO Instrument Release 4/06 (13 July): Sub- 

millimetre Astronomy in Full Swing on Southern 

Skies 

ESO Organisation Release 5/06 (18 July): Towards 

a European Extremely Large Telescope 

ESO Science Release 6/06 ( 1 July): Looking Deep 

with Infrared Eyes 

ESO Press Photo 7/06 ( 6 July): Island Universes 

with a Twist 

ESO Science Release 8/06 (3 August): A Sub-Stellar 

Jonah 

ESO Science Release 9/06 (4 August): The 

‘Planemo’ Twins 

ESO Science Release 30/06 (10 August): Stars Too 

Old to be Trusted? 

ESO Science Release 31/06 (17 August): Far Away 

Galaxy Under The Microscope 

ESO Organisation Release 3 /06 ( 4 August): 

Catherine Cesarsky elected President of the 

International Astronomical Union and Ian Corbett 

elected Assistant General Secretary 

ESO Science Release 33/06 (31 August): Long- 

lasting but Dim Brethren of Cosmic Flashes 

ESO Science Release 34/06 (1 September): A 

“Genetic Study” of the Galaxy 

ESO Science Release 35/06 ( 0 September): To Be 

or Not to Be: Is It All About Spinning? 

ESO Science Release 36/06 ( 8 September): Watch- 

ing How Planets Form 

ESO Science Release 37/06 ( October): Stellar 

Vampires Unmasked 

ESO Science Release 38/06 (4 October): Increasing 

the Odds of the Sweep 

ESO Science Release 39/06 (19 October): The Star, 

the Dwarf and the Planet 

ESO 40/06 ( October) - Organisation News: Ex- 

tremely Large Telescope Project Selected in 

ESFRI Roadmap 

ESO Science Release 41/06 (7 November): Cut from 

Different Cloth 

ESO Organisation News 4 /06 (1 November): Catch 

a Star! 

ESO Press Photo 43/06 (11 November): The Topsy- 

Turvy Galaxy 

ESO Science Release 44/06 (30 November): Asym- 

metric Ashes 

ESO Science Release 45/06 (6 December): Do 

Galaxies Follow Darwinian Evolution? 

ESO Organisation Release 46/06 (11 December): 

The Rise of a Giant 

ESO EIROforum Release 47/06 (14 December): 

Magna Carta for Researchers 

ESO Press Photo 48/06 ( 0 December): It Is Too 

Early To Be Santa’s Sleigh, Isn’t It? 

ESO Science Release 49/06 ( 0 December): The 

Dark Side of Nature: the Crime was Almost 

Perfect 

ESO Press Photo 50/06 ( 1 December): Portrait of a 

Dramatic Stellar Crib 

ESO Press Photo 51/06 ( December): Little 

Brother Joins the Large Family 

ESO Organisation Release 5 /06 ( December): 

Czech Republic to Become Member of ESO 

ESO Press Photo 53/06 ( 4 December): Season’s 

Greetings!

The starburst galaxy NGC 908 (FORS/VLT). 


69

Relations with Chile 

The year 006 marked an important anniversary: 

a decade of the Supplementary 

Agreement between the Republic of Chile 

and ESO, which has allowed the successful 

installation of the VLT at Paranal 

and strengthened the cooperative 

relations between ESO and the Chilean 

scientific and local communities. To 

celebrate this, rectors of Chilean universities 

and representatives of the Chilean 

Ministry of Foreign Affairs gathered at the 

ESO offices in Santiago to launch a 

commemorative book, “10 Years Exploring 

the Universe”. This publication 

presented an external, independent overview 

of the broad impact of the ESO– 

Government of Chile Joint Committee, 

an annual fund for the development of 

astrophysics and scientific culture in the 

country, which was established by the 

Supplementary Agreement. 

In January 006, Dr. Michelle Bachelet 

became the first woman in the history of 

Chile to be elected President of the 

Republic. One of the first international 

events in which the new government 

participated was the opening of the 006 

International Air and Space Fair, held 

in Santiago in March. There, more than 

150 000 people visited the Space & 

Astronomy Pavilion, which presented realistic 

scale models of the VLT, ALMA 

and the E-ELT as well as a collection of 

most impressive astronomical pictures. 

The exhibition in the Pavilion was 

organised by ESO Santiago and the 

Planetario USACH. 

As a step forward in the well-established 

ESO astronomical outreach program- 

mes in Chile, a new strategic partnership 

was launched with the Chilean Ministry of 

Education to improve the teaching of 

astronomy in primary schools, within the 

framework of a national programme 

called “Science Education Based on Research”. 

ESO staff astronomers worked in 

collaboration with education specialists 

to design a learning module on basic 

astronomy, which is currently being 

tested by the Ministry of Education in pilot 

schools in Santiago and cities close 

to the observatory sites. 

70 


Another new initiative promoted by ESO, 

in a joint effort with the French Embassy 

in Chile, was the organisation of the first 

Cafés Scientifiques, in which adults and 

youngsters could freely ask questions of 

specialists while enjoying an informal café 

atmosphere. Inspirational issues like 

exoplanets and the possibility of life in the 

Universe attracted the interest of many in 

Santiago and Antofagasta. 

The Universidad Católica del Norte Astronomy 

Institute, in partnership with ESO 

Vitacura, continued an extensive programme 

of public lectures and star parties 

in Antofagasta, Taltal and San Pedro 

de Atacama, the closest neighbours to 

Paranal and the ALMA site. Also in Chile’s 

Region II, ESO supported partial scholarships 

of 170 undergraduates studying 

at regional universities, in a joint programme 

with the Municipality of Taltal. 

Near La Silla, the educational agreement 

with the Municipality of La Higuera 

entered its second year of cooperative 

work to support local schools. 

ESO also played an active role in the 

Chilean National Science and Technology 

week, in partnership with the “Explora” 

Programme of CONICYT. Enthusiastic 

young students and teachers visited the 

ESO stand at the recently opened 

Biblioteca de Santiago, and more than 

300 schools received copies of a new 

documentary produced in-house about 

recent science highlights obtained at La 

Silla and Paranal. 

In the framework of ALMA, the regional 

fund financed by ESO, AUI and NAOJ 

supported several social and educational 

projects in San Pedro de Atacama and 

Toconao in 006. The only primary school 

in the village of San Pedro de Atacama 

has, in particular, increased its regular 

staff of teachers thanks to this fund. 

Besides this, ALMA is contributing to other 

areas of education and culture. A site 

museum located near the ALMA road was 

inaugurated in 006, in the presence 

of the Intendenta of Region II, the Mayor 

of San Pedro de Atacama, and members 

of the local communities. The site 

museum – in the form of a reconstruction 

of an abandoned estancia – provides 

physical evidence of the way of life of 

shepherds from the ancient Likan Antai 

culture. In order to support the understanding 

and protection of the archaeological 

heritage in the area, a book edited 

by ESO, “Footprints in the Desert”, was 

published and distributed among all 

schools of Region II, teachers, and regional 

authorities. 

In partnership with ESO and ALMA, the 

University of Antofagasta and University 

of Chile, in collaboration with the University 

of Copenhagen, launched a joint 

research programme on high-altitude 

medicine, taking advantage of the operations 

on the Chajnantor plateau at 5 050 

metres above sea level. For the very 

first time, scientists will have systematic, 

detailed statistics on the long-term 

reaction of the human body to regular 

commuting between sea level and 

high sites. This information will help to 

solve some intriguing, open questions of 

human physiology and high-altitude 

illness. 

Continuing our promotion of scientific 

interaction with the Chilean community, 

ESO held joint open houses with the 

Astronomy Department at the Pontificia 

Universidad Católica and Universidad de 

Chile with the participation of about 60 

young researchers in each of the events. 

ESO Santiago also sponsored the 

international conference on Globular 

Clusters organised by Universidad de 

Concepción in March, and the Fourth 

Advanced Chilean School of Astrophysics 

organised by the Pontificia Universidad 

Católica de Chile in December. 

Several delegations from Europe and all 

over the world were hosted in Santiago 

and the observatories, in particular three 

delegations from China, including that 

of the Vice-President of the Academy of 

Sciences. All scientific delegations gave 

informative seminars on science and 

technology in their countries.

Inaugurating the ALMA site museum. 

Launch of the “10 Years Exploring the Universe” book. 

ESO at the 006 International Air and Space Fair. 


71

European Affairs 

European Affairs at ESO is coordinated 

by the Public Affairs Department, but 

frequently involves several other departments 

within the organisation as well 

as external partners, notably the EIROforum. 

European Affairs focuses on EUrelated 

policy aspects of relevance to 

ESO. These can manifest themselves in 

many ways, which has increased the 

scope of ESO’s EU-related activities in recent 

years. This development is in line 

with the overall changes in Europe as 

European integration progresses. Hence, 

our activities are not necessarily limited 

to direct interaction with the primary institutions 

of the European Union, such as 

the European Commission and the European 

Parliament. The main conceptual 

frame within which this development 

follows is the European Research Area. 

The end of 006 marked the termina- 

tion of the EU Sixth R&D Framework 

Programme (FP6) and the new Seventh 

Framework Programme (FP7) was 

launched at the beginning of 007. 

ESO’s FP6 participation can be judged as 

very positive and successful, both because 

it has allowed us to carry out projects 

that could not have been funded 

otherwise, and as a vehicle for a more 

general interaction with the EU at a time 

when the Union is emerging as a new, 

but potentially important actor in the field 

of setting European science policy. In 

this sense, the activities deserve continuation 

in the context of FP7. Currently 

ESO still has 11 running FP6 projects, 

most of which will terminate in 008. 

From the running FP6 projects the E-ELT 

preparatory-phase, the ESTI project 

and the VO project are already aiming for 

continuation in FP7. 

Obviously, the preparation of the Seventh 

Framework Programme played an important 

role in 006. From ESO’s perspective, 

the challenge has been to be able to 

deal with the first FP7 calls, which were 

launched by the Commission in December 

006. The complications of this were 

linked to the preceding legislative process, 

which meant that many important 

details still remained unclear by the end 

of the year. Other issues were not subject 

to the direct political process, but nonetheless 

remained important. This was the 

case for the E-ELT project, which became 

7 


included in the so-called ESFRI-list that 

was published by the European Strate- 

gy Forum for Research Infrastructures 

(ESFRI) in October 006. The ESFRI-list 

is a ‘road-map’ describing 35 major research 

infrastructure projects that are 

deemed to be “Research Infrastructures 

of European interest” (from the Competitiveness 

Council Conclusions, 5– 6 

November 004), and thus pre-qualify for 

potential co-funding, however limited, 

from the Seventh Framework Programme. 

Furthermore, EU member states were 

encouraged to develop national roadmaps 

that are aligned with the ESFRI-list, 

in order to determine funding priorities. 

ESFRI was tasked with developing a longterm 

European view of the development 

of Research Infrastructures of pan-European 

interest, covering a wide range of 

sciences. In the meantime, another activity 

took place, focusing on Astronomy and 

Space Sciences. This occurred under 

the auspices of ASTRONET (http://www. 

astronet-eu.org/), a network comprising 

ESO Council member Jean-Pierre Swings at the Walloon Space Days. 

national funding agencies and ESO (with 

ESA as an observer), which was set up 

under the FP6 ERA-net scheme. ESO’s 

main responsibility in the ASTRO-NET 

programme is to coordinate the development 

of a common Science Vision for 

European Astronomy in the next 0 

years, with NWO in charge of collating 

the scientific content from the community. 

To prepare for this development and 

the follow-up construction in 007– 008 

of a prioritised Infrastructure Roadmap 

under the responsibility of PPARC, a 

web-based census tool has been 

developed by ESO. It currently contains 

all available European national prospectives 

and a comprehensive list of existing 

and planned medium- to large-scale 

infrastructures. The activity picked up 

much momentum in the autumn of 006 

with the preparation for a dedicated 

symposium scheduled to take place 

towards the end of January 007 in 

Poitiers to discuss and refine the draft 

Science Vision released by NWO by 

mid-December 006.

As mentioned, ESO’s European Affairs activities 

are linked to basic policy changes 

in Europe that have a bearing on many 

parts of society. Since these changes are 

a result of constant negotiation between 

stakeholders at the European and national 

levels, our activities must also be of 

a broad nature and involve contacts with 

decision-takers beyond the EU system. 

Thus, on 15 March, ESO was pleased to 

host the Education Committee of the 

Finnish Parliament, an event which created 

a fine opportunity for dialogue 

between ESO and national policy-makers 

as well as a chance to present ESO’s future 

plans. Further visits by diplomatic 

representatives of the UK and Switzerland 

occurred in the spring. On 8– 9 March, 

ESO played a major role in the First 

Walloon Space Days, organised by the 

Walloon Space Cluster and intended 

to become a recurring event focusing on 

technologies for astronomy and space sciences, 

including R&D policy issues. The 

event coincided with the delivery of the 

fourth Auxiliary Telescope for the VLTI 

and provided a forum for European 

companies to meet with ESO experts. 

Visit by the Education Committee of the Finnish 

Parliament. 

In November, we welcomed to Paranal 

a high-ranking delegation from the Academy 

of Sciences of the Czech Republic 

(CAS), led by its President, Václav Pačes, 

and Jan Palouš, responsible for international 

relations of the CAS. The visit was 

related to the negotiations regarding the 

Czech Republic’s membership of ESO. 

In December these negotiations were 

successfully concluded with the approval 

both of the ESO Council and the Czech 

government, paving the way for the signing 

of the agreement on December 

and enabling the parliamentary ratification 

procedure to be initiated. Whilst a 

Czech accession to the ESO Convention 

is not in itself of formal institutional EU 

relevance, it may open possibilities with 

respect to EU funding for national Czech 

activities that follow in the wake of the 

membership – illustrating the complexities, 

but also the importance, of ESO’s 

European Affairs activities. 

Finally, within the EIROforum partnership, 

three events deserve particular men- 

tion. On 15 November, a brainstorming 

session was organised between the 

EIROforum Directors General and key 

Commission officials to discuss long- 

term perspectives for the European Research 

Area. 

On November, EIROforum organised a 

‘Breakfast Event’ at the European Parliament 

on the topic “Fostering Scientific 

Understanding Among Young People – 

Reinforcing scientific education initiatives 

in Europe”. The event was hosted by 

Prof. Jerzy Buzek MEP, and attended by 

more than 10 MEPs and a further 0 people 

from the European Parliament. 

On 13 December, a get-together was organised 

between senior staff from the 

EIROforum partner organisations and research 

attachés of the permanent representations 

of the EU member states. 

The topic for discussion was how to 

achieve synergies between the activities 

of the intergovernmental research organisations 

and the EU-based actions as 

conducted through the Framework Programme. 

In 006, the Research Directorate General 

of the Commission established a 

dedicated unit to facilitate contacts with 

the European Intergovernmental Research 

Organisations. This is clearly an 

expression of the intensification of 

the interactions between the EC and the 

EIROforum in relation to both project 

funding and policy-related interactions. 

Delegation from the Czech Academy of Science visits Paranal. 


73

The ESO Council in session on 6 December 006.

Council 

The Council is ESO’s ruling body, which 

delegates day-to-day responsibility to 

the Executive under ESO’s Director General. 

In 006, Council held two ordinary 

meetings, both in Garching. Committee 

of Council met three times, in February in 

Berne, Switzerland, in September in Santiago, 

Chile, and in October in Munich. 

The President of Council, Prof. Richard 

Wade, chaired all the meetings. 

In 006, Council approved the extension 

of the agreement for APEX until 01 , the 

agreements for the instrument SPHERE, 

and the agreement for a fourth star-separator 

for the VLT, including the proposed 

guaranteed observing time, in accordance 

with the standing rules. 

Council received the usual VLT/VLTI, Instrumentation 

and ALMA biannual reports, 

and the reports from the Chairs of 

the Finance Committee, the Scientific 

Technical Committee, and Observing Programmes 

Committee. Council also endorsed 

the document “ESO Medium 

Range Implementation Plan, 006– 010” 

and examined the document “ESO Future 

Perspectives, 006– 03 ”. 

In December, Council adopted a resolution 

authorising the move of the E-ELT 

project, based on the innovative five-mirror 

design, to Phase B (detailed design) 

and requested the Executive to provide a 

detailed work plan by early 007. 

Council had been kept informed about 

the developments in the negotiations with 

the Czech Republic, and at its meeting 

in December adopted the necessary resolutions 

on the accession of the Czech 

Republic to ESO as the 13th member 

state from 1 January 007. 

The issue of a new Headquarters building 

in Garching was still of concern. However, 

progress in obtaining the necessary land 

could be reported, and Council agreed to 

give the Executive freedom to pursue the 

most cost-effective solution, including the 

option of purchasing the land. 

76 


Council dealt with various other issues 

and approved the schedule and terms of 

reference for the visiting committee. 

The visiting committee will come to the 

sites in Chile and the Headquarters 

in Garching in early 007. New terms of 

reference for the Finance Committee 

were also approved and the working 

group which had been chaired by Dr. Finn 

Karlsson was discharged. Council agreed 

on a new remit and membership of 

the Scientific Strategy Working Group. 

The Working Group will meet again in 

early 007. 

At the meeting in December, Prof. 

Richard Wade was re-elected President 

of Council for 007 and Dr. Monnik 

Desmeth was re-elected Vice-President. 

Ms. Rowena Sirey was re-appointed 

Chair of the Finance Committee for 007. 

Dr. Simon Morris was appointed Chair 

of the Observing Programmes Committee 

for 007 and Dr. Svetlana Berdyugina 

was appointed Vice-Chair. 

Dr. Monnik Desmeth was appointed Assessor 

to the ALMA Board for 007. 

The President of Council and the Director 

General are members ex officio. 

Council set up an ELT Standing Review 

Committee and appointed Prof. Roger 

Davies as its Chair. This Committee met 

twice in 006 and subsequently reported 

to Council. 

The Scientific Strategy Working Group 

met twice during 006. In January it 

met with three representatives of the 

European Square Kilometre Array (SKA) 

Consortium and the initial findings 

were reported on at the meeting of Committee 

of Council in February. The working 

group met again in April and presented 

an interim report to the Council at 

its meeting in June. Council requested 

the working group to elaborate on some 

of the scenarios included in the interim 

report and to look into related European 

Union issues. In addition, it was decided 

to organise a meeting of the Council 

members representing the funding agencies. 

Council and Committee of Council 

2006 

President Richard Wade 

Belgium Monnik Desmeth 

Jean-Pierre Swings 

Denmark Jens Viggo Clausen 

Henrik Grage 

Finland Kalevi Mattila 

Pentti Pulkkinen 

France Philippe Barré 

(until November 006) 

Julien Galabru 

(as of November 006) 

Laurent Vigroux 

Germany Ralf Bender 

Andreas Drechsler 

Italy Vicenzo Dovì 

Bruno Marano 

The Netherlands P. Tim De Zeeuw 

(until September 006) 

Piet C. van der Kruit 

(as of September 006) 

Jan A. C. van de Donk 

Portugal Fernando Bello 

Teresa Lago 

Sweden Claes Fransson 

Finn Karlsson 

Switzerland Michel Mayor 

Martin Steinacher 

United Kingdom Gerry Gilmore 

Rowena Sirey 

The ESO Tripartite Group, chaired by Dr. 

Ugo Sessi, met in Garching in April and in 

October. The issue of the CERN Pension 

Fund continued to be a very important 

topic. Among the other discussion points 

were the changes to the regulations regarding 

cost-of-living adjustment, expatriation 

allowance, and regarding family/ 

spouse and related leave. The Tripartite 

Group received information concerning 

the and the collective bargaining for local 

staff in Chile.

The Scientific Technical Committee 

The Scientific Technical Committee 

2006 

José Afonso (P) 

Willy Benz (CH) 

Joris Blommaert (B) 

Jean-Gabriel Cuby (F) 

Raffaele Gratton (I) 

Lauri Haikala (FIN) 

Thomas Michael Herbst (D) 

Richard Hills (UK) 

Hans Kjeldsen (DK) 

Yannick Mellier (F) 

Dante Minniti (RCH) 

Goran Olofsson (SE) 

Patrick Roche (UK) 

(Chair for first meeting in 006) 

Linda Tacconi (D) 

(Chair as of second meeting in 006) 

Leonardo Testi (I) 

Huib Jan van Langevelde (NL) 

Dr. Artemio Herrero participated in the 

meetings as the representative of Spain, 

first as an observer, and then as the 

interim Spanish member of the committee. 

Due to personal reasons, Dr. Ikka 

Tuominen resigned from the committee 

and in the interim was replaced by 

Dr. Juhani Huovelin. 

006 was an extremely busy year for the 

Scientific Technical Committee (STC), in 

particular in relation to the European Extremely 

Large Telescope (E-ELT). In addition 

to the two regular meetings (6 nd 

and 64th) in April and October, STC met 

for two extra one-day sessions in May 

and November. In order to cope with the 

wide range of technical projects currently 

going on at ESO, STC appointed two 

additional sub-panels which, in addition 

to members of the committee, incorporate 

experts from the community. These 

are the ELT Science and Engineering 

(ESE) sub-panel and the Very Large Telescope 

Interferometer (VLTI) sub-panel. 

Together with the ALMA European Science 

Advisory Committee (ESAC), these 

three panels advise STC in all matters 

related to these important components of 

the ESO programme. 

STC 62nd Meeting 

At its 61st meeting, STC had encouraged 

ESO to explore ways of achieving the 

goal of a large, deep, multi-colour survey, 

which would be substantially deeper than 

the multipurpose Sloan Digital Sky Survey 

whilst also tackling the nature of dark 

energy. A detailed report about achieving 

this goal with the two VLT survey telescopes 

(VST and VISTA) was presented 

at the 6 nd meeting that took place on 

6 and 7 April. Recognising that VST and 

VISTA have the potential to play a leading 

role in investigating some of the major 

current astronomical questions such as 

the nature of dark energy, STC encouraged 

the Director General to find ways of 

maximising the fraction of time that these 

telescopes will dedicate to public surveys. 

In particular, STC suggested that 

the OPC should award only up to 15 % of 

the available ESO time with these telescopes 

to PI projects (down from the 

5 % foreseen originally), and that this 

fraction should be considered in scientific 

competition with the public surveys 

such that any unallocated time should be 

returned to public surveys. 

A full report by the Director of the La Silla 

Paranal Observatory on the activities of 

the Interferometry Task Force (ITF) was 

presented at the meeting. STC was “enormously 

impressed by the heroic efforts” 

of the ITF that found solutions to many of 

the issues which were limiting the performance 

of the VLTI. STC congratulated 

ITF and Paranal for these achievements, 

and in particular for demonstrating fringe 

tracking with FINITO and the Auxiliary 

Telescopes. 

Following the recommendations at the 

60th meeting of STC, proposals for 

Phase A studies for three second-generation 

VLTI instruments were presented 

to the committee: MATISSE, VSI (a merging 

of VITRUV and BOBCAT), and GRAVI- 

TY. Reassured by the progress in understanding 

the performance of the VLTI 

infrastructure reported at the meeting, 

STC made the following recommendations 

regarding second-generation VLTI 

instruments: 

1. The three consortia should proceed 

with Phase A studies for secondgeneration 

instruments. 

. ESO should issue a draft Interface 

Control Document (ICD) reflecting the 

current state of knowledge of the 

VLTI system, which should be updated 

during these Phase A studies as ITF 

further defines the VLTI performance. 

3. Phase A studies should proceed 

on timescales consistent with the ITF 

investigations. At the end of these 

studies, and following the review of the 

Phase A instrument studies, a new 

definition of the VLTI mission and a new 

ICD will be put in place. 

Extraordinary STC 63rd meeting 

Another STC meeting took place on 

11 May. The need for this extraordinary 

meeting was dictated by the fast pace 

of the E-ELT project established by Coun- 

cil in December 005. Extensive reports 

by the five ELT working groups and by 

the Core ELT Science and Engineering 

(Core-ESE) working group were presented 

at the meeting. STC welcomed 

these reports and congratulated the 

committees for the “admirable job of investigating 

potential telescope design 

and adaptive optics solutions”. STC recommended 

to develop an operational 

model for the E-ELT, which will inform 

telescope and instrument design options. 

The committee also recommended that 

the highest priority of the ESE should be 

to define, together with ESO and the community, 

“the key science and technology 

that Europe will want to pursue”. STC emphasised 

that the combination of the 

E-ELT and the VLT will be unparalleled in 

the world, and recommended ESO to devote 

a significant effort to identify the 

science cases that would uniquely utilise 

both the E-ELT and the VLT. 

A very important item of the agenda was 

the nomination of the ESE committee 

that would take over from the Core-ESE 

as a sub-panel advising STC in all matters 

related to the E-ELT project. The STC 

endorsed ESO’s proposal that the 

members of the Core-ESE continue to 

serve in the ESE, and thus formally 

nominated Daniel Enard (France), Roland 

Gredel (Germany), Colin Cunningham 

(UK), Gerard Rousset (France), Marijn 

Franx (the Netherlands), and Isobel Hook 


77

(UK) as members of the ESE. As STC 

members of the ESE, STC nominated 

Jean-Gabriel Cuby (France), Raffaele 

Gratton (Italy), Thomas Herbst (Germany), 

and Göran Olofsson (Sweden). To 

complete the committee, STC proposed 

names of experienced astronomers 

from the community at large. STC also 

appointed Daniel Enard as Chair and 

Thomas Herbst as co-Chair. 

STC 64th meeting 

ESO received a partnership offer to participate 

in the Large Synoptic Survey 

Telescope (LSST) project, which was presented 

to STC for advice at its 64th meeting 

on 3 and 4 October. While STC 

recognised the enormous scientific potential 

of LSST, it also recognised that 

the financial impact of such partnership 

would stress ESO, given the on-going 

developments for the E-ELT, ALMA, VLTI, 

and the VLT. Therefore STC recommended 

the creation of a small working 

group of ESO and STC members to 

further explore and identify viable options 

for an ESO LSST collaboration, and indicated 

the terms of reference for this 

group. STC proposed Yannick Mellier and 

Artemio Herrero as members of the 

group with Dante Minniti as an alternative. 

For ESO the members are Bruno Leibundgut 

and Paolo Padovani. 

Following a presentation of the status of 

the APEX project, and the request of the 

partners to extend the APEX agreement 

until the end of 01 , STC, encouraged 

by the recent progress on commissioning 

APEX instruments, and recognising the 

potential unique nature of this facility 

in the Southern Hemisphere, unanimous- 

ly agreed that ESO should extend the 

APEX agreement as proposed. STC also 

strongly supported the development and 

expansion of APEX/ALMA synergies, 

and in particular, the development of surveys 

using the APEX instruments to provide 

targets for ALMA (as well as for the 

VLT and even the E-ELT). 

78 


The STC endorsed the ESAC recommendations 

concerning the enhanced capabilities 

for Early Science operations of 

ALMA, and the optimisation of the time 

allocation process by having a single 

international Time Allocation Committee. 

The ESAC also recommended names 

to replace two of its members whose 

terms expire at the end of 006 and early 

007. STC also recommended that, given 

their expertise in sub-millimetric systems, 

the ESAC should also be the forum where 

APEX matters could be discussed. 

Concerning the E-ELT development, STC 

fully endorsed the recommendations of 

the ESE concerning the importance of retaining 

nine science cases for the Design 

Reference Mission (DRM) and that three 

demonstrator science cases be selected 

in the early evaluation by ESO. The ESE 

also made a number of technical and organisational 

recommendations including 

a request for a detailed plan for instrument 

development and selection, and an 

organisation chart of the E-ELT effort 

within ESO. The ESE lauded the efforts of 

the E-ELT Project Office in rapidly advancing 

in the study of both the five-mirror 

and the Gregorian optical designs, 

and recommended that the project office 

continue contacts to understand the 

potential of segmented secondaries. 

The VLTI sub-committee met for the first 

time in September 006. While recognising 

the progress made in some areas, 

especially by the ITF, and that the resources 

required for VLTI are both adequate 

and necessary, the sub-panel 

recommended that the ITF be maintained 

and even strengthened with the addition 

of one or two persons. The sub-panel 

considered that the development of an 

AMBER data reduction package within 

the framework of the SAMPO project 

in the Data Management Division (DMD) 

is an asset to the VLTI that should be extended 

to all VLTI instruments. The members 

of the sub-committee were impressed 

by the progress on PRIMA and, 

while recognising that PRIMA is well 

on track, recommended that the project 

establishes contacts with the VLBI community 

since they have experience in 

solving similar technical problems. These 

and other technical recommendations 

made by the sub-panel were endorsed by 

STC, especially the recommendation of 

maintaining the ITF effort. 

Extraordinary STC 65th meeting 

Developments of the E-ELT and their related 

impact on ESO’s Medium Range 

Implementation Plan (MRIP) prompted a 

special meeting of the STC, on 3 November, 

to discuss these developments 

and make related recommendations 

prior to the December meeting of Council. 

Noting that the highest priority components 

of the ESO programme, and especially 

the Phase B of the E-ELT project, 

are included in the document, STC endorsed 

the MRIP presented by ESO. It 

took note of the fact that the MRIP does 

not include initiatives for a next-generation 

deep-sky survey. STC also discussed 

the document on Long Term Perspectives 

(LTP) and noted that it does not include 

funding for the La Silla Observatory 

beyond 010, indicating that the scientific 

impact of this will be evaluated in 007. 

STC emphasised the requirement to 

deliver the E-ELT on a competitive timescale, 

and encouraged Council to seek 

extra funds to make this a reality. STC 

reaffirmed that the scientific importance 

of the VLT and ALMA will not wane in 

the era of the E-ELT, and stressed that it 

will be critical to maintain these facilities 

as world-class even then. 

At the meeting, the E-ELT Project Office 

presented STC with comprehensive information 

on the E-ELT Basic Reference 

Design, including a detailed analysis of 

the pros and cons of the Gregorian and 

five-mirror designs. On the basis of the 

evidence acquired from within ESO and 

from industry so far, STC was convinced 

that there are no showstoppers for the

five-mirror option, which they considered 

would be the most ambitious project 

that ESO had thus far endeavoured to 

undertake. 

The ESE held a special meeting after the 

E-ELT conference in Marseille, France, 

during which it essentially confirmed the 

statements made by STC. In particular, 

the ESE considered that a 4 -m aperture 

is a good balance between very ambitious 

scientific goals, risks, cost, and 

schedule, and recommended to adopt 

the nominal 4 -m aperture for the E-ELT. 

Considering that the Gregorian design 

bears as a single high-risk item the large 

secondary mirror, for which there is no 

mitigation, the ESE recommended that 

ESO and its governing bodies adopt the 

4 -m five-mirror concept as the E-ELT 

project baseline and that the project proceeds 

to Phase B as soon as possible. 

STC fully endorsed the recommendations 

of the ESE. 

A report on the status of the VST was 

presented at the meeting. Gianpaolo 

Vettolani, representing INAF, assured STC 

that INAF was working together with 

ESO to enable as quickly as possible the 

start of scientific operations of VST on 

Paranal. STC recommended that ESO engage 

fully in the critical design review 

of the primary and secondary mirror supports 

that will take place in early 007, 

and requested that STC be represented 

at the review. Noting that the delay in VST 

is impacting key components of ESO’s 

scientific programme, and that completion 

of the project is very urgent, STC 

urged ESO to start immediately a study 

of alternative plans or possible back-up 

solutions. 

Finally, STC endorsed the recommendation 

of ESAC concerning the implementation 

of a sub-reflector tilt capability for 

the European ALMA antennas, noting this 

enhancement is a cost-effective means 

to regain some of the sensitivity lost by 

descoping the project to 50 antennas. 

NGC 5917, the ‘Hooked’ Galaxy and its companion 

(FORS/VLT). 


79

Finance Committee 

80 

Finance Committee 

2006 

Chair Rowena Sirey 

Belgium Alain Heyen 

Denmark Cecilie Tornøe 

Finland Jaana Aalto 

France Patricia Laplaud 

Germany Marlene Lohkamp- 

Himmighofen 

Italy Ugo Sessi 

The Netherlands Coen J. van Riel 

Portugal Fernando Bello 

Sweden Sofie Björling 

Switzerland Jean-Pierre Ruder 

United Kingdom Colin Vincent 

In 006 the Finance Committee held two 

ordinary meetings. It met in addition 

twice in extraordinary sessions. All the 

meetings were chaired by Ms. Rowena 

Sirey and took place in Garching. 

The committee dealt with various financial 

issues (annual accounts, budget, 

cash-flow situation, financial projections, 

member state contributions) and with 

personnel issues concerning international 

as well as local staff. These subjects were 

discussed in detail and recommendations 

were made to Council. 

Finance Committee approved the awarding 

of 15 contracts exceeding 300 000 € 

and 31 single-source procurements exceeding 

150 000 €. Conditions governing 

forthcoming ALMA production contracts 

were also approved and information was 

received concerning procurement statistics, 

forthcoming calls for tenders and 

price inquiries. 

A major item was the approval of a contract 

for the construction of the technical 

facilities at the Operation Support Facility 

(OSF) site of the ALMA Observatory in 

Chile. 

The committee received regular progress 

reports on the implementation of the ERP 

system, and appreciated the outcome of 

the external ERP review. 


The Users’ Committee 

The Users’ Committee 

2006 

Belgium Griet Van de Steene 

Denmark Uffe Gråe Jørgensen 

Finland Merja Tornikoski 

France Pascale Jablonka 

(Chairwoman) 

Germany Jochen Heidt 

Italy Bianca Maria Poggianti 

The Netherlands Walter Jaffe 

Portugal Nuno Cardoso Santos 

Sweden Sofia Feltzing 

Vice-Chairwoman) 

Switzerland Fréderic Courbin 

United Kingdom Malcolm Bremer 

Chile Wolfgang Gieren 

The Users’ Committee (UC) held its annual 

meeting on 3 and 4 April. The meeting 

was chaired by Pascale Jablonka. 

Representatives from ESO gave presentations 

to the Committee about the 

La Silla Paranal Observatory, ALMA, the 

proposal submission and time allocation 

processes and the revised OPC procedures, 

the forthcoming User Portal, 

and the SAMPO project for data reduction. 

The UC in turn provided feedback 

from the users on the usage of ESO facilities, 

based in part on the outcome of 

a survey designed and distributed by the 

Committee. The level of satisfaction of the 

users with respect to observations carried 

out both at the La Silla and Paranal 

sites is in general high. Most of the expressed 

concerns are related to the diffusion 

of information from ESO to its 

community, in particular about the current 

and future status of available instrumentation, 

and to the transparency of 

the OPC processes. This is reflected in 

a number of action items and recommendations 

assigned by the UC to ESO following 

the open and constructive discussion 

of these topics. The number of such 

action items and recommendations from 

005 that could be closed at the 006 

meeting, or on which significant progress 

had been achieved following corresponding 

action by ESO, is a testimony to efficiency 

of the UC process for improvement 

of ESO’s service to its user 

community in the direction expected by 

the latter. 

As usual, half a day was devoted to a 

‘special topic’, this time the VLT secondgeneration 

instruments. Given the nature 

of this topic, exceptionally, no frequent 

users were invited to contribute. Instead, 

presentations were given by ESO representatives, 

starting with an overview of 

the instrumentation under development, 

followed by specific talks on the individual 

instruments HAWK-I, X-Shooter, KMOS, 

MUSE and SPHERE. The subsequent discussion 

featured a first exchange of views 

about possible additional candidates 

for developments to start around 010. 

Finally, ESO presented a report on the 

status of the E-ELT project. 

The globular cluster 47Tuc (FORS/VLT).


81

The Observing Programmes Committee 

8 

The Observing Programmes Committee 

2006 

Xavier Barcons 

Svetlana Berdyugina (Period 79) 

Eric F. Bell 

Hermann Böhnhardt 

Sven de Rijcke 

Hans de Ruiter 

Gösta Gahm (Period 79) 

Martin Groenewegen (Period78) 

Michiel Hogerheijde 

Jari Kotilainen 

Donald W. Kurtz (Period 79) 

Rafael Rebolo Lopez (Period 78) 

André Moitinho de Almeida (Vice-chairman) 

Simon Morris 

Tom Richtler 

Daniel Rouan (Period 78) 

María Teresa Ruíz (Period 78) 

Monica Tosi 

Lutz Wisotzki (Chairman) 

Sebastian Wolf (Period 79) 

In 006, the Observing Programmes 

Committee (OPC) held its two annual 

meetings in May/June and in November. 

While the number of proposals received 

for Observing Period 78 (P78: 1 Octo- 

ber 006 to 31 March 007), at 8 7, was 

somewhat lower than in recent periods, 

a new all-time record was hit for Observing 

Period 79 (P79: 1 April to 30 September 

007), with the submission of 913 

proposals. This corresponds primarily 

to an increased demand in the ‘Galactic’ 

scientific areas: interstellar medium, star 

formation and planetary systems (OPC 

category C ), and stellar evolution (OPC 

category D). Indeed, since the introduction 

of the current OPC categories for 

Period 66 (starting in October 000), the 

number of proposals submitted in 

categories C and D has nearly doubled, 

while this number has remained approximately 

constant for the ‘extragalactic’ 

proposals of categories A (cosmology) 

and B (galaxies and galactic nuclei). 

In Period 78, the ratio between the requested 

time and the available time (the 

‘pressure factor’) has risen above 6 on 

some of the Unit Telescopes (Antu and 

Kueyen) for the first time since the start of 

science operations of the VLT in April 

1999, while demand for the La Silla telescopes 

has decreased by about 10 % 

from 005 to 006. The workhorse instrument 

FORS , which has been in operation 

since early 000, remains extremely 

popular: the amount of time that is re- 


quested on it is considerably higher than 

on any other VLT instruments. Most 

of the latter experience similar demand, 

within about 0 % of one another. The 

only exception is VISIR: the significantly 

lower demand on this instrument can 

be attributed to the specific nature of 

the science for which it is designed. The 

last first-generation VLT instrument, 

CRIRES, which was offered to the community 

for the first time in Period 79, 

was immediately on a par with more established 

instruments in terms of the 

amount of requested time. Visitor Instruments 

were also scheduled at the VLT 

in both P78 (DAZLE on Melipal) and P79 

(ULTRACAM on Melipal and DAZLE on 

Yepun). 

As in P75 and P77, joint telescope time 

applications for coordinated observations 

with the VLT and with the XMM-Newton 

X-ray observatory have been invited in 

P79. These proposals fall within the framework 

of an agreement between ESO 

and ESA for a joint telescope time application 

scheme, which aims to take full 

advantage of the complementary nature 

of ground-based and space-borne observing 

facilities. Of the four joint applications 

evaluated by ESO’s OPC in P79, 

one was allocated time on both the VLT 

and XMM-Newton telescopes; one of 

the nine proposals evaluated by the XMM 

Time Allocation Committee was also successful. 

In 006, the field of gamma-ray bursts 

(GRBs) continued to account for about 

half of the successful Target of Opportunity 

(ToO) proposals. A large fraction of 

the GRB proposals make use of the 

Rapid Response Mode (RRM) of the VLT, 

with which observation of a transient 

event can be automatically started within 

minutes of its triggering. The unique 

performance of the VLT in this mode, 

combined with ESO’s policy to allow it to 

override both Visitor and Service Mode 

observations, have positioned the VLT 

and the GRB community of the ESO 

member states at the forefront of this 

field of research. We further support the 

optimisation of the scientific return of the 

GRB programmes carried out at its 

observatory sites by inviting the Principal 

Investigators (PIs) of the successful 

GRB proposals to observational strategy 

meetings in Garching twice a year. 

Large Programmes 

Large Programmes (LPs) are projects requiring 

more than 100 hours of observing 

time per year over no more than two 

years, and that have the potential to lead 

to a major advance or breakthrough in 

the considered field of study. In P78, the 

OPC evaluated 0 LP proposals, and 

recommended five of them for implementation. 

A sixth proposal, submitted as a 

preliminary step towards the construction 

of a Visitor Instrument for the NTT, was 

also supported. In P79, four of the 15 LP 

proposals that had been submitted were 

approved. In total, between the start of 

VLT science operations in 1999 and 006 

(P79), 7 LP proposals that received 

favourable evaluation from the OPC were 

allocated time on the La Silla Paranal 

Observatory telescopes. They cover almost 

all current astronomical topics, 

from the Solar System to cosmological 

studies.

Public Surveys 

Surveys provide large, homogeneous 

data sets covering a variety of combinations 

in the parameter space of wavelength, 

depth and sky area. Often surveys 

span longer time intervals and have 

a broader scope than LPs. From their 

databases, large uniformly-treated products 

can be generated, which can be 

used for a variety of scientific purposes. 

For optimal exploitation of the wide-field 

telescopes VST and VISTA, ESO, recognising 

that it does not have the resources 

to conduct public surveys on behalf of 

its user community, has put in place in 

005 a new scheme for the implementation 

of such surveys, allowing them to 

be treated as a separate category of LPs. 

Within this framework, a Public Survey 

is understood to be an observing programme 

in which the investigators commit 

to produce and to make publicly 

available, within a defined time, a fully 

reduced and scientifically usable data 

set that is likely to be of general use to a 

broader community of astronomers. Following 

recommendations by the STC and 

the OPC, 75 % of the ESO time on both 

VST and VISTA will be devoted to Public 

Surveys. 

For evaluation of Public Survey proposals, 

ESO established a Public Survey Panel 

(PSP), comprising scientists with expertise 

in a broad range of current astronomical 

research, with particular emphasis on 

the areas that can profit from Public Surveys. 

The PSP prime mandate is to review 

the proposals and to elaborate a scientifically 

and observationally well-coordinated 

set of Public Surveys. 

Similarly to what had been done in 004 

for the VST, a call for VISTA Public Survey 

proposals was issued at the beginning 

of 006. In response to this call, 15 proposals 

were received. The PSP held a 

first meeting in Garching on –3 May, at 

which it identified those proposals that 

indeed qualified as scientifically valid public 

surveys. A second meeting took place 

in Edinburgh in June, with participation 

of the PIs of the selected projects. At this 

meeting, possible revisions of these proposals 

and the merging of some of them 

with the aim of enhancement of the scientific 

value of the coordinated set were 

discussed, and corresponding recommendations 

were issued. This resulted in 

the submission of six revised proposals 

by the P79 OPC deadline. Following their 

evaluation by the PSP at a final meet- 

ing in Garching on 31 October, and formal 

endorsement of the conclusions of the 

PSP by the OPC at its November meeting, 

these six programmes were recommended 

for execution. 

OPC procedures 

Starting with P78, the revised OPC procedures 

that had been worked out in 

005 were implemented. The most significant 

changes took place in the areas 

of the nomination of the members of the 

OPC and of its Panels, and of the duration 

of their terms of service. As a result, 

as of P78, OPC members are no longer 

proposed by the member states. Instead, 

members of the OPC and of its panels 

are selected on scientific excellence. They 

are appointed by ESO’s Director Gener- 

al based on the recomendations of the 

Nominating Committee for the OPC. This 

Nominating Committee, which was constituted 

and held its first two meetings 

in 006, comprises three astronomers 

from the community and two ESO astronomers. 

In order to reduce the burden 

of the commitment required from astronomers 

who serve on the OPC or on its 

panels, and to allow a greater fraction of 

the community to participate more actively 

in the selection of the observing 

programmes, and hence in the definition 

of the orientation of European astronomy, 

the term of service was reduced to two 

years for OPC members (compared to 

four years previously) and to one year for 

panel members (from two years). 

On the other hand, in order to face the 

increasing number of proposals in scientific 

categories C and D, new sub- 

panels were created for each of these 

categories. Thus as of P78, the OPC 

consisted of a total of 10 sub-panels: two 

for each of categories A and B (unchanged) 

and three for each of categories 

C and D (instead of two until P77). 

The beneficial effect of this change on the 

workload of the referees of categories C 

and D was already offset by P79, where 

due to the unexpectedly steep increase in 

the numbers of proposals submitted in 

these categories, the amount of work of 

the members of the corresponding subpanels 

was back to its P77 level. Further 

steps to be taken to address this extremely 

fast evolution were discussed 

at the P79 OPC meeting, for implementation 

in 007. 


83

Summary of Use of Telescopes by Discipline 

The scientific categories referred to in 

the following tables correspond to the 

OPC classifications given below: 

OPC Categories and Sub-Categories 

A: Cosmology 

A1 Surveys of AGNs and high-z 

galaxies 

A Identification studies of extragalactic 

surveys 

A3 Large-scale structure and evolution 

A4 Distance scale 

A5 Groups and clusters of galaxies 

A6 Gravitational lensing 

A7 Intervening absorption-line systems 

A8 High-redshift galaxies (star formation 

and ISM) 

B: Galaxies and Galactic Nuclei 

B1 Morphology and galactic structure 

B Stellar populations 

B3 Chemical evolution 

B4 Galaxy dynamics 

B5 Peculiar/interacting galaxies 

84 


B6 Non-thermal processes in galactic 

nuclei (incl. QSRs, QSOs, blazars, 

Seyfert galaxies, BALs, radio galaxies, 

and LINERS) 

B7 Thermal processes in galactic nuclei 

and starburst galaxies (incl. ultraluminous 

IR galaxies, outflows, 

emission lines, and spectral energy 

distributions) 

B8 Central supermassive objects 

B9 AGN host galaxies 

C: Interstellar Medium, Star Formation 

and Planetary Systems 

C1 Gas and dust, giant molecular 

clouds, cool and hot gas, diffuse 

and translucent clouds 

C Chemical processes in the interstellar 

medium 

C3 Star-forming regions, globules, 

protostars, H ii regions 

C4 Pre-main-sequence stars (massive 

PMS stars, Herbig Ae/Be stars and 

T Tauri stars) 

C5 Outflows, stellar jets, HH objects 

C6 Main-sequence stars with circumstellar 

matter, early evolution 

C7 Young binaries, brown dwarfs, 

exosolar planet searches 

C8 Solar system (planets, comets, 

small bodies) 

D: Stellar Evolution 

D1 Main-sequence stars 

D Post-main-sequence stars, giants, 

supergiants, AGB stars, post-AGB 

stars 

D3 Pulsating stars and stellar activity 

D4 Mass loss and winds 

D5 Supernovae, pulsars 

D6 Planetary nebulae, nova remnants 

and supernova remnants 

D7 Pre-white dwarfs and white dwarfs, 

neutron stars 

D8 Evolved binaries, black-hole 

candidates, novae, X-ray binaries, 

CVs 

D9 Gamma-ray and X-ray bursters 

D10 OB associations, open and globular 

clusters, extragalactic star clusters 

D11 Individual stars in external galaxies

85 


Percentage of scheduled observing time/telescope/instrument/discipline 

Telescope 

. -m 

Total 

Instrument 

FEROS 

WFI 

B 

3 

5 

8 

C 

14 

6 

20 

D 

45 

3 

48 

Total 

66 

34 

100 

A 

4 

0 

24 

Scientific Categories 

Telescope 

3.6-m 

Total 

Instrument 

EFOSC 

HARPS 

Special3.6 

TIMMI 

B 

7 

0 

0 

9 

C 

1 

51 

1 

7 

60 

D 

6 

1 

0 

1 

19 

Total 

6 

63 

1 

10 

100 

A 

1 

0 

0 

0 

12 


Telescope 

APEX 

Total 

Instrument 

APEX- A 

FLASH 

B 

1 

14 

C 

35 

57 

D 

14 

13 

27 

Total 

63 

37 

100 

A 

0 

2 


Telescope 

NTT 

Total 

Instrument 

EMMI 

SOFI 

SUSI 

SpecialNTT 

B 

8 

5 

5 

0 

18 

C 

9 

4 

37 

D 

1 

9 

1 

1 

23 

Total 

46 

43 

8 

3 

100 

A 

17 

5 

0 

0 

22 


Telescope 

UT1 

Total 

Instrument 

FORS 

ISAAC 

B 

17 

5 

22 

C 

3 

11 

14 

D 

14 

1 

26 

Total 

64 

36 

100 

A 

30 

8 

38 


Telescope 

UT3 

Total 

Instrument 

DAZLE 

VIMOS 

VISIR 

B 

0 

5 

27 

C 

0 

4 

19 

23 

D 

0 

4 

4 

8 

Total 

4 

68 

8 

100 

A 

4 

38 

0 

42 


Telescope 

UT 

Total 

Instrument 

FLAMES 

FORS1 

UVES 

B 

8 

5 

5 

18 

C 

10 

5 

5 

20 

D 

7 

15 

17 

39 

Total 

5 

41 

34 

100 

A 

0 

16 

7 

23 


Telescope 

UT4 

Total 

Instrument 

NACO 

SINFONI 

B 

11 

1 

32 

C 

9 

31 

D 

1 

4 

16 

Total 

45 

55 

100 

A 

0 

1 

21 


Telescope 

VLTI 

Total 

Instrument 

AMBER 

MIDI 

B 

0 

1 

1 

C 

10 

13 

23 

D 

11 

65 

76 

Total 

1 

79 

100 

A 

0 

0 

0 

Scientific Categories

Publications 

Publications in refereed journals based on ESO data 

Ábrahám, P.; Mosoni, L.; Henning, T.; Kóspál, Á.; 

Leinert, C.; Quanz, S. P.; Ratzka, T.; First AU-scale 

observations of V1647 Orionis with VLTI/MIDI; 

A&A 449, L13–L16 

Acke, B.; van den Ancker, M. E.; Resolving the disk 

rotation of HD 97048 and HD 100546 in the [O i] 

6300 Å line: evidence for a giant planet orbiting 

HD 100546; A&A 449, 67– 79 

Acke, B.; van den Ancker, M. E.; A survey for nano- 

diamond features in the 3 micron spectra 

of Herbig Ae/Be stars; A&A 457, 171–181 

Ádámkovics, M.; de Pater, I.; Hartung, M.; 

Eisenhauer, F.; Genzel, R.; Griffith, C. A.; Titan’s 

bright spots: Multiband spectroscopic measurement 

of surface diversity and hazes; JGRE 111 

Aerts, C.; de Cat, P.; de Ridder, J.; van Winckel, H.; 

Raskin, G.; Davignon, G.; Uytterhoeven, K.; Multiperiodicity 

in the large-amplitude rapidly-rotating 

b Cephei star HD 03664; A&A 449, 305–311 

Afonso, C.; Glicenstein, J. F.; Gould, A.; Smith, M. C.; 

Wagner, R. M.; Albert, J. N.; Andersen, J.; Ansari, 

R.; Aubourg, É.; Bareyre, P.; Beaulieu, J. P.; Blanc, 

G.; Charlot, X.; Coutures, C.; Ferlet, R.; Fouqué, 

P.; Goldman, B.; Graff, D.; Gros, M.; Haissinski, J.; 

Hamadache, C.; de Kat, J.; Leguillou, L.; Lesquoy, 

É.; Loup, C.; Magneville, C.; Marquette, J. B.; 

Maurice, É.; Maury, A.; Milsztajn, A.; Moniez, M.; 

Palanque-Delabrouille, N.; Perdereau, O.; Prévot, 

L.; Rahal, Y. R.; Rich, J.; Spiro, M.; Tisserand, P.; 

Vidal-Madjar, A.; Vigroux, L.; Zylberajch, S.; 

The OGLE-II event sc5 859: a classical nova outburst?; 

A&A 450, 33– 39 

Alcalá, J. M.; Spezzi, L.; Frasca, A.; Covino, E.; 

Porras, A.; Merín, B.; Persi, P.; The first brown 

dwarf with a disk in Chamaeleon II; A&A 453, 

L1–L4 

Allen, D. M.; Barbuy, B.; Analysis of 6 barium stars. 

II. Contributions of s-, r-, and p-processes in the 

production of heavy elements; A&A 454, 917–931 

Allen, D. M.; Barbuy, B.; Analysis of 6 barium stars. 

I. Abundances; A&A 454, 895–915 

Allen, P. D.; Driver, S. P.; Graham, A. W.; Cameron, 

E.; Liske, J.; de Propris, R.; The Millennium Galaxy 

Catalogue: bulge-disc decomposition of 10095 

nearby galaxies; MNRAS 371, –18 

Alvarez-Candal, A.; Duffard, R.; Lazzaro, D.; 

Michtchenko, T.; The inner region of the asteroid 

Main Belt: a spectroscopic and dynamic analysis; 

A&A 459, 969–976 

Alves-Brito, A.; Barbuy, B.; Zoccali, M.; Minniti, D.; 

Ortolani, S.; Hill, V.; Renzini, A.; Pasquini, L.; Bica, 

E.; Rich, R. M.; Meléndez, J.; Momany, Y.; 

VLT-UVES abundance analysis of four giants in 

NGC 6553; A&A 460, 69– 76 

Andreon, S.; Quintana, H.; Tajer, M.; Galaz, G.; 

Surdej, J.; The Butcher-Oemler effect at z ~ 0.35: 

a change in perspective; MNRAS 365, 915–9 8 

Annibali, F.; Bressan, A.; Rampazzo, R.; Zeilinger, W. 

W.; Nearby early-type galaxies with ionized gas. 

II. Line-strength indices for 18 additional galaxies; 

A&A 445, 79–91 

Antonello, E.; Mantegazza, L.; Rainer, M.; Miglio, A.; 

Probable nonradial g-mode pulsation in early 

A-type stars; A&A 445, L15–L18 

Antonello, E.; Fossati, L.; Fugazza, D.; Mantegazza, 

L.; Gieren, W.; Variable stars in nearby galaxies. 

VII. P-L relation in the BVRI bands of Cepheids in 

IC 1613; A&A 445, 901–906 

86 


Antonelli, L. A.; Testa, V.; Romano, P.; Guetta, D.; 

Torii, K.; D’Elia, V.; Malesani, D.; Chincarini, G.; 

Covino, S.; D’Avanzo, P.; Della Valle, M.; Fiore, F.; 

Fugazza, D.; Moretti, A.; Stella, L.; Tagliaferri, G.; 

Barthelmy, S.; Burrows, D.; Campana, S.; Capalbi, 

M.; Cusumano, G.; Gehrels, N.; Giommi, P.; 

Lazzati, D.; La Parola, V.; Mangano, V.; Mineo, T.; 

Nousek, J.; O’Brien, P. T.; Perri, M.; The multiwavelength 

afterglow of GRB 0507 1: a puzzling 

rebrightening seen in the optical but not in the 

X-ray; A&A 456, 509–515 

Argiroffi, C.; Favata, F.; Flaccomio, E.; Maggio, A.; 

Micela, G.; Peres, G.; Sciortino, S.; XMM-Newton 

survey of two upper Scorpius regions; A&A 459, 

199– 13 

Arias, J. I.; Barbá, R. H.; Maíz Apellániz, J.; Morrell, 

N. I.; Rubio, M.; The infrared Hourglass cluster in 

M8; MNRAS 366, 739–757 

Asplund, M.; Lambert, D. L.; Nissen, P. E.; Primas, F.; 

Smith, V. V.; Lithium Isotopic Abundances in 

Metal-poor Halo Stars; ApJ 644, 9– 59 

Astier, P.; Guy, J.; Regnault, N.; Pain, R.; Aubourg, 

E.; Balam, D.; Basa, S.; Carlberg, R. G.; Fabbro, 

S.; Fouchez, D.; Hook, I. M.; Howell, D. A.; Lafoux, 

H.; Neill, J. D.; Palanque-Delabrouille, N.; Perrett, 

K.; Pritchet, C. J.; Rich, J.; Sullivan, M.; Taillet, R.; 

Aldering, G.; Antilogus, P.; Arsenijevic, V.; Balland, 

C.; Baumont, S.; Bronder, J.; Courtois, H.; Ellis, R. 

S.; Filiol, M.; Gonçalves, A. C.; Goobar, A.; Guide, 

D.; Hardin, D.; Lusset, V.; Lidman, C.; McMahon, 

R.; Mouchet, M.; Mourao, A.; Perlmutter, S.; 

Ripoche, P.; Tao, C.; Walton, N.; The Supernova 

Legacy Survey: measurement of ΩM, Ω∆ and w 

from the first year data set; A&A 447, 31–48 

Ausseloos, M.; Aerts, C.; Lefever, K.; Davis, J.; 

Harmanec, P.; High-precision elements of doublelined 

spectroscopic binaries from combined interferometry 

and spectroscopy. Application to the b 

Cephei star b Centauri; A&A 455, 59– 69 

Bagnulo, S.; Landstreet, J. D.; Mason, E.; Andretta, 

V.; Silaj, J.; Wade, G. A.; Searching for links between 

magnetic fields and stellar evolution. 

I. A survey of magnetic fields in open cluster A- 

and B-type stars with FORS1; A&A 450, 777–791 

Bagnulo, S.; Boehnhardt, H.; Muinonen, K.; 

Kolokolova, L.; Belskaya, I.; Barucci, M. A.; 

Exploring the surface properties of transneptunian 

objects and Centaurs with polarimetric FORS1/ 

VLT observations; A&A 450, 1 39–1 48 

Bains, I.; Wong, T.; Cunningham, M.; Sparks, P.; 

Brisbin, D.; Calisse, P.; Dempsey, J. T.; Deragopian, 

G.; Ellingsen, S.; Fulton, B.; Herpin, F.; Jones, P.; 

Kouba, Y.; Kramer, C.; Ladd, E. F.; Longmore, S. 

N.; McEvoy, J.; Maller, M.; Minier, V.; Mookerjea, 

B.; Phillips, C.; Purcell, C. R.; Walsh, A.; Voronkov, 

M. A.; Burton, M. G.; Molecular line mapping of 

the giant molecular cloud associated with RCW 

106 – I. 13CO; MNRAS 367, 1609–16 8 

Bamford, S. P.; Aragón-Salamanca, A.; Milvang- 

Jensen, B.; The Tully-Fisher relation of distant field 

galaxies; MNRAS 366, 308–3 0 

Barbuy, B.; Zoccali, M.; Ortolani, S.; Momany, Y.; 

Minniti, D.; Hill, V.; Renzini, A.; Rich, R. M.; Bica, 

E.; Pasquini, L.; Yadav, R. K. S.; VLT-UVES analysis 

of two giants in the bulge metal-poor globular 

cluster HP-1. Analysis of two giants in HP-1; A&A 

449, 349–358 

Barucci, M. A.; Merlin, F.; Dotto, E.; Doressoundiram, 

A.; de Bergh, C.; TNO surface ices. Observations 

of the TNO 55638 ( 00 VE95; A&A 455, 7 5–730 

Bassa, C. G.; Jonker, P. G.; in’t Zand, J. J. M.; 

Verbunt, F.; Two new candidate ultra-compact Xray 

binaries; A&A 446, L17–L 0 

Bassa, C. G.; van Kerkwijk, M. H.; Koester, D.; 

Verbunt, F.; The masses of PSR J1911-5958A and 

its white dwarf companion; A&A 456, 95–304 

Bastian, N.; Emsellem, E.; Kissler-Patig, M.; 

Maraston, C.; Young star cluster complexes in 

NGC 4038/39. Integral field spectroscopy using 

VIMOS-VLT; A&A 445, 471–483 

Bastian, N.; Saglia, R. P.; Goudfrooij, P.; Kissler- 

Patig, M.; Maraston, C.; Schweizer, F.; Zoccali, M.; 

Dynamical mass estimates for two luminous star 

clusters in galactic merger remnants; A&A 448, 

88–891 

Battaglia, G.; Tolstoy, E.; Helmi, A.; Irwin, M. J.; 

Letarte, B.; Jablonka, P.; Hill, V.; Venn, K. A.; 

Shetrone, M. D.; Arimoto, N.; Primas, F.; Kaufer, A.; 

Francois, P.; Szeifert, T.; Abel, T.; Sadakane, K.; 

The DART imaging and CaT survey of the Fornax 

dwarf spheroidal galaxy; A&A 459, 4 3–440 

Baume, G.; Moitinho, A.; Vázquez, R. A.; Solivella, 

G.; Carraro, G.; Villanova, S.; NGC 401: a template 

of the young population of the Norma- 

Cygnus arm in the Third Galactic Quadrant; 

MNRAS 367, 1441–1449 

Beaulieu, J.-P.; Bennett, D. P.; Fouqué, P.; Williams, 

A.; Dominik, M.; Jorgensen, U. G.; Kubas, D.; 

Cassan, A.; Coutures, C.; Greenhill, J.; Hill, K.; 

Menzies, J.; Sackett, P. D.; Albrow, M.; Brillant, S.; 

Caldwell, J. A. R.; Calitz, J. J.; Cook, K. H.; 

Corrales, E.; Desort, M.; Dieters, S.; Dominis, D.; 

Donatowicz, J.; Hoffman, M.; Kane, S.; Marquette, 

J.-B.; Martin, R.; Meintjes, P.; Pollard, K.; Sahu, 

K.; Vinter, C.; Wambsganss, J.; Woller, K.; Horne, 

K.; Steele, I.; Bramich, D. M.; Burgdorf, M.; 

Snodgrass, C.; Bode, M.; Udalski, A.; Szymański, 

M. K.; Kubiak, M.; Wie¸ ckowski, T.; Pietrzyński, G.; 

Soszyński, I.; Szewczyk, O.; Wyrzykowski, Ł.; 

Paczyński, B.; Abe, F.; Bond, I. A.; Britton, T. R.; 

Gilmore, A. C.; Hearnshaw, J. B.; Itow, Y.; Kamiya, 

K.; Kilmartin, P. M.; Korpela, A. V.; Masuda, K.; 

Matsubara, Y.; Motomura, M.; Muraki, Y.; 

Nakamura, S.; Okada, C.; Ohnishi, K.; Rattenbury, 

N. J.; Sako, T.; Sato, S.; Sasaki, M.; Sekiguchi, T.; 

Sullivan, D. J.; Tristram, P. J.; Yock, P. C. M.; 

Yoshioka, T.; Discovery of a cool planet of 5.5 

Earth masses through gravitational microlensing; 

Nature 439, 437–440 

Beccari, G.; Ferraro, F. R.; Possenti, A.; Valenti, E.; 

Origlia, L.; Rood, R. T.; The Dynamical State and 

Blue Straggler Population of the Globular Cluster 

NGC 6 66 (M6 ); AJ 131, 551– 560 

Beccari, G.; Ferraro, F. R.; Lanzoni, B.; Bellazzini, M.; 

A Population of Binaries in the Asymptotic Giant 

Branch of 47 Tucanae?; ApJ 65 , L1 1–L1 4 

Becker, W.; Kramer, M.; Jessner, A.; Taam, R. E.; Jia, 

J. J.; Cheng, K. S.; Mignani, R.; Pellizzoni, A.; de 

Luca, A.; Słowikowska, A.; Caraveo, P. A.; A Multiwavelength 

Study of the Pulsar PSR B19 9+10 

and Its X-Ray Trail; ApJ 645, 14 1–1435

Bedding, T. R.; Butler, R. P.; Carrier, F.; Bouchy, F.; 

Brewer, B. J.; Eggenberger, P.; Grundahl, F.; 

Kjeldsen, H.; McCarthy, C.; Nielsen, T. B.; Retter, 

A.; Tinney, C. G.; Solar-like Oscillations in the 

Metal-poor Subgiant b Indi: Constraining the 

Mass and Age Using Asteroseismology; ApJ 647, 

558–563 

Bedregal, A. G.; Aragón-Salamanca, A.; Merrifield, 

M. R.; Milvang-Jensen, B.; S0 galaxies in Fornax: 

data and kinematics; MNRAS 371, 191 –19 4 

Behrend, R.; Bernasconi, L.; Roy, R.; Klotz, A.; Colas, 

F.; Antonini, P.; Aoun, R.; Augustesen, K.; Barbotin, 

E.; Berger, N.; Berrouachdi, H.; Brochard, E.; 

Cazenave, A.; Cavadore, C.; Coloma, J.; Cotrez, V.; 

Deconihout, S.; Demeautis, C.; Dorseuil, J.; Dubos, 

G.; Durkee, R.; Frappa, E.; Hormuth, F.; Itkonen, T.; 

Jacques, C.; Kurtze, L.; Laffont, A.; Lavayssière, 

M.; Lecacheux, J.; Leroy, A.; Manzini, F.; Masi, G.; 

Matter, D.; Michelsen, R.; Nomen, J.; Oksanen, A.; 

Pääkkönen, P.; Peyrot, A.; Pimentel, E.; Pray, D.; 

Rinner, C.; Sanchez, S.; Sonnenberg, K.; Sposetti, 

S.; Starkey, D.; Stoss, R.; Teng, J.-P.; Vignand, M.; 

Waelchli, N.; Four new binary minor planets: (854) 

Frostia, (1089) Tama, (1313) Berna, (449 ) Debussy; 

A&A 446, 1177–1184 

Bellazzini, M.; Correnti, M.; Ferraro, F. R.; Monaco, L.; 

Montegriffo, P.; The age of the main population of 

the Sagittarius dwarf spheroidal galaxy. Solving 

the “M giant conundrum”; A&A 446, L1–L4 

Belloche, A.; Parise, B.; van der Tak, F. F. S.; Schilke, 

P.; Leurini, S.; Güsten, R.; Nyman, L.-Å.; The evolutionary 

state of the southern dense core Chamaeleon-MMS1; 

A&A 454, L51–L54 

Bellazzini, M.; Newberg, H. J.; Correnti, M.; Ferraro, 

F. R.; Monaco, L.; Detection of a population gradient 

in the Sagittarius stream; A&A 457, L 1–L 4 

Beltrán, M. T.; Brand, J.; Cesaroni, R.; Fontani, F.; 

Pezzuto, S.; Testi, L.; Molinari, S.; Search for 

massive protostar candidates in the southern 

hemisphere. II. Dust continuum emission; A&A 

447, 1– 33 

Benetti, S.; Cappellaro, E.; Turatto, M.; Taubenberger, 

S.; Harutyunyan, A.; Valenti, S.; Supernova 00 ic: 

The Collapse of a Stripped-Envelope, Massive 

Star in a Dense Medium?; ApJ 653, L1 9–L13 

Bennert, N.; Jungwiert, B.; Komossa, S.; Haas, M.; 

Chini, R.; Size and properties of the NLR in the 

Seyfert- galaxy NGC 1386; A&A 446, 919–93 


Chini, R.; Size and properties of the narrow-line 

region in Seyfert- galaxies from spatially-resolved 

optical spectroscopy; A&A 456, 953–966 


Chini, R.; Size and properties of the narrow-line 

region in Seyfert-1 galaxies from spatially-resolved 

optical spectroscopy; A&A 459, 55–69 

Bensby, T.; Feltzing, S.; The origin and chemical 

evolution of carbon in the Galactic thin and thick 

discs; MNRAS 367, 1181–1193 

Bergond, G.; Zepf, S. E.; Romanowsky, A. J.; 

Sharples, R. M.; Rhode, K. L.; Wide-field kinematics 

of globular clusters in the Leo I group; A&A 

448, 155–164 

Berta, S.; Rubele, S.; Franceschini, A.; Held, E. V.; 

Rizzi, L.; Lonsdale, C. J.; Jarrett, T. H.; Rodighiero, 

G.; Oliver, S. J.; Dias, J. E.; Buttery, H. J.; Fiore, F.; 

La Franca, F.; Puccetti, S.; Fang, F.; Shupe, D.; 

Surace, J.; Gruppioni, C.; The ESO-Spitzer Imaging 

extragalactic Survey (ESIS). I. WFIB, V, R 

deep observations of ELAIS-S1 and comparison 

to Spitzer and GALEX data; A&A 451, 881–900 

Bettoni, D.; Moles, M.; Kjærgaard, P.; Fasano, G.; 

Varela, J.; The scaling relation of early-type galaxies 

in clusters. II. Spectroscopic data for galaxies 

in eight nearby clusters; A&A 45 , 811–817 

Bigot, L.; Kervella, P.; Thévenin, F.; Ségransan, D.; 

The limb darkening of b Centauri B. Matching 3D 

hydrodynamical models with interferometric 

measurements; A&A 446, 635–641 

Bik, A.; Kaper, L.; Waters, L. B. F. M.; VLT K-band 

spectroscopy of massive young stellar objects in 

(ultra-)compact HII regions; A&A 455, 561–576 

Biller, B. A.; Kasper, M.; Close, L. M.; Brandner, W.; 

Kellner, S.; Discovery of a Brown Dwarf Very 

Close to the Sun: A Methane-rich Brown Dwarf 

Companion to the Low-Mass Star SCR 1845- 

6357; ApJ 641, L141–L144 

Biver, N.; Bockelée-Morvan, D.; Crovisier, J.; Lis, D. 

C.; Moreno, R.; Colom, P.; Henry, F.; Herpin, F.; 

Paubert, G.; Womack, M.; Radio wavelength 

molecular observations of comets C/1999 T1 

(McNaught-Hartley), C/ 001 A (LINEAR), C/ 000 

WM1 (LINEAR) and 153P/Ikeya-Zhang; A&A 449, 

1 55–1 70 

Biviano, A.; Salucci, P.; The radial profiles of the 

different mass components in galaxy clusters; 

A&A 45 , 75–81 

Blondin, S.; Dessart, L.; Leibundgut, B.; Branch, D.; 

Höflich, P.; Tonry, J. L.; Matheson, T.; Foley, R. J.; 

Chornock, R.; Filippenko, A. V.; Sollerman, J.; 

Spyromilio, J.; Kirshner, R. P.; Wood-Vasey, W. M.; 

Clocchiatti, A.; Aguilera, C.; Barris, B.; Becker, A. 

C.; Challis, P.; Covarrubias, R.; Davis, T. M.; 

Garnavich, P.; Hicken, M.; Jha, S.; Krisciunas, K.; 

Li, W.; Miceli, A.; Miknaitis, G.; Pignata, G.; Prieto, 

J. L.; Rest, A.; Riess, A. G.; Salvo, M. E.; Schmidt, 

B. P.; Smith, R. C.; Stubbs, C. W.; Suntzeff, N. B.; 

Using Line Profiles to Test the Fraternity of Type Ia 

Supernovae at High and Low Redshifts; AJ 131, 

1648–1666 

Blondel, P. F. C.; Djie, H. R. E. Tjin A.; Modeling of 

PMS Ae/Fe stars using UV spectra; A&A 456, 

1045–1068 

Bondar, A.; Galazutdinov, G.; Patriarchi, P.; Krełowski, 

J.; On the Homogeneity of the Extinction Law in 

our Galaxy; JKAS 39, 73–80 

Borissova, J.; Ivanov, V. D.; Minniti, D.; Geisler, D.; 

Discovery of new Milky Way star cluster candidates 

in the MASS point source catalog. V. 

Follow-up observations of the young stellar cluster 

candidates RCW 87, [BDSB 003] 164 and 

[DBSB 003] 17 ; A&A 455, 9 3–930 

Borissova, J.; Minniti, D.; Rejkuba, M.; Alves, D.; 

Properties of RR Lyrae stars in the inner regions 

of the Large Magellanic Cloud. II. The extended 

sample; A&A 460, 459–466 

Bornancini, C. G.; Lambas, D. G.; De Breuck, C.; 

Clustering and properties of K-band companion 

galaxies around ultrasteep spectrum radio 

sources; MNRAS 366, 1067–1074 

Boschin, W.; Girardi, M.; Spolaor, M.; Barrena, R.; 

Internal dynamics of the radio halo cluster Abell 

744; A&A 449, 461–474 

Bouwens, R. J.; Illingworth, G. D.; Blakeslee, J. P.; 

Franx, M.; Galaxies at z ~ 6: The UV Luminosity 

Function and Luminosity Density from 506 HUDF, 

HUDF Parallel ACS Field, and GOODS i-Dropouts; 

ApJ 653, 53–85 

Bouy, H.; Martín, E. L.; Brandner, W.; Zapatero- 

Osorio, M. R.; Béjar, V. J. S.; Schirmer, M.; 

Huélamo, N.; Ghez, A. M.; Multiplicity of very lowmass 

objects in the Upper Scorpius OB association: 

a possible wide binary population; A&A 

451, 177–186 

Bragaglia, A.; Tosi, M.; Carretta, E.; Gratton, R. G.; 

Marconi, G.; Pompei, E.; Photometric and spectroscopic 

study of the intermediate-age open 

cluster NGC 3960; MNRAS 366, 1493–150 

Brannigan, E.; Takami, M.; Chrysostomou, A.; Bailey, 

J.; On the detection of artefacts in spectroastrometry; 

MNRAS 367, 315–3 

Brandeker, A.; Jayawardhana, R.; Khavari, P.; 

Haisch, K. E., Jr.; Mardones, D.; Deficit of Wide 

Binaries in the b Chamaeleontis Young Cluster; 

ApJ 65 , 157 –1584 

Brandeker, A.; Jayawardhana, R.; Ivanov, V. D.; 

Kurtev, R.; Infrared Spectroscopy of the Ultra- 

Low-Mass Binary Oph 16 5- 40515; ApJ 653, 

L61–L64 

Bressan, A.; Falomo, R.; Valdés, J. R.; Rampazzo, 

R.; Ongoing Star Formation in the BL Lacertae 

Object PKS 005-489; ApJ 645, L101–L104 

Bresolin, F.; Pietrzyński, G.; Urbaneja, M. A.; Gieren, 

W.; Kudritzki, R.-P.; Venn, K. A.; The Araucaria 

Project: VLT Spectra of Blue Supergiants in WLM- 

Classification and First Abundances; ApJ 648, 

1007–1019 

Brookes, M. H.; Best, P. N.; Rengelink, R.; Röttgering, 

H. J. A.; CENSORS: A Combined EIS-NVSS 

Survey of Radio Sources – II. Infrared imaging and 

the K-z relation; MNRAS 366, 1 65–1 88 

Brotherton, M. S.; De Breuck, C.; Schaefer, J. J.; 

Spectropolarimetry of PKS 0040-005 and the 

orientation of broad absorption line quasars; 

MNRAS 37 , L58–L6 

Brunetto, R.; Barucci, M. A.; Dotto, E.; Strazzulla, G.; 

Ion Irradiation of Frozen Methanol, Methane, and 

Benzene: Linking to the Colors of Centaurs and 

Trans-Neptunian Objects; ApJ 644, 646–650 

Burgarella, D.; Pérez-González, P. G.; Tyler, K. D.; 

Rieke, G. H.; Buat, V.; Takeuchi, T. T.; Lauger, S.; 

Arnouts, S.; Ilbert, O.; Barlow, T. A.; Bianchi, L.; 

Lee, Y.-W.; Madore, B. F.; Malina, R. F.; Szalay, A. 

S.; Yi, S. K.; Ultraviolet-to-far infrared properties of 

Lyman break galaxies and luminous infrared 

galaxies at z ~ 1; A&A 450, 69–76 

Buson, L. M.; Cappellari, M.; Corsini, E. M.; Held, E. 

V.; Lim, J.; Pizzella, A.; NGC 7679: an anomalous, 

composite Seyfert 1 galaxy whose X-ray luminous 

AGN vanishes at optical wavelengths; A&A 447, 

441–451 

Canto Martins, B. L.; Lèbre, A.; de Laverny, P.; Melo, 

C. H. F.; Do Nascimento, J. D., Jr.; Richard, O.; de 

Medeiros, J. R.; S1 4 : a lithium-rich subgiant 

star in the open cluster M 67; A&A 451, 993–997 

Caputi, K. I.; McLure, R. J.; Dunlop, J. S.; Cirasuolo, 

M.; Schael, A. M.; Further constraints on the evolution 

of Ks-selected galaxies in the GOODS/ 

CDFS field; MNRAS 366, 609–6 3 

Caputi, K. I.; Dole, H.; Lagache, G.; McLure, R. J.; 

Puget, J.-L.; Rieke, G. H.; Dunlop, J. S.; Le Floc’h, 

E.; Papovich, C.; Pérez-González, P. G.; Linking 

Stellar Mass and Star Formation in Spitzer MIPS 

4 μm Galaxies; ApJ 637, 7 7–740 

Caputi, K. I.; Dole, H.; Lagache, G.; McLure, R. J.; 

Dunlop, J. S.; Puget, J.-L.; Le Floc’h, E.; Pérez- 

González, P. G.; The role of the LIRG and ULIRG 

phases in the evolution of Ks-selected galaxies; 

A&A 454, 143–150 


87

Caratti o Garatti, A.; Giannini, T.; Nisini, B.; Lorenzetti, 

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Claeskens, J.-F.; Smette, A.; Vandenbulcke, L.; 

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Space Density and Colors of Massive Galaxies at 

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ApJ 638, L59–L6 

Sauer, D. N.; Mazzali, P. A.; Deng, J.; Valenti, S.; 

Nomoto, K.; Filippenko, A. V.; The properties of 

the `standard’ Type Ic supernova 1994I from 

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Thompson, R. I.; Sauvage, M.; Kennicutt, R. C., Jr.; 

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Financial Statement 

Financial Statements 2006 

(in € 1000) 

Balance Sheet 

Assets 

Cash and short-term deposits 

Claims, advances, refundable taxes and other assets 

Total assets 

Liabilities and equity 

Dues 

Advance payments received and other liabilities 

Total liabilities 

Cumulated result previous years 

Annual result 

Total equity 

Total liabilities and equity 

Statement of Income and Expenditure 

Income 

Contributions from member states 

Contributions from third parties and partners 

Income from sales and other income 

Total income 

Expenditure 

Expenditure for staff 

Operating and other expenditure 

Total expenditure 

2006 Result 

Statement of Cash flow 

Cash flow from operating activities 

Receipts 

Income 

Net movements on accounts receivable 

Total 

Payments 

Expenditure 

Net movements on accounts payable 

Total 

Net cash flow from operating activities 

Cash flow from financing activities 

Net cash flow from financing activities 

Net cash flow = Net increase/decrease in cash 

and short-term deposits 

31.12.2006 

89 

60 40 

149 624 

6803 

0 616 

27419 

46 675 

75 530 

122205 

149 624 

31.12.2005 

76 880 

4 958 

81838 

18 438 

16 7 5 

35163 

1 977 

33 698 

46 675 

81838 

01.01.2006–31.12.2006 

179 089 

5 00 

4 6 3 

188 912 

49 734 

63 648 

113 382 

75 530 

01.01.2006–31.12.2006 

188 91 

–55 443 

133469 

–113 38 

–14140 

–127522 

5 947 

6 395 

12 342 

Budget for 2007 

(in € 1000) 

Income budget 

Contributions from member states 

Other income from member states 

Income from third parties 

Various income 

Total income budget 

Payment budget 

Personnel cost 

Other cost 

Total payment budget 

Commitment budget 

Personnel cost 

Projects commitments without personnel 

Operations commitments without personnel 

Total commitment budget 


2007 

117 73 

4 388 

1 014 

4 000 

138134 

2007 

51170 

149 7 8 

200 898 

2007 

51170 

158 09 

37 61 

246 640 

Since 003, the ESO annual accounts have shown a positive cash flow 

development, which is reflected in the amount of cash and short-term deposits at 

end of year. In 006, the positive cash flow amounted to 1 ,3 M€ and the cash 

and short-term deposits as of 31 December 006 amounted to 89, M€. 

The net result of the statement of income and expenditure for 006 was 

+ 75,5 M€. The high income figure of 188,9 M€ included in particular the amount 

of the entrance fee due by Spain following the country’s accession as a new 

ESO member state as of 1 July 006. 

The budget for 007 was approved by the ESO Council in December 006. 

The budget comprises three sections: the income budget, the payment budget 

and the commitment budget. 

With 00,9 M€, the 007 payment budget is driven by the payment profile of 

the ALMA project. It also includes a provision for the detail design phase of the 

European ELT. In total, it is expected to be significantly higher than the 007 

income budget, which amounts to 138,1 M€. 

The commitment budget for 007 is 46,6 M€. 

105

Four Seasons at a Glance 

January 

First Light for the Laser Guide Star on 

UT4 of the VLT. 

Astronomers find 5 Earth-mass exoplanet 

with microlensing technique, using a 

worldwide network of telescopes, including 

the 1.5-m telescope at La Silla. 

Meeting of the Scientific Strategy Working 

Group. 

15th release of the VLT Software. 

Workshop on ALMA (From Z-Machines 

to ALMA: (Sub)millimeter Spectroscopy of 

Galaxies), NRAO Charlottesville. 

ALMA European Science Advisory Committee 

meeting, Garching. 

ALMA Science Advisory Committee 

meets in Washington, US. 

February 

Signing of the agreement between Spain 

and ESO about membership. 

Committee of Council meets in Berne, 

Switzerland. 

Breakfast press briefing for the UK media 

in connection with the yearly Astrofest 

in London, organised by ESO and PPARC. 

ESO is also present at the Astrofest 

with a scale model of the VLT and display 

panels. 

ESO is present at the annual AAAS meeting 

in St. Louis, Missouri. 

Yearly ESO Status Overwiew held in 

Garching. 

106 


March 

Visit to the ESO HQ by the Education 

Committee of the Finnish Parliament. 

Walloon Space Days in Liège and delivery 

ceremony for the 4th VLT Auxiliary Telescope 

at AMOS, Belgium. 

Launch of the first international, multidisciplinary 

journal for innovative science 

teaching, “Science in School”, by 

EIROforum at EMBL in Heidelberg. 

Joint ESO-FONDAP Workshop on Globular 

Clusters, Concepción, Chile. 

European ALMA Board meets in Garching. 

ALMA Board meeting, Kyoto, Japan. 

Extraordinary Finance Committee in 

Garching. 

Danish Minister of Education, Bertel 

Haarder, visits Paranel. 

April 

Preliminary Acceptance Europe review of 

CRIRES. 

8 7 proposals are received in answer 

to the Call for Proposals for observing in 

Period 78. 

CRIRES AO system (MACAO) installed 

and commissioned at UT1. 

An image made of about 300 million pixels 

is released by ESO, based on more 

than 64 hours of observations with the 

Wide-Field Imager on the . -m telescope 

at La Silla. 

VLT observes fragment B of the comet 

Schwassmann-Wachmann 3, that had 

split a few days earlier. 

Meeting of the Scientific Strategy Working 

Group. 

6 nd Meeting of the Scientific Technical 

Committee. 

The Users’ Committee meets in Garching. 

Meeting of the ESO Tripartite Group. 

Opening of the IPP/ESO Crèche. 

May 

HARPS helps discover a nearby star 

hosting three Neptune-mass planets. 

Strong ESO participation at the SPIE 

Astronomical Telescopes and Instrumentation 

Symposium in Orlando, Florida. 

First recoating of M of UT1 successfully 

completed. 

114th Finance Committee Meeting in 

Garching. 

Extraordinary 63rd meeting of the 

Scientific Technical Committee. 

European ALMA Board meeting, Garching. 

Public Survey Panel meets in Garching. 

Workshop on “Complex Molecules 

in Space: Present status and prospects 

with ALMA”, Fuglsøcentret, Denmark.

June 

First spectra on-sky obtained by CRIRES 

on the VLT. 

ESO establishes a dedicated E-ELT 

Project Office. 

X-shooter passes Final Design Review in 

Europe. 

The ESO Council meets in Garching. 

ALMA Board meeting, Santiago, Chile. 

Signing of the ALMA agreement with 

Japan. 

Observing Programmes Committee 

meeting in Garching. 

ESO and the Government of Chile launch 

the book “10 Years Exploring the Universe”, 

written by the beneficiaries of the 

ESO-Government of Chile Joint Committee. 

Public Survey Panel meets in Edinburgh, 

UK. 

ESO participates with a major information 

stand at the nd Salon Européen de 

la Recherche & de l’Innovation in Paris, 

France. 

EuroSummer School, Observation and 

data reduction with the Very Large 

Telescope Interferometer, Château de 

Goutelas, France. 

Conference “Library and Information 

Services in Astronomy V: Common Challenges, 

Uncommon Solutions”, Cambridge, 

Mass., USA. 

July 

6 articles based on early science 

with APEX are published in the research 

journal Astronomy & Astrophysics. 

The first of seven years of data of 

the UKIRT Infrared Deep Sky Survey 

(UKIDSS) enters ESO’s archive. 

The Fifth NEON Observing School, 

Observatoire de Haute-Provence, France. 

EIROforum takes part in the Euroscience 

Open Forum 006 Conference in 

Munich with a major information stand, 

press conferences and a reception. 

ESO is also visible in the German Science 

Festival with an on-stage show at 

Munich’s Marienplatz, involving a live 

videoconference with Paranal. 

August 

The new SINFONI spectrograph scrutinises 

a distant protodisc galaxy with a 

record-breaking resolution of a mere 0.15 

arcseconds. 

Provisional Design Review for the ALMA 

Transporter. 

“Heating vs. Cooling in Galaxies and 

Clusters of Galaxies”, MPA/ESO/MPE/ 

USM Joint Astronomy Conference, 

Garching, Germany. 

The Second NEON Archive Observing 

School takes place at ESO. 

ESO is present at the IAU XXVIth General 

Assembly in Prague with presentations 

and information stands. ESO’s 

Director General Catherine Cesarsky 

is elected President of the International 

Astronomical Union while ESO’s 

Deputy Director General Ian Corbett is 

elected Assistant General Secretary 

September 

Thomas Wilson is appointed as ESO’s 

Associate Director. 

Committee of Council meets in Santiago, 

Chile. 

ALMA European Science Advisory Committee 

meeting, Garching. 

ALMA Science Advisory Committee 

meets in Florence, Italy. 

Joint ESO-Lisbon-Aveiro University 

Conference on Precision Spectroscopy in 

Astrophysics, Aveiro, Portugal. 

October 

KMOS passes Preliminary Design Review. 

913 proposals are received in answer 

to the Call for Proposals for observing in 

Period 79, a new all-time record. 

DAZLE visitor instrument successfully 

commissioned on UT3. 

UT4 recoating of M1/M3 completed. 


107

Visit to the ESO Headquarters by a group 

of university rectors from Chile. 

Committee of Council meets in Munich. 

ESO exhibition at major astronomy festival 

in Vaulx-en-Velin, France. 

ESO exhibition in Montpellier, France. 

64th Meeting of the Scientific Technical 

Committee. 

Extraordinary Finance Committee in 

Garching. 

Public Survey Panel meets in Garching. 

ALMA Commissioning meeting. 

Meeting of the ESO Tripartite Group. 

UNAWE Workshop in Leiden, the 

Netherlands. 

Almost 3000 people visit the ESO HQ 

at the Open House. On that occasion 

ESO together with other institutes on the 

Garching campus, receives the “Deutschland 

– Land der Ideen” Trophy for its 

public communication activities. 

ESO releases its 007 Calendar. 

November 

Visit to Paranal by a delegation from the 

Academy of Sciences of the Czech 

Republic. 

More than 50 European astronomers 

gather at the ‘Towards the European ELT’ 

conference in Marseille, France. 

International ALMA Conference on 

“Science with ALMA: a new era for Astrophysics”, 

held in Madrid, Spain. 

108 


European Extremely Large Telescope is 

selected in the European Strategy Forum 

on Research Infrastructures (ESFRI) 

Roadmap. 

EIROforum breakfast meeting at the 

European Parliament discusses science 

education issues in Europe. 

ESO and the European Association 

for Astronomy Education launch the 007 

edition of ‘Catch a Star!’, their international 

astronomy competition for school 

students. 

The Finance Committee (116th) meets in 

Garching. 

ALMA board meets in Madrid, Spain. 

Extraordinary 65th meeting of the 

Scientific Technical Committee. 

Observing Programmes Committee 

meeting in Garching. 

EIROforum Assembly in Grenoble, 

France. 

A top-level meeting on exoplanets takes 

place in Washington D.C. between ESO, 

ESA and NASA. 

December 

ESO participates at major astronomy and 

space exhibition, Astro-expo, in Dublin, 

Ireland. 

The ESO Council meets in Garching. 

Council decides to proceed with Phase B 

studies for the European Extremely 

Large Telescope. Council also approves 

the Agreement with the Czech Republic 

about membership. 

Fourth and last-to-be-installed VLTI Auxiliary 

Telescope (AT4) obtains its ‘First 

Light’. 

EIROforum issues statement of support 

for the European Charter for Researchers 

and the Code of Conduct for the Recruitment 

of Researchers. 

ESO releases 56 million pixel image of 

30 Doradus. 

UT recoating of M1/M3 completed. 

Laser Guide Star Facility on VLT successfully 

commissioned. 

The Multi-conjugate Adaptive optics 

Demonstrator (MAD) passes its PAE 

(Preliminary Acceptance Europe). 

Fourth Advanced Chilean School of Astrophysics 

(co-sponsored by ESO), 

“Interferometry in the Epoch of ALMA and 

VLTI”, P. Universidad Católica de Chile, 

Santiago, Chile. 

Signing Ceremony in Prague of the 

Agreement between ESO and the Czech 

Republic regarding Czech membership of 

ESO.

Glossary of Frequently Used Acronyms 

4LGSF Four-Laser Guide Star Facility 

AAAS American Association for the 

Advancement of Science 

A&A Journal “Astronomy & Astrophysics” 

ACS Advanced Camera for Surveys (HST) 

ACS ALMA Common Software 

ADP Advanced Data Products (VOS) 

AEM Alcatel Alenia Space France, Alcatel 

Alenia Space Italy, European Industrial 

Engineering s.r.L., MT 

Aerospace Consortium (ALMA) 

ALMA Atacama Large Millimeter/Submilli- 

meter Array 

ALMA ARC ALMA Regional Centre 

AMBER Astronomical Multi-BEam combineR 

(VLTI Instrument) 

ANSYS ANSYS Multiphysics, general- 

purpose finite element analysis 

software 

AO Adaptive Optics 

AOF Adaptive Optics Facility 

AOS Array Operations Site 

APEX Atacama Pathfinder Experiment 

ASAC ALMA Science Advisory Committee 

ASI Italian Space Agency (Agenzia 

Spaziale Italiana) 

ASSIST Adaptive Secondary Setup and 

Instrument Simulator 

AT Auxiliary Telescope for the VLTI 

AVO Astrophysical Virtual Observatory 

BMBF German Federal Ministry for Education 

and Research 

CADC Canadian Astronomy Data Centre 

CAS Academy of Sciences of the Czech 

Republic 

CCD Charge-Coupled Device 

CES Coudé Echelle Spectrometer (3.6-m) 

CERN European Organisation for Nuclear 

Research (Conseil Européen pour la 

Recherche Nucléaire, Switzerland) 

CDR Conceptual Design Review 

CFD Computational Fluid Dynamics 

CI corporate identity 

CMMS computerised maintenance management 

system 

CNRS Centre National de la Recherche 

Scientifique (France) 

CRIRES Cryogenic InfraRed Echelle Spectrometer 

(VLT) 

CSIC Spanish National Research Council 

(Consejo Superior de Investigaciones 

Científicas) 

darkCAM dark energy camera for VISTA 

DAZLE Dark Age ‘Z’ Lyman-alpha Explorer 

DBCM Database Content Management 

DCA EURO-VO Data Centre Alliance 

DCU Dublin City University 

DFO Data Flow Operations 

DMD Data Management Division 

DMO Data Management and Operations 

Division 

DRM Design Reference Mission 

DSM Deformable Secondary Mirror 

EAAE European Association for Astronomy 

Education 

EFOSC ESO Faint Object Spectrograph and 

Camera (3.6-m) 

EIS ESO Imaging Survey 

ELT Extremely Large Telescope 

E-ELT European Extremely Large Telescope 

EMC Electromagnetic Compatibility 

EMMI ESO Multi-Mode Instrument (NTT) 

110 


ERA-net European Research Area Network 

ESA European Space Agency 

ESAC European Science Advisory Committee 

(for ALMA) 

ESE ELT Science and Engineering 

ESFRI European Strategy Forum on/for 

Research Infrastructures 

ESRC ELT Standing Review Committee 

ESRIN ESA Centre for Earth Observations 

ESTI EIROforum European Science 

Teachers’ Initiative 

EURO-VO European Virtual Observatory 

FDR Final Design Review 

FE Front End 

FEIC Front End Integration Centres 

FEM Finite Element Method 

FEROS Fibre-fed, Extended Range, Échelle 

Spectrograph ( . -m) 

FINITO Fringe Tracking Instrument Nice 

Torino (VLTI) 

FLAMES Fibre Large Array Multi Element 

Spectrograph (VLT) 

FOC Faint Object Camera 

FORS FOcal Reducer/low dispersion 

Spectrograph 

FP Framework Programme 

FP6 Sixth Framework Programme 

FP7 Seventh Framework Programme 

GALACSI Ground Atmospheric Layer Adaptive 

Optics for Spectroscopic Imaging 

GENIE Ground based European Nulling 

Interferometer Experiment (VLTI) 

GHRS Goddard High-Resolution Spectrograph 

GRAAL GRound-layer Adaptive opctics 

Assisted by Lasers 

GRAVITY AO assisted, two-object, multiplebeam-combiner 

(VLTI) 

GRB Gamma-Ray Burst 

GROND Gamma-Ray burst Optical/Nearinfrared 

Detector 

HARPS High Accuracy Radial Velocity 

Planetary Searcher (3.6-m) 

HAWK-I High Acuity Wide field K-band 

Imager (VLT) 

HLA Hubble Legacy Archive 

HOT High Order Test-bench 

HST Hubble Space Telescope 

IAU International Astronomical Union 

ICD Interface Control Document 

IEM Instituto de Estructura de la Materia 

(Madrid, Spain) 

INAF Istituto Nazionale di Astrofisica (Italy) 

INSU Institut National des Sciences de 

l’Univers (France) 

INTA Instituto Nacional de Tecnica Aeroespacial 

(Spain) 

IPP Max-Planck-Institut für Plasmaphysik 

IPT Integrated Project Team (ALMA) 

IR InfraRed 

IRAM Institut de Radioastronomie Millimétrique 

(France) 

ISAAC Infrared Spectrometer And Array 

Camera (VLT) 

IT Information Technology 

ITF Interferometry Task Force 

ITRE European Parliament’s Committee 

on Industry, Research and Energy 

IVOA International Virtual Observatory 

Alliance 

JBO Jodrell Bank Observatory (UK) 

KMOS K-band multi-object spectrograph 

(VLT) 

LABOCA Large APEX Bolometer CAmera 

LAOG Laboratoire d’Astrophysique de 

Grenoble 

LERMA Laboratoire d’Étude du Rayonnement 

et de la Matière en Astrophysique 

(France) 

LGS Laser Guide Star 

LGSF Laser Guide Star Facility 

LP Large Programme 

LTP Long Term Perspectives 

MACAO Multi-Application Curvature Adaptive 

Optics (VLT/VLTI) 

MAD Multi-Conjugate Adaptive Optics 

Demonstrator 

MATISSE Multi AperTure mid-Infrared 

SpectroScopic Experiment (VLTI) 

MEC Minsitry of Education and Science 

(Ministerio de Educación y Ciencia, 

Spain) 

MIDI Mid-Infrared Interferometric 

Instrument (VLTI Instrument) 

MoU Memorandum of Understanding 

MPE Max Planck Institute for Extraterrestrial 

Physics (Germany) 

MPIfR Max Planck Institute for Radioastronomy 

(Germany) 

MRIP Medium Range Implementation Plan 

MUSE Multi Unit Spectroscopic Explorer 

(VLT) 

MVM Image processing library 

NACO NAOS-CONICA (VLT) 

NAOJ National Astronomical Observatory 

of Japan 

NAOS Nasmyth Adaptive Optics System 

(VLT) 

NASA National Air and Space Administration 

(US) 

NGAS Next Generation Archiving System 

NGC New General detector Controller 

NICMOS Near Infrared Camera and 

Multi-Object Spectrograph (HST) 

NIST National Institute of STandards 

NOTSA Nordic Optical Telescope Scientific 

Association 

NOVA Dutch Research School for Astronomy 

(Nederlandse Onderzoekschool 

voor Astronomie) 

NSF National Science Foundation 

NTT New Technology Telescope 

OmegaCAM Optical Camera for the VST 

OPC Observing Programmes Committee 

OPD Optical Path Differences 

OPTICON Optical Infrared Coordination 

Network for Astronomy 

OSF Operations Support Facility (ALMA) 

OSO Onsala Space Observatory 

OWL OverWhelmingly Large Telescope 

P PP Phase Preparation Tool 

P75 Period 75 

P76 Period 76 

P77 Period 77 

P78 Period 78 

P79 Period 79 

PAD Public Affairs Department 

PAE Preliminary Acceptance Europe 

PARSEC Sodium line laser for VLT AO 

PDM Product Data Management 

PDR Preliminary Design Review 

PI Principal Investigator 

PPARC Particle Physics and Astronomy 

Research Council (UK)

PRIMA Phase-Referenced Imaging and 

Micro-arcsecond Astrometry facility 

(VLTI) 

PSP Public Survey Panel 

QC Quality Control 

R&D Research and Development 

RADIONET Radio Astronomy Network in Europe 

RDS Rat Deutscher Sternwarten 

(Germany) 

RoHS Restriction on the use of Hazardous 

Substances 

RRM Rapid-Response Mode 

SAC EURO-VO Science Advisory Committee 

SAF Science Archive Facility 

SAO Science Archive Operation 

SEI System Engineering and Integration 

SINFONI Spectrograph for INtegral Field 

Observations in the Near Infrared 

SMI Structural Modelling Interface 

SMA SubilliMeter Array 

SOCHIAS Chilean Astronomical Society 

SOFI SOn oF Isaac (NTT) 

SPHERE Spectro-Polarimetric High-contrast 

Exoplanet Research instrument 

SPIE International Society for Optical 

Engineering 

SSWG Scientific Strategy Planning Working 

Group 

STC Scientific Technical Committee 

ST-ECF Space Telescope European 

Coordination Facility 

STIS Slit spectrograph (HST) 

STScI Space Telescope Science Institute 

(USA) 

SUSI SUperb Seeing Imager (NTT) 

TAC Time Allocation Committee 

TB TeraBytes 

TFB Turnable Filter Bank 

TIMMI Thermal Infrared MultiMode 

Instrument (3.6-m) 

TMT Thirty Meter Telescope 

ToO Target of Opportunity 

UC Users’ Committee 

UK United Kingdom 

UKIDSS UKIRT Infrared Deep Sky Survey 

UKIRT UK Infrared Telescope 

ULTRACAM ULTRA-fast, triple-beam CCD 

CAMera 

USD User Support Department 

UT1–4 VLT Unit Telescope 1–4: Antu, 

Kueyen, Melipal and Yepun 

UVES UV-Visual Echelle Spectrograph 

(VLT) 

VCM Variable Curvature Mirrors 

VIMOS VIsible MultiObject Spectrograph 

(VLT) 

VINCI VLT INterferometer Commissionning 

Instrument 

VIRCAM VISTA IR Camera 

VISA VLTI Sub-Array 

VISIR VLT Mid-Infrared Imager Spectrometer 

VISTA Visible and Infrared Survey 

Telescope for Astronomy 

VITRUV Near-IR spectro-imager using fibre 

(VLTI) 

VLT Very Large Telescope 

VLTI Very Large Telescope Interferometer 

VO Virtual Observatory 

VOFC EURO-VO Facility Centre 

VOS Virtual Observatory System 

VOTC EURO-VO Technology Centre 

VSI VLTI Spectro Imager 

VST VLT Survey Telescope 

VTK Vibration Tracking 

VVDS VIMOS VLT Deep Survey 

WFCAM Wide-Field Camera (UKIDSS) 

WFI Wide Field Imager ( . -m) 

X-Shooter Wideband UV-IR single target 

spectrograph (VLT) 


111

ESO Europe 

Headquarters 

Karl-Schwarzschild-Straße 

85748 Garching bei München 

Germany 

Phone +49 89 3 0 06 -0 

Direct lines 

Director General - 6 

Visiting Astronomers -553/473 

Science Office - 9/ 86 

Technology Division - 58 

Data Management Division -69 

Public Affairs Department - 76 

Instrumentation Division -506 

Telescope Division -347 

Administration - 38 

Fax +49 89 3 0 3 6 

www.eso.org 

ESO Chile 


La Silla Site 

IV Región 

Chile 

Phone +56 464 4100 

Fax +56 464 4101 


Paranal Site 

II Región 

Chile 

Phone +56 55 43 5100 

Fax +56 55 43 5101 

APEX Radio Observatory 

Séquitor 

II Región 

Chile 

Phone +56 55 44 8 00 

Fax +56 55 44 8 1 

Santiago Office 

Alonso de Córdova 3107 

Vitacura 

Casilla 19001 

Santiago de Chile 19 

Chile 

Phone +5 6 463 3100 

Fax +5 6 463 3101 

11 


La Serena Office 

Avenida El Santo 1538 

Casilla 567 

La Serena 

Chile 

Phone +56 51 53 87 

Fax +56 51 15175 

Guest House 

Rey Gustavo Adolfo 4634 

Las Condes 

Santiago de Chile 

Chile 

Phone +56 08 4 54 

Fax +56 8 93 33 

Antofagasta Office 

Avenida Balmaceda 536 

Office 504 

Edificio ‘Don Guillermo’ 

Antofagasta 

Chile 

Phone +56 55 6 00 3 

Fax +56 55 6 00 81 

ESO is a partner in the international 

ALMA project 

ALMA Office San Pedro de Atacama 

Kilómetro 1 1 CH 3 

II Región 

Chile 

Phone +56 55 44 8416 

Fax +56 55 44 84 81 

ALMA Office Santiago 

El Golf 40, Piso 18 

Las Condes 

Santiago de Chile 

Chile 

Phone +56 4676100 

Fax +56 4676101 

DVD (Mac/PC and DVD Player) 

The ESO Annual Report 006 DVD 

contains two parts. It should play 

automatically when inserted in any DVD 

player, featuring a set of videos made by 

ESO. 

In addition, on a Mac or a PC, it is 

possible to open it to access additional 

content: 

– All the ESO Press Releases and Press 

Photos having been published in 006. 

– The four Messenger issues of 006. 

– The list of all publications based on ESO 

telescopes that appeared in 006. 

– A gallery of photos. 

To access these features, simply view the 

index.html file in your favourite browser. 

All images are copyright ESO except 

where otherwise indicated. 

Produced by the 

Public Affairs Department 

© ESO 007 

ISSN 0531-4496 

Back cover photo: 

The Laser Guide Stars System at Paranal.


113

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