ESO
European Organisation for Astronomical Research in the Southern Hemisphere
Annual Report 2008
presented to the Council by the Director General Prof. Tim de Zeeuw The European Southern Observatory
ESO, the European Southern Observatory, is the foremost intergovernmental as tronomy organisation in Europe. It is sup ported by 14 countries: Austria, Belgium, the Czech Republic, Denmark, France, Finland, Germany, Italy, the Netherlands, Portugal, Spain, Sweden, Switzerland and the United Kingdom. Several other countries have expressed an interest in membership.
Created in 1962, ESO carries out an am bitious programme focused on the de sign, construction and operation of pow erful ground-based observing facilities enabling astronomers to make important scientific discoveries. ESO also plays a leading role in promoting and organising cooperation in astronomical research.
ESO operates three unique world-class observing sites in the Atacama Desert ESO’s first site at La Silla. region of Chile: La Silla, Paranal and Chajnantor. ESO’s first site is at La Silla, One of the most exciting features of the Each year, about 2000 proposals are a 2400 m high mountain 600 km north VLT is the option to use it as a giant opti made for the use of ESO telescopes, re of Santiago de Chile. It is equipped with cal interferometer (VLT Interferometer or questing between four and six times several optical telescopes with mirror VLTI). This is done by combining the light more nights than are available. ESO is the diameters of up to 3.6 metres. The from several of the telescopes, including most productive ground-based observa 3.5-metre New Technology Telescope one or more of four 1.8-metre moveable tory in the world, which annually results broke new ground for telescope engineer Auxiliary Telescopes. In this interferomet in many peer-reviewed publications: in ing and design and was the first in the ric mode, the telescope has a vision as 2008 alone, 700 refereed papers based world to have a computer-controlled main sharp as that of a telescope the size of on ESO data were published. mirror, a technology developed at ESO the separation between the most distant and now applied to most of the world’s mirrors. For the VLTI, this is 200 metres. current large telescopes. While La Silla As soon as the Sun has set the telescopes are remains at the forefront of astronomy, and pointed to the first sky objects to be observed that night. remains among the most scientifically productive in ground-based astronomy, the 2600 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 Antofa gasta in Chile, 12 km inland from the Pa cific coast in one of the driest areas in the world. Scientific operations began in 1999 and have resulted in many extremely suc cessful 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 8.2 metres in diameter. With one such telescope, im ages of celestial objects as faint as mag nitude 30 have been obtained in a one- hour exposure. This corresponds to seeing objects that are four billion times fainter than those seen with the naked eye.
2 ESO Annual Report 2008 The Atacama Large Millimeter/submil A view towards the west of limeter Array (ALMA), the largest ground- the Japanese ALMA antenna and the Operational Support based astronomy project in existence, Facility at sunset. is a revolutionary facility for world astron omy. ALMA will comprise an array of 66 giant 12-metre and 7-metre diameter antennas observing at millimetre and submillimetre wavelengths. Construction of ALMA began in 2003 and it will start scientific observations in 2011. ALMA is located on the high altitude Llano de Chajnantor, at 5000 m elevation. The ALMA project is a partnership between Europe, East Asia and North America, in cooperation with the Republic of Chile. ESO is the European partner in ALMA.
The Chajnantor site is also home to the 12-metre APEX millimetre and submillime tre telescope, operated by ESO on behalf of the Onsala Space Observatory, the Max Planck Institute for Radio Astronomy and ESO itself.
The next step beyond the VLT is to build the European Extremely Large optical/ infrared Telescope (E-ELT) with a primary mirror 42 metres in diameter. The E-ELT An artist’s impression of the will be “the biggest eye on the sky” — the E-ELT mirror in close-up. largest optical/near-infrared telescope in the world and ESO is drawing up detailed construction plans, together with the scientific community in its member states. The E-ELT will address many of the most pressing unsolved questions in astron omy. It may, eventually, revolutionise our perception of the Universe, much as Galileo’s telescope did, 400 years ago. The go-ahead for construction is expected in late 2010, with the start of operations planned for 2018.
The ESO Headquarters are located in Garching, near Munich, Germany. This is the scientific, technical and administra- tive centre of ESO where technical devel opment programmes are carried out to provide the observatories with the most advanced instruments. It is also home for the Space Telescope — European Co ordinating Facility, operated jointly by ESO and the European Space Agency.
The annual member state contributions to ESO are approximately 135 million € and ESO employs around 700 staff.
ESO Annual Report 2008 3
Contents
The European Southern Observatory 2 Foreword 6 Introduction 7 Science 10 Research Highlights 11 Allocation of Telescope Time 20 Outreach 22 Operations 30 La Silla Paranal Observatory 31 Data Management and Operations Division 40 ST-ECF 47 Programmes 50 European Extremely Large Telescope 51 Survey Telescopes 54 Instrumentation for the La Silla Paranal Observatory 56 Technology Developments 64 ALMA 66 Software Development 78 Administration 84 Finance and Budget 86 Human Resources 88 List of Staff 92 Organigram 97 Committees 98 Council 99 Finance Committee 100 Scientific Technical Committee 101 Observing Programmes Committee 103 Users Committee 105 International Relations 108 Chile Relations 110 Four Seasons at a Glance 112 Publications 119 Glossary of Acronyms 142
ESO Annual Report 2008 5 Foreword
One of the most important achievements In this situation, the European Astronomy for ESO in 2008 has been the new man Infrastructure Roadmap, prepared by agement organisation, put in place by ASTRONET, is a very strong signal in the ESO Director General. With the crea favour of the E-ELT. For the first time, the tion of four main directorates, ESO man whole European astronomical community agement now has a new configuration, has defined its priorities for new infra tailored to meet the challenges that ESO structures, taking a comprehensive view, faces today: operating Paranal and La considering space-borne and ground- Silla, completing ALMA and preparing for based observatories, and covering the the E-ELT. In addition to these challeng entire electromagnetic spectrum from ing programmes, ESO is also increasingly gamma rays to radio astronomy. ESO, becoming the leading organisation for with its VLT, VLTI and ALMA has been astronomy in Europe, as the number of recognised as a key part of this future, member states has grown continuously. and the ASTRONET Roadmap identifies In the near future, ESO may play the the E-ELT as a top priority, acknowl same role for European astronomy that edging that everything is being put in CERN does for particle physics. The re place to enable a rapid decision. This structured management should help ESO should help in the decision process, and to fulfil the important task of supporting ESO should continue to work with the the European astronomy community in ASTRONET funding agencies on the the best possible way. Roadmap implementation.
In this short foreword it is impossible The fact that several European countries to give proper credit to all the outstanding who are not yet members of ESO have scientific and technical results obtained expressed an interest in joining ESO in with ESO telescopes. This report high the near future is also a sign of the vitality lights some of them, but it is, of course, and attractiveness of the organisation. just a small fraction of the many important We have been very pleased with the ac research projects carried out over the cession of Austria, recognising the addi year. European astronomers recognise the tional strength that it will bring to the importance of the facilities offered by organisation. ESO to maintain their position at the fore front of astronomical research. Over the recent years, ESO has been able to maintain a prominent role as an ESO’s continued success demonstrates observatory, while actively pursuing new what can be achieved when countries and ambitious projects like the second decide to join together in a common effort. generation instruments for the VLT/VLTI, ESO can, and indeed should, deal with ALMA and the design studies for the projects that exceed the capability of indi E-ELT. This has been achieved through vidual member states, but for this to hap the immense dedication of the whole ESO pen, the support of the member states staff, and the commitment of the Direc must remain at the highest level. This was tors General. A good relationship be true for the VLT; it should be the same for tween the Council and the ESO manage the next large endeavour, the European ment has also been key to this success. Extremely Large Telescope. It will be a I would like to thank the previous Council challenging project in every respect: tech President, Richard Wade, for his work nically, programmatically and politically. during the last three years, which has Design studies, and the manufacturing of been very helpful in maintaining this col key subsystem prototypes have made laborative spirit among the member great progress in 2008, and there are very states and with the organisation. good prospects that the end of this design phase will be completed by mid-2010. But, even if member states express their good will for this project, there is still a long way to go before achieving the final agreement to start construction, including securing its funding. The next two years President of the ESO Council are crucial for a timely start. Dr. Laurent Vigroux
6 ESO Annual Report 2008 Introduction
The year 2008 saw much progress on all Operations aspects of ESO’s ambitious programme, including major scientific discoveries, de The month of May marked ten years livery of new telescopes and instrumenta since First Light at the VLT, followed by tion and continued strong support from the first Call for VLT (UT1+FORS1/ISAAC) the member states. Proposals in Period 63 issued in Septem ber 1998. The complete first generation infrastructure of VLT/VLTI is operational, New member states the first second generation instrument, X-shooter, has already been installed, In June, Austria signed the accession PRIMA is being commissioned as the next agreement, successfully concluding large VLTI infrastructure, and Paranal jus a courtship which commenced more than tifiably prides itself on achieving a world- three decades ago. Austria will become leading on-sky efficiency. ESO’s 14th member state upon comple tion of the ratification procedure. It is a A special event occurred in March, when pleasure to welcome the Austrian scientific the filming of the climactic ending of the community to ESO, and I look forward latest James Bond movie, Quantum of to an active Austrian contribution to ESO’s Solace, took place on Paranal. While the entire programme. In view of the expected telescopes do not feature in the movie, ALMA further expansion of ESO’s programme, the cinematic destruction of the Residen Council adopted a new policy for candi cia was seen all over the world, and the ESO represents Europe in the construc date member states, which includes whole event generated much publicity for tion of the Atacama Large Millimeter/ the possibility of non-European member ESO. submillimeter Array on the Chajnantor states. plateau in northern Chile. ALMA is a global astronomy project carried out in VLT instrumentation developments partnership with North America and Science East Asia. ESO is responsible for the front There was good progress on the other ends, antennas, roads, power supply, The demand on ESO telescopes contin second generation instruments KMOS, and various buildings. In the past year ues to increase, with 925 (Period 82) and MUSE, SPHERE, GRAVITY and MATISSE, the giant Technical Building at the Ob 961 (Period 83) proposals submitted. No and on the VLT Adaptive Optics Facility. servatory Support Facility south of San other observatory provides data for more Pedro de Atacama was completed. refereed publications than ESO. High The custom-built antenna transporters lights of the past year include the accu Survey telescopes now routinely move antennas in Chile. rate measurement of the motions of many stars orbiting the supermassive black The M1 and M2 mirror units for the VLT The year also saw a change in leadership hole at the Galactic Centre based on 16 Survey Telescope (VST) were com- at ALMA. After five years of dedicated years of observations with telescopes on pleted in Italy, and will be installed during service Massimo Tarenghi stepped down La Silla and Paranal; the first VLTI high 2009. The wide-field camera OmegaCAM, as ALMA Director. Thijs de Graauw suc resolution survey with AMBER of interme which had been in storage at ESO ceeds him. diate-mass infant stars; a remarkable Headquarters, has also been shipped spectro-astrometric study of protoplane to Paranal. The primary mirror of VISTA tary discs with CRIRES; direct imaging finally arrived on Paranal, by coincidence European Extremely Large Telescope of a planet in the debris disc surrounding right in the middle of the shooting of the star Beta Pictoris; study of the cold Quantum of Solace, and the telescope The design study for the European gas in star-forming regions with LABOCA achieved first light in mid-year. As the Extremely Large Telescope (E-ELT) made on APEX; the deepest-ever ground-based year ended, the commissioning of VISTA excellent progress in its second year, U-band image of the Universe obtained continued, but the hope is that regular in close cooperation with industry. The ac with VIMOS; and a stunning picture of survey operations can start late in 2009. tivity includes the Active Phasing Experi Jupiter taken by MAD. ment on the VLT, intended to characterise four different methods of phasing a seg mented mirror.
ESO Annual Report 2008 7 The E-ELT is not only the highest priority Headquarters building extension new programme for ESO, it is also the highest priority near-term project for In December the ESO Council approved ground-based astronomy identified in the the selection of the Auer & Weber con ASTRONET Infrastructure Roadmap, and ceptual design for the planned Headquar it is one of only two astronomy projects on ters extension. It will consist of an Office the high-profile ESFRI list of research infra Building, which includes a new auditorium structures. The ESO Council is actively and a new Council room, and a separate engaged in the development of a funding Technical Building, both connected to the scenario that will make this possible. existing building. When completed, the new signature Headquarters will house all ESO personnel in Garching. Organisation
Early in the year a new management structure was implemented with four main directorates — for Science, Operations, Programmes and ALMA, as well as “cross-directorate” services (Administra Prof. Tim de Zeeuw tion, Software Development, Human ESO Director General Resources). A single IT Department, con sisting of two groups, one in Chile and one in Garching was created within the Software Development Division. It pro The Orion Nebula. vides IT services to the whole organisa tion. The Observing Programmes Office, formerly known as the Visiting Astrono mers Section, the programme scientists and the Outreach Department were transferred from the Office of the Director General (ODG) to the Directorate for Science and the ODG was augmented by the International Relations Office and the Legal Service.
This year the roles of the ESO science- related committees were clarified and re- focused. Council approved new terms of reference for the Scientific Technical Committee (STC) and its three subcom mittees, the La Silla Paranal Committee (LSP), the European Science Advisory Committee (ESAC) for ALMA, and the ELT Science and Engineering Committee (ESE). With the help of a Finance Com mittee Working Group, new Financial Rules and Regulations are being prepared which include the adoption of IPSAS (International Public Sector Accounting Standards) for financial management.
8 ESO Annual Report 2008 Aerial view of the ESO Headquarters in Garching. Science
The Chandra Deep Field South. Research Highlights
The La Silla Paranal Observatory contin As in previous years, the scientific high and the collective of the Milky Way. ESO ues to be the most productive astronomi lights range across the whole Universe, telescopes have also observed out to cal facility in the world. The number of with new results on Solar System ob the far reaches in the Universe, detecting refereed publications per year based on jects, nearby stars, their dust discs and molecules at an early phase of the data from ESO telescopes is larger than their planets, interstellar gas Universe. from any other astronomical organisation. There were 706 publications in refereed journals in 2008, with a marked increase in papers based on APEX observations. The impact of these publications remains high, and above average for the astron omy community in general, demonstrat ing that ESO telescopes make significant contributions to the understanding of the Universe and its components. The most prolific instruments remain FORS1 and FORS2, together with UVES and ISAAC, the four original instruments on the VLT. They are followed by the newer instruments NACO, VIMOS and FLAMES, which are exploring specific observational niches. The most recent additions to the instrument complement are all still in the initial data-gathering phase and will produce their publications in due course. The same is true for the VLTI instruments AMBER and MIDI, which are beginning to contribute their fair share to the publi cations list.
ESO has continued its successful fellow ship and studentship programmes in Garching and Chile. Many of the post doctoral fellows have moved on to prestig The technique of Adaptive Optics (AO) removes at two different altitudes. ESO’s Multi-conjugate ious positions in astronomy. A recent sur the blurring introduced into astronomical images by Adaptive-optics Demonstrator (MAD) was so suc turbulence in the Earth’s atmosphere. The method cessful that it was opened to proposals from the vey indicated that 92% of all fellows in was pioneered at the 3.6-metre telescope on La Silla community in Science Demonstration mode for a Garching (this programme started in 1976) more than 20 years ago, and today is a standard total of 23 nights at the visitor focus of UT3. A team are still working as research astronomers. tool, used in essentially all the large ground-based of astronomers from the University of Berkeley no The number of applications to this pro telescopes in the world. The major drawbacks of AO ticed that during the third MAD Science Demonstra are that (a) it requires a relatively bright star near the tion run in August 2008, two of the Galilean moons gramme continues to increase and well targets to measure the distortions of the wavefront of Jupiter — Io and Europa — were in a very favour over 100 applications are received every by atmospheric turbulence, and (b) that these cor able position to be used as AO references on either year. The studentship programme allows rections are accurate only over angular distances of side of the planet. Using just these two reference young astronomers to experience the sci a few arcseconds from the targets. In the past few objects MAD was able to obtain the sharpest images years the use of artificial laser stars has been suc of Jupiter ever taken with a ground-based telescope, entific environment in an observatory and cessfully implemented to solve the first shortcoming, covering an area almost 30 times larger than that to be in close contact with the develop but the second remains a fundamental limitation of possible with conventional AO instruments. The MAD ment of technical and operational innova conventional adaptive optics systems. A theoretical images of Jupiter are comparable in sharpness tions. In addition, ESO continues to or solution to the problem — atmospheric tomography with the best images of the planet obtained with the — has been known for some time. Because the tur Hubble Space Telescope. With this unique series ganise workshops and conferences and bulence of the Earth’s atmosphere extends from very of images, the team found a major alteration in the supports observational schools through close to the ground up to several kilometres altitude, brightness of the equatorial haze, which lies in a tutoring. The visitor programme continues several reference stars are needed to calculate the 16 000-km wide belt over Jupiter’s equator. More to attract astronomers for extended stays blur produced by atmospheric turbulence over wider sunlight reflecting from the upper atmospheric haze angles by reconstructing the 3D turbulence profiles means that either the amount of haze has increased, at either Vitacura or in Garching. These using tomographic techniques. As part of the E-ELT or that it has moved up to higher altitudes. Com regular interactions with the community design studies, ESO built an instrument for the parison with images taken in 2005 by the Hubble allow ESO staff to stay connected and VLT to demonstrate atmospheric tomography using Space Telescope revealed that the brightest portion provide a good overview of the wishes a technique called multi-conjugate adaptive optics of the haze had shifted south by more than 6000 kil (MCAO). MCAO uses several (two in the demonstra ometres, thus providing important clues to under and requirements of the community. tor) deformable mirrors focused on turbulent layers standing the weather on Jupiter.
ESO Annual Report 2008 11 Imaging a planet within a debris disc
Imaging a planet outside the Solar System Detection of a candi is a formidable technical achievement. date planet in the inner disc of Beta Finding the faint “dot” next to the bright Pictoris. star requires the best possible image quality and has only recently become feasible, with either the use of adaptive debris disk optics from the ground or dedicated coronagraphic observations from space. size of Saturn´s orbit around the Sun The first such planetary object was ob served some years ago around a brown dwarf with NACO at the VLT. Most plan ets have been inferred indirectly through β Pictoris b observations of their gravitational effects β Pictoris on their parent star or from the dimming location of the star of the stellar light when the planet passes in front of the star. In 2008 several direct detections, i.e., images, of exoplanets North were announced by several of the major observatories. Among them is the image East of a planet inside the dust disc of the famous object Beta Pictoris, the second brightest star in the constellation of Pictor and one visible to the unaided eye. This object has been known for many years to have a massive dust debris disc, which has been imaged by several groups over the past few decades. The existence of a planet was deduced from the apparent The detection was confirmed through Given the distance and age of the parent distortion in the disc and the observed various tests that considered the faintness star Beta Pictoris and the brightness infall of comets onto the star. The inner of the planet candidate. Since there are of the candidate planet, its mass can be part of the disc is relatively free of matter no second epoch observations, it is not inferred. Depending on the evolutionary within 50 astronomical units of the star, yet clear whether this object could be model for planets used, this comes out to which could be due to the presence of a a foreground or a background star. How be about 8–9 times the mass of Jupiter, Jupiter-sized planet. Three datasets of ever, there are several lines of reasoning orbiting at a projected distance of about differing image quality were extracted indicating why this is unlikely. Given the eight times the Earth-Sun distance, which from a series of archival NAOS–CONICA faintness and the non-detection at optical is about the distance of Saturn in our observations at a wavelength of 3 microns wavelengths with the Hubble Space Solar System, and still cooling, with a tem and examined. By subtracting the point- Telescope, the object would have to be a perature of about 1500 Kelvin. This very spread function of an isolated star it was very low mass star. Using the number nicely confirms the predictions for the possible to obtain a clean image of the density of such dwarf stars the probabil planetary-mass object required to shape inner region around Beta Pictoris. All ity of a chance superposition is about the observed inner debris disc and pro three datasets yielded a candidate object 10–10. Even without restrictions on the vide the source for the comets known at a location of 0.4 arcseconds from the type of object this probability would still to fall onto Beta Pictoris. The final confir primary and a position angle of 32°. only be 10–5, making this hypothesis mation of this planet should come from rather unlikely. observations of a second epoch, which are under way with the VLT.
Based on Lagrange et al. 2009, A&A, 493, L21
12 ESO Annual Report 2008 Star formation in a bubble
Massive stars have a profound effect on their surroundings. They ionise large regions around them through their ex treme ultraviolet luminosity. However, the intense stellar wind also sweeps up the interstellar material and creates cold gas regions where intensive star formation could be expected. Studies of star forma tion typically require observations at many different wavelengths. Hot gas emits at ultraviolet and optical wavelengths, while warm gas, expected for the first stellar cores as they warm up deep inside a dust cocoon, is best observed in the mid-infrared at wavelengths of several microns. Cold gas needs to be observed at millimetre and submillimetre wave lengths, the domain of the current APEX and the future ALMA instruments. The ionised (HII) region RCW 120 has the rather simple morphology of a bubble and lends itself to studies of star forma tion in the shell.
Based on Deharveng et al. 2009, A&A, 496, 177
Colour composite of RCW 120. The Hα emission is in red and the emission of cold dust at 870 microns in blue. The transition from ionised, hot inner gas to the outer cold gas is called the ionisation front and can be clearly seen when the optical Hα emis sion — coming from the ionised hydrogen gas — and the 870-micron thermal continuum radiation from the cold regions are displayed. The cold gas has been observed with the LABOCA on APEX. The dense, cold gas swept up by the HII region encom passes about 2000 solar masses and shows signs of star formation. The HII region has been observed in the thermal infrared with the Spitzer Space Tele scope. The shell is clearly fragmenting and displays signs of new stars. Secondary star formation is in full swing (about 40 objects, which could evolve into stars have been detected). One particular object is still very deeply embedded in the dust, but could have a mass of 250 solar masses and appears to be the most massive fragment. Observing objects throughout the electromagnetic spectrum provides astronomers with the full range of information and for the case where the different emission regions can be resolved, gives us detailed images with the various components clearly separated.
ESO Annual Report 2008 13 The rotation of the Milky Way
The rotation of the Sun around the A Cepheid star cannot release energy HARPS measurements allowed astrono centre of the Milky Way has been well rapidly enough to establish a stable con mers to measure the line profile of the star established, and is based on several figuration. Instead a Cepheid will heat over their entire pulsational period. The different methods. One of the most accu up and expand until it is so large that the high spectral resolution of HARPS made it rate methods, the distances and radial excess energy can escape, the star cools possible to determine that the small line velocities of Cepheid variable stars, has down and shrinks, and so the cycle be shifts are intrinsic to the Cepheids and suffered from a nagging problem. These gins again. Cepheid cycles are very regu need to be taken into account when de measurements, if taken at face value, lar, and the more luminous a Cepheid riving the radial velocity. The Cepheid have indicated that the Cepheids were the longer its pulsation period. This has atmosphere is strongly affected by pulsa falling towards the Sun with about 2 km/s, become known as the period–luminosity tional dynamics, convective flows and a independent of the direction in which they relation (sometimes also referred to rather complex radiative transport mecha were observed. This was a rather peculiar as the Leavitt law) and has been used to nism. Which of these effects is dominant result and needed to be explained. measure the distances to Cepheid stars is still to be established, but the problem and hence to establish the current expan now rests with theorists to detail the at A small sample of Cepheids was observed sion rate of the local Universe. mospheric effects further in these pulsat with HARPS to check whether internal ing stars. The observations have proven gas motion in the star’s atmosphere could The odd result concerning the distances that the additional effect, when removed be responsible for the effect. Cepheids and radial velocities of Cepheids within the from the radial velocity, results in a per are pulsating stars, which means that Milky Way, indicated a fundamental lack fectly smooth Galactic rotation field. they change size significantly in a periodic in either our understanding of the Galactic manner as a result of radiative effects. rotation or the physics of Cepheids. The Based on Nardetto et al. 2008, A&A, 489, 1255
A thermometer at the end of the Universe
According to the Big Bang theory the Observing molecules at high redshift is and a deuterium atom together), carbon Universe cooled down from a very hot difficult as their signature lines are very monoxide (CO) and atomic neutral car early phase to its current 2.7 Kelvin, weak. However, it turns out that the bon (CI), together with many other atomic measured in the cosmic microwave back number of molecules seems to correlate lines. This is the first detection of these ground. This means that objects in the with the strength of atomic neutral car molecular lines in a damped Lyman-α early Universe would experience a bon lines, a high metallicity and a particu system at such a high redshift. Several warmer background radiation than that lar signature of the abundances of certain absorption line components are blended measured today. It has been exceedingly elements. Damped Lyman-α absorption together and a very careful analysis has difficult to measure this temperature in systems arise from the densest gas been made to disentangle the different very distant objects. clouds, presumably the precursors of contributors to the absorption lines. With galaxies, known in the distant Universe. this delicate treatment the individual col The UVES spectrograph on UT2 can ob Some of these systems do show molecu umn densities can be derived and com serve the absorption lines of gas in front lar hydrogen, but very few other mole pared. Lines from 11 different chemical of luminous, but very distant, quasars. A cules. A recent search of about a dozen elements can be identified. Also several large telescope is needed to acquire a objects with H2 absorption for other mol rotationally excited transitions from neu spectrum of such a faint object with suffi ecules with the VLT was unsuccessful. tral and singly ionised elements have cient signal to explore faint absorption However, a candidate object was identi been observed. While the abundance of lines. By observing molecular gas at a fied from the Sloan Digital Sky Survey sulphur and zinc appears similar to that redshift of 2.42, which corresponds to database of quasar spectra, which con in the Sun, silicon and iron show a much about 80% of the look-back time to the tains tens of thousands of object spectra. lower abundance, presumably because Big Bang, it was possible to determine A high resolution spectrum was obtained they have been depleted onto dust the temperature of the cosmic microwave as part of a Director’s Discretionary Time grains, as is also observed in the cold background at that redshift. It corre programme with UVES. It was possible gas in our Milky Way. The kinetic temper sponds exactly to the prediction of the to identify lines of molecular hydrogen (H2), ature in the gas can be derived from current leading theory of cosmology. deuterated hydrogen (HD — a hydrogen the molecular hydrogen transition. The
14 ESO Annual Report 2008 density of the carbon monoxide is also 25 Different measurements of determined. The ratio of these two mole the cosmic microwave background temperature at cules is similar to that measured along different redshifts. The red Galactic sightlines, but is much less than point is the new determina that derived in dense molecular clouds. 20 tion. The blue lines are pre The rotational energy of the carbon mon vious determinations based on UVES. The light blue oxide lines is twice what is observed in arrows indicate upper limits. the diffuse Galactic interstellar medium. The line gives the expected Since other excitation mechanisms can 15 relation of the temperature be excluded it follows that the carbon ) as a function of redshift,
(K according to the standard monoxide is heated by the cosmic micro Big Bang model. MBR wave background. The measured tem C T perature is fully consistent with the adia 10 batic evolution of the cosmic ray background temperature in the standard Big Bang model. 5 Based on Srianand et al. 2008, A&A, 482, L39
T(z) = 2.725 x (1 + z)K
0 0 1 2 3 4 5 Redshift
Constraining dark energy
Although astrophysics is primarily the sci ence of gravity, there are only a handful of astrophysical problems that deal with the fundamentals of gravitation. One of them concerns the nature of the mysteri ous force that seems to be accelerating the expansion of the Universe. Within the Credit: Springel V. et al. (MPA) framework of Einstein’s general relativity, the accelerating expansion originates from a pervasive field of negative pres sure, which is now universally known as dark energy. In order to accelerate the expansion, dark energy must have nega tive pressure, but very little is known z = 6
z = 2
Computer simulation of the formation of structure in the Universe within a volume of 50 Mpc. The simula tion starts at redshift z = 6, when the Universe was z = 0 just a few percent of its present age and ends at the present age, z = 0. The rate at which structures grow in the Universe provides a way of measuring the strength of gravity.
ESO Annual Report 2008 15 20
2dFGRS 15 2SLAQ VVDS–Wide F22 )
10 (z 1 g New VIPERS survey
1 f
5 c) 0.1 nction Mp Fu
0 –1 te (h
π –5 0.01 0.5 th Ra
–10 ow Gr DM+DE Time–Dependent Coupling DM+DE Constant Coupling Standard, = 0.25, = 0.75 (flat) –15 Ωm ΩΛ
Standard, Ωm = 0.25, ΩΛ = 0 (open) DGP Braneworld –20 –20 –15 –10 –5 0 5 10 15 20 1 2 –1 1 + z rp (h Mpc)
Left: Estimate of the degree of distortion induced by about the (energy) density of this field. In the Einstein equations, which would allow coherent motions on the measured large-scale dis particular, if the energy density, r, of the observations of the cosmic expansion to tribution of galaxies at high redshift. For a given mean density of matter, the distortion depends on field is constant (does not change with be described similarly well. A modification the amount of dark energy and is quantified by the time and is the same everywhere) and its of gravity, however, also has an impact level of anisotropy in the correlation in position and pressure P is equal to minus one times on the growth rate of structure in the Uni velocity among galaxy pairs (the so-called correla the energy density (P = –r), then dark verse, allowing us to discriminate be tion function). The figure shows a colour-coded rep resentation of the galaxy correlation function meas energy would correspond to the famous tween these scenarios. The Universe as a ured using ~6000 galaxy redshifts with 0.6 < z < 1.2 cosmological constant introduced by whole expands, but locally regions that (effective redshift
16 ESO Annual Report 2008 to be measured simultaneously for more half its present age). The ellipticity of the constraints on either dark energy or grav than 500 galaxies. VIMOS data were used outer contours (far from the centre ity, but the team is now engaged in a to compile a catalogue of about 10 000 and where the physics is dominated by survey ten times larger on the VLT that velocities that was then used to investi strongly nonlinear effects) provides a should collect velocities for 100 000 gal gate the nature of dark energy by observ measure of the strength of gravity in the axies, and which will allow them to ing the distortions of the universal expan weak-field regime. reduce the error bars by a factor of four, sion over wide angular distances. The and thus begin to provide critical clues figure in the left image on the opposite Comparison with similar observations at about the nature of dark energy. The page shows the galaxy auto-correlation lower redshifts from previous surveys expected constraints from this new sur function in redshift space plotted as a using smaller telescopes allows both the vey (VIPERS) are shown as stars in the function of galaxy separation parallel (p) equation of state of dark energy and graph, assuming, of course, that the and perpendicular (rp) to the line of sight the physics of gravity to be constrained. standard cosmological model with cos and calculated over a volume of slightly The comparison is shown in the graph on mological constant (red solid line) is the more than 6 million cubic Mpc at an ef the opposite page. Clearly the error bars correct one! fective redshift of z = 0.77 (corresponding are still much too large to place useful to the time when the Universe had about Based on Guzzo et al., Nature 451, 541
Gamma-ray bursts
For a few minutes gamma-ray bursts are that GRBs are caused by the ejection of scientific community has installed two ro the most luminous objects in the Uni a highly relativistic collimated outflow of botic telescopes on La Silla, REM and verse. They then fade rapidly and within matter — a jet produced by a newly TAROT, that can react to GRB alerts in a in a few days or weeks have disappeared formed black hole. GRBs seem to come matter of minutes, so the light curves of beyond the reach of even the most pow in two flavours: the fast and the slow, these events can be followed from almost erful telescopes in the world. The burst of with the occasional ugly interloper. The immediately after the explosions. These gamma rays itself is extremely short, so dividing line between the short and long telescopes move extremely fast, but are the identification of the sources for sub bursts is at about 2 seconds. There is also relatively small, so there are many sequent follow-up with large telescopes now a substantial body of evidence, to GRBs that they cannot follow, or that they relies on X-ray images taken by instru which ESO telescopes have contributed cannot detect at all. Another instrument ments onboard the same satellites that substantially, that long bursts are pro dedicated to observing GRBs, called detect the gamma radiation. Owing to the duced by the extremely energetic super GROND, has been installed by a German combination of its different instruments, nova explosions that occur when massive team at the MPG/ESO 2.2-metre tele and the increased sensitivity, the interna stars collapse to form black holes at the scope on La Silla. GROND observes in tional Swift satellite has been incredibly ends of their lives. The origin of the short seven bands, from the optical to the successful, detecting gamma-ray bursts bursts is still debated among astrono near-infrared, simultaneously, so it can at an average rate of about 100/yr and mers, but there seems to be a general detect and obtain photometric redshifts occasionally more than one burst per consensus that they are likely to originate of even the most distant (and therefore day. Data from the previous generation of from the coalescence of two compact reddest) objects. It is able to filter a signif satellites showed that the progenitors of objects (such as black holes or neutron icant number of Swift alerts before trig gamma-ray bursts (or GRBs as they are stars) in binary systems. Again ESO tele gering follow-up observations with the best known) are at cosmological dis scopes are contributing valuable insights VLT. With the VLT/RRM, REM, TAROT tances and therefore, owing to their ex to this debate. and GROND, the ESO community is at tremely high luminosities, can be used to the forefront of GRB research and the re probe the physics of galaxies at large The combination of four 8-metre-class sults have been truly spectacular. redshifts, and even to measure cosmo telescopes with a large suite of instru logical parameters. ments and the Rapid Response Mode GROND discovered the most distant GRB (RRM) has made the VLT the most impor known to date. GRB 080913 (the number Understanding the physics of GRBs is a tant player in the study of the physics indicates that this was discovered on 13 fundamental challenge to observers and of GRBs, their environment, and their use September 2008) has a spectroscopic theoreticians. Most researchers agree as cosmological probes. In addition, the redshift measured with the VLT of z = 6.7.
ESO Annual Report 2008 17 GROND images of the GROND i’ 2 GROND z’ GROND J most distant GRB known at three different wavebands, 10" peaked approximately at 780 nm, 900 nm and 4 1200 nm. Notice that the source is not detected 3 in the shortest wavelength band. SWIFT XRT SWIFT XRT SWIFT XRT
5
N 6
7 E
(The previous record holder, GRB 050904, substantially different from those today. Ricerca dei Transiti Ottici RApidi) when a had a redshift of z = 6.29.) The figure When compared with the properties second burst exploded within its field above shows the GROND images of of GRB 050904, the other GRB known at of view, roughly 10 degrees from the first. GRB 080913 in three red bands (i’,z’,J) z > 6, the new record-holder has a sub So fortuitously, in a time span of 30 min from left to right. The object is not de stantially shorter duration, a lower utes there were two GRBs separated by tected at wavelengths bluer than the gamma-ray luminosity, and a much dim less than 10 degrees in the sky! Not only z’ band at 900 nm, providing a strong in mer afterglow, indicating that even at that, but the second turned out to be the dication that it lies at a very high redshift z = 6.7 GRBs show the same diversity as brightest GRB ever observed. Since — although GRBs highly reddened by observed in bursts at low z. GRBs are objects of great interest, there interstellar extinction are also known to are typically several other telescopes exist. The seven-band data of GROND Another striking GRB observation took around the world that are following any allowed the team to estimate a photomet place, this time serendipitously, in March given explosion. The object observed by ric redshift of about z = 6.4 that immedi 2008. The REM telescope on La Silla TORTORA was also being followed by ately led them to trigger the observations was following a recent burst using a other telescopes, and in particular, by the with the VLT that obtained a spectro wide-field-of-view host instrument called KONUS gamma-ray detector onboard scopic redshift of z = 6.7. The light from TORTORA (Telescopio Ottimizzato per la the Wind satellite. The figure below shows GRB 080913 has taken almost 13 billion years to reach us. 600 30 The most distant galaxies for which a red ) shift has been measured spectroscopi cally have z ~ 7, so GRB 080913 is indeed close to the visible edge of the Universe. 5.5 In spite of its remoteness, the intrinsic properties of GRB 080913 are typical of 400 20 a long-duration burst, indicating that y) (J ounts per 64 ms e y even when the Universe was only 6% of (c
its present age, massive stars were not te 6.0 Magnitud
Prompt emission light curve of GRB 080319B. 200 10 Flux densit The optical emission observed by TORTORA (red) begins within seconds of the onset of the burst. ind count ra W The optical curve shows three peaks reaching a 7.0 (white) magnitude of 5.3, while the gamma-ray light curve shows multiple short peaks. Although there nus- is no detailed correlation between the gamma and Ko 8.0 the optical peaks, the optical flash begins and 0 0 9.0 ends at approximately the same time as the prompt gamma-ray emission, providing strong evidence 0 20 40 60 80 that they originate at the same site. Time since BAT trigger (s)
18 ESO Annual Report 2008 the optical and gamma-ray light curves in the first 80 seconds after the burst was first detected by Swift. The La Silla ob servations (TORTORA) are shown in red and the KONUS-Wind gamma-ray curve in black. The blue points show observa tions by another robotic telescope on Las Campanas. During the first minute GRB 080319B reached a (white) magni tude of 5.3, making it the brightest GRB ever observed. As it later turned out, GRB 080319B is at a redshift of z = 0.94, so anyone looking at the sky from a dark site in March 2008 would have been able to see an object at z ~ 1 — an ob ject lying more than halfway across the Universe — with the unaided eye!
The exceedingly good time resolution provided by the TORTORA observations coupled with the gamma-ray light curve from KONUS-Wind and observations with several other telescopes from X-rays to radio has provided invaluable information about the physics of GRBs. For example, the temporal coincidence between the optical flash and the gamma-ray burst, something that had not been possible to ascertain before, suggests that the prompt optical and gamma-ray emission originate from the same physical region. However, the detailed structure of the light curve indicates that the optical flash did not arise from a reverse shock that decelerates the outflow as it sweeps up the external medium, although there is solid evidence that the explosion did in deed take place inside the wind of the progenitor star. All in all, the observations of GRB 080319B provided a wealth of invaluable information to refine our under standing of the physics of GRBs. Astron omers now know, for example, that the unusually large optical luminosity of the burst arises from the exceedingly large bulk Lorenz factor of the outflow. In other words, the flow is extremely well colli mated and expands at 99.9997% of the velocity of light — the ultimate limit — pointing almost directly towards us.
Based on Racusin et al. 2008, Nature, 455, 183 and Greiner et al. 2009, ApJ, 693, 1610
The amazing intricacies of the stellar nursery Gum 29. Allocation of Telescope Time
OPC Categories and Subcategories B6 Non-thermal processes in galactic C6 Main-sequence stars with circum nuclei (incl. QSRs, QSOs, blazars, stellar matter, early evolution The scientific categories referred to in Seyfert galaxies, BALs, radio galax- C7 Young binaries, brown dwarfs, the following tables correspond to the ies, and LINERS) exosolar planet searches Observing Programmes Committee B7 Thermal processes in galactic nuclei C8 Solar system (planets, comets, (OPC) classification given below: and starburst galaxies (incl. ultra small bodies) luminous infrared galaxies, outflows, A: Cosmology emission lines, and spectral energy D: Stellar Evolution A1 Surveys of AGNs and high-z distributions) D1 Main-sequence stars galaxies B8 Central supermassive objects D2 Post-main-sequence stars, giants, A2 Identification studies of extragalactic B9 AGN host galaxies supergiants, AGB stars, post-AGB surveys stars A3 Large scale structure and evolution C: Interstellar Medium, Star Formation D3 Pulsating stars and stellar activity A4 Distance scale and Planetary Systems D4 Mass loss and winds A5 Groups and clusters of galaxies C1 Gas and dust, giant molecular D5 Supernovae, pulsars A6 Gravitational lensing clouds, cool and hot gas, diffuse D6 Planetary nebulae, nova remnants A7 Intervening absorption line systems and translucent clouds and supernova remnants A8 High redshift galaxies (star forma C2 Chemical processes in the inter D7 Pre-white dwarfs and white dwarfs, tion and ISM) stellar medium neutron stars C3 Star forming regions, globules, pro D8 Evolved binaries, black-hole candi B: Galaxies and Galactic Nuclei tostars, H ii regions dates, novae, X-ray binaries, CVs B1 Morphology and galactic structure C4 Pre-main-sequence stars (massive D9 Gamma-ray and X-ray bursters B2 Stellar populations: unresolved and PMS stars, Herbig Ae/Be stars and D10 OB associations, open and globular resolved T Tauri stars) clusters, extragalactic star clusters B3 Chemical evolution C5 Outflows, stellar jets, HH objects D11 Individual stars in external galaxies, B4 Galaxy dynamics resolved stellar populations B5 Peculiar/interacting galaxies D12 Distance scale stars
Percentage of scheduled observing time/telescope/instrument/discipline
Scientific Categories Scientific Categories Telescope Instrument A B C D Total Telescope Instrument A B C D Total 2.2-metre FEROS 0 8 27 49 84 UT1 CRIRES 0 0 18 12 30 WFI 9 4 3 0 16 FORS2 23 11 6 7 47 Total 9 12 30 49 100 ISAAC 6 3 7 7 23 Total 29 14 31 26 100 3.6-metre HARPS 0 2 78 20 100 Total 0 2 78 20 100 UT2 FLAMES 0 6 6 22 34 FORS1 7 5 2 14 28 NTT EFOSC2 16 13 16 17 62 UVES 7 5 10 16 38 SOFI 4 4 13 9 30 Total 14 16 18 52 100 Special NTT 0 1 7 0 8 Total 20 18 36 26 100 UT3 VIMOS 51 17 9 5 82 VISIR 0 6 7 5 18 APEX APEX-2A 0 2 9 4 15 Total 51 23 16 10 100 LABOCA 15 18 15 5 63 SHFI 0 10 11 1 22 UT4 HAWK-I 14 2 6 2 24 Total 25 30 35 10 100 NACO 1 5 21 7 34 SINFONI 21 15 5 1 42 Total 36 22 32 10 100
VLTI AMBER 0 0 34 36 70 MIDI 0 5 5 20 30 Total 0 5 39 56 100
20 ESO Annual Report 2008 VLT mirror cleaning. Credit: ESO/Y. Beletsky Outreach
An external in-depth review of the various The mission of ePOD is: on long-term strategic gains to optimise outreach activities at ESO was conducted the visibility of the organisation. in 2008. This resulted in a report with 13 – To increase awareness of ESO and detailed recommendations. One of these ESO’s projects, ESA and ESA’s involve In short, all outreach at ESO has been re was to merge all the existing education ment in the Hubble Space Telescope, structured into an integrated department and public outreach (EPO) resources the International Year of Astronomy with a coherent strategy. Production has at ESO into one group to benefit from the 2009 and the International Astronomi visibly increased, and the department synergy that would arise. The merger be cal Union through production of excel can claim to be a world leader in several gan on 1 September and a new Head of lent EPO materials targeted towards the EPO areas such as video production/dis Department was appointed after eight community of media, educators, deci tribution, production of images from raw months of interim leadership by Bob Fos sion-makers, the scientific community, data and event management (as seen in bury (ST-ECF). A joint strategy was written local communities and the public. the case of the International Year of As to capture the many inputs from the inter tronomy 2009). nal and external EPO experts involved. – To promote astronomy and the scien This detailed 100-page strategy document tific process as a fundamental part of extends across the whole range of depart our culture and heritage. Press activities mental activities from the Vision statement to details of the precise implementation, – To propagate the awareness that Eu Press activity has been above average including individual objectives and deliver rope is a major player in ground-based this year and the resulting press coverage ables. The strategy focuses on improving astronomy with ESO and in space- was fully satisfactory. ESO had 49 press the operation of the new ESO education based astronomy with ESA. releases (down 11%), ESA/Hubble had and Public Outreach Department (ePOD) 23 releases (up 15%) and the IAU had 10 in the critical areas of press releases, im – To contribute to the strengthening of releases (up 350%). In each case, great age production from raw science data, European and global astronomy care was taken to provide high quality exhibitions, print products, web services, communication. visual support, often including HD video audiovisual production and more. material. The department now has seven main The resulting synergy has made it possi groups: a) the PIOs, b) ePOD Chile, c) Targeted efforts were put into collaborat ble to appoint dedicated Public Informa Advanced Projects (development of out ing with other institutions to make co- tion Officers (PIOs) for the most important reach applications and technical solu releases, thereby amplifying the impact. ESO projects (ALMA/APEX, E-ELT, La tions), d) Images (scouting/acquisition, Silla Paranal and the new Survey Tele processing and archiving), e) the Interna The special “Bond at Paranal” campaign scopes), each developing press releases, tional Year of Astronomy Secretariat coincided with the release of the James web pages, background stories, print (2008—2010), f) Audiovisual Coordinators Bond movie, Quantum of Solace, and products and more. and g) Audiovisual Assistants. Individual succeeded in raising considerable interest staff assignments in the different areas in both ESO and the VLT, notably reaching The new ePOD serves four organisations: are fluid and are addressed on a project- audiences who are not normally exposed ESO, ST-ECF (ESA/Hubble), the Interna to-project basis (matrix-structure). to — and do not normally seek — infor tional Year of Astronomy 2009 (IYA2009) mation about science, such as film devo and the International Astronomical Union ePOD continues to be a horizontal serv tees, architecture connoisseurs and (IAU). ice to ESO employees, but with the focus others. A dedicated website, targeted at
ESO News Releases 2008: Popularity
200000 Relative popularity of individual ESO press releases 180000 45-Sci Eurekalert (relative) as measured by three different methods. In blue, 160000 Meltwater online media coverage, in red, hits per re Meltwater (relative) 140000 46-Sci lease (measured with Google Analytics) and in Google Analytics 39-Pho green, Eurekalert (a portal for journalists) hits. Note 120000 that the scale is different for the three estimators. 100000 26-Ins 80000 60000 19-Sci 40000 5-Sci 20000 1- 2- 3-Sci 4- 5-Sc 6- 7- 8-Sci 9- 10 11 12 13 14 15 16 17 18 19 20 21 23 24 22 28 29 25 27 26 30 31 42 32 3 38 39 40 41 43-org 44 45-Sci 46 47 48-Pho 34 37 49 35-Sci 36 3-Pho Or Or Pho Pho Sci Sci -Pho Sci Sci Sci Sci -O -Sci -Sci -Sci -Pho -Pho -Sci -Sci -O -Sci -Sci -Sci -O -Sci -O -Sci -Sci -Sci -O -Pho -Sci -Sci -Ins -Pho -Pho -O -Ins -O -Ins -Sci -Pho -Sci -Pho -Sci g g g g rg i i rg rg rg rg rg rg rg
22 ESO Annual Report 2008 this less mainstream astronomy audience, Periodicals The Messenger: 4 issues was set up and efforts were made on ST-ECF Newsletter: 2 issues YouTube, Myspace etc. A very successful Capjournal: 3 issues press visit by the European media to ESO Books ESA/ESO Working Groups Report no. 4 sites resulted in wide coverage and long- Eyes on the Skies: in English and German (with Wiley) term interest, including in new (Austria) Hidden Universe: in English and German (with Wiley) and potential (Ireland) member states. ASTRONET Infrastructure Roadmap. The Strategic plan for European Astronomy (for ASTRONET) A “10 years of VLT” campaign celebrated Communicating Astronomy with the Public 2007 Conference Proceedings the 10th anniversary of First Light at the Brochures Swedish version of “A Universe of Discoveries”. VLT with several visible products. The Paranal booklet: for the release of the James Bond movie Quantum of Solace. ePOD was invited to present ESO’s vision Foldable poster/brochure about the European Extremely Large Telescope on media relations at an AlphaGalileo Foldable poster/brochure about the 10th anniversary of the VLT meeting in Paris. Foldable poster/brochure about ALMA IYA2009 Brochure v.3 As part of the new workflow, a well- ASTRONET Brochure. A summary of the Strategic plan for European Astronomy defined set of success estimators was (for ASTRONET) set up for evaluation purposes. The UNAWE Brochure: in English and French (for UNAWE) figure on the opposite page shows some Other ESO Annual Report 2007 the estimators used for press releases. ESO Calendar 2009 New HR Staff Pack Garching New HR Staff Pack Chile Publications 6 “pretty pictures” posters 15 posters with conference announcements Several printed publications were pub Electronic publications ESO Style Guide lished during 2008 by ESO, ESA/Hubble 1 poster and IYA2009. The table on the right shows List of ePOD’s print publica an overview. This was a fairly typical year tions in 2008. for publications although the total produc tion was significantly increased. Improved workflow and planning allowed the layout manpower spent on The Messenger to be reduced to 4—5 weeks per issue. Some of the publications mentioned in the table above.
ESO Annual Report 2008 23 Exhibitions Name Local Date Attendance ECRI Versailles, France 9-11 December 500 In 2008, a record number of 13 exhibitions European City of the Sciences Grand Palais, Paris, France 14-16 November 42 000 were held in various venues around Eu JENAM Vienna, Austria 8-12 September 800 rope (up 30%). 145 exhibition panels were Meet the buyers Botanical Society, London, 16 September 250 produced in English, French, German and UK Italian. The estimated number of exhibition Solar Eclipse Event Oslo, Norway 31 July-1 August 30 000 visitors exceeded 150 000 people. ESOF Barcelona, Spain 18-22 July 4000 SPIE Marseille, France 23-28 June 2000 Explore Science Mannheim, Germany 8-11 June 30 000 Web and software development FEST Trieste, Italy 16-20 April 40 000 RAL - NAM Belfast, Ireland 31 March-4 April 700 By the end of 2008 ePOD maintained AAAS Boston, MA, USA 26 January 6500 16 websites of various sizes. A simple web Galway Astronomy Festival Galway, Ireland 26 January 100 Content Management System (CMS, called AAS 211th Meeting Austin, TX, USA 7-11 January 2000 Simplicity) has successfully been running ESO exhibitions in 2008. spacetelescope.org for several years and it was decided to apply this methodology to the new outreach websites. Simplicity’s successor, Djangoplicity, was developed and deployed on new versions of iau.org (IAU) and astronomy2009.org (the Interna tional Year of Astronomy 2009). The sys tem is tuned to deliver very high perform ance under great load and to deliver a
first-class experience for users and an effi Credit: Pascal Blondé (OBSPM) cient workflow for content coordinators.
Several new features were developed for the IAU website, such as the Travel Grant application form, an IAU individual mem ber nomination form, symposium pro posal submission, eVoting for organising committees, mass mailing to various sub sections of the members and more.
A handful of smaller websites were also set up during the year.
The ESO web CMS study, initiated in 2006/7 continues, but was transferred to the IT Department, which is a more suita ble home for an IT infrastructure project of this magnitude. Selecting a CMS is a large effort that will allow ESO’s many web authors easier ESO-wide publishing access and is planned for mid-2009.
A new evaluation workflow was set up using a set of standard success estima ESO at the European City of Science. Henri Boffin tors. These use the web statistics exten from ESO (left) explaining the model of the European Extremely Large Telescope to Valérie Pécresse, the sively and can be studied in the figures French Minister of Higher Education and Research on the next page. (centre) and Janez Potočnik, the European Commis sioner for Science and Research (right).
24 ESO Annual Report 2008 Visitors/day 45000
40000 eso.org spacetelescope.org 35000 astronomy2009.org 30000 iau.org
25000
20000
15000 10000 Visitors per day in 2008 for ePOD’s four main web 5000 sites: eso.org (dark blue), spacetelescope.org (red),
0 astronomy2009.org (green) and iau.org (light blue). 20 20 20 20 20 20 20 20 20 20 20 20 20 20 08-Dec 08-Dec-3 08-N 08-Sep 08-Oct 08 08-M 08-Jun 08-Jul 08 08-Mar 08-Jan 08-F 08-Jan -A -A eb ug pr ov ay -1 -2 -0 -2 -0 -1 -2 -2 -0 -1 -0 -0 -2 0 5 7 2 7 9 9 2 2 1 1 5 6 6 4 0 2 9
PageViews/day 250000
eso.org 200000 spacetelescope.org astronomy2009.org iau.org 150000
100000 Pageviews per day in 2008 for ePOD’s four main 50000 websites: eso.org (dark blue), spacetelescope.org (red), astronomy2009.org (green) and iau.org (light 0 blue). 20 20 20 20 20 20 20 20 20 20 20 20 20 20 08-Jan 08-Jan 08-F 08-Mar 08 08-M 08-Jun 08-Sep 08-Oct 08-N 08-Jul 08 08-Dec 08-Dec-30 -A -A eb ug pr ov ay -1 -2 -0 -0 -2 -1 -2 -2 -0 -1 -0 -0 -2 5 7 2 9 7 2 1 5 6 4 0 2 9
Data traffic (GB/month)
1000000
Space Telescope 100000 ESO web
10000
1000 Web traffic for eso.org (blue) and spacetelescope.org 100 (red) in GB/month over the past six years. The top of the graph corresponds to 1 PB/month. Some data
10 are missing for eso.org. 20 20 20 20 20 20 20 04 05-Dec-3 06 07 08-Dec-3 02 0 3-Dec-3 -Dec-3 -Dec-3 -Dec-3 -Dec-3 1 1 1 1 1 1 1 1 1 1
Alexa Global Web Ranking 20 20 20 20 20 20 20 20 20 20 20 20 20 20 20 20 20 08-Dec 08-N 08-M 08-F 08-Mar 09-F 08-Sep 09-Mar 08-Mar 08-Jan 08 09 08-Jun 09 08 08-Oct 08-Jul -A -Jan-3 -A -A eb-0 eb ov ug ay pr pr -0 -0 -0 -0 -2 -2 -2 -2 -2 -2 -2 -1 -1 -1 -1 9 1 5 6 1 8 1 6 8 3 9 1 8 5 6 2 1 10000 Alexa rank for ePOD’s four main websites: eso.org (dark blue), spacetelescope.org (red), astronomy2009.org (green) and iau.org (black). The baseline comparison at the top is the hugely successful hubblesite.org from NASA (light blue). 100000
1000000 eso.org Spacetelescope.org IYA2009 IAU.org hubblesite.org
ESO Annual Report 2008 25 The development of the ESA/ESO/NASA distributed. It is presented by “Dr. J.”, aka public observatory (Region of Coquimbo), FITS Liberator v.2.3 for state-of-the-art Dr. Joe Liske, from ESO. A Blu-ray version and the launch of a new network of ama processing of “pretty pictures” was initi of the movie will be distributed in 2009. teur astronomy academies in the Regions ated. The main features are multi-proces of Antofagasta and Copiapo. sor support (up to 5—10 times faster) and Several high quality animations were pro support for Planetary Data Systems (the duced during the year for a variety of pur The ESO weekend public visits pro FITS analogue of planetary science). Un poses, including press releases. A short- gramme to La Silla Paranal Observatory fortunately the multi-threading proved form HD movie called “The VLT Secret attracted more than 8000 tourists and more difficult to implement than expected Files” was produced for the Quantum of students during the year. and the release has slipped to 2009. Solace campaign. ePOD Chile also coordinated and sup An Astronomy Visualization Metadata Several HD video products were pro ported dozens of media visits to La Silla, standard has been developed in collabo duced for the International Year of As Paranal, APEX and ALMA, for a wide ration with other EPO groups and is a use tronomy 2009 including a trailer in more range of productions, including news sto ful tool for expanding the utility of image than 50 nationalised versions and a full ries for print, electronic and audiovisual files and facilitates search and access. dome version. media, large science documentaries for The web lends itself naturally to this pur the general public and innovative art/mul pose and all available material from ESO In addition, dozens of logos were pro timedia projects. Two major productions and Hubble should be presented through duced for ePOD projects and special il involved complex organisation: National the web. Once the files are tagged, they lustrations were often designed on short Geographic´s “The World’s Toughest will be available for third-party software turnaround times for press releases. Fixes” (detailing the delicate and exciting such as Microsoft’s World Wide Tele process of recoating of one of the UT´s scope, Google Sky, Stellarium etc. Photography and HD filming was carried primary mirrors at Paranal for the first out on site in Chile for inclusion in the im time for the public) and the shooting of age and video archive. sequences in the Paranal Residence for Audiovisuals Quantum of Solace. Interesting stereoscopic (polarised) 3D One of the highlights of the audiovisual animations were produced in collabora ESO also played a prominent role at the production was the October’s launch of tion with José Francisco Salgado from National Science and Technology Week, the ESOcast, a high-definition video pod Adler Planetarium. the largest science popularisation event cast series dedicated to bringing the in Chile. In November, around 20 000 public the latest news and research from people visited a public expo at Quinta ESO. Three episodes have been released Chilean projects Normal, Santiago, where ESO held an as so far. tronomy exhibition. In the same week, Activities for local communities played a more than 10 000 schools in Chile re Video News Releases (VNRs) are in particularly important role for ePOD activ ceived copies of an ESO mountable plan tended for the broadcast media around ities in Chile this year. A new astronomi isphere, as well as VLT´s anniversary Europe and two were produced in 2008. cal exhibition at the MIM Interactive Mu posters, flyers and ESO brochures. seum in Santiago was inaugurated. This Another large, ongoing project is the digi is partially funded by the ESO-Chile Joint Around 1300 students from 148 schools tisation, archiving and online publishing of Committee. The annual visitor count is in Chile participated in the Eratostenes historical as well as recent ESO images around 500 000 people. The educational Project, an educational activity to meas and videos. Over 1500 new images were grant programme in Taltal provided ure the Earth’s radius, organised by the uploaded, bringing the image archive up scholarships for secondary and under science foundation PROFISICA and sup to 2300 images. An elaborate video ar graduate students in a joint effort with the ported by ESO. Simultaneous measure chive with ten different formats was im Municipality of Taltal. An outreach collab ments were performed in several cities in plemented and 400 new videos, partly in oration programme, with the Universidad November, including an official launch in high-definition were made available to the Catolica del Norte in Antofagasta, re front of La Moneda, with more than 50 public. sulted in a series of regular public talks, students taking measurements in public. star parties and science cafes during the The Eyes on the Sky HD movie was pub year. A Science Expo was organised at San lished on a standard DVD in both major Pedro de Atacama, as part of a local an video formats (PAL and NTSC). The movie The ESO-Chile Joint Committee provided niversary celebration. Around 90% of the is a 60-minute documentary that tells the funds for a wide variety of outreach students attending schools in the area fascinating story of the telescope through projects: workshops for school teachers, visited the exhibition. words and a wealth of stunning photo general support for the Museum of Sci graphs, animations and time-lapse pho ence and Technology in Santiago, train A new media training programme for ESO tography. Roughly 140 000 copies were ing for astronomy guides at Mamalluca science staff in Chile was launched, in a
26 ESO Annual Report 2008 ESO collaborated with the Association of French-speaking Planetariums (APLF) and other partners in Europe to produce the new half-hour planetarium show, In Search of our Cosmic Origins (www. cosmicorigins.org).
The members of the ALMA Educational and Public Outreach Integrated Project Team, including ESO, worked to create a new, joint ALMA public website (www.al maobservatory.org). A special effort was made in December when the first an tenna was handed over, with a Video News Release, an ESOCast, a press re lease and more.
Survey telescopes EPO
As part of the new strategy a targeted ef fort is being made to raise the profile of the two coming survey telescopes at Paranal, VISTA and the VST. Generic ma Students at Paranal during one of the public terial has been prepared for the web and tours that take place every weekend. print (hand-outs etc.) along with draft re leases for the arrival of the mirror as well as the first light/inauguration event. joint effort with the Office for Science in signatures and finally compression of the Vitacura. More than 30 staff astronomers, large dynamical range with the ESA/ESO/ fellows and post-docs were trained in NASA FITS Liberator. All images were Hubble EPO how to deal with the media. cosmetically cleaned and corrected and the colour balance corrected on colour- During 2008, ePOD has been active in the calibrated monitors. Several datasets are public dissemination of the discoveries Image processing in the pipeline for 2009. from Hubble for ST-ECF. 23 news and photo releases and 26 smaller “Hubble The combination of astronomical and PR Updates” were produced. The European image processing experience gained E-ELT EPO Hubble website had 2.2 million visitors from many years of work with Hubble and (down 11%) and distributed 550 TB of mul ESO data was applied to set up a rigor As part of the new outreach strategy a timedia materials (up more than 400%). ous image processing pipeline with the handful of E-ELT products were produced main aim of streamlining the exploitation with the general aim of elevating the pro The production and distribution of the of science data. A systematic search of file of the project among the most impor Hubblecasts in Full HD is running the ESO Science Archive was initiated tant target groups such as decision mak smoothly, with 14 episodes produced and using advanced queries that make use of ers and scientists. New E-ELT models distributed during 2008. The video pod the filter equivalence table and an instru received a lot of exposure and attracted cast continues to be an iTunes hit, often ment’s “photogenic qualities” to identify considerable interest at exhibitions. One ranking in the top five in iTunes science- promising datasets. such example was the successful “Euro related podcasts. In total, an estimated pean City of the Sciences” at the Grand minimum of five million Hubblecast epi “Complete” datasets were marked for re Palais, Paris, France, organised with sodes were downloaded in 2008. trieval, and “incomplete” datasets that French partners and centred on the E-ELT could be supplemented by later acquisi and its science. Another highlight of 2008 was the publi tion through small Director’s Discretion cation of the bestselling books, Eyes on ary Time proposals were identified. Sev the Skies and Hidden Universe, produced eral datasets were processed with the ALMA EPO in a unique collaboration between the new pipeline, making use of the latest ar IAU, ESO, ESA and the international pub chive features (such as associations and As part of a wide range of education and lisher Wiley–VCH (ranked second and advanced data products), processing public outreach activities prepared for the eighth respectively on the publisher’s with THELI to remove instrumental International Year of Astronomy 2009, 2008 bestseller list).
ESO Annual Report 2008 27 The International Astronomical Union At the end of 2008 around € 560 000 had A major effort was undertaken to revamp been raised for the global coordination, the EIROforum website, to make it more Several activities were carried out for the including funding for the Cornerstone appealing to visiting outsiders as well as IAU, including most notably the launch of projects. a useful internal repository for EIROforum a comprehensive new website, iau.org, documents. with a restructured membership data During 2008 IYA2009 developed to be base (10 000 members together with his come the biggest network ever in astron ESO, as a member of EIROforum, contin torical information) and much new infor omy and in science education and public ues to support Science in School, the mation, including “Themes”, web essays outreach and ePOD is proud to lead this European journal for science education presenting the most popular IAU topics. work. aimed at European teachers and educa A significant number of questions — es tors. Three issues were published during pecially on Solar System bodies, Plutoids 2008 (30 000 copies each). The Science and Pluto — were answered and Education in School website (www.scienceinschool. archived. org), is, with about 250 000 visitors per The Catch a Star 2008 competition took month, much visited. Hundreds of press clippings were also place, with 300 students entering the archived. Early preparations for the IAU written categories (up ~30% over the pre ESO, through EIROforum, supported the General Assembly 2009 took place, with vious year) and just over 1000 in the art 2008 EU Contest for Young Scientists an analysis of press office requirements. work category (up ~160% over the previ (EUCYS) in Copenhagen. This was the In addition, limited support to Division XII ous year). The top prize was a trip to the 20th anniversary of the competition, and and Commission 55 were given. ESO VLT on Cerro Paranal in Chile. New thus a special occasion for celebration. in 2008, Garry Harwood, a volunteer EIROforum had an appealing stand. At from the International Association of As tending the event were six previous win The International Year of Astronomy tronomical Artists, also awarded special ners of EIROforum prizes, including one 2009 prizes (www.eso.org/catchastar/cas2008). of the ESO Special Award winners, and two EIROforum speakers, with one repre Since early 2006 ESO has been heavily The second ESO–EAAE Summer School senting ESO. There was also a live video engaged in the International Year of As took place in Granada, Spain, in July conference link to Paranal from Copen tronomy 2009. ESO hosts the Secretariat 2008, with about 50 participants. The hagen, giving the young scientists a for the IYA2009 on behalf of the IAU, event, which was also supported by the chance to ask questions to an astrono which is the central hub for the imple EC’s Comenius Programme, was a suc mer at the VLT. At the Special Awards mentation and coordination of the global cess, with positive feedback from the Ceremony at the National Museum, at activities. In addition ESO leads three of teachers. It was co-organised by ESO tended by journalists and VIPs such as the eleven Cornerstone projects: Cosmic and EAAE with the cooperation of the Danish Education Minister Bertel Haarder, Diary, 100 Hours of Astronomy and the Instituto Astrofísico de Andalucía and ESO presented one of the EIROforum Portal to the Universe. ESO will also im Granada University. Scientists and edu special prizes, a visit to the VLT, to Mar plement specific projects to exploit the cators from ESO gave talks. ion Deriot, for her work on the project added interest in astronomy in 2009. A “Physics from breakfast”. EUCYS has planned series of “Science Cafés” in San 300 participants (www.eurocontest.dk). tiago and local communities close to the EIROforum EPO observatories in Northern Chile is just The 20th EUCYS was a clear success, one of several activities. ESO has chaired the EIROforum, and the in which EIROforum played a major role Outreach and Education Working Group and in which it (and its member organisa The global coordination and planning of (O&E WG) since 1 July. tions) received significant exposure. It this enormous project increased as ex should be mentioned that EUCYS was pected in the second half of 2008. The EIROforum was present at ESOF 2008, also visited several times by the Minister project grew to: which was held on 18–22 July in Barce for Science, Technology and Innovation, lona, with a large and impressive stand. Mr. Helge Sander, and by Prince Joachim – 137 National Nodes In addition, the O&E WG organised two and Princess Marie of Denmark. – 35 Organisational Nodes sessions during the ESOF programme: – 99 National Websites Careers in Science and an Education – 11 Cornerstone Projects session. – 11 Special Task Groups – 9 Special Projects – 5 Official Products – 3 Global Sponsors (Thales Alenia Space, Celestron and History) – 27 Organisational Associates – 17 Global Media Partners
28 ESO Annual Report 2008 The Cone Nebula and surroundings. Operations
The domes of the ESO 3.6-metre and the 1.4-metre Coudé Auxiliary Telescope reflecting the Moon’s light. La Silla Paranal Observatory
Operations In addition to its regular VLT and La Silla coating all the large telescopes in a single operations, the VLTI was scheduled for year will be rewarded in future by a Ten years after “First Light” on the Antu scientific observations using baselines mirror coating schedule that is optimised telescope, the ESO Very Large Telescope with either the UTs or the ATs for an addi across the two observatory sites for the (VLT) has four 8.2-metre Unit Telescopes tional 169 nights. The remaining nights availability of manpower and time re (UTs) and its complete suite of eleven of the year were used for technical activi sources and avoids the windy season on first generation instruments in operation. ties and for the further development Paranal. Strong winds have been one of The Laser Guide Star Facility (LGSF) and commissioning of the interferometer. the major causes for delays in the coating provides an artificial reference star to two The installation and commissioning of the process of the UTs in the past because of the three VLT instruments supported new PRIMA facility required 88 nights they impose tight restrictions on when by adaptive optics. The VLT Interferom alone over the course of the year. Out of the large 8.2-metre mirrors can actually eter (VLTI) combines the light of either the the scheduled VLTI science time, 8% was be transported the four kilometres by Unit Telescopes or the Auxiliary Tele lost due to technical problems. road between the unit telescopes on the scopes (ATs) to feed one of the two first mountaintop and the mirror maintenance generation interferometric instruments This year the primary and tertiary mirrors building at base camp. with a coherent wavefront that is further of all four UTs of the VLT and the mirrors stabilised by the VLTI fringe tracker. of the three major La Silla telescopes The combination of high operational effi have been recoated with fresh layers of ciency, system reliability and up-time of The instrument suite on La Silla has been aluminium to maintain the high reflectivity the La Silla and Paranal telescopes and reduced to six instruments, operating on and low micro-roughness of the mirror instruments for scientific observations the New Technology Telescope (NTT), the surfaces. The coating of the Kueyen tele has again resulted in high scientific pro 3.6-metre and the 2.2-metre telescopes. scope (UT2) in May was the 25th mirror ductivity. We have counted 483 peer- coating in the history of the VLT and was reviewed papers published in various sci The observatory also provides operations documented in great detail by the Na entific journals and at least partially support for the Atacama Pathfinder Exper tional Geographic Channel in its “World’s based on data collected with the VLT and iment (APEX), with its 12-metre sub-mm Toughest Fixes” series, featuring the ESO VLTI instruments at Paranal. There were radio antenna and its recently completed VLT as the “Giant Telescope” as it under 299 refereed papers published referring suite of heterodyne and bolometer facility went its difficult but crucial mirror mainte to La Silla observations and 17 to APEX instruments located on the high plateau of nance procedure. The extra effort of observations. Chajnantor at an altitude of 5100 m.
The observatory continues to operate efficiently and has maintained the high availability and low technical downtime of its telescopes and instruments — key elements for productive scientific obser vations. In 2008, a total of 2217 nights
were scheduled for scientific observations Credit: Gianluca Lombardi/ESO with the four UTs at the VLT and with the three major telescopes at La Silla. This is equivalent to about 88% of the total number of nights theoretically available over the whole year. The remaining 12% of nights were scheduled for planned engineering and maintenance activities necessary to guarantee the continuous performance of the telescopes and in struments and to include time slots to commission new instruments and facili ties. Out of the available science time for Paranal, only 3.5% was lost due to tech nical problems and about 7.5% was lost due to bad weather conditions. On La Silla bad weather accounted for losses of about 12%, technical problems for 1.5%.
Night scene at the ESO’s Very Large Tele scope (VLT). This 45-minute exposure shows the trails of the stars in their dance around the Celestial South Pole.
ESO Annual Report 2008 31 New instruments and facilities HAWK-I will be supported by the Adap follow-up of the quickly fading optical tive Optics Facility (AOF), making it even counterparts of gamma-ray burst is ex HAWK-I, the High Acuity Wide field less dependent on the quality of the at pected to be one of the most intensively K-band Imager, is the eleventh facility mosphere and able to deliver the highest used types of observations with X-shooter. instrument to go into operation at the resolution images constantly. The AOF The commissioning of X-shooter is being VLT. HAWK-I started science operations will convert the Yepun telescope into an carried out at the Cassegrain focus of the at the Nasmyth A focus of the Yepun (UT4) adaptive optics telescope with a large Melipal telescope (UT3), temporarily re telescope from the beginning of Period deformable secondary mirror and the placing VISIR in the observing period 82. 81 in April 2008. HAWK-I is a cryogenic Four Laser Guide Star Facility (4LGSF). X-shooter will be transferred to the Cas wide-field imager operating in the near- An adaptive optics module named segrain focus of Kueyen (UT2) at the be infrared wavelength range from 0.85 to GRAAL, specially designed for HAWK-I, ginning of Period 83, where regular sci 2.5 μm with an on-sky field of view of will provide a wide field of view corrected ence operation is expected to commence 7.5 arcminutes x 7.5 arcminutes. This cor for the effects of the atmosphere. in Period 84, i.e., in October 2009. responds to a field of view of about nine times that of the very successful VLT in The first of the second generation VLT in The arrival of X-shooter at Kueyen will re frared camera ISAAC and a field of view struments, X-shooter, started its installa quire the decommissioning of FORS1, the comparable to or even larger than that of tion and commissioning programme in very first of the first generation VLT instru the optical cameras FORS1 and FORS2. the last quarter of 2008. X-shooter is a ments, after ten years of highly success Whenever the atmosphere above Paranal highly efficient, medium resolution spec ful science operations. To date FORS1 allows it, HAWK-I routinely delivers exqui trograph providing simultaneous spectral observations have contributed to more site infrared images with an almost con coverage from 300 to 2450 nm, i.e., from than 675 refereed publications in astro stant full width at half maximum for the ultraviolet to near-infrared wavelengths. nomical journals. The decommissioning stellar point sources of about 0.2 arcsec The high efficiency and unprecedented of a workhorse instrument like FORS1 will onds across the whole field of view. simultaneous wavelength coverage, com undoubtedly have an impact on the ESO HAWK-I has not only been optimised for bined with the ability of the VLT to act on community, for example, by increasing the best image quality, but also for the external triggers and acquire targets rap pressure on FORS2. Fortunately, FORS2 highest sensitivity and allows the deepest idly when in the Rapid Response Mode will remain in operation for the foreseea looks into the infrared sky with the VLT. (RRM), make X-shooter a powerful tool ble future and the polarimetry optics of The figure below shows an example of for studying transient phenomena in FORS1 are being transferred to FORS2 at the spectacular views of the infrared sky the sky, where the shape and redshift of Antu to maintain this unique capability provided by HAWK-I. the spectra are a priori unknowns. Fast at the VLT. In addition, the high efficiency I Commissioning Team - Credit: HAWK
The Tarantula Nebula in the Large Magellanic Cloud observed with ESO’s Very Large Telescope, in the visible with FORS (to the left) and in the infrared with HAWK-I (to the right).
32 ESO Annual Report 2008 filters, grisms and the blue-sensitive CCD assuming negligible technical loss times, explored: adaptive optics observations detector system of FORS1 will also move no more than 20 observing nights are ex using an artificial laser guide star still re to FORS2. pected to be available to the ESO com quire a nearby natural star to correct for munity with the LGSF in each observing tip-tilt effects introduced by the Earth’s The single Laser Guide Star Facility period. atmosphere equally into the light paths (LGSF) achieved First Light at the Yepun of the science target and the laser guide telescope in 2006. Since then the LGSF Regular science operations using the star. If no such “tip-tilt” star is available has provided a bright artificial reference new operating protocols were resumed near the science target no diffraction- star for the adaptive optics systems of with the LGSF in August and immediately limited images can be obtained. How the SINFONI and NACO instruments. The resulted in considerably higher perform ever, experiments with SINFONI and laser guide star is required to enable the ance, stability and reliability of the LGSF. NACO and the LGS have shown that an AO systems to work in regions of the sky Six Watts of laser power on sky are now image quality better than the ambient where no bright natural star can be found regularly achieved, providing a sufficiently seeing can still be obtained. The “seeing close enough to the scientific target. bright artificial reference star to the AO enhancer” mode was offered with systems of NACO and SINFONI. SINFONI for the first time, starting with In 2008 a major effort was made by the Period 82. maintenance and operations teams in Improved LGS performance and stability Paranal, the Garching LGSF team and the have meant that the commissioning of Following its spectacular success during PARSEC laser team from the MPE in the LGS modes of NACO and SINFONI commissioning, MAD, the Multi-Conjugate Garching and the MPIA in Heidelberg to could be completed. In addition, a novel Adaptive Optics Demonstrator, returned increase the reliability and performance “seeing enhancer” mode has been to the Melipal telescope on Paranal as a of the LGSF further. After a period when the overall performance of the system had degraded rapidly, the LGSF was taken out of regular science operation for a period of four months during which a rigorous analysis of the root causes of the
instabilities experienced by the system Credit: ESO/H. Heyer was carried out, followed by the execu tion of an aggressive recovery and im provement plan to bring the LGSF back to its nominal performance and to stabi lise its operation. In the course of the re covery process sophisticated monitoring systems with hundreds of sensors were introduced so as to be able to detect and counteract deviations from the nominal performance of the LGSF before they im pacted on operations. In addition, based both on the experience collected during the first years of operation and mainte nance, and on the findings of the recov ery process, the relevant operation and maintenance procedures were optimised.
The LGSF is currently being scheduled in monthly blocks of three preparation and start-up days followed by seven nights of science operations with NACO and SINFONI. This results in 42 sched uled LGSF nights per six-month observ ing period, equivalent to about 25% of all available science time at the Yepun tele scope. Taking into account the statistical probability of having the atmospheric conditions required for successful LGS operation (clear skies, with seeing better The LGS System in than 0.8 arcsec) and optimistically operation.
ESO Annual Report 2008 33 visitor instrument for two additional sci ence verification runs to allow the com munity to exploit these new capabilities with the VLT further. By using multiple and relatively bright natural guide stars, MAD provides multi-conjugate adaptive optics corrections in the K-band (around 2.2 μm) over a wide field of view of 2 arcminutes x 2 arcminutes, resulting in unprecedented wide-field high resolution images in the near-infrared (see the MAD image of Jupi ter shown on page 11).
Another demonstrator, the Active Phasing Experiment (APE), was commissioned at the visitor focus on Melipal to evaluate different possible phasing techniques for the active wavefront control of segmented telescope mirrors. The experiment will continue into the first quarter of 2009 to collect valuable experience for the E-ELT primary mirror control.
Upgrades The HAWK-I instrument mounted on the telescope’s To maintain the competitiveness of the Nasmyth (side) port. HAWK-I is attached to Yepun, UT4 at the VLT. VLT and VLTI it is necessary not only to continue to deliver new instruments and facilities, but also to follow a rigorous up For NACO, the adaptive optics camera at transmitted to the telescope and NACO grade programme for the existing instru the Yepun telescope, the new Sparse Ap can now be operated without any Strehl- ments. Several such upgrades have been erture Mask Interferometry (SAM) mode ratio degradation. Vibrational effects on carried out by the Instrumentation Divi was commissioned. This mode uses spe the VLTI have also been returned to the sion in Garching in 2008 in collaboration cial aperture masks in the cold pupil pre-HAWK-I level. with the instrument builders and the wheel inside the instrument to transform observatory. the single 8-metre telescope pupil into a Increased vibrations from the CRIRES sparse interferometer array. The SAM high resolution near-infrared spectrograph The CCD detector of the FLAMES- mode allows observers to obtain the very at the Antu telescope have also affected GIRAFFE medium-high resolution visible highest angular resolution at the diffrac the interferometer. Liquid nitrogen cooling spectrograph was replaced in May with a tion limit of the telescope. Covering base is not a viable option in this case, but deep depletion E2V CCD of 40 μm nomi lines shorter than 8 m, SAM is a comple new low vibration cryo-coolers have been nal thickness. The new detector has a mentary mode to the longer (up to 150 m) identified and will replace the originals in special, custom-made two-layer coating baselines of the VLT Interferometer. early 2009. Until then, the CRIRES instru
(HfO/SiO2) optimised for broadband sen ment has to be warmed up and the cryo- sitivity. During commissioning of the new The new HAWK-I instrument at the Yepun coolers stopped during VLTI observations device the overall efficiency of the instru telescope has been found to introduce that involve the Antu telescope. ment was measured to have increased additional vibrations into the telescope by a factor 1.5 at 800 nm and by 2.5 at optics, which can affect the performance The CRIRES control software was suc 1000 nm, while the fringing amplitude of the VLT Interferometer and the adap cessfully upgraded over the year to im was reduced from 30% to 5%. This, to tive optics system of the NACO instru prove the control and interfaces between gether with very good “cosmetics” and ment at the opposite Nasmyth focus sta the CRIRES instrument itself, the MACAO linearity and unchanged geometry, read tion. To minimise these vibrations, which adaptive optics module and the telescope. out noise and dark current of the detec were introduced by the instrument’s cryo- The new control software correctly imple tor, resulted in a substantial improvement cooler cold heads, HAWK-I was equipped ments the treatment of all differential of the red sensitivity of GIRAFFE. This is with a liquid nitrogen continuous flow wavelength-dependent effects in the ac of great benefit to the numerous science cooling system. This measure has con quisition of science targets on the instru programmes that make extensive use of siderably reduced the vibrations ment slit, the adaptive optics field selec this spectral region. tor and the telescope guider.
34 ESO Annual Report 2008 number if the complexity of the VLTI sys tem is considered. The operational effi ciency of the VLTI is being continuously improved as the alignment and acquisi tion procedures both on AMBER and MIDI are optimised. The acquisition time is less than five minutes with the ATs and ten minutes with the UTs, including clos ing the active and adaptive optics loops. Fringe tracking with FINITO requires an additional four minutes.
The AMBER instrument allows up to three UT or AT beams to be combined interfer ometrically and was offered to the com munity with the FINITO fringe tracker and the ATs for the first time in 2007. After this critical milestone was achieved with the ATs, the VLTI team focused its 2008 ef forts on providing FINITO fringe tracking with the UTs as well. Vibrations of the optical surfaces of the UTs transmitted to Paranal’s new multi-fuel power generator can provide the VLTI had earlier been identified as the up to 2.2 MW of electrical power. The two tanks for primary obstacle to fringe tracking with LPG can be seen in the background. the UTs. In 2008 a vibration suppression system was deployed and fully commis An upgrade of a very different nature, but more easily to the fast-changing market of sioned to, at least partially, overcome the of fundamental importance for the Paranal available energy sources. Currently the vibration problem. This included the in site, was completed early this year: the MFPG runs on the most economical — stallation of accelerometers on all the installation of a new Multi-Fuel Power liquefied propane gas (LPG) — for which main vibrating mirrors of the UTs and the Generator (MFPG) to upgrade the Paranal dedicated tanks had to be installed. The commissioning of the active Vibration power station from diesel generators to a observatory continues to monitor the pos Tracking (VTK) system. FINITO fringe gas turbine generator. Continuous and sibility of obtaining a natural gas supply tracking with AMBER and the UTs was reliable on-site power generation at a re from the commercial gas pipeline passing delivered to the science operations team mote and isolated place like Paranal, close to the observatory. and the community after an extended which requires clean and stable electrical characterisation period in early 2008 just power and cannot be connected to the in time for Period 81, starting in April electricity grid, is absolutely crucial for the The VLT Interferometer 2008. While AMBER at the UTs had pre smooth operation of the observatory. Re vioously been limited by the variability cent experience has shown that a power The VLT Interferometer operated for about of the Earth’s atmosphere to integration station based on diesel generators is a 169 nights of scientific observations with times of 25 milliseconds, with FINITO it is major and costly challenge to run and MIDI and AMBER using UT and AT base now possible to integrate for up to 10 maintain. A very reliable, low maintenance lines in 2008. The remaining time was seconds, equivalent to a theoretical gain multi-fuel gas turbine generator was pur intensively used for engineering and com of a factor of 400. FINITO is now fully inte chased in 2007 and commissioned on missioning activities to complete and im grated into science operations and is schedule at the beginning of 2008. The prove the interferometer infrastructure. used on most AMBER observations with new MFPG has supplied the Paranal Ob The installation and commissioning of the ATs and UTs and is essential for its me servatory with electricity since February new PRIMA astrometric and phase refer dium- and high-resolution spectroscopic and has matched all expectations for reli encing facility started in July and required modes. able and efficient low maintenance opera an investment of 88 nights over the tion. The diesel generators have been course of the year. The AMBER instrument itself was also retained as an automatic backup system upgraded over the year. The new science and are only used for few hours per The technical downtime of the VLTI has detector largely removes interference month to check their availability. The been reduced to 8% of the scheduled noise, clearly improving data quality. Fur MFPG can be supplied by several differ science time — a percentage that is still ther, a fast guiding system (IFG) to stabi ent energy sources, from natural gas to higher than for single-telescope instru lise the flux entering the instrument fibres ship diesel, and this will allow us to react ments at the VLT, but a respectable was designed and commissioned for
ESO Annual Report 2008 35 AMBER. A new set of polarisers elimi La Silla offered for Large Programmes with a nates unwanted spectral fringes, which maximum length of up to four years, i.e., had affected the unique high spectral La Silla Observatory continued to prepare two more years than are available at the resolution mode of AMBER. In general, for the streamlined operations model that VLT. These new opportunities have been the stability of the instrument and the will be introduced in October 2009. In the welcomed by the astronomical commu efficiency of the instrument operation im course of these preparations the SUSI2 nity and a number of Large Programme proved over the year. In November, three imager and the EMMI multi-mode instru proposals have been received. nights of science verification of AMBER ment at the NTT were decommissioned. with FINITO and the UTs were scheduled At the same time EFOSC2 was transferred The number of visitor instruments at to demonstrate the scientific potential of from the 3.6-metre telescope and re-com the 3.6-metre telescope and the NTT this newly offered mode. While the missioned at the NTT to replace EMMI has noticeably increased. AstraLux, unique capabilities of FINITO-supported after 18 years of service. As from Period ULTRASPEC, IQuEye, the Max-Planck- AMBER observations in its highest spec 81 (April 2008) the three large La Silla tele Institut für Radioastronomie Speckle tral resolution were appreciated by the scopes have operated with a fixed set Camera were the successful visitor in science verification team, the constraints of instruments. Instrument changes are struments in 2008. All these visitor instru on observing sensitivity due to the limited now only made to accommodate visitor in ments used the La Silla telescopes to sensitivity of FINITO itself and the still struments. The 3.6-metre telescope now test novel instrumentation, detectors and high level of vibrations became evident. operates exclusively with HARPS, the NTT observing techniques. These ranged The active identification and elimination of with EFOSC2 and SOFI, and the 2.2-metre from lucky and speckle imaging to beat vibration sources in the UT interferometer telescope with FEROS, WFI and GROND. the atmosphere to obtain diffraction- are now the highest priority for the VLTI limited images to photon counting sys team. In addition, as of Period 82, VLT-style tems to explore the application of quan service mode observations are no longer tum statistics techniques to astronomy. The four Auxiliary Telescopes form the supported at La Silla. All observing runs VLTI Sub Array (VISA) and have become are carried out in classical visitor mode In June 2008 a new operations agree the workhorses of the VLT Interferometer. with a minimum run length of three ment was signed between ESO and the Several improvements to the ATs have nights, providing additional opportunities Max-Planck-Institut für Astronomie (Hei been implemented over the year, includ for young astronomers to obtain hands- delberg, Germany) for the continued op ing the newly refurbished STRAP tip-tilt on experience with state-of-the art tele eration of the 2.2-metre telescope until sensors and new focusing devices, which scopes and instrumentation. To encour 2013. As part of this agreement, the ESO are expected to improve the performance age large scientific studies extending community, who are regular applicants of the ATs further. over several years using La Silla instru for this instrument, will receive three ments and telescopes, the NTT and the months of observing time per year with 3.6-metre telescopes have again been the FEROS and WFI instruments.
A view of a rare cloudscape over La Silla, in the southern edges of the Atacama Desert, home of ESO’s first observing site.
36 ESO Annual Report 2008 APEX 200 –5.25 APEX reached its full complement of fa cility instruments in 2008. After the arrival of LABOCA in 2007, the Swedish hetero dyne facility (SHFI) receivers, covering all –5.3 150 four atmospheric windows from 200 to 1400 GHz, were delivered by the Onsala Space Observatory and installed during
the Bolivian winter break in January and ] –5.35 100 February 2008. Bands 1, 2 (replacing eg
APEX-2A) and 4 were made immediately [d ) available to the community while Band 3 00 will be fully commissioned in early 2009. –5.4 20 (J 50 The Shortwave Apex BOlometer Camera δ SABOCA developed by the Max-Planck- Institut für Radioastronomie (Bonn, Ger –5.45 many) was commissioned in September. SABOCA operates at a wavelength of 0 370 μm and provides a field of view of approximately 1 square arcminute using –5.5 an array of 37 superconducting pixels to map large areas of the sky efficiently (see figure on the right). –50 83.9 83.85 83.8 83.75 83.7 This complete suite of new facility instru α (J2000) [deg] ments allows APEX to exploit fully the ex ceptional conditions available at the high SABOCA 350 μm map of Orion altitude site of Chajnantor. observed during the commis sioning run in October 2008. Map units are Jy/beam.
ESO Annual Report 2008 37
Completing a 60-km drive, from the base at Sequitor up to the APEX site, an astronomer finishes his somewhat ex- traordinary route to work at 5000 metres above sea level. Data Management and Operations Division
The mission of the Data Management and Operations (DMO) Division is to pro vide very reliable support in the operation of ESO facilities and to its users in the framework of an integrated end-to-end system, and also to maintain the archive facility and its data holdings as a power ful resource, both scientific and opera tional. For the duration of the E-ELT Phase B, the DMO Division includes the E-ELT Operations Project Office, which is in charge of developing the E-ELT Sci ence Operations plan and of coordinating Science Operations support systems studies. In 2008 the DMO went through an extensive internal restructuring so as to match its core activities better with the departmental structure.
User Support
The User Support Department (USD) of the ESO Data Management and Opera The SABOCA instrument being filled with helium. tions Division released its new, over hauled web pages in mid-December. The pages had undergone a major re-styling the commissioning of two new APEX in – assisting the user community with the so that navigating all the material and struments, the Swedish Heterodyne technical preparation of observing documentation related to the preparation Facility Instrument (SHFI) and SABOCA. proposals; and support of Service Mode observa tions was faster and simpler. The USD also supported E-ELT opera – ensuring that the observing pro tions planning, participated in commis grammes comply with the requirements Preparation for the support of VISTA Pub sioning and upgrade activities (HAWK-I, set by their scientific goals and make lic Surveys has increased during 2008. FLAMES, AMBER+FINITO and X-shooter) efficient use of the facility; A dedicated Public Surveys Phase 2 and observing schools (e.g., the NEON Workshop was held in September at ESO and VLTI schools). It organised a 2.5-day – operating a helpdesk for proposal sub Headquarters, attended by representa Workshop on “Six years of FLAMES mission and the submission of observ tives of all survey teams. This was in Operations”, during which the instrument ing programmes, the delivery of data to tended to present the observing tools to performance was thoroughly discussed principal investigators; the teams and included practical by its most frequent users and ESO sessions. FLAMES staff. – maintaining and refining the ALMA data archive; and Service Mode (SM) has continued to be the most requested observing mode European ALMA Regional Centre – providing feedback to the software de at the VLT: the demand for SM observing velopment teams about the data reduc has been a factor of 2.5-3 times higher The European ALMA Regional Centre tion pipeline and the off-line reduction than the time requested for Visitor Mode (ARC) is currently set up as a network of software systems and all other opera during Periods 81 and 82. The number nodes throughout Europe, coordinated tional critical software. of SM runs supported by the USD at the by a central node located at ESO Head VLT, VLTI and the MPG/ESO 2.2-metre quarters in Garching. In this distributed Although full ALMA operations will only telescope during 2008 has remained network, user support and operations start in 2013, pre-operation activities above 1000 (including Director’s Discre experience at ESO can be mixed with the have already started. The ARCs are or tionary Time proposals). existing millimetre-wave astronomy expe ganising the support system, testing the rience in the scientific community to cre software, writing “cookbooks” and manu APEX Service Mode operations have ate optimal science support services. als and preparing the commissioning and reached a stable modus operandi. Two science verification phase, which will calls for Science Verification proposals Core ARC activities at the central node start in the autumn of 2009. The first Call were issued in connection with consist of: for Proposals for Early Science will be
40 ESO Annual Report 2008 issued in 2010 and the ARCs must be above the ARC core functions. This help The Science Operations Integrated functioning at full speed before then. includes, for example, advanced user Product Team support for special projects and refining ARC staff have been actively involved in the data reduction process. According to the approved version of the the following projects in 2008: Operations Plan, a Science Operations To ensure that the face-to-face help, Integrated Product Team, consisting of – participation in the ALMA Technical Fa which is a project deliverable for the first the three ARC Managers and led by the cility activities; years of operations, is accomplished, a Head of Science Operations, has been Memorandum of Understanding was established. The goal is to set up project- – participation in user tests organised by signed by all partners in December 2008. wide operations, define distinct tasks and the developers of the offline data reduc Funding to support the work of the ARC common goals, supervise science re tion system (CASA); nodes has been sought from the Euro quirements and provide feedback for the pean Community FP7 call: operations related software packages. – in-house testing of the offline system; and – Nine additional ESO Fellows have been funded through the MarieCurie COFUND Data Products Department – participation in user tests of the ALMA programme. Six of these will be sta Observing Tool. tioned at the ARC nodes to pursue their In addition to collecting raw science own research there and to help with and calibration data at its observatories, All the activities of the European central user support activities. ESO processes this data with the dual node and the required manpower are de goal of monitoring instrument perform scribed in the Implementation Plan of the – The European ARC will be partially in ance and delivering processed data and ALMA Operations Plan. cluded in the EC-funded RadioNet ac tools to its community. Also, ESO collects tivities through a JRA (Joint Research highly processed data from Principal Activity), including software integration Investigators (PIs) and makes them avail ARC activities in Europe coordinated by and implementation for ALMA. able through its Science Archive Facility ESO to the community at large. These activi – The ESO ARC coordinates this network ties are grouped under the umbrella of The ARC nodes will provide face-to-face of nodes. Activities started in 2006 and the newly created Data Products Depart help and additional support, over and are routinely discussed and imple ment (DPD). mented with teleconferences and visits.
The ALMA Observing Tool (OT) is the main interface between users and the Joint ALMA Observatory (JAO) at the proposal and scheduling stage of a project. All proposals will be created and submitted to the JAO using the OT, which will also produce the observing scripts required to run the observations. The figure shows a typical view of the OT in its scheduling mode. A spectral visualisa tion of the receiver setup, including the atmospheric transmission curve (purple line), dominates the view. The tree on the left shows the structure of a typical project, which also includes observations with the ALMA Compact Array.
ESO Annual Report 2008 41 Paranal Observatory Data Processing and Quality Control
The Data Processing and Quality Control group works closely with the Paranal Sci ence Operations Department to ensure that the VLT/VLTI instruments (including HAWK-I, in regular operations since April 2008) are always performing within the expected and published ranges. Taking advantage of the newly implemented fast data transfer link, the Quality Control loop between Paranal and Garching is now closed on a timescale of about one hour.
During 2008 the Data Processing and Quality Control group processed more than 8 TB of raw data in 190 000 processing jobs to create 1160 service mode packages with VLT/VLTI data, which were distributed to their respective PIs. The group also packages data from La Silla, but without performing quality Next generation VLT Instrument Control Software checks on them. In 2008, 100 such testing and development in the Software Develop ment Division Instrumentation Laboratory. packages were produced and shipped to the corresponding PIs. worked closely with the Pipeline Systems Phase 3: Returning data products to the Department, in charge of the develop ESO Science Archive Facility Science Data Products ment and maintenance of ESO pipelines, to set priorities that reflect these findings. PIs of ESO Public Surveys carried out The data that astronomers obtain with In parallel, new test data were also taken with the VISTA and VST telescopes, as ESO telescopes at the La Silla Paranal with HAWK-I, and FORS 1 and 2 data well as PIs of all ESO Large Programmes Observatory take a long route before they were analysed with the goal of improving from observing Period 75 on are required can be used by astronomers for scientific the photometry accuracy attainable with to return advanced data products to analysis. This includes taking calibration these instruments. ESO. The External Data Product group is data to characterise the instrument and the Earth’s atmosphere during a particu lar science observation, and running the ESO pipeline software to remove the in strumental and atmospheric effects from the science data themselves. The whole process from planning the observations to producing the final data product has to be carried out with the scientific use of the data in mind. To assure the highest possible data quality, a new group was formed to coordinate the various steps in this process. The Science Data Products group started its work in July 2008. Ini tially, the group undertook an ESO-inter nal survey of the status of data products from all VLT instruments. The survey re vealed a number of areas that apply to several VLT instruments where the sci ence quality can be improved. The group
The ESO data centre.
42 ESO Annual Report 2008 charged with coordinating the activity, – Hubble Space Telescope (HST) archive – Direct data transfer from Paranal began dubbed “Phase 3” by analogy with the support. in July 2008, replacing the old system submission of observing proposals relying on disk shipments. (Phase 1) and the specification of the de The following describes the 2008 high tailed observing strategies (Phase 2). The lights of the activities by the teams pres – HAWK-I and AMBER are now fully sup data products returned as part of Phase ently in the Archive Department: ported by the archive. This includes in 3 are then made available to the commu strument-specific archive query forms nity at large through the ESO Science Ar – An option for the PIs to retrieve their and instrument-specific database tables. chive Facility. This enhances the scientific own raw data prior to the delivery of the value of the ESO Archive tremendously PI Package has been implemented, – APEX weather database in Garching has by complementing its holdings of raw with a starting date of 1 April. More been developed and put into operation. data and pipeline products with highly than a thousand such requests have al processed data products suitable for im ready been served (see also “Archive – The Advanced Data Product query form mediate scientific exploitation. At the time Delivery” below). was released in May 2008. of writing, the ESO Archive holds about 0.7 TB of highly processed data prod – PIs can now obtain their own TAR files – As of December 2008, fully calibrated ucts, corresponding to some one and a from the APEX query form. HST data are ready for immediate half million files. download from the cache, removing the – First test VIRCAM data were archived in necessity for waiting for on-the-fly PIs are offered a standardised procedure June 2008. processing. with a unique entry point for returning their reduced data products to ESO. Ba sic functionalities are in place, including a transfer mechanism using secure copy to Data releases through the ESO Archive: Database holdings: a dedicated staging area, and more will – 30 Doradus HAWK-I Commissioning Data – In 2008 the ESO data flow back-end be added with time. Release databases ingested information on ~1.25 – AMBER/FINITO/UTs Science Verification million raw observation frames, 260 000 Data Release processed science frames and 370 000 Science Archive Facility – Advanced Data Products from zCOSMOS master calibration frames, bringing the DR2 totals to 9.5 million raw files, 1.1 million The Archive Department (ADE) was cre – MAD Science Demonstration Data Release master calibration files and 350 000 ated on 1 June 2008. ADE assumed part – APEX SHFI Science Verification Data processed science files. of the responsibilities from the Data Flow Release – The FITS header keywords repository – VLTI RMN recorder commissioning Data database in the IQ server ingested full Operations (DFO) and Virtual Observatory Release header information from 1.9 million Systems (VOS) Departments, which were – GaBoDS/WFI data release: Version 1.1 frames, both raw and processed. The reorganised. – GOODS/VIMOS Spectroscopy Data total number of new entries is 880 million Release V1.0 rows and a total of 4.3 billion rows. ADE is responsible for the operations of – “Monitor” NGC 2547/WFI Data Release: – The operations log database in the IQ the ESO Science Archive Facility, includ Version 1.0 server ingested 490 million rows, for a ing the following areas: total of 2.9 billion rows. Archive holdings: – data ingestion from the ESO sites in – Total holdings for ESO data: 12.3 million Archive delivery: Chile; files, totalling 94 TB – Unique archive requests from external – Total holdings for HST data: 10.1 million users for ESO data in 2008: 12 250 – raw data ingestion from non-ESO sites files, 20 TB requests for 1.5 million files, totalling or groups as appropriate (e.g. surveys, – New ESO data added in 2008: 2.2 million 26 TB. This includes the requests by WFCAM/UKIDSS); files, 19 TB the PIs for their own raw data: 1035 – New HST data added in 2008: 4.6 million requests for 48 000 files, 2 TB – data delivery to various user communi files, 17 TB – Unique archive requests from external ties (e.g. Paranal Service Mode users, – Total holdings of WFCAM data: 930 000 users for HST data in 2008: 1800 files, 16 TB requests for 240 000 files, 8 TB archive researchers); – New WFCAM data added in 2008: – HST Data delivered via the Download 190 000 files, 3 TB Manager: 9000 files, 0.5 TB – archive/database content management; – Total holdings of APEX data: 95 000 files, – Number of VLT/VLTI PI packages this includes management of the ESO 645 GB deliveries: 1250 data flow front- and back-end data – New APEX data added in 2008: 32 300 – Number of pre-imaging deliveries: 233 bases, as well as offline databases files, 270 GB (library, weather, operations logs, etc.);
– management of archive interfaces; and
ESO Annual Report 2008 43 ADE will face several challenges in 2009. – A public release of the final version of Community Workshop on “Multi-wave The beginning of science operations the ESO/MVM data reduction software, length Astronomy and the Virtual Observ of the VISTA telescope will require much including a configuration editor and atory” on 1-3 December at the European larger data volumes to be serviced, step-by-step instructions for VLT/ISAAC Space Astronomy Centre (ESAC), Madrid. both in terms of the total size and in the reduction. The workshop brought together experts number of files. To improve user interac in multi-wavelength galactic and extraga tions with the archive, we anticipate the – To facilitate the location and retrieval of lactic astronomy and scientists and engi implementation of several new tools/serv ADPs from the ESO archive, a unified neers actively involved in the VO initiative ices, with the most prominent being the science-oriented search interface for in an effort to exchange ideas and get new request handler, the upgraded cali both imaging and spectral data was feedback. The Euro-VO SAC, which pro bration selection tool, an upgrade to the made public. The new interface pro vides scientific advice to the project, met back-end database scheme to provide vides a unique entry point to all ESO twice in 2008: on 11-12 March in Cam a clean-cut separation between the oper ADPs, with the same look and feel as bridge and on 11-12 December in Stras ational and query databases and en the main archive interface. bourg. SAC members were also updated hancements to the archive query forms. on the latest Euro-VO developments. – Several improvements were made to VirGO, the new visual browser to the Virtual Observatory ESO archive, which provides a modern Euro-VO Data Centre Alliance and intuitive way to access ESO data The Virtual Observatory Project Office by displaying the field of view of imag The Euro-VO Data Centre Alliance (DCA) (VOP), created in June 2008 as a succes ing detectors and slits of spectrographs Project mid-term review was held very sor to the former Virtual Observatory on the sky. These include a new user successfully on 10 January in Brussels. Systems Department, has the task of interface, multi-resolution texture load A Euro-VO workshop on how to publish providing Virtual Observatory (VO) input ing for very large preview image or data to the Virtual Observatory was to ESO in general, and to the DMO Ar background surveys, used for Digitized organised at ESO Headquarters by ESO chive and Data Products Departments in Sky Survey colour images, improved and ESA, in collaboration with the particular, and with coordinating ESO’s VO compatibility, and high speed other Euro-VO partners, on June 23–27. involvement in the VO, namely in the optimisations. It attracted about 60 participants and 20 Euro-VO project and the International Vir advisers and organisers. It was geared tual Observatory Alliance (IVOA). The towards data centres and large projects VOP ensures that ESO’s data products Euro-VO Facility Centre to acquire the knowledge and experience are interoperable and up-to-date and that necessary to allow them to become “pub ESO’s voice is heard at the international The Euro-VO project, through its Science lishers” in the VO. In hands-on sessions, level when astronomical data access and Advisory Committee (SAC) and the Facil participants were introduced to VO proto exchange standards are discussed. ity Centre, selected three projects (one of cols in the view of publishing their data which is being supported by ESO staff), holdings through the VO. The VO initiative is a global collaboration which are making use of VO tools and of the world’s astronomical communities applications to carry out astronomical re The Euro-VO DCA project came to an under the auspices of the IVOA. ESO has search. The projects are receiving scien end in December. DCA-like activities will been very active in the VO arena from the tific support and will be completed by continue in AIDA. start and is a founding member of the October 2009. Euro-VO project to deploy an operational VO in Europe. Euro-VO, which is partly VOP staff were present at the third NEON EURO-VO Technology Centre funded by the European Community, has Archival School at ESO on 29 August at established three interlinked structures: the Joint European National Astronomy The eighth and last cycle of the VOTech the Facility Centre, which is hosted at Meeting (JENAM) in Vienna, 8-12 Sep project was completed in December. The ESO and managed in collaboration with tember, where they also manned a Euro- project is now in the close-out phase. the European Space Agency, the Data VO booth with astronomers from other VOP, which is VOTech-like, maintains the Centre Alliance, and the Technology Euro-VO partner projects, and at the 21st Euro-VO project website, which, in seven Centre. International CODATA Conference in Kiev, months of 2008, served 280 GB of con Ukraine, 6-9 October. tent resulting from 1.2 million web hits in A number of so-called Advanced Data 65 000 user sessions. VOP is also in Products (ADPs), or reduced data that The Euro-VO Astronomical Infrastructure charge of the IVOA project website, which astronomers can use for scientific pur for Data Access (AIDA) project started in served 295 GB of web content resulting poses with little or no effort, have been February. AIDA, with a significant contri from 6.2 million web hits in 220 000 user made available. Namely: bution from VOP staff, organised its first sessions.
44 ESO Annual Report 2008 Operations technical support The reliability of operations around critical scopes and the VLT second generation periods such as the late stages of the instruments begin operations. ESO operations rely heavily on the use proposal submission period is ensured and replication of relational databases. by providing overnight support for mis The path towards higher reliability of mis The primary ESO relational database sion-critical computer systems, as well as sion-critical systems extends also to server was migrated to improve mainte by periodically migrating these systems the increase in the safety of the ESO Data nance, ensure the support of new de to more reliable, higher performance Centre inaugurated in mid-2007, which mands, and improve network connectiv hardware. Such improvements must nat currently hosts the vast majority of such ity. The migration to the new server, urally include the primary archive system, systems. For instance, the smoke detec hosting 38 operational databases, has whose migration toward higher density tors, the air-conditioning and the heat improved performance by a factor of storage media has already started to pre exchangers have been serviced, and an five. In parallel, ways to improve and sim pare for the increase in the data holdings extension of the cooling capacity to plify database replication have been that will take place when the survey tele increase the space for new systems and investigated. related hardware is already planned.
ReaderReader ReReport:port: OOldld SySystemstem
800000–0–900000 900000 70000700000–0–800000 600000600000–700000700000 800000800000 50000500000–0–600000
700000700000 40000400000–0–500000 300000–0–400000 600000600000 200000–0–300000
ec 500000500000 100000100000–200000200000 /S 0–10000–1000000 tes
y 400000 b Kbytes/Sec K 300000300000
200000 1638416384 100000 40964096 10241024 0 256256 RecordRecord SSizeize 64 64 128 256 512 16 1024 2048 096 40964 8192 16384 32768 4 65536 31072 1310721 262144 524288 048576 10485761 2097152 4194304 8388608 File SizeSize
ReaderReader ReReport:port: OOldld SySystemstem
20000002000000–25000002500000 2500000 15000001500000–2000000 10000001000000–1500000–1500000 500000500000–1000000–1000000 2000000 0–0–550000000000
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500000 1638416384 40964096 10241024 0 256 RRecordecord SSizeize 64 64 128 56 An example of the consequences of migration of 2562 512 048 16 1024 20482 operationally critical services to higher performance 4096 8192 16384 2768 4 hardware: the input/output performance of the sys 327683 65536 131072 tem supporting quality control operations showed 262144 524288 1048576 2097152 388608 a threefold increase after the latest such migration 419430483886088 FileFile SizeSize that took place in 2008.
ESO Annual Report 2008 45 produced by the ST-ECF in April. in ST-ECF the by produced images galaxy Interacting 59 of 12out
Credit: NASA, ESA, the Hubble Heritage Team (STScI/AURA)-ESA/Hubble Collaboration and A. Evans (University of Virginia, Charlottesville/NRAO/Stony Brook University), K. Noll (STScI), and J. Westphal (Caltech) ST-ECF
ESO and the European Space Agency Following the delay of SM4, a Cycle 16 describing the NICMOS release appeared continued their collaboration through the supplementary call was issued late in the in A&A in November. Space Telescope — European Coordinat year, producing four ESA PIs and an ad ing Facility (ST-ECF). In August, Hubble ditional 32 Co-Is. Attention then switched to enabling the completed its one hundred thousandth extraction and calibration of the extensive orbit, celebrated with an image of NGC The principal focus of ST-ECF technical set of ACS grism observations by tuning 2074 in the LMC taken with the WFPC2. activity continued to be the support of the parameters used in the software and In December, the observatory achieved its the slitless spectroscopy modes offered collecting the direct images and grism highest ever on-target efficiency of 88.5% by several of Hubble’s cameras. By formal exposures into their appropriate “associ for a week by maximising the opportuni agreement with the STScI, the ST-ECF ations”. The slitless mode of the Wide ties provided by a programme that stud carries responsibility for the calibration Field Channel (WFC) delivers spectra with ies astroseismology. and user support for most of these a resolving power R ~ 100 over a wave modes and has developed an extensive length range of 600–1000 nm. There are In September, there was a failure of the suite of software for the optimum extrac about 150 ACS/WFC grism associations NICMOS cryo-cooler system, requiring a tion of accurately calibrated data from covering about 600 square arcminutes of restart. Despite repeated attempts, the grism and prism observations. Following the sky and capable of delivering spectra cooling system is still not operating and it an extensive pilot project using data from to a limiting magnitude of at least 26. The appears likely that further start attempts the principal NICMOS grism mode, the work on the pipeline processing of these will not take place until after Servicing ST-ECF released 2470 individually vali data aims at a preliminary (sampler) re Mission 4 (SM4). Consequently, the cur dated NICMOS extracted grism (G141) lease to the HLA of a few thousand rent complement of operating HST instru spectra as part of Data Release 1 (DR1) sources early in 2009 with a full release ments is limited to: WFPC2, the Solar of the Hubble Legacy Archive (HLA) in of some 20 000 spectra later in the year. Blind Channel of the ACS and the Fine February 2008. Spectra from about 80% This promises to be a highly significant Guidance Sensors that can be used for of all in-focus NICMOS G141 pointings resource of currently unexploited data of astrometric measurements. up to July 2007 are available. A paper unique quality and depth. Considerable
Following the delay of SM4 from October 2008, caused by the failure of redundant on-board hardware concerned with in strument commanding, data formatting and telemetry, intense preparations for the servicing mission are continuing. The launch is currently scheduled for May 2009. SM4 will restore the lost redun dancy as well carry out other mainte nance, including the necessary units to Credit: NASA, ESA and M. Livio (STScI) re-enable full three-gyro operation. In addition to the installation of the Cosmic Origins Spectrograph (COS) and the Wide Field Camera 3 (WFC3) the mission will bring STIS and ACS back to full func tionality. ST-ECF staff are supporting some of these activities — notably the preparations for WFC3 spectroscopy.
Two observing time allocation processes took place during 2008. The Cycle 17 Time Allocation Committee and Panels met during May. Thirty-two of the 197 distinct principal investigators (16.2%) were from ESA member states and they received 531/3411 (15.6%) of available or bits. Also, 210 of the Cycle 17 co-investi gators are from ESA member states.
The nebula near the star cluster NGC 2074 (upper, left). The region is a firestorm of raw stellar creation, perhaps triggered by a nearby supernova explosion.
ESO Annual Report 2008 47 effort has been devoted to improving the As well as working on the content, some In addition to participating in the accuracy of the photometry and astrome research effort is being devoted to devel ASTRONET Infrastructure Roadmap study, try of the targets and this now leads to oping new and innovative methods for ST-ECF and ESO public outreach staff agreement between spectroscopic and searching and retrieving data. As an al were responsible for the layout, printing imaging magnitudes to a level of a few ternative to the traditional “form-based” and distribution of the ASTRONET hundredths and to astrometric discrepan interface where the user has to specify a Roadmap book and executive summary cies with respect to the best catalogues number of values in pre-defined fields, a booklet. (i.e., within the GOODS fields) of little more intuitive Google-like process is be more than 100 milliarcseconds. ing developed to allow the user to exploit Most of the group’s activities are some of the technology used by com described in more detail in issues of the In preparation for the launch and installa mercial search engines, ADS etc. This ST-ECF Newsletter, currently published tion of WFC3, the ST-ECF has been work can be used to enter keywords, descrip twice per year and widely distributed. ing closely with the instrument and HST tors and values in a string and have them This was a pioneer publication in astron projects by collaborating on the thermal used by an intelligent parsing mechanism omy desktop publishing and has just vacuum testing of the camera, by prepar to home in on the data being sought. passed its 45th issue. ing the ground calibrations and orbital calibration plans for the infrared and ultra As part of the activity spawned by During 2008, there were changes to violet-visible spectral modes, providing the regular meetings of the ESA and ESO the way in which the Hubble-related out slitless observation simulation support in executives and representatives of their reach activities are carried out. Following the form of the aXeSIM software for Cycle science advisory structures, the fourth of a period of seven months during which 17 proposals and making available a ver the series of ESA–ESO Working Group the ESO Outreach Department was led sion of the well-known TinyTim software reports has been published by the ST-ECF. by the head of the ST-ECF, the ESO and for computing the camera point-spread Entitled: “Galactic Populations, Chemistry Hubble outreach groups have been functions. and Dynamics” and chaired by Catherine merged into a single entity within the Sci Turon and Francesca Primas, this study ence Directorate. Consequently, reports The expertise in slitless spectroscopy de contemplates the forthcoming Gaia mis of the Hubble public information and out veloped within the group has resulted in sion and considers the opportunities reach achievements appear under the collaborations with the EUCLID and for supporting ground-based activities. Outreach heading in this Annual Report. SNAP teams to investigate the suitability of the technique to attain the goals of these missions. Simulations have been carried out using the aXeSIM software and a number of comparisons have been made between ACS and FORS2 observations.
The European HST archive, housed within the ESO science archive facility infra structure, is being shaped for low mainte nance/cost operations from the end of 2010 when the ST-ECF closes. Involving both hardware and software develop ments, data are now being served much faster and more conveniently from an online “cache” that contains the latest versions of calibrated data products. The development of the cache has been carried out in collaboration with the Ca nadian Astronomy Data Centre (CADC). During this process, efforts have been made to improve the quality of the asso ciated scientific metadata and to check the status of the calibration reference files. The STScI, CADC and ST-ECF Cover of the report from the ESA–ESO Working Cover of the ST-ECF Newsletter. together now serve some 35 TB of HST Group on Galactic Populations, Chemistry and Dynamics. data per year to users.
Colour-composite image of the Carina Nebula, revealing exquisite details in the stars and dust of the region.
48 ESO Annual Report 2008
Programmes
A computer rendering of the E-ELT in its enclosure.
50 ESO Annual Report 2008 European Extremely Large Telescope
The Directorate of Programmes was cre 2008 was the second year of the E-ELT In early 2008 the contract for the prelimi ated as part of ESO’s management re- Phase B Design Study. The design phase nary design of the primary mirror support structuring in early 2008 and has resulted for the telescope is largely an industrial was also completed and has also ad in a closer working relationship between activity orchestrated by ESO, thereby vanced to tendering for its FEED con the Telescope, Instrumentation and Tech bringing the construction expertise directly tracts. The contract for the preliminary nology Divisions to achieve its mission into the project at the earliest possible design of the electromechanical unit for of “delivering world class astronomical opportunity. In early 2008, two sets each the tip-tilt M5 mirror has been running well programmes (observatories, telescopes, of preliminary design studies were com and passed its internal milestone of pre instruments) necessary to fulfil the major pleted for the dome and main structure liminary design, allowing the fabrication of aspirations of the ESO astronomical com of the telescope. The designers of the the scale-one prototype unit to start. munity”. It covers E-ELT, the Survey tele main structure drew strongly on their past scope projects, instrumentation develop experience of large telescopes for both Two contracts that have been underway ment and technology. the radio and optical domains. As a result since mid-2007 for the preliminary design of these studies the project has revised and prototyping of the quaternary adap its baseline design for the main structure tive mirror have made good progress to one with an equally good performance, in 2008. Large-scale prototypes are now but a simpler concept, based on two under construction. Besides folding rather than four cradles, seen below. the light, the main function of these two flat mirrors (M4 and M5) is to correct The two designs of the dome have pro wavefront aberrations, caused mainly by vided interesting and profoundly different atmospheric turbulence, and thus to solutions for the structural support of this deliver diffraction-limited images to the massive building. At the end of 2008, telescope’s focal plane. Image motion is ESO tendered for the follow-up to the corrected by the field stabilisation unit, preliminary design studies, the Front End which is a tip-tilt mechanism for the tele Engineering Design (FEED) studies for scope’s fifth mirror, M5, an ultra-light both the dome and the main structure. weight elliptical mirror with a maximum
3D-CAD rendering of the 42-metre E-ELT telescope design.
ESO Annual Report 2008 51 dimension of about 3 m. Higher order ab 100 Pixel sizes currently errations are corrected by the quaternary under consideration for the different E-ELT in mirror, M4, an adaptive mirror with more OPTIMOS struments under study. than 6000 actuators and a maximum di MICADO is a diffraction- mension of about 2.6 m, located close to limited camera, EPICS the telescope’s exit pupil. CODEX a planet imager and spectrograph, EAGLE HARMONI a multi-object near- Two contracts have been running with in infrared spectrograph, dustrial suppliers since the beginning METIS a mid-infrared of the year to fabricate 14 full-scale seg imager-spectrograph, SIMPLE SIMPLE a high resolu 10 ments (seven each) meeting the exact METIS tion near-infrared spec specifications of the final primary mirror. trograph, HARMONI These activities, which include the con an integral field near- struction of sophisticated test equipment, infrared spectrograph, CODEX a high stability, are advancing and the mirrors are already Pixel/Spaxel Size (mas) EAGLE high resolution optical in the fabrication stage. Several other spectrograph and industrial contracts were started in 2008 OPTIMOS a multi- and are progressing. The designs for EPICS object, optical and J-band spectrograph. secondary and tertiary mirror cells are contracted, as is the design for the pre- MICADO focal station. 1
In parallel, significant effort has been 1000 104 placed on establishing the framework for λ (nm) the E-ELT work, including mechanical and electrical standards, interfaces and the basic architecture of the telescope The studies are considering pixel scales explore the scientific parameter space control system. A number of studies for imaging and for spectroscopy (spax for the E-ELT further and to provide fun aimed at understanding the effects of els), which range from seeing-limited to damental input to establish the require wind on large structures better have been the telescope diffraction limit (to be ments of science operations. carried out to characterise the effects of achieved with the aid of adaptive optics. wind generated turbulence within the Science operations mode scenarios have telescope dome. Both wind tunnel exper A detailed examination of the operations been further developed by considering iments and computational fluid dynamics scenarios, staffing plans and infrastruc in detail three observing modes: Service calculations have been used. ture needs for the operations has started. Mode (fully flexible scheduling, without real-time interaction by the user); Remote The E-ELT instrumentation programme is Characterisation of potential sites has Mode (highly flexible scheduling giving advancing well, with ten phase A studies continued. This activity is partly sup the remotely located user the option to (six pre-selected instrument concepts, ported through the EC co-funded FP6 interact with the observatory in real time); two identified through an open call and ELT-DS initiative and a Site Selection and Visitor Mode (non-flexible time allo two post-focal adaptive optics modules) Advisory Committee (SSAC) has been cation with the presence of the observer being carried out by several consortia of appointed by the ESO Director General at the facility). The baseline observing institutes. The scope of these studies is to advise him on site selection, which is mode is Service Mode, whose case is well to verify that instruments capable of ad foreseen for the end of 2009. established as all the science projects dressing the highest priority scientific collected in the DRM can be executed in goals can be built at an affordable cost. The E-ELT programme has been support this mode. Scientists and engineers from over 30 ing the Science Working Group (SWG) institutes in ten ESO member states and work on the Design Reference Mission The requirements on telescope instru one in Chile are involved in this phase. (DRM) for the observatory. Many science ments (derived from the top level scien Two of the studies are led by ESO and cases from the DRM have been exten tific requirements) and operations (which eight by external PIs, in line with the suc sively simulated in-house by a group of include science operations as well as cessful VLT experience, when other insti scientists partly supported by the EC day-to-day engineering and maintenance tutes also contributed to a large fraction through its FP7 initiative. An analysis of activities) and their interfaces have been of the instrumentation. the impact of site characteristics on the consolidated. science cases has been carried out. The instruments under study are focused The E-ELT programme has also focused on exploiting the two unique capabilities of A community questionnaire has been on the overall safety aspects as the the E-ELT: high angular resolution and the launched in order to build a Design Refer top priority for the observatory design, unsurpassed photon-collecting power. ence Science Plan (DRSP) to be used to construction and operation; on quality
52 ESO Annual Report 2008 E-ELT site testing: The E-ELT programme office is currently studying the potential sites for the new The two-year FP7 E-ELT Preparatory 200 European high-tech industries around observatory. Top left: Aklim (Morocco). Top right: Roque de los Muchachos (La Palma, Spain). Bottom Phase programme started on 1 January the E-ELT, organising networks of pro left: Cerro Ventarones (Chile). Bottom centre: Cerro 2008. E-ELT Prep activities are conducted spective instrument builders, and prepar Vizcachas (Chile). Bottom right: Cerro Macon by ESO in collaboration with 26 third-party ing management tools and science ac (Argentina). institutes in eight ESO member states. cess requirements for the building phase. They complement the current detailed E-ELT design in helping to bring the Four R&D areas that will bring advanced policies, in relation to configuration con project to the level of maturity needed for observing capabilities to E-ELT instru trol (hardware, software, documentation); taking the political decision to build. ments are being explored with very good and on performance monitoring. progress made already: 1) ultra-accurate E-ELT Prep activities had their general wavelength calibration techniques, e.g. for The FP6 ELT Design Study initiative has kick-off meeting on 24 January 2008. By low-mass exoplanet indirect detection; 2) been extended to June 2009 to allow the end of the year, 21 of the 24 delivera wide patrol field multi-object adaptive all tasks and milestones to be completed. bles programmed in that first period had optics concept validation e.g. to study the The R&D activities, originally design- been completed. Similarly, of the 15 mile build-up of galaxies in the early Universe; independent, but realigned to the E-ELT stones for 2008, all but two were met and 3) development of a high contrast diffrac specifications in 2006, include studies and one has been re-scoped. Highlights from tion-limited imaging toolbox for direct de breadboards whose results have been 2008 include speeding up the building tection of low-mass exoplanets and 4) fed into the E-ELT design. About two of the E-ELT DRM with feedback from the wide-field imaging multi-conjugate adap thirds of the work packages completed community at large, rallying more than tive optics performance evaluation, e.g. to their tasks in 2008. perform stellar “population archaeology”.
ESO Annual Report 2008 53 Survey Telescopes
The VISTA 4.2-metre infrared survey tele scope, being developed for ESO by the UK Astronomy Technology Centre in Edinburgh, is part of the UK in-kind entrance contribution to ESO. A key mile stone for the project in 2008 was the ar rival of the primary mirror on Paranal. This is the largest F/1 mirror ever produced and proved a very challenging task for the manufacturer. Although the polishing of this mirror took significantly longer than originally anticipated, it finally passed its factory acceptance tests at the manufac turer’s premises in Moscow in early March. It was then air-freighted directly to Antofagasta in an Antonov AH-124 transport plane, finally arriving at Paranal by road on 27 March. In early April the mirror was given its reflective coating of protected silver and installed in the tele scope. This was the final missing piece of the telescope, but the late arrival of this mirror has had an impact on the planned schedule for bringing the telescope into operation. Starting in May, the VISTA 4.2-metre primary mirror being project team began the detailed verifica lowered into the VISTA telescope. tion and commissioning phase of the project. By the end of 2008, VISTA still had a few technical problems, but was in regular night-time use for on-sky tests and commissioning of the advanced data flow system. The ESO acceptance of VISTA and the Science Verification period are scheduled for the first half of 2009, after which VISTA will start regular public survey operations.
Commissioning of the telescope structure and drives for the VST continued on Paranal and its secondary mirror unit was shipped at the end of the year, while its primary mirror cell was being prepared and tested for shipment in early 2009.
VISTA with all mirrors and camera installed.
54 ESO Annual Report 2008 The VISTA telescope at
Paranal Observatory. Credit: ESO/H. Heyer Instrumentation for the La Silla Paranal Observatory
Innovative, high performance instrumen was fully assembled by staff from the anti-reflection coated, deep depletion tation is a crucial component in the suc instrument consortium and ESO and CCD, resulting in much higher red sensi cess of any modern telescope. In the extensive tests confirmed that while no tivity and reduced fringing. case of the VLT and the VLTI, ESO main damage had occurred due to transport, tains a large effort dedicated to the de one of the CCDs had developed a severe Interventions were made to the interfero velopment, maintenance and upgrade of malfunction and will need to be replaced metric instrument AMBER to improve the astronomical instrumentation. The com before the beginning of scientific opera alignment of the detector with respect missioning of a new instrument is always tions. OmegaCAM at the VST and to the spectrograph, as well as to make an exciting milestone and the culmination VIRCAM on VISTA will become ESO changes to the grating wheel and control of many years of work by scientists and workhorses. Together they will enable the electronics. An extensive commissioning engineers. ESO community to perform wide-area run after these modifications showed imaging surveys from the atmospheric much improved behaviour and perform In 2008 the first commissioning run was cut-off in the ultraviolet through to the in ance of the instrument. A further prob completed for X-shooter, the wide-band frared K-band. lem, the Fabry-Perot-like beating of the (U- to K-band), intermediate resolution, phase, was fixed by replacing the polaris high efficiency spectrograph and the first ers in October. of the second generation VLT instruments. Upgrades and repairs Activities at ESO during the first half of As part of the ongoing effort to reduce 2008 included integration of the instru An important way of improving instru the level of vibration seen by the VLTI, a ment backbone and ultraviolet-blue and ment performance over time at relatively plan has been developed for either visible spectrographs from the Danish and modest cost and effort is to upgrade ex removing or damping the closed cycle Italian consortium partners and the near- isting components and subsystems as cooler vibrations in cryogenic instru infrared spectrograph from the Nether the technology develops. This is particu ments. The HAWK-I infrared imager was lands, along with the control electronics larly important in the case of detectors, the first to be modified, with its radiation and software. The flexure compensation an area of technology that is still under shield and cold structure cooling con system, which corrects for flexure in going rapid development. The GIRAFFE verted to circulating liquid nitrogen. Al the backbone, was tuned and made to medium-high resolution visible spec though one closed cycle cooler was still work reliably, and the remaining hardware trograph, which is used with the FLAMES kept for the detector and filter wheel issues in the spectrographs were ad fibre-positioner, had its CCD replaced cooling, the resulting reduction in vibra dressed with the help of consortium part in April and May by a new E2V two-layer tions was significant and removed the ners. The first commissioning run on UT3 was conducted without the near-infrared spectrograph and confirmed that all major ultraviolet/visible performance require ments had been met. The near-infrared spectrograph remained in Garching during this period so that its image quality and the reliability of the cryogenic housekeep ing electronics could be improved. These issues have now been resolved and the near-infrared spectrograph will be com missioned in March 2009.
OmegaCAM, the VST camera, was shipped to Paranal in 2008 to ensure that a reliable working camera would be operational for the commissioning of the VST in 2009. Its mosaic of 8 x 4, 2k x 4k CD44-82 charge-coupled detectors (CCDs) covers a field of view of 1 degree x 1 degree on the sky. The instrument
X-shooter mounted on the VLT at the Cassegrain focus of UT3. The orange mass is a 500 kg dummy weight representing the near-infrared spectrograph. It will be replaced by the real instrument in March 2009.
56 ESO Annual Report 2008 instrument as one of the major sources of The Adaptive Optics Facility (AOF) is and SPHERE passed its Final Design vibration on Yepun. CRIRES will be retro a major project to upgrade one of the VLT Review and a full-scale prototype demon fitted with low vibration closed cycle cool 8.2-metre telescopes, Yepun, with an strating the required computing power ers early in 2009. adaptive secondary mirror, four laser for SPHERE and the AOF was completed. guide stars and two adaptive optics mod The optical test-bench, ASSIST, to be ules: GRAAL for HAWK-I and GALACSI built by the Netherlands to test the com Instruments under development for MUSE. The aim is to provide both plete system in Europe before shipping instruments with “enhanced seeing” per it to the observatory, passed its optical ESO maintains an ambitious large pro formance and also to achieve diffraction- Final Design Review. gramme of new instrument construction limited performance in a small field of for the VLT and VLTI. In general, new in view for MUSE. Substantial progress was Both GRAVITY and MATISSE are second struments are constructed with a major achieved in the design and start of manu generation VLTI instruments designed involvement from consortia of European facture of the various subsystems during to combine four telescopes (either UTs or institutes. the year. The Deformable Secondary ATs). They were recommended by the Mirror (DSM) manufacture has advanced STC, endorsed by Council at the end of KMOS is a cryogenic spectrometer with well, with the start of machining of the 2007 and started preliminary design as 24 deployable integral field units. The 1.1-metre Zerodur back-plate, the manu concrete ESO projects at the beginning many motors and mechanisms mean that facture of the hexapod components and of 2008. GRAVITY will operate in the reliability and successful prototyping are the development of the control electron K-band, with low-to-medium spectral res critical. Final design approval was de ics. The GALACSI module successfully olution, and is designed primarily to layed to 2008, allowing the UK members passed its preliminary design and optical detect and measure astrometric motions of the KMOS team to complete cryogenic Final Design Reviews. Preliminary design of stars close to Galactic Centre as well testing of its prototype robotic arms and studies for the laser unit of the Four Laser as the location and orbit of the infrared to demonstrate excellent reliability, with Guide Star have been subcontracted flashes seen there. It should achieve thousands of movements being achieved to industry. The real-time computer plat an accuracy of 10 microarcseconds, without fail. form, SPARTA, used for both the AOF sufficient to measure the gravitational
Similarly, the first tests of a full prototype diamond-turned integral field unit were successful. The project has now entered its manufacturing phase.
2008 was also a successful year for the MUSE instrument team and the project is now into its final design phase. MUSE is a giant optical integral field spectrograph that will slice a 1 arcminute x 1 arcminute One of the 24 field into slits feeding 24 spectrographs. cryogenic R-theta All critical contracts for the optics, includ robotic pickoff ing spectrographs, VPH gratings and a arms used by derotator were awarded and started. An KMOS to select its targets. engineering grade detector prototype was successfully tested with ESO’s new NGC controller, and full CCD procure ment contract for MUSE has now been awarded. The Final Design Review is planned for March 2009.
The VLT planet finder SPHERE will use extreme adaptive optics to obtain direct images, polarimetry and spectra of plan ets. Prototypes of several key compo The 1377-actua nents have been developed and tested tor deformable and the Final Design Review was passed mirror for the in December. The 1377-actuator deform SPHERE instru able mirror was also successfully tested ment after deliv ery to ESO by and delivered to ESO by the manufac the manufacturer turer CILAS. CILAS.
ESO Annual Report 2008 57 potential and general relativistic effects associated with the supermassive black hole at the centre of the Galaxy. MATISSE will observe simultaneously in two differ ent bands, at 3-5 microns (entirely new for the VLTI) and at 10 microns. It is aimed at the interferometric imaging and spectroscopy of dust around young stars, evolved stars and active galactic nuclei.
Interferometer (VLTI)
PRIMA
The year 2008 was marked by the so- called PRIMA Big Bang. All subsystems have reached completion and accept ance in Europe, been installed at Paranal and are now in commissioning. First on- sky results are very encouraging and demonstrate a stable system with good performance. The goal is to offer at least a large part of the multiple PRIMA opera tion modes (for faint phase referenced imaging and astrometry) to the commu nity in 2010.
The first two star separators for the Aux iliary Telescopes have been installed on AT3 and AT4 respectively. These sys tems can pick up two stars anywhere in a 2 arcminute field of view and send the corresponding beams to the VLTI labora tory. They can also be used for chopping and counter-chopping.
Functionalities and performance up to PRIMA subsystems during integration on Paranal. auto-guiding have been successfully Above are the optical bench and relay optics structure for the star separators. Below, the fringe tested on-sky. The performance with field sensor units. stabilisation will be tested in 2009. Some coating degradation problems (under warranty) delayed the tests, but with no The new cold camera for the fringe sen astrometric data reduction software and impact on the global PRIMA planning. sor units has been implemented and the differential delay lines, under devel tested in Garching, recovering the stabil opment by the DDL-PAOS Consortium Two additional star separators have been ity requirement necessary for the chal (Geneva Observatory, Heidelberg Ob ordered for the ATs and are being manu lenging astrometric goal of PRIMA. The servatory and Max-Planck Institute for factured, for installation in 2011. The star fringe sensor units, together with the Astronomy in Heidelberg) also passed separators for the Unit Telescopes are un calibration source MARCEL, the PRIMA their preliminary acceptance in Europe der final manufacturing and testing. Coat end-to-end metrology (used on the same successfully. ings were re-done preventively to avoid a test bench) and the PRIMA operation repeat of the problem encountered by the software, passed their preliminary ac All these systems were installed at Auxiliary Telescopes. The final systems ceptance in Europe successfully in June Paranal during a seven-week period in should be delivered by the end of this year 2008. Shortly afterwards, the PRIMA July and August 2008 dedicated exclu and installed soon after in Paranal. sively to the PRIMA Big Bang. The efforts
58 ESO Annual Report 2008 10 Typical fringe tracking performance (K-mag = 7.6; seeing = 0.75”; t0 = 5 ms; B = 64 m) – Top graph: 8 measured optical path difference (blue), measured group delay (red), corrections applied to the delay 6 lines (black) – Lower graph: status of the loop 4 (level 7 = phase-tracking loop closed – level 5 = flux lost, waiting for fringes – level 0 = searching for on 2 fringes). 0
D / micr −2 OP −4
−6 smoothed Group Delay −8 Phase Delay RTOffset −10 0 5 10 15 20 25 30 8 6 4 2 OPDC state 0 0 5 10 15 20 25 30 Time / s of the whole PRIMA Garching team, sec these fundamental changes is progress obtained, confirming the power of this onded by a very collaborative Paranal ing smoothly and is also being used to technique for reaching larger adaptive- team and a motivated team from Geneva introduce some improvements to the optics-corrected fields of view. In particu and Heidelberg, culminated in September classical VLTI operations. lar a record two-hour infrared observation with first fringe detection and tracking of Jupiter produced the sharpest whole- with one of the fringe sensor units ahead Naturally much work remains to be done planet picture (and movie) ever taken of schedule. before PRIMA can be offered to the com from the ground (see photo on page 11). munity on a fully reliable and automatic Since then, three commissioning runs basis. Nevertheless, both the Paranal and The high stability and accuracy required have taken place. They allowed opera Garching teams are actively working to for the new generation of high resolution tions in single-feed (without using the star offer the new capabilities that PRIMA pro spectrographs demands new calibration separators) and testing of the capabilities vides for off-axis fringe tracking for deeper systems. A very promising new technique of the fringe sensor units. Fringes were imaging and astrometry with AMBER and is the use of Laser Frequency Combs observed down to magnitude 10 and MIDI. (LFC) developed initially by the Max- tracked to magnitude 9, which represents Planck-Institut für Quantenoptik (MPQ). a gain of about 2 magnitudes relative to In parallel with PRIMA activities, many Since 2007, ESO and the MPQ have been FINITO. The tests gave also a good confi other activities designed to improve the collaborating to adapt this principle to dence level on the stability and reliability overall VLTI performance are underway the specific calibration needs of high res of the fringe sensor units as well as of the and are described under La Silla Paranal olution astronomical spectrographs. The PRIMA metrology (typical results are operations. first major milestone of this programme shown above). Preliminary tests confirmed was reached in March 2008 when spectra the improvement in fringe tracking per from the demonstrator unit were obtained formance when using a faster actuator Demonstrators with the high resolution spectrograph (differential delay lines versus main delay at the KIS–VTT solar telescope on Ten lines). The technique of multi-conjugate adap erife. Measurements were obtained near tive optics (MCAO), first technically 1.5 µm, with a spectral resolution about The general interferometric control demonstrated on-sky in 2007 with the 300 000. The comb line separation was software (interferometry supervisor soft MCAO demonstrator MAD, went through exactly 10.5 GHz and establishes a “per ware) is also undergoing huge changes a period of science demonstration this fect ruler” for spectral calibration. Further to adapt to the PRIMA subsystems year. Several scientific results were tests of the system performance in the and operation. The implementation of infrared range were made by using the
ESO Annual Report 2008 59 infrared arm of X-shooter in the ESO lab 1583.60713(3) nm and a 1-km long fibre which brought the 1584.5 1584 1583.5 (nm) comb light from MPQ. In the meantime parallel work has succeeded in bringing the LFC into the optical spectral range, Th and further tests are planned for January 2009 with the HARPS spectrograph. Fe Fe Atm Fe Si Atm Fe The Active Phasing Experiment (APE) is a project that has been carried out within the scope of the FP6-supported ELT Design Study to compare methods to phase a segmented mirror. The primary mirror of the E-ELT will comprise 984 hexagonal segments, each of which has to be aligned in piston, tip and tilt with a precision of a few nanometres. APE has four different phase detectors in a single instrument to allow evaluation and com 189.25 189.30 189.35 (Thz) parison under realistic observing condi tions. ESO was the lead organisation 189.312509989(10) Thz for the project and was responsible for the development of the test bench, the 61-segment active mirror and a Shack- 1584 1582 1580 1578 1576 (nm) Hartmann Phasing Sensor (SHAPS). The project also had three partner institutes, each of which developed and optimised one specific type of phase sensor. These were the Instituto de Astrofisica de Ca narias (IAC), responsible for the Zernike Unit for Segment Phasing (ZEUS), the Osservatorio Astrofisico di Arcetri (INAF), responsible for the Pyramid Phasing Sen sor (PYPS) and the Laboratoire d’Astrophysique de Marseille (LAM) that 189.25 189.50 189.75 190.00 190.25 (Thz) developed the Diffraction Image Phase Sensing Instrument (DIPSI). An industrial Spectrum of absorption lines in the solar spectrum partner, Fogale Nanotech, developed a with the superimposed regular calibration line se quence of the laser comb. The upper panel shows a dual wavelength interferometer that was zoomed-in portion of the spectrum. used as a metrology system to drive the active segmented mirror. extensive testing in September and De The FP6 ELT-DS also includes a major APE successfully achieved first light at cember 2008, with the emphasis on effort towards developing and testing the visitor focus of Melipal on 6 Decem dynamic performance and friction control. adaptive optics technologies, including ber 2008 when all phase sensors were With the kinematics of large-scale struc mirror technologies, actuation mecha able to demonstrate closure of the con tures, this technology may be seen as a nisms, sensing techniques, and control trol loop. Measurements will continue into cost-effective alternative to hydrostatic strategies and algorithms. Detailed design 2009 to be able to evaluate the perform bearings and direct drive, which are far reviews of mirror prototypes with low and ance under various conditions and with more demanding in terms of dimensional medium actuator density were passed in reference stars of different brightness. tolerances. Results so far indicate that April 2008, and preproduction actuators the (inevitable) loss of performance were ready for integration and testing by A breadboard to test and characterise should be manageable. Another advan the end of the year. A demonstrator with a friction drive, bearing and hydraulic tage of the friction drive and bearing a high actuator density (piezo-curvature whiffletree system was designed and built technology is the reduced risk of oil pol deformable mirror) was manufactured by by AMOS within the framework of the lution above the primary mirror compared autumn 2008 and will be tested in spring FP6 ELT-DS initiative. It went through to that from a hydrostatic bearing. 2009.
60 ESO Annual Report 2008 The APE instrument being lowered onto the Nasmyth platform of the 8-metre Melipal Unit Telescope, on Paranal.
Detectors extend the pre-development of HgCdTe Meudon for the SPHERE instrument. A avalanche photodiode arrays. The 4k x 4k engineering grade CCD231 de Detector development and delivery to in AQUARIUS 1k x 1k mid-infrared array, tector for MUSE was delivered to ESO in strument projects remains an important funded by ESO and developed by May and found to meet requirements. area of work for the Instrumentation Divi Raytheon, is expected to become the A contract was signed with E2V for deliv sion. Low noise, high speed detectors new state-of-the-art device for ground- ery of five deep depletion (red sensitive) are critical to the successful operation of based applications in the thermal infrared. CCDs for installation in VIMOS. adaptive optics systems. Funding through The multiplexer design was completed FP6 OPTICON and ESO has allowed in November, with the first devices ex The development of the NGC, ESO’s New the development at E2V of the CCD220, pected next year. In the meantime, hard General detector Controller, which com which aims to achieve sub-electron read ware is being optimised and developed bines, and significantly expands, the ca noise at KHz frame rates. In addition LAM in preparation for the high data through pabilities of its predecessors FIERA (opti (Marseille) and LAOG (Grenoble) have put resulting from the 150 Hz frame rate. cal) and IRACE (infrared), is reaching a been developing the OCAM test control steady-state production phase with first ler/camera for delivery to E2V for testing The first substrate-removed Hawaii-2RG deliveries having been made to MUSE, and acceptance of the detector. Some array received by ESO was installed in KMOS, and SPHERE in 2008. A record 15 AO detector systems will need to be the infrared arm of X-shooter and has re low read noise of 6.9 e– rms was achieved built between 2009 and 2011 with the sulted in the complete disappearance with simple double-correlated sampling CCD220 as the baseline detector. High of the strong fringing seen initially with an on the first science-grade Hawaii-2RG performance AO detectors are also criti older, non substrate-removed, device. detector for KMOS. In 2008 development cal to the E-ELT and during 2008 three In addition complete ultraviolet-blue and continued of faster variants for use with fixed-price contracts were awarded to visible band CCD systems were supplied high speed infrared detectors in the E2V, Sarnoff and Teledyne to develop for the X-shooter instrument. The first thermal infrared and for interferometric technology demonstrators that meet the KMOS 2k x 2k detector system will instruments, an adaptive optics version noise and speed requirements. In the be delivered in early 2009. A complete of NGC with sustained frame rates of area of infared wavefront sensors, a con 4-channel Hawaii-1 assembly has order 1 kHz, and an interface to the AO tract has been placed with SELEX (UK) to been delivered to Observatoire de Paris/ real-time computer system SPARTA.
ESO Annual Report 2008 61
Auxiliary Telescope 2 arriving at its new observational position. This configuration with the other ATs is one of the most ex treme for the interferometer. Technology Developments
Laser guide stars are an essential require laser and yet much simpler to build and to assess their suitability for the E-ELT. ment for advanced optical telescopes. maintain. The system uses Raman fibre Under the general name, E-ELT Technol The adaptive optics systems used to cor amplification at 1178 nm with conversion ogy Demonstrator Programme, several rect atmospheric turbulence require a to 589 nm using a high efficiency fre studies have been carried out in 2008 to bright reference star close to the science quency doubling LBO-based cavity. evaluate new standards, determine mar object being observed. Unfortunately, ket trends and estimate future develop the number of stars available in the sky of Another important breakthrough in 2008 ment potential. In many cases these sufficient brightness is very limited and has been the discovery, through detailed studies have been backed up by labora these only allow a very small fraction of simulations of the mesospheric sodium tory evaluations. This work has already the sky to be observed in this way. A atom transitions and atmospheric condi led to recommendations or decisions in laser guide star overcomes this problem tions, that by optimising the laser spectral several areas important for the control of by projecting a powerful laser beam, and temporal formats, a substantially the E-ELT. These include adoption of tuned to the sodium D2 transition wave higher laser guide star brightness can be Ethernet as the future real-time field bus; length, along the telescope axis. This obtained without increasing the laser the IEE 1588 standard for precise sub- excites sodium atoms in the upper at launch power. If confirmed through ex microsecond time synchronisation; MIMO mosphere to create an artificial reference perimental verifications planned for 2009, (Multiple Input/ Multiple Output) control star anywhere in the sky. ESO, together this could lead to a significant reduction systems and multi-core processor tech with Max-Planck Institutes in Garching in the cost of the lasers for the E-ELT. nology capable of large matrix calculation and Heidelberg, developed and commis operations for the E-ELT active and adap sioned the Laser Guide Star Facility in ESO technical standards, and electronic tive optics systems. Siemens Program 2006, as described in the 2007 Annual standards in particular, have always mable Logic Controllers (PLC) products Report. This is currently in regular opera played a major role in assuring the long have been an ESO standard for many tion on UT4. term serviceability and maintainability years. A more recent innovation has been of ESO’s major projects like the VLT. With the certification of certain product lines Unfortunately, lasers suitable for adaptive a very large number of components pro for the implementation of safety critical optics correction are not commercially vided by many different commercial firms industrial automation systems. These available. The LGSF, although successful, and institutes, it is clearly important to Safety PLCs are widely used in the indus is complex, requires skilled maintenance maximise the commonality of the hard try and use certified programming blocks support on Paranal and does not deliver ware to reduce the number of spare parts for safety-critical applications. They enough power for future ESO projects. needed at the observatory, to minimise would allow a simpler and safer way to The Technology Division has therefore the training needed for maintenance staff implement interlocks and other E-ELT been undertaking an R&D programme and to simplify upgrades. The standards safety systems and form a natural exten to develop the laser technologies needed developed some 15 years ago for the VLT sion to the previous PLC standards. to achieve powerful, robust and cost- are no longer appropriate for the E-ELT Siemens Safety PLCs have already been effective sodium lasers for current projects project. In 2007, a programme was there used for the implementation of interlock like the VLT Four Laser Guide Star Facility fore started to test and benchmark key and safety systems for both PRIMA and and the future E-ELT laser systems. This technologies available on the market, and the X-shooter cryo-controller. programme comprises both computer simulations as well as the development of laboratory prototypes as technology demonstrators. We have also worked closely with industrial firms for the devel opment of the final turn-key production units. The transfer of ESO-developed laser technology to industry, which has many potential applications outside as tronomy and which led to a patent appli cation in 2008, is a good example of how the organisation can provide indirect long-term benefits to the economies of its member states.
A significant achievement in 2008 was to obtain a stable 14.5 W CW output power at 589 nm with less than 3.5 MHz line- width, a figure unequalled elsewhere. It is about three times brighter than the LGSF
Safety PLC Technology Demonstrator.
64 ESO Annual Report 2008 Although commercial off-the-shelf prod ucts are preferred wherever possible, it is sometimes necessary to develop in- house designs where no suitable prod ucts can be obtained commercially. An example in 2008 was the production of a four-channel version of the standard ESO CANbus motion controller. The first deliv ery of these units to second generation VLT instruments is planned for July 2009.
Telescopes are becoming more and more complicated, with a huge number of de pendencies between the various subsys tems. The design of such a system is largely driven by the top-level require ments of the project. These top-level re quirements then generate, together with available design solutions, requirements for subsystems at lower levels. Keeping track not only of the requirements, but also the continual changes to the require ments and their dependencies, can now adays be supported by modern dedicated software for requirement management. Essentially, the heart of such a software package is a database that is broken down into modules for every subsystem at all levels. There are many advantages related to this approach compared with the traditional approach. Firstly, each re quirement can be supplemented with at tributes like the rationale, the verification method and comments. Secondly, re quirements can be linked, allowing the system engineer to trace the effect of a change in any particular requirement throughout the whole system. Currently, much of this information is often only in the heads of the designers and based on a variety of data sources making it difficult to retrieve and review. ESO has initiated an effort to introduce these methods into the design process of large and complex devices. The project which would profit most would be the E-ELT. In 2006, a pilot project was launched to evaluate the use of the DOORS requirement management software. This has now been applied to the E-ELT project. To date, the structure of the database has been defined and modules have been created for all the top level requirements as well as the specifi cations for some of the subsystems like the pre-focal station and the M4 adaptive mirror.
Routine cleaning and adjustment of the laser guide star facility. ALMA
ALMA antennas at the Opera- tions Support Facilities. The Atacama Large Millimeter/submillim eter Array (ALMA) is a highly sensitive, high resolution array of telescopes being built on the high altitude plateau, Llano de Chajnantor, in northern Chile. The ALMA Observatory will operate at least 54 antennas of 12 metres in diameter and 12 antennas of 7 metres in diameter in an interferometric mode. Each antenna will be equipped with seven receiver bands, with the option of installing three more re ceivers, thus covering a frequency range from 30 GHz to 950 GHz (equivalent to a wavelength range of about 0.3 mm to 10 mm). ALMA construction is in full swing and 2008 marked important deliv eries to the site in Chile.
Site construction work
The ALMA Observatory comprises two sites. One site is the ALMA Operations Support Facilities (OSF) at an altitude of 2900 m near San Pedro de Atacama, The road from Chilean Highway 23 to the ALMA sites. Chile. The OSF is the operations centre for the entire ALMA Observatory and Surfacing for this access road, which is over the duration of the project. During is also where the final assembly of the still a gravel road, was planned and spec 2008 it accommodated all ALMA staff antennas produced by the contractors ified during the year 2008 and will be ten and contractors, who live in temporary takes place. The Assembly, Integration dered in early 2009. Construction will camps for up to 500 people and work and Verification (AIV) for the antennas start in June 2009 and be completed in either at the OSF or the AOS. Most ALMA and other advanced equipment will be late 2010. staff are involved in supervising construc completed there before they are moved tion activities, AIV activities or the start to the Array Operations Site (AOS), lo The OSF includes multi-functional facili up of operational activities of the observ cated at 5000 m altitude on the Llano ties that will host a number of activities atory. Contractors are mainly involved in de Chajnantor, 28 km from the OSF.
Operations at the AOS are limited to an The two ALMA antenna transporters during tests absolute minimum by the harsh environ between the OSF and the AOS. One is loaded with a “dummy antenna”. ment. The antenna foundations, together with road links and an electrical and a fibre optic cable network are under con struction there. The AOS Technical Build ing will house the correlator, which will process the digitised signals from the an tennas before they are transmitted further via fibre optic lines to the data storage fa cilities at the OSF.
The OSF is connected to Chilean High way 23 by a 15-km-long access road, which then continues for a further 28 km to the AOS. The OSF–AOS link road is up to 14 metres wide, so that the antennas can be moved between the two sites by a special transport vehicle. The new gate house, at the intersection of the ALMA road with the highway, was completed in 2008.
ESO Annual Report 2008 67 antenna construction at the OSF, con struction of the antenna foundations at the AOS and of the interconnecting road systems at the high site.
ESO signed the contract for the construc tion of the OSF Technical Facilities in August 2006. These facilities were com pleted in February 2008. Subsequently, and in the course of occupying the build ings, additional user requirements surfaced and are being implemented as required.
In 2008 the OSF became the central point for all antenna assembly and AIV activities. Antennas are being assembled at the OSF in three separate areas, one each for the antennas provided by North America (Vertex), Japan (Melco) and Eu rope (AEM Consortium) respectively. AIV activities are being carried out at the OSF The Technical Facilities at the OSF. after preliminary acceptance of the an tennas, and prior to moving them to the AOS. The corresponding work areas for were received and evaluated. Contract permanent power availability on site is Vertex, AEM and Melco have been com negotiations with the potential overhead October 2010. In the meantime power is pleted. Seven additional antenna founda line constructors and electricity compa being provided to the OSF and AOS in tions are being provided on request from nies were ongoing at the end of 2008. In stallations and facilities by temporary Vertex, Melco and AEM. These founda view of the uncertain outcome, other power generators, which will later be tions will be completed in early 2009. options for ALMA’s electricity supply were used as part of the permanent power being pursued. back-up system of the observatory. Significant construction activities, led by ESO, began at the AOS area in 2008. Proposals for a 23-kV power system The design of the ALMA Santiago Central ESO signed a contract for the construc (transformers, switchgear and power line Office has been completed and the tion of 192 antenna foundations on 17 from the OSF to the AOS) within the ob construction of this facility has been ten October 2007. Approximately 30 founda servatory have been received and evalu dered. Proposals were received and tions have been partially completed. ated. The target date for the start of evaluated in December 2008 and the
The AOS Technical Building and the AOS Transporter Hangar have been com pleted. The excavation and grading work for the ALMA central cluster is close to completion. Work on the interconnecting road network, led by our ALMA North American partner, has begun.
Supplying electrical power to an observa tory at altitudes of 2900 and 5000 metres in the Chilean Atacama Desert is not a trivial task. Following a call for tender, pro posals for the construction of an overhead line connecting the observatory to the electricity grid in northern Chile have been received and evaluated. Simultaneously, proposals for the supply of electricity
One of the 192 ALMA antenna founda tions at 5000 m altitude at the AOS.
68 ESO Annual Report 2008 contract will be placed in early 2009, with The Technical Building completion scheduled for August 2010. at the AOS.
Antennas
In 2008 the activities of the ESO ALMA Antenna group concentrated on:
– trial assembly of the first antenna in Europe;
– follow-up of the antenna serial produc tion; and
– testing and acceptance of the two ALMA antenna transporters at the OSF. Architectural design of the ALMA Santiago Central Office. The Project Plan for the ALMA serial an tenna contract with the AEM Consortium (Thales Alenia Space, European Industrial Engineering, and MT-Mechatronics) in cludes a trial assembly of the first antenna in Europe. This trial assembly started in January 2008 on the premises of the company Asturfeito (Spain), a subcontrac tor of the AEM Consortium and the sup plier of the steel structure. One 3.6-metre diameter azimuth bearing was set on the Assembly of the receiver first antenna base and the antenna yoke cabin on the steel structure for testing in structure installed. In the following weeks Europe. extensive tests were performed to verify that the very tight tolerances demanded for the stability of the azimuth axis were achieved. Despite considerable efforts in adjusting the antenna it became evi dent that the required performance was not achieved. Based on test results and detailed analyses, intensive investigations began.
The results showed that, due to the asymmetric configuration of the system with a triangular base, deflections in the azimuth bearing were potentially affecting the performance of the antenna and the azimuth strip encoder. In late spring the AEM Consortium provided a compre hensive set of analyses and proposed a design modification inside the base that ESO approved. In parallel to manufactur ing the modified bases, the AEM Consor tium continued to prepare the trial as sembly of the first antenna according to the original design.
ESO Annual Report 2008 69 As a result of detailed studies of the as evaluating compliance with specifica AEM put a great deal of effort into the lo sembly plan, and so as to minimise as tions, and on examining the associated gistics associated with the transport of sembly time at the OSF, ESO agreed to data packages. equipment to Chile. Various transport jigs AEM’s proposal to extend the scope of have been procured to ensure the contin the tests in Europe. As a consequence, Production of other units and parts con uous flow of antenna parts to the OSF. not only the first receiver cabin (as origi tinued in parallel, incorporating any rele For delicate equipment, like the receiver nally planned), but also the linear motors, vant recommendations from ESO. Con cabin and the BUS, special jigs with the encoders and the electric cabinets siderable efforts have been made by damping structures have been designed were shipped to Spain for trial assembly European industry to reach the nominal and tested so as to reduce the risks of and mounted there. This allowed both the production rate of one antenna every few handling and transport. functionality and the specific perform weeks. By the end of 2008, four CFRP ance of the system to be verified. The receiver cabins were completed and The preparation of the antenna assembly tests were concluded in August. The three BUS units were stored at the fac area and the facility at the OSF was functionality of a number of interfaces tory, ready for transport. Many parts pro largely completed by the end of 2008. In has been verified and the commissioning vided by subcontractors were also inter August, AEM could begin to put together team has benefitted from the initial nally accepted by the consortium, and the assembly and alignment hangar training. were in the process of being prepared for for the BUS, the reflector panels and the transport. These parts include various apex structure. By December the work The trial assembly of the first AEM an sets of quadripods and apexes, subre was essentially completed; in time for the tenna included other elements than the flectors and associated hexapod mecha arrival of the first antenna parts on site. steel structure and the cabin. The Back- nisms, electronic cabinets, heating, venti Planning for the assembly and commis Up Structure (BUS) was assembled at the lation and air-conditioning components, sioning activities was also complete, premises of the manufacturer, Duqueine feed shutters, reflector panels, etc. We subject to a detailed review by the ALMA Composites (France). In late spring a are closely monitoring these activities in project. complete BUS assembly, together with various ESO member states, to ensure the quadripod legs, the apex, the subre that the quality assurance documentation By the end of 2008 the antenna produc flector and its mechanism was com is properly collected. In most cases tion had accumulated delays with respect pleted. A number of reflector panels were the expected production rate for these to the original schedule. A significant also mounted and assembled, with the parts has been reached or will soon be part of this delay is due to a more exten adjusters, to the specified precision. The reached. sive testing programme in Europe than purpose of these activities was to verify the performance of the individual subsys tems, their interfaces and the various as sembly procedures, so that these could then be applied at the OSF assembly site. Personnel from the Chilean contractor in charge of assembling the antennas took part in this phase as preparation and training for the assembly in Chile.
The first modified base was manufactured and ready for trial assembly in October. The steel structure was assembled, aligned and verified for its most relevant performance parameters, including the stability of the azimuth axis. By the end of the year the structure was ready for in spection by ESO personnel.
Numerous other AEM Consortium pro duction activities were carried out in 2008, closely monitored and inspected by the members of the ESO ALMA An tenna Integrated Product Team (IPT). The team focused on inspecting the first items and their detailed implementation,
Antenna BUS at the manufacturer’s premises.
70 ESO Annual Report 2008 systems have not yet been installed, both antenna transporters have been fully op erational since 2008.
The front ends
The design and pre-production activities of the Front Ends (FEs) were closed and serial production started in 2008. The first products were delivered by the front end IPT to the ALMA site.
A few years ago the ALMA Project decided to manufacture a pre-production series of eight complete FE units. Follow ing the ALMA Project Plan, ESO is in charge of providing the Band 7 (270–373 GHz) and Band 9 (602–720 GHz) receiv ers. By the end of 2008 all pre-produc tion receivers had been delivered by the Institut de Radioastronomie Millimétrique (IRAM, Grenoble, France) and the Neder landse Onderzoekschool voor Astronomie First move of a NAOJ antenna at the OSF in (NOVA, Groningen, The Netherlands). December 2008. The pre-production phase was concluded and the full production phase began originally planned. Meanwhile the neces carried out on the safety of the system with Manufacturing Readiness Reviews, sary industrial structure to support the and on the braking system. When loaded, held in July 2008 (for the Band 9 receiv continuous delivery of antenna parts for the total weight of the vehicle is about ers), and in November 2008 (for the Band final integration in Chile was set up. 250 tons and this sets challenging re 7 receivers). quirements on the brake systems. Re ESO is responsible for another major dundant brake systems for the vehicle During the year both IRAM and NOVA component system of the ALMA Observ and several other safety systems, both prepared for the serial production phase, atory, namely the two antenna transport operator-driven and automatic are built hired additional staff, set up additional ers. This project was completed in 2008. into the system. infrastructure and enlarged test facilities During the northern spring, shortly after to respond to the increased production their arrival at the OSF, the two vehicles By the end of April the formal acceptance rate and to comply with the demanding were reassembled on site by the contrac tests were successfully completed in project schedule. Much of the compo tor, Scheuerle Fahrzeugfabrik GmbH presence of ESO and of ALMA personnel. nent production has been subcontracted (Germany), and commissioning tests In June a formal review took place at to industry. NOVA completed the first started. After the first series of functional Scheuerle’s premises and the two trans Band 9 production receiver in December tests without load, the two vehicles porters were accepted. Shortly after 2008. The first production Band 7 receiv started their commissioning with an an wards ALMA moved the first antenna, re ers were in an advanced state of integra tenna dummy. This dummy has the same locating a Vertex antenna from inside tion by the end of 2008 and will be deliv interfaces to the transporter and to the the assembly facility to an antenna station ered to ESO in early 2009. antenna stations as the real antennas. outside the hangar. Further antennas The tests lasted some weeks and in were moved in the following months. ESO has contracted the supply of com cluded various cycles of driving to the pletely functional cryostats for the ALMA AOS site, either unloaded or loaded with In 2009 the ESO Antenna group is plan FE units to the Rutherford Appleton Lab the dummy. The operation of the trans ning to add and commission an active oratory (RAL, Didcot, UK). In turn, RAL porters at the chilling temperatures and in damping system to eliminate the risk of has placed numerous contracts with sub the thin air encountered at 5000 m was oscillations caused by a possible deterio contractors. Some delays have been also tested and the engines tuned as ration of the road profile between the OSF encountered as a result of late deliveries necessary. Beyond the operational as and the AOS. Furthermore, the transport from subcontractors, but the first compli pects linked to the time for driving up and ers will be equipped with an automatic fire ant cryostat vessel was delivered to RAL down and manipulating antennas from extinguishing system. Although these two in December 2008, somewhat behind and to a station, extensive tests were schedule.
ESO Annual Report 2008 71 Credit: NOVA, the Netherlands
Six Band 9 (600-720 GHz) receiver cartridges (of a First ALMA front end assembly ready for acceptance total of eight) of the pre-production series. testing at the European Front End Integration Centre (RAL, UK).
Europe will also provide the mechanical Officer at the end of 2008. He will take up operation without sacrificing the high per housings for the receivers, the so-called his position to support the FEIC in early formance needed. The expert review blank cartridge bodies. ESO has placed a 2009. Several meetings between ESO team scrutinised the design carefully and contract with RAL to provide these car and the JAO management were held with concluded that it was, after closing out a tridge bodies. RAL has manufactured and STFC/RAL to explore options for the opti limited set of action items, to their satis delivered several blank cartridge bodies, mal support and organisation of the FEIC. faction and ready for production. Delivery according to the needs of the partners in This has led to several initiatives to ac of a first set of two WVRs is scheduled the ALMA Project. quire more staff. A new project manager for early 2009. was allocated by STFC/RAL in Septem A first Amplitude Calibration Device (ACD) ber 2008 and new technical staff are be In addition to the European front end was delivered by ESO to the ALMA ing hired. ESO took over some activities, deliverables agreed between the interna Observatory in September 2008. An ESO e.g. providing special test equipment. tional ALMA partners, ESO formed a team assisted in the acceptance and consortium with European institutes installation of the hardware in an ALMA During November and December 2008 a which receive funding from the European antenna at the OSF. This ACD has a proto first complete European front end assem Commission from 2006 to 2010 for the type hot load installed, while the design bly was integrated and was ready for veri so-called “Enhancement of ALMA Early of a final load continues at ESO, with fication by the end of 2008. In consulta Science” project, regarding a number support from expert groups. The design tion with the JAO, it has been decided to of Band 5 (171–203 GHz) receivers. The of the robotic arm used in the ACD has carry out a subset of verification tests so partners are ESO (coordinator) Chalmers been finalised and a production contract this front end assembly can be delivered University of Technology (Gothenburg, was concluded with NTE SA (Barcelona, more rapidly to the observatory in early Sweden), IRAM (Grenoble, France), the Spain) in August 2008. 2009. University of Cambridge (Cambridge, UK), RAL (Didcot, UK) and the University Progress was made on setting up the Omnisys Instruments AB (Gothenburg, of Chile (Santiago, Chile). European Front End Integration Centre Sweden) demonstrated a design for the (FEIC) at RAL. Unfortunately, progress Water Vapour Radiometer (WVR) operat Significant progress was made on this has been slower than originally foreseen ing at 183 GHz at a Critical Design Re project. The Chalmers University group due to staffing issues at both STFC/RAL view in November 2008. The design has successfully passed the Preliminary and ESO. ESO recruited a suitable candi been optimised for production as well as Design Review for the Band 5 cartridge date for the position of FEIC Liaison in April 2008.
72 ESO Annual Report 2008 The back end
During 2008 the ALMA back end entered the production phase and the most impor tant contracts for the manufacture of all ESO back end deliverables were placed:
– 281 digitiser assemblies; – 68 Digitiser Clock assemblies (DGCK); and – 500 photomixers; which will be supplied by the University of Bordeaux, IRAM and RAL, respectively.
The digitiser and the DGCK are both part of the Data Transmission System (DTS) within the antenna back end system. They process and digitise the scientific data before transferring the data through a sin gle optical fibre at a rate of 96 Gbit/s to the correlator located in the Technical Building at the AOS. The digitiser samples the signal produced by the front end and processed by the first stages of the back The ALMA patch panel, installed at the AOS. The end at a rate of 4 Gsamples/second. eight fibres coming from each of the 192 antenna stations are terminated here. The signal is then converted to a digital stream. The DGCK is an accurate pro grammable clock for the digitiser. These in the DTS: the Multiplexer (MUX) and ESO is in charge of supplying the patch components can be fully remote-control the Fibre Optic Amplifier/Demultiplexer panel that allows any antenna station to led and were custom designed to meet (FOAD). The MUX is installed in the an connect to any correlator input and to the functional requirements, as well as the tenna and injects the 12 laser beams en any PLO source. The patch panel and the demanding operating conditions: low coding the scientific data into one single patch cables were manufactured in Eu air pressure, reduced power dissipation fibre. The FOAD increases the power and rope, shipped to the site, installed in the and high reliability. In 2008 we received extracts the original 12 data streams to AOS Technical Building and tested. They 35 digitiser assemblies and all 68 DGCK be fed into the correlator. The production contain more than 4000 optical connec assemblies. is done at ESO, based on the original tors and several kilometres of fibre. design developed at the Jodrell Bank The photomixers are a key component of Observatory. During 2008 20 MUX and the Photonic Local Oscillator (PLO) sys 48 FOAD were manufactured. The FOAD Correlator tem that will provide a timing signal with were shipped, installed and tested at the an accuracy of femtoseconds (10–15 sec AOS, while four MUX were installed in the The ALMA correlator is a specialised onds) to antennas as far as 15 km away first antenna rack sets. The manufacture computer that can process data at a rate from the AOS building. They convert the of the remaining 60 MUX and 32 FOAD in the order of 1015 operations per sec double laser beam generated by the PLO has started. ond. It will operate at the AOS at 5000 m and conveyed through an optical fibre altitude and will be contained in 32 full- into the original microwave reference in During 2008 two complete antenna back size racks. The power dissipation is the range of 80–120 GHz. Each front end end rack sets were assembled at the roughly 200 kW. The first of four correla receiver cartridge is equipped with one Back End Integration Centre in Socorro tor quadrants was installed during the photomixer. The preliminary photomixer (New Mexico, USA). ESO staff partici second quarter of 2008 in the Technical production phase was concluded in 2008 pated in the test and acceptance process Building at the AOS by the North Ameri and devices for the first three front end of these assembled racks, which have can ALMA partner. assemblies were provided. First deliveries been delivered to the AIV team at the of the serial production are planned for ALMA Observatory. One set has already Since its installation the correlator has the first quarter of 2009. been installed in an antenna. Two more been in continuous operation and has sets were completed and will be shipped been tested with self-generated data ESO is also responsible for the production to the observatory in 2009. patterns (as an actual signal from the an of the electro-optical components used tennas is not yet available). This testing
ESO Annual Report 2008 73 has confirmed that no issues related to Computing The main achievements of the computing the peculiar site conditions (which could team during 2008 have been: not be pre-tested in the lab, e.g. cosmic Computing work for ALMA includes not rays) are likely to affect its operations. only the development of ALMA software, – Development of software for Releases but also the procurement of the hardware R5.1 and R6.0. This software includes Each of the four correlator quadrants necessary to install the software at the functionality to support end-to-end contains 128 Tunable Filter Bank (TFB) ALMA sites in Chile. optical pointing, holography, single cards, a sophisticated high speed digital field interferometry and total power filter processor based on state-of-the-art The ALMA software has been planned observations. field programmable gate array technol and developed from the beginning as an ogy. The TFB was developed and pro end-to-end system including proposal – All the above functionality has been duced at the University of Bordeaux un preparation, dynamic scheduling, instru successfully tested at the ATF, which der an ESO contract. The difficulties ment control, data acquisition and for has been in operation for all of 2008. caused by the complexity of the card, in matting, online telescope calibration, data ESO computing staff have made a sub conjunction with the implementation of archiving and retrieval, automatic and stantial contribution to the tests carried the ROHS (Restriction Of Hazardous manual data processing and support for out at the ATF. The ATF results have Substances) requirements, encountered observatory operations. Examples of the been excellent and allowed significant in the early stages of the production, observing tool in the observation prepara progress to be made in view of the were overcome. All 549 units have been tion subsystem are shown on page 41. integration work at the OSF foreseen delivered. A screen snapshot of the spatial editor for 2009. tool, which is used to select a portion of A downscaled version of the correlator, the sky to conduct mosaic observations, The main European development contri the so called “two antenna correlator”, is shown in the figures on the opposite butions have been in the area of the was installed at the OSF to allow interfer page. The figure to the right shows a view ALMA Common Software (ACS), archive, ometry and testing of the antennas there. of the spectral editor tool, used to define observing preparation tools, observatory A similar unit was in operation at the An the frequencies for observation. support software and software engineer tenna Test Facility (ATF) in Socorro (New ing. ESO has also made a major contri Mexico, USA). Once these test activities Work in Europe is organised through ESO, bution to integration and testing and will are complete this unit will most likely be with many software packages being de continue to play an important role once recycled as a supplementary source of veloped by ESO in collaboration with Eu the ALMA software has been delivered to spare parts. ropean institutes, based on agreements the ALMA Observatory in Chile. that run until the end of 2011.
(Top) The ALMA TFB cards to be installed in the correlator.
(Left) The first quadrant of the ALMA correlator in stalled at the AOS.
74 ESO Annual Report 2008 Credit: A. Bridger/United Kingdom Astronomy Technology Centre (Top) Screenshot of the spectral editor.
(Left) Screenshot of the spatial editor.
Main events during 2008 were: System Engineering and Integration performance of the ALMA cryogenic and vacuum system under the harsh environ – Establishment of contracts for: The ALMA System Engineering and Inte mental, transport and operational condi gration (SEI) team covers a wide variety tions. A design for the compressor enclo – Archive computers needed for the of different tasks from design and analy sures was prepared and manufacture OSF site in Chile. A set of 18 com sis of the ALMA system and subsystems. of a prototype is in progress. Test results puters has been tested and is ready It supports the other IPT’s design activi are expected by mid of 2009. for archive deployment at the OSF. ties and chairs and attends design and – Frame contract for the purchase of acceptance reviews. The SEI team is also The SEI team has carried out electromag Oracle licenses over a period of five involved in equipment procurement, sys netic compatibility tests on the Vertex and years for the Archive database of tem integration and verification as well as MELCO antennas as part of the antenna ALMA. system requirements verification. design verification and acceptance. The – Frame contract for the purchase team is also closely following the supply of of the CISCO routers over a period The project-wide requirements and Inter the Computerised Maintenance Manage of five years, to be installed at the face Control Documents (ICDs) are now ment System (CMMS). This project is car ALMA AOS and OSF sites. completed to a level of 95% and 97%, re ried out in close co-operation with the spectively. Maintaining and keeping re ALMA Operations team in Chile and will be – Recruitment of two developers to work quirements under control is one of the handed over to the Observatory in 2009. on the offline ALMA data reduction key tasks of system engineering. The package, and also providing a link with next review of the system requirements The ALMA Product Assurance (PA) group the activities of the European ALMA will be held in 2009 and preparations for is organising and conducting most of Regional Centre. this review have started. the acceptance reviews. The conditional acceptances of the first Vertex and – The annual Critical Design Review The requirements database DOORS is MELCO antennas were supervised by PA (CDR6) was held in Santiago in July, kept up to date and used for verification throughout the whole process in which with ALMA observers representing inte and acceptance. ALMA system block regular meetings were held and inspec gration and commissioning activities. diagrams and the sensitivity budget were tions were done. Existing processes were further refined and used for system de refined and new processes like the Cor – Computing was also reviewed by an sign trade-offs and analysis tasks. rective Action Process was introduced. external review committee in Novem More staff was employed, mainly based ber. The global result was positive. A New activities started on the ALMA cryo in Chile, to support the on site product comprehensive set of comments and genic system. Tests at the OSF and AOS assurance activities. Several audits were recommendations was given. were planned and set up to verify the performed and this will continue in 2009.
ESO Annual Report 2008 75 AIV activities in Chile increased substan Science activities with working on a preliminary report for tially in 2008. The Observatory has made the ALMA Board outlining the highest about 20 new appointments, so that Testing the ALMA software system and profile scientific projects that will not be there are about 45 people now working developing commissioning procedures within the grasp of the baseline ALMA, for AIV. The main tasks of the AIV staff at the ATF was one of the prime activities but could be carried out by upgrading have been the procurement of technical of the Science IPT during the year 2008. the ALMA observatory in the coming equipment to outfit the laboratories, and This activity culminated in December decade. These upgrades could be part acceptance of equipment arriving at the 2008. During the final few days of ATF of the ALMA development plan during OSF, including the first engineering front operations the end-to-end functionality science operations. These plans and the end assemblies, back end antenna com of the ALMA software system was dem scientific synergies between ALMA and ponents, amplitude calibration devices, onstrated for a basic total power science the ELT will be discussed with the ESO etc. Much attention was given to and sig observing mode. The ATF ceased opera community in the next few years. nificant efforts were made in accepting tions after several very successful years the first Vertex and MELCO antennas: as a facility for testing ALMA hardware As part of the FP7 COFUND Marie Curie and software. Testing is now being con initiative, the European Commission ap – Support was given on testing pointing tinued at the OSF in Chile. proved ESO’s proposal to enhance the and surface setting. ESO Fellowship Programme with addi Almost all the science IPT staff required tional fellows, to be hired in 2009 and – Work started on the antenna bracket for commissioning the ALMA array in dedicated to ALMA science. These fel and the ridge installation on the an Chile have been recruited and are partici lows will be based at institutes participat tenna station. pating in the initial tests at the OSF. ing in the European ALMA Regional Cen tre and will be closely linked to the ALMA – The first engineering front end assem The ALMA Design Reference Science Plan activities in Europe. bly and back end elements were in (DRSP) was reviewed; version 2.1 is now stalled in the MELCO antenna. available online. A comparison of the In 2008 ESO has organised four scientific DRSP projects and a pool of ALMA sci and technical workshops related to In the course of the first AIV activities we ence projects proposed by ESO astrono ALMA, in collaboration with RadioNet: concluded that more support and training mers was published in The Messenger. of the AIV staff by the IPTs is needed to This comparison highlighted the scientific – Gas and Stars Dynamics in Galaxies; cope with the upcoming work. Significant expectations from ALMA, expressed by a – Interstellar Medium and Star Formation effort is being made to accelerate the community mostly focused on optical and with ALMA; schedule by organising parallel activities infrared observations. – Simulations for ALMA; and and also by starting commissioning activ – Imaging and Calibration Algorithms for ity, even when equipment is not yet fully The ALMA Science Advisory Committee EVLA, e-MERLIN and ALMA. accepted. has formed a working group charged
Sunset on the last day of ATF operations at the VLA site near Socorro (New Mexico, USA). Credit: L. Testi/ESO
76 ESO Annual Report 2008 One of the ALMA antenna transporters. Software Development The mission of the Software Development IT Department will be a unified Collabora traffic (e.g. viruses, worms, spyware, tro Division (SDD) is to provide software re tion and Messaging system, followed by jans), this is blocked to prevent any suc sources and products to the VLT, ALMA the WEB Content Management System cessful attack. The IPS can be seen as a and ELT projects and to maintain a high and an upgrade of the telephone system. kind of “network anti-virus” system. level of quality while containing the costs. In June 2008 the SDD also took over re The network hardware and topology un sponsibility for general IT services across derwent a major upgrade at all Chilean The Systems Engineering Department the organisation, with the creation of a ESO sites so that newer equipment could dedicated department within the division. be used, redundancy implemented and The System Engineering Department future development enabled. In particular, (SED) provides the development teams The division is organised around three Quality of Service (QoS) was introduced with software engineering services such major development departments, a Sys at all ESO sites to assign guaranteed as the environment and tools to support tems Engineering Department, which pro bandwidth to certain applications. This is the software life cycle, software quality vides services to all development units important to maintain good voice and assurance and control. The department and, as of June 2008, an IT Department. video quality. It also ensures that enough is also in charge of integrating software bandwidth is available so that scientific modules and preparing and validating data transfer from Paranal to Garching releases before they are delivered to the The IT Department can be completed within 24 hours. Secu customer. All planned VLT releases rity is a growing issue for IT. An Intrusion (VLTSW 2008, DFS MAR2008 and Data IT services at ESO were re-organised in Prevention System (IPS) was introduced Transfer) and ALMA software (5.0 and 2008 around functions rather than loca into the ESO network to improve IT secu 5.1) have been successfully validated and tion. The general IT Department consists rity and to cope with the constant threats. deployed. of two groups, one in Chile and one in In 2008 the first IPS was installed in Garching and is responsible for providing Garching, and a second IPS will be in So as to exploit synergies across projects general IT services to the whole organi stalled in Santiago in 2009. The IPS analy SED has created and coordinates a few sation, including support for network and ses network traffic from and to the inter working groups, some with participation communication, general purpose servers net. If it detects any kind of malicious from other departments and divisions, and desktop/laptops, general purpose applications as well as helpdesk. IT pro Automatic test report produced by NRI (example cures, configures and maintains a high taken from VLTSW2009 integration). performance, secure and reliable IT infra structure while ensuring cost-effective ness and compliance with the ESO rules. It provides fast and quality support to all users, whatever the standard platform or operating system used.
The primary focus of the new IT Depart ment was and will continue to be improv ing the service quality and user satisfac tion. Changes in the helpdesk processes have already been put in place. As an example, all tickets are now logged and priorities are being assigned to each ticket so that user requests and issues can be traced and responded to in a quick and effective manner. The impact of these changes will be assessed via User Satisfaction Surveys.
A modus operandi with the IT User Group (ITUG) for adopting ESO-wide IT policies and standards has been defined. A first policy for Windows User rights has been adopted. IT will continue to standardise the desktop equipment used by ESO staff.
One of the main new pieces of infrastruc ture that will be introduced by the new
ESO Annual Report 2008 79 focused on specific areas: software qual An instrument software workshop was requested by the user community possi ity assurance, software quality control organised by the department in collabo ble: since April 2008, PIs can get access infrastructure, testing, virtualisation, soft ration with Paranal Software. The goal to their observational data as soon as the ware change control and software version of this workshop was to provide the con data are archived. 66 000 proprietary files control. sortia building second generation VLT/ have been delivered since the introduc VLTI instruments with all the information tion of this functionality. Platform virtualisation technologies have needed to build control software that been extended in ALMA and introduced meets Paranal’s requirements. Finally, ef The astronomical survey programmes to in the VLT development and test environ forts were also put into preparing a re be carried out by VISTA and the VST ments to optimise resources and invest lease of the VLT common software, which will introduce a paradigm shift with re ments further. Virtualisation will also be supports the newer version of VxWorks. spect to the classic service mode observ deployed on target machines, in close ing. There are very few programmes, collaboration with the operational sites in On the ALMA side, releases of the ACS but either massive, identical observations Chile. are still on our priority list. In 2008, the are carried out on a large set of targets, team participated actively in the software or a large set of very similar Observation Proposals to streamline the software test campaigns, with the goal of improv Blocks (OBs) is executed. The current set change control process and unify soft ing the robustness and quality of the soft of tools to support astronomers during ware version control systems have been ware, as well as clarifying/cross-checking the preparation and short-term schedul presented for implementation in the system requirements with the users. As a ing of observations needed to be adapted course of 2009. result, applications such as the Executive to this new scenario. The concept of could be upgraded. scheduling containers was introduced to The functionality of the ESO software provide the means of expressing schedul quality control infrastructure, called NRI, The E-ELT demonstrator has provided the ing interdependencies. As an example, has been further enhanced and made VLT, ALMA and E-ELT teams with oppor a time link defines a sequence of OBs to more homogeneous between ALMA and tunities for sharing experience, ideas and be executed in a given order, while main the VLT (metrics and reports). concepts. The goal of the project is to taining the relative time intervals for each evaluate potential hardware and software link. The Phase II tools used by astrono Testing takes up a large fraction (two- architecture and technologies that could mers to prepare their Observation Blocks thirds) of the resources dedicated to soft be used to implement the E-ELT tele have been upgraded to support the con ware quality, and special efforts are being scope control software. As an example, cept of scheduling containers, while the made to automate test procedures the teams evaluated middleware technol observing tool generates a priority list of (ALMA and VLT DFS) further, so as to be ogies suitable for a distributed real-time OBs that takes all possible scheduling in able to cope with the wider range of control system and a new data driven formation into consideration. This relieves projects and applications to be tested in approach. the operator from having to sift though the future. hundreds or thousands of OBs to select the best ones to be executed. The Data Flow System Department The Control & Instrument Software The department is increasingly involved in Department The successful deployment of the Data the development of ALMA data flow appli Transfer project was one of the highlights cations. In 2007, it was limited to helping The Control & Instrument Software De of the Data Flow System Department in to develop the ALMA archive. ALMA Ob partment is responsible for the design, im 2008. VLT/VLTI data have been trans servatory operations support tools started plementation and maintenance of control ferred to the archive at Headquarters as development this year and we hope that software for the VLT, the VLTI and their in the data are generated at the observatory ideas and concepts from the experience struments, as well as for ALMA and the since July 2008. The Data Transfer sys with the VLT can be applied. E-ELT. Most of the time spent on the VLT/ tem takes operational priorities into ac VLTI software concerns developing control count (e.g. ToO data will always have a software for its new facilities. In 2008, the higher priority) and makes optimal usage The Pipeline Systems Department department was heavily involved in the de of the high latency network between velopment of software for PRIMA and all Chile and Garching. An additional web The Pipeline Systems Department (PSD) its subsystems, including the fringe sensor application has been developed to pro is responsible for designing, implement unit, fringe tracking, the metrology system vide interested parties such as Quality ing and maintaining data reduction pipe and the astrometric instrument. The Active Control or Science Operations with a lines for the VLT and VLTI instruments. Phasing Experiment, which was installed convenient way of monitoring the queue The department is also developing expo and tested at UT3 in the last quarter of of pending transfers. The introduction sure time calculators, used by the 2008 required a considerable effort on the of the User Portal made the implementa community to prepare their observations. part of our engineers. tion of some of the functionalities/tools The PSD has also participated in the
80 ESO Annual Report 2008 development of the ALMA data reduction LabVIEW GUI cRIO 9014 with: – NI 9505 DC brushed Servo Drive with Encoder system CASA since the autumn of 2008. – NI 9425 32-channel Digital Input Module – NI 947732-channel Digital Output Module Development priorities are determined by a committee involving all the product users, i.e. the Instrumentation Division, Legend Paranal and the DMO. First priority is al Simple TCP/IP Simple TCP/IP Messaging (STM) Messaging (STM) ACS component ways given to the support of the new in struments. In 2008 the X-shooter instru Java C ment and pipeline were commissioned STM Invoke STM ACS service ACS-LabVIEW Bridge Tracking on Paranal. The PSD did not just work on integrating the software into the auto p p ublis ublis General purpose library matic pipeline environment, but also fy fy ti ti h h participated actively in developing some no no Asynchronous reduction recipes. CORBA call ACS Notification Channel The Pipeline Committee also decided Synchronous ALMA Common Software (ACS) CORBA call that it was time to implement support for the spectroscopy mode of NACO and the polarimetry mode of FORS. Both of these High level architecture of the ACS/LabVIEW packages were delivered to the operation prototype for the E-ELT Technology Demonstrator. teams for acceptance during the course of the year.
ESO management decided in 2007 to im prove the quality of the science products generated by existing pipelines on a one- to-one basis. As an example, substantial improvements in the MIDI HIGH_SENS data reduction have been obtained with a new 2D profile estimation method based on the analysis of about 100 Gigabytes of data. This recipe derives the 2D profile of the spectrally dispersed photometric signal and calculates an optimised profile- mask to apply to all observations. In many cases the visibility accuracy could be improved by a factor of 5 to 10. More over, the wavelength coverage was also doubled in most cases.
All ESO pipelines are based on the ESO Common Pipeline Library to facilitate maintenance and sharing of functionali The data transfer monitor - provid ties. They are released for public use ing various views and statistical www.eso.org/pipelines when they have information on the data transfer reached an acceptable level of quality and system, allowing verifcation of the stability. status and detection of possible issues.
ESO Annual Report 2008 81 The ALMA antennas seen from inside the OSF building.
Administration The Finance Department had new tasks New contract negotiations for OPTICON by encouraging the commercial use of to cover in 2008, such as the accounting and RadioNet started in 2008 to ensure technologies developed in relation to and budget activities generated in Chile the continuation of the projects into ESO activities. by the start of ALMA operations and the the 7th Framework Programme. In addi preparation of different scenarios for the tion to these new contracts ESO had The Administration Division is also in financing of the E-ELT, which will need to fourteen EU contracts running in 2008, charge of general safety, facilities man be refined regularly in future; the Finance three under the 7th Framework Pro agement and logistics. Studies have Department also contributed to the work gramme and eleven under the 6th Frame started to remedy to the scarcity of office of the Finance Committee Working Group work Programme. space. on the Financial Governance of ESO with an evaluation of existing international ac A revision of ESO’s Technology Transfer Finally, towards the end of the year, the counting standards. (TT) activities has commenced. Admin Administration became responsible acts as the central point and coordinator for the administrative information systems Much of the Contracts and Procurement of the effort, and is tasked with conclud (ERP) and for Budgets and Financial effort was devoted to supporting the ing a new Technology Transfer policy that Planning. A new document on the Budget ALMA project, specifically, in Chile with supports the technological and financial 2009 and Forward Look for the years respect to site construction activities, and interests of ESO as well as strengthening 2010—2012 was presented to the Finance in Europe in relation to the production of the competitiveness of European industry Committee and Council. the antennas and the front end and back end equipment. Several competitive pro curements were made in relation to the E-ELT project to complement the detailed design activities started in 2007. There has been a high staff turnover in 2008 both at Headquarters as well as in Chile.
The responsibilities of the Administration Division (Admin) were extended to the coordination of the European Union Pro grammes (EU Programmes) and by the Technology Transfer activities of ESO. For coordination reasons, a close collabora tion with the International Relations Office is maintained.
ESO’s long-standing approach towards the EU is to exploit the opportunities arising from the different EU programmes and policies for the benefit of ESO activi ties. In order to maximise the exploitation of EU Programmes, Admin provides ESO management and ESO staff with the necessary information about EU pro grammes and policies, and provides the relevant legal and contractual support Finance Department and coordination. ESO reached a mile staff at work. stone at the EU projects level in 2008 — the first two Marie Curie fellowship con tracts were signed between ESO and the EU Commission, establishing financial support for six fellows to ALMA and one fellow to the VLT.
ESO Annual Report 2008 85 Finance and Budget
Financial Statements 2008 Budget for 2009 (in € 1000) (in € 1000)
Balance Sheet 31.12.2008 31.12.2007 Income budget 2009 Contributions from member states 129167 Assets Other income from member states 11640 Cash and short-term deposits 149 415 144 544 Income from third parties 13322 Claims, advances, refundable taxes and other assets 3095 4488 Various income 7700 Total assets 152 510 149 032 Total income budget 161 829
Liabilities and equity Dues 7007 12 371 Payment budget 2009 Advance payments received and other liabilities 19 538 14627 Personnel cost 59 894 Total liabilities 26545 26 998 Other cost 172148 Cumulated result previous years 122 034 122 205 Total payment budget 232 042 Annual result 3931 –171 Total equity 125 965 122 034 Total liabilities and equity 152 510 149 032 Commitment budget 2009 Personnel cost 59 894 Projects commitments w/o personnel 58 047 Statement of Income 01.01.– 01.01.– Operations commitments w/o personnel 84745 and Expenditure 31.12.2008 31.12.2007 Total commitment budget 202 686
Income Contributions from member states 133 583 134 649 Contributions from third parties and partners 8465 5227 Income from sales and other income 12 400 7643 Total income 154 448 147 519
Expenditure Expenditure for staff 56 410 51 893 Operating and other expenditure 94107 95797 Total expenditure 150 517 147 690
Annual Result 3931 –171
Statement of 01.01.– 01.01.– Cash flow 31.12.2008 31.12.2007
Cash flow from operating activities Receipts Income 154 448 147 519 Net movements on accounts receivable 1414 55 913 Total 155 862 203 432 Payments Expenditure –150 516 –147 690 Net movements on accounts payable –6127 7449 Total –156 643 –140 241 Net cash flow from operating activities –781 63191
Net cash flow from financing activities 5652 –7870
Net cash flow = Net increase/decrease in cash and short-term deposits 4871 55 321
Spiral Galaxy Messier 83.
86 ESO Annual Report 2008
Human Resources One of the main tasks for Human Re All positions were advertised on the ESO improving soft-skills and creating an envi sources (HR) in 2008 was to provide full homepage. In addition, the positions for ronment to implement and embed ESO support for the changes to ESO’s organi Staff Members and Paid Associates were policies. sational structure both overall and within sent out to all members of Council, Fi the Directorates and Divisions. These nance Committee and delegates of other changes resulted in approximately 40 indi ESO Committees, as well as to national Management development vidual reassignments and further definition and international research centres and of about 15 new or amended assign observatories. High priority advertising in During 2008 a Management Development ments, as well as in corresponding recruit appropriate specialist publications/recruit Programme was introduced and started ment activities. The reorganisation of ment web pages was used for selected in parallel in Chile and Garching to sup activities at La Silla continued successfully positions, with the aim of increasing the port managers in their roles. Key areas in throughout 2008, in close collaboration awareness of vacancies across all mem clude: managing styles and managing with the staff and the unions. ber states throughout the campaigns. change; performance management; inter viewing skills and managing teams in a Training and professional development multi-cultural environment. The delivery of Activity In % 2008 also saw the introduction of a coor the modules is over a 12-month period, Accepted new position 26 dinated, transparent approach to the and the first cohort of managers will com Reassignment 38 planning, organisation and delivery of tai plete the programme in mid-2009. The Retirement 6 lored training across ESO, as described training will become integral to the training Planned retirement 9 below. Some corporate training activities of all new and future managers. To sup Early retirement 2 were undertaken to provide support in plement this training, we also delivered Early retirement offered 11 Exiting the organisation 8
La Silla - Redeployment/Reorganisation activities at Project Management 31 December 2008. training.
Recruitment and selection
A new approach to recruitment and se lection was introduced. A review of ESO Guidelines for the recruitment of Interna tional Staff Members and Local Staff Members in Chile led to the introduction new tools, including:
– a Competence framework;
– a Recruitment Interview Pack for Selec tion Board Members; and
– the inclusion of required competences in the advertisement.
Using this new approach, ESO has pub lished vacancy notices for 92 positions and received 2560 applications in total:
Contract Type No. of Campaigns No. of Applications International Staff Member 59 1584 Local Staff 20 783 Paid Associates 13 193
ESO Annual Report 2008 89 training on internal procedural matters in Relations with Staff representatives and The meetings took place in a constructive the area of Annual Performance Reviews. Joint Committees in Garching and Chile and open atmosphere and a shared wish to find mutually satisfactory solutions Regular consultation and interaction with to the various matters. In the course of Project management the International Staff Committee and the year three internal appeals were the Unions in Chile took place. In 2008, a brought to the Joint Advisory Appeals Training in project management was initi total of 20 meetings were held in Garching Board (JAAB) and settled in line with the ated, with the aim of working towards and Vitacura, as well as on the sites in recommendation received. One meeting a common terminology and processes in Chile, to inform, discuss and exchange of the Standing Advisory Committee this area. Initial training has been devel opinion in the areas of organisational de (STAC) took place to evaluate proposed oped in close collaboration with the Data velopments, amendments in policies, amendments to the Staff Regulations and Management Division and the Software regulations, training and individual cases. specific guidelines. Development Division to ensure that training activities address all areas for de velopment. This has been extremely suc cessful and plans are being developed to widen the delivery to other areas of the Administrative Engineers organisation. 18.1% 42.6%
Staff exchanges Technical In order to maximise knowledge manage 10.5% ment and skills transfer, an exchange programme between the Observatories/ the Administration in Chile and the Head quarters in Garching is being tested with a small number of staff. The programme Astronomer/ is being implemented through longer-term Scientists 28.7% missions or temporary transfers.
Summer Student Programme — Chile Distribution of Staff by Job Category — 31 December 2008. In close collaboration with the manage ment of the La Silla Paranal Observatory, a Summer Programme has been intro duced to enable university engineering Sweden Others students over 20 years of age to become 1.3% 14.0% acquainted with our organisational envi Portugal Belgium ronment. The programme supports and 3.5% enables students to practice their ac 1.5% Switzerland quired knowledge and skills — while still The Netherlands 1.2% studying at university — by means of a 4.0% dedicated training programme, which is Czech Italy Republic followed up and assessed by an ESO 15.4% 0.4% supervisor, who has been especially as Germany signed to them. Ten students took part United Kingdom 7.9% 29.6% during the last quarter of 2008, gaining practical experience in the Maintenance France Denmark and Engineering Departments of the 14.6% 3.1% Paranal Observatory. Finland Spain 0.4% 3.3%
Staff Members by Nationality — 31 December 2008.
90 ESO Annual Report 2008 Human Resources representation and collaborations
As a member of the ALMA Human Re sources Advisory Group and involved in the recruitment of International Staff for the Joint ALMA Office/Observatory (JAO), the ESO Human Resource Division has participated in three meetings and contrib uted decisively to a revised classification system, compensation and benefit pro gramme for JAO Local Staff and resource requirements for the JAO HR Department.
The Head of Human Resources has chaired the HR Working Group of EIRO forum since 1 July 2008. Three meetings were held during the year, mainly on the following subjects:
– common training events for scientists and engineers;
– further developments/exchanges on equal opportunities, and in particular, management development for women; and
– working to improve the level of skills in the field of recruitment.
Human Resources also organised and participated in two meetings of the ESO Tripartite Group.
HR administration
Beside a comprehensive and service- oriented contract administration HR handles a wide spectrum of personnel- oriented activities, including operation of the payroll and the social security sys tems, the settlement of about 3700 travel claims, the practical implementation and further development of ESO Rules and Regulations, organising formal Induction Days for new staff members, providing access for the children of ESO staff to a crèche/kindergarten on the Garching Campus (now with 17 places for ESO chil dren), organising medical examinations to ensure that staff are fit to take up em ployment, as well as to work at high altitude when required to do so, and many other tasks.
The Helix Nebula. List of Staff
Office of the Director Directorate for ALMA Directorate of General Programmes
Tim de Zeeuw Thomas Wilson Alan Moorwood
Mark Robinson Josef Strasser
Administration Division Human Resources Software Development ALMA Construction Telescope Division Division Division
Patrick Geeraert Roland Block Michele Peron Wolfgang Wild Roberto Gilmozzi
Mary Bauerle Patricia Adriazola Angela Arndt Roberto Abuter Eric Allaert Constanza Araujo Laura Comendador Andrés Arias Samantha Austin-May Luigi Andolfato Gareth Aspinall Hauck Frutos Juan Carlo Avanti Isabell Heckel Pascal Ballester Fabio Biancat Marchet Dina Arbogast Mary Dinjens-D’Lazarus Michael Böcker Katharina Kammermaier Klaus Banse Claudio Cabrera Mustafa Basbilir Robert Fischer Jean-Michel Bonneau Nathalie Kastelyn Thierry Beniflah Massimiliano Camuri Bertrand Bauvir Karin Hansen Renate Brunner Elizabeth Kerk Peter Biereichel Alessio Checcucci Annalisa Calamida Isolde Kreutle Marcela Campos Katjuscha Lockhart Thomas Bierwirth Emanuela Ciattaglia Marc Cayrel Milla Laaksonen Karina Celedon Betül Meil Reynald Bourtembourg Jörg Eschwey Françoise Delplancke Luis Felipe Lira Claudia Silvina Cerda Anna Michaleli Alessandro Caproni Preben Grosböl Frédéric Derie Claus Madsen Tommaso Di Dio Jorge Moreno Sandra María Castro Christoph Haupt Philippe Dierickx Igor-Félix Mirabel Andrea Dinkel Mauricio Quintana Maurizio Chavan Jennifer Hewitson Giorgio Filippi Thomas Naets Günther Dremel Rosa Ivonne Riveros Gianluca Chiozzi Jorge Ibsen Szymon Gladysz Enikő Patkós Sabine Eisenbraun Francky Rombout Mauro Comin Andreas Kempf Bertrand Koehler Valérie Saint-Hilaire Willem Arie Dirk Eng Marcia Saavedra Livio Condorelli Hervé Kurlandczyk Aybüke Küpcü Yoldaş Rowena Sirey Sonia Garnica Nadja Sababa Paulo Correia Nunes Robert Alexander Laing Samuel Lévêque Massimo Tarenghi Rebonto Guha Heidi Schmidt Dario Dorigo Paul Lilley Jochen Liske Elisabeth Völk Adriana Gutierrez María Soledad Silva Philippe Duhoux Robert Lucas Gianluca Lombardi Priya Nirmala Hein Roswitha Slater Sylvie Feyrin Massimiliano Marchesi Serge Menardi Charlotte Hermant Lone Vedsø Marschollek Vincenzo Forchi Pascal Martínez Samantha Milligan Hans Jahreiss Robert Frahm Rainer Mauersberger Guy Monnet Kristel Jeanmart Bruno Gilli Ferdinand Patt Markus Patig Georg Junker Percy Glaves Gianni Raffi Duc Thanh Phan Katarina Kiupel Carlos Guirao Sánchez Silvio Rossi Florence Puech Hans-Jürgen Kraus Birger Gustafsson Hans Rykaczewski Johannes Sahlmann Caterina Kuo Florian Heissenhuber Joseph Schwarz Marc Sarazin Ignacio López Gil Carlo Izzo Stefano Stanghellini Christian Schmid Qiao Yun Ma Bogdan Jeram Donald Tait Dominik Schneller María Madrazo Yves Jung Gie Han Tan Jason Spyromilio María Angélica Moya Robert Karban Eugenio Ureta Isabelle Surdej Hélène Neuville Mario Kiekebusch Pavel Yagoubov Gerard van Belle Christine Nieuwenkamp Maurice klein Gebbinck Elena Zuffanelli Daniela Villegas Mansilla Oscar Orrego Jens Knudstrup Nataliya Yaitskova Thomas Penker Jonas Larsen Rolando Quintana Antonio Longinotti Andre Ritz Henning Lorch Elke Rose Simon Lowery Johannes Lars Kristian Lundin Schimpelsberger Holger Meuss Guido Serrano Andrea Modigliani Erich Siml Christophe Moins Beatrice Sivertsen Michael Naumann Alexandra Specht Ralf Palsa Albert Triat Moreno Pasquato Michael Weigand Martine Peltzer Yves Wesse Dirk Petry Gerd Wieland Werther Pirani Dan Popovic Eszter Pozna Marcus Schilling Diego Sforna Paola Sivera Fabio Sogni Heiko Andreas Sommer Stefano Turolla Jakob Vinther Michèle Zamparelli Stefano Zampieri Gabriele Zech
92 ESO Annual Report 2008 Directorate of Operations
Andreas Kaufer
Instrumentation Technology Division La Silla Paranal Division Observatory
Mark Casali Martin Cullum Andreas Kaufer
Matteo Accardo Domenico Bonaccini Sergio Abadie Leonardo Gallegos Jorge Miranda Alex Segovia Emmanuel Aller Calia Luis Aguila Rodrigo Gesswein Faviola Molina Fernando Selman Carpentier Henri Bonnet Claudio Agurto Gordon Gillet Juan Molina Waldo Siclari Robin Arsenault Roland Brast Bernardo Ahumada Alain Gilliotte Nelson Montano Peter Sinclaire Gerardo Avila Enzo Brunetto Yazan Al Momany Philippe Gitton Francisco Miguel Nicolas Slusarenko Dietrich Baade Bernard Buzzoni Mario Alfaro Andrés González Montenegro Montes Alain Smette Andrea Balestra Ralf Dieter Conzelmann Jaime Alonso Domingo González Katia Montironi Jonathan Smoker Clémentine Béchet Bernard-Alexis Delabre Nilso Alquinta Javier Andrés González Alex Morales Fabio Somboli Paul Bristow Nicola Di Lieto José Luis Alvarez Leonardo González Sebastien Morel Stanislav Stefl Iris Bronnert Canio Dichirico Paola Amico Sergio González Iván Muñoz Michael Fritz Sterzik Andrew Bruton Martin Dimmler Andreas Andersson Patricia Guajardo Julio Navarrete Sandra Strunk Richard Clare Michel Duchateau Lundgren Carlos Guerra Hernan Nievas Thomas Szeifert Claudio Cumani Toomas Erm Gaetano Andreoni Stéphane Guisard Dieter Nürnberger Richard Tamblay Sebastian Deiries Yan Feng Iván Aranda Serge Guniat Jared O’Neal Mario Tapia Klaas Johannes Dekker Gerhard Fischer Ernesto Araya Fernando Gutiérrez Kieran O’Brien Alexis Thomas Sandro D’Odorico Christoph Frank Juan Carlos Arcos Flavio Gutiérrez Francisco Olivares Manuel Torres Robert Donaldson Domingo Gojak Javier Argomedo Juan Pablo Haddad Rodrigo Olivares Josefina Urrutia Reinhold Dorn Frédéric Yves Joseph Pablo Arias Nicolas Haddad Ernesto Orrego Guillermo Valdés Mark Desmond Gonte Karla Aubel Pierre Haguenauer Juan Osorio José Javier Valenzuela Downing Iván María Guidolin Francisco Azagra Juan Pablo Henriquez Juan Carlos Palacio Karen Vallejo Christophe Dupuy Ronald Guzmán José Báez Cristian Herrera Ricardo Parra Oscar Varas Siegfried Eschbaumer Wolfgang Hackenberg Pedro Baksai Swetlana Hubrig Rodrigo Parra Enrique Vera Enrico Fedrigo Andreas Haimerl Rogelio Bascunan Gerhard Hüdepohl Andrés Parraguez Jorge Vilaza Gert Finger Volker Heinz Juan Beltrán Rodrigo Huerta Marcus Pavez Stefan Wehner Christoph Geimer Guy Hess Guillaume Blanchard Ramón Huidobro Eduardo Peña Ueli Weilenmann Andreas Glindemann Renate Hinterschuster Carlos Bolados Gerardo Ihle Jorge Pilquinao Luis Wendegass Juan Carlos González Ronald Holzlöhner Pierre Bourget Valentin Ivanov Juan Pineda Gundolf Wieching Norbert Hubin Georgette Hubert Stéphane Brillant Nestor Jimenez Andrés Pino Andrew Wright Olaf Iwert Georg Igl Armando Bruna Ismo Kastinen Aldo Pizarro Gerd Jakob Paul Jolley Erich Bugueno Nicholas Charles Andrés Pizarro Lieselotte Jochum Andreas Jost Francisco Cáceres Kornweibel Manuel Pizarro Markus Kasper Lothar Kern Blanca Camucet Carlos La Fuente Emanuela Pompei Hans-Ulrich Käufl Barbara Klein Luis Alejandro Francisco Labraña Hugo Quijón Florian Kerber Franz Koch Caniguante Octavio Lavin David Rabanus Jean Paul Kirchbauer Maximilian Kraus Michael Cantzler Paul Le Saux Andrés Ramírez Johann Kolb Christian Lucuix Ruben Carcamo Cedric Ledoux Claudio Reinero Paolo La Penna Ruben Mazzoleni César Cárdenas Alfredo Leiva Claudia Reyes Miska Kristian Le Louarn Jean-Michel Moresmau Mauricio Cárdenas Gino Leon Miguel Riquelme Jean-Louis Lizon à Michael Müller Giovanni Carraro Ramón Leyton Leonel Rivas L’Allemand Frank Nittel Duncan Castex Christopher Lidman Thomas Rivinius Pierre-Yves Madec Lothar Noethe Mónica Castillo Gaspare Lo Curto Pascal Robert Antonio Ramón Edouard Pomaroli Roberto Castillo Ignacio López Chester Rojas Manescau Hernandez Marco Quattri Jorge Castizaga Fernando Luco Cristian Romero Enrico Marchetti Jutta Quentin Susana Cerda Felipe Mac-Auliffe José Rosas Patrice Martínez Michael Schneermann Cecilia Ceron Agustin Macchino Félix Alberto Rozas Leander H. Mehrgan Babak Sedghi Claudia Cid Gianni Marconi Francisco G. Ruseler Manfred Meyer Armin Silber Alex Correa Pedro Mardones Claudio Saguez Luca Pasquini Arkadiusz Swat Angela Cortes Kiriako Markar Antonio Saldias Jérôme Paufique Roberto Tamai José Ignacio Cortés Mauricio Martínez Fernando Salgado Jean-François Pirard Luke Taylor Jaime Costa Elena Mason Ariel Sanchez Suzanne Ramsay Arno Van Kesteren Reinaldo Donoso Eduardo Matamoros Stefan Sandrock Roland Reiss Véronique Ziegler Javier Duk Rolando Medina Roberto Sanhueza Javier Reyes Christophe Dumas Angel Mellado Pierre Sansgasset Andrea Richichi Michael Dumke Alejandra Mena Jorge Santana Gero Rupprecht Carlos Durán Antoine Mérand Lilian Sanzana Markus Schöller Carlos Ebensperger Steffen Mieske Ivo Saviane Ralf Siebenmorgen Cristian Elao Linda Schmidtobreick Christian Sönke Cristian Esparza Ricardo Schmutzer Jörg Stegmeier Lorena Faundez Oliver Schuetz Stefan Ströbele José Figueroa Nicolas Schuhler Marcos Suárez Valles Erito Flores Mirko Todorovic Juan Carlos Fluxa Sebastien Tordo Eloy Fuenteseca Elise Vernet Sergio Gaete Joël Daniel Roger Javier Gallardo Vernet
ESO Annual Report 2008 93 Directorate for Science
Bruno Leibundgut
Data Management/ Space Telescope-ECF ALMA Joint Office Operation Mattheus Thijs Fernando Comeron Robert Fosbury de Graauw
Paola Andreani Jonas Haase Andrea Verónica Jean-Baptiste Le Paulina Bocaz Angelika Beller Richard Hook Ahumada Bouquin William Dent Andrew Biggs Martin Kümmel Pedro Viana Almeida Silvia Leurini Richard Hills Andrew Burrows Harald Kuntschner Gonzalo Argandoña Karin Lind Richard Kurz Fabien Chereau Marco Lombardi Giuseppina Battaglia Gautier Mathys Jacques Lassalle Thomas Dall Mariya Lyubenova Yuri Beletsky Jorge Melnick Lars Å. Nyman Carlos De Breuck Piero Rosati Thomas Lennart Bensby Ingo Misgeld Pere Planesas Claudio De Figueiredo Britt Sjöberg Stéphane Blondin Margaret Moerchen Russell Smeback Melo Felix Stoehr Henri Boffin Lorenzo Mónaco Nicholas Whyborn Nausicaa Delmotte Jeremy Walsh Jutta Boxheimer Dominique Naef Danuta Dobrzycka Pamela Bristow Nadine Neumayer Adam Dobrzycki Claudio Cáceres Lars Holm Nielsen Nathalie Fourniol Lars Lindberg Carolina Andrea Nunez Wolfram Freudling Christensen Santelices Monika Gotzens Lise Bech Christensen Tania Marcela Penuela Reinhard Hanuschik Blair Campbell Conn Douglas Pierce-Price Evanthia Hatziminaoglou Silvia Cristiani Olga Pinto Moreira Michael Hilker Joana Mafalda da Cruz Anna Raiter Christian Hummel Carmo Martins Suzanna Randall Wolfgang Hummel Cristiano da Rocha Luca Ricci John Lockhart Itziar De Paula Valentina Vincenzo Mainieri Gregorio-Monsalvo Rodríguez Jean-Christophe Gayandhi Manomala Jan Ruppert Malapert De Silva Pedro Miguel Russo Stéphane Marteau Antonio De Ugarte Ricardo Salinas Sabine Mengel Postigo Hugues Sana Sabine Moehler Jörg Dietrich Gina Santangelo Palle Møller Michelle Doherty Julia Scharwächter Sangeeta Mysore Michaela Döllinger Ulf Seemann Petra Nass Brigitta Eder Raquel Yumi Shida Mark Neeser Christopher Erdmann Colin Snodgrass Paolo Padovani Lu Feng Thomas Stanke Ferdinando Patat Andrew Fox Josef Stöckl Isabelle Percheron Matthias Frank Christina Stoffer Francesca Primas Audrey Galametz Cezary Szyszka John Pritchard Alexandre Gallenne Masayuki Tanaka Marina Rejkuba Diego Alex Paula Stella Teixeira Jörg Retzlaff Garcia-Appadoo Leonardo Testi Bruno Rino Mark Gieles Svea Teupke Jesús Rodríguez Ulloa Carla Gil Sune Toft Martino Romaniello Rachel Emily Gilmour Elena Valenti Remco Slijkhuis Raphael Gobat Bram Venemans Dieter Suchar María Eugenia Gómez Giulia Lowell Tacconi-Garman Luis Gonçalves Calçada Ventimiglia-Werner Mario Van Den Ancker Uta Grothkopf Laura Ventura Eelco van Kampen Olivier Hainaut Rein Warmels Ignacio Vera Sequeiros Camilla Juul Hansen Michael West Andreas Wicenec Hans Hermann Heyer Iryna Yegorova Markus Wittkowski Frank Heymann Herbert Zodet Burkhard Wolff Renate Hoppe-Lentner Monica Zorotovic Bodo Ziegler Marc Huertas-Company Martin Zwaan Gaitee Hussain Yara Lorena Jaffe Ribbi Behrang Jalali Gaël James Edmund Janssen Paulina Jiron Iva Karovicova Pamela Klaassen Heidi Helena Korhonen Martin Kornmesser Daniel Kubas
94 ESO Annual Report 2008 Top view of the Paranal Residencia at the ESO VLT Observatory.
Organigram
Director General Office of the Director General Tim de Zeeuw
Directorate for Directorate of Directorate of Directorate for ALMA Programmes Operations Science Thomas Wilson Alan Moorwood Andreas Kaufer Bruno Leibundgut
Software ALMA Data Management Administration Human Resources Telescope Instrumentation Technology La Silla Paranal ST-ECF Development Construction & Operations Division Division Division Division Division Observatory Division Division Division Division Patrick Geeraert Roland Block Roberto Gilmozzi Mark Casali Martin Cullum Andreas Kaufer Robert Fosbury Michele Peron Wolfgang Wild Fernando Comerón
European SDD Finance HR ALMA EU TSD Instrumentation TEC Management DMO Coordinating Outreach Office Department Chile Project Office Office Division Office Office Office Office Facility Off.
Office for Data Flow HR Optical Electronic User Science and FIN Chile ALMA JAO VLTI Logistics Science Infrastructure Garching Instruments Systems Support Data Products Garching/Vitacura
Control / Observing Contracts and E-ELT Optical Mechanical Data Instrument SITE Engineering Archive Programmes Procurement Project Office Detectors Systems Analysis Software Office
System Infrared Optical Science Data Programme CAP Chile Antenna Archive Engineering Instruments Systems Operations Products Scientists
Operations Pipeline Administration Infrared Laser Front End Maintenance and Technical Systems Chile Detectors Technology Support
Integration Virtual Facility, Back End Systems & IT & APEX Observatory Transport And Correlator Analysis Vacuum / cryo Project Office
ALMA E-ELT INS Guesthouse Computing Regional Project Office Center
Facility, System Eng. Adaptive E-ELT DMO Logistics, & Integration Optics Project Office Transport
ALMA Science
This Organigram shows the status of the Organisation as of December 2008.
The main organisational and managerial units of ESO are the Directorates which currently include: the Directorate of Programmes, Operations, Science and ALMA. The Directorates are organised in Divisions. Because of their matrix functionalities the Divisions Software Develoment, Administration and Human Resources have a special status.
ESO Headquarters in Vitacura, Chile.
ESO Annual Report 2008 97 Committees
Flags of the ESO member states flying outside the Headquarters in Garching. Council
The Council is ESO’s ruling body. It dele Vigroux and the Director General. Addi gates the day-to-day responsibility for tionally, Prof. Ewine van Dishoeck was re Council and Committee of Council the Organisation to the Executive under appointed to the ALMA Board for two 2008 ESO’s Director General. The Director years, Prof. Xavier Barcons was elected President Richard Wade General, in turn, reports back to Council to the Board for two years and Prof. on a quarterly basis via two Council Patrick Roche was appointed assessor to Austria Sabine Schindler Meetings and Committee of Council the Board for the same period. (as of 1 July*) Daniel Weselka Meetings, respectively. In 2008, Council Belgium Monnik Desmeth held its ordinary meetings in Prague on At the December meeting Council wel Christoffel Waelkens 3 and 4 June and in Garching on 2 and comed the merged VLT Biannual Progress Czech Republic Jan Marek 3 December. Committee of Council met Report that was presented for the first Jan Palouš in Stockholm on 3 and 4 March and in time and the verbal report from the ALMA Denmark Jens Viggo Clausen Copenhagen on 6 and 7 October. All Director. Henrik Grage meetings were chaired by the President, Finland Kalevi Mattila Prof. Richard Wade. In December Council approved a joint Pentti Pulkkinen agreement with Uppsala University and France Julien Galabru At the June meeting, Council unanimously the Geneva Observatory to carry out Laurent Vigroux approved the accession of Austria to upgrades to HARPS to maintain its lead Germany Andreas Drechsler ESO from 1 July 2008. The delegations ership in the domain of high precision Thomas Henning welcomed Austria as ESO’s 14th member radial velocity studies and to extend its Italy Vicenzo Dovì state. Council also approved the Terms scientific capabilities in return for specified Bruno Marano of Reference and Rules of Procedure for amounts of guaranteed observing time. The Netherlands Jan A. C. van de Donk the STC and the Terms of Reference for Konrad H. Kuijken STC subcommittees. The E-ELT Standing Review Committee, Portugal Fernando Bello chaired by Prof. Roger Davies met twice in Teresa Lago At the same meeting Council unani 2008 to receive updates on progress with Spain Xavier Barcons mously agreed to the reappointment of the Phase-B design study, site selection Jordi Torra Prof. Roger Davies as Chair of the E-ELT activities, funding and instrument studies, Sweden Claes Fransson Standing Review Committee for a period which were subsequently reported to Sofie Björling of two years. Council. (until 31 August 2008) David Edvardsson (as of 1 September 2008) Council commended the successful The Scientific Strategy Working Group, implementation of the recommendations chaired by Prof. Bruno Marano, met twice Switzerland Georges Meylan Martin Steinacher made by the Visiting Committee the in 2008. In February it met to reach con previous year and reported by the Direc sensus on a number of issues, including United Kingdom Patrick Roche Rowena Sirey tor General at the June meeting. composition of the STC and STC sub (until 31 May 2008) committees, its nomination and Terms John Womersley Council received the usual VLT/VLTI, of References for both committees. (as of 1 June 2008) Instrumentation and ALMA Biannual In September it convened to discuss the * as observers, pending completion of the ratification Reports, and the reports from the Chairs policy of ESO “operating beyond its procedure of the Finance Committee, the Scientific budget” for surveys, and address the issue Technical Committee and Observing of spectroscopic surveys (e.g., follow up Programmes Committee. of VISTA, VST, Gaia, etc.). Reports on the Regulations regarding special leave, adop outcome were presented to Council. tion leave and unemployment benefits At its meeting in December, Council bid were discussed and further developed farewell to Prof. Richard Wade whose In 2008 the ESO Tripartite Group met in with the aim to provide corresponding rec term of office as President had come to May and in October. The meetings were ommendations to the Finance Committee an end. Council subsequently elected Dr. chaired by Dr. Patricia Laplaud. The Group and Council in spring 2009. The Tripartite Laurent Vigroux as President of Council received updates on developments on the Group received information concerning for 2009. Prof. Thomas Henning was re- work of the CERN Pension Fund Govern the results of the annual advancement re elected Vice-President for the same pe ing Board, on the terms of appointment view and the progress on measures (reas riod. Mr. Alain Heynen was reappointed for the members of the Governing Board signments, early retirement scheme) taken Chair of the Finance Committee for 2009. as well as on the CERN-ESO Agreement. to adjust the staffing on La Silla to meet Prof. Elias Brinks was appointed Chair of A summary report and conclusions of the the requirements of the La Silla 2010+ the Observing Programmes Committee for ESO Management on the possibility of in operation. 2009 and Prof. Willy Benz was appointed troducing a two-fold Pension scheme as Chair of the STC for the same period. well as the proposed salary adjustment for ESO ended the year on a high note when international staff were discussed and rec Council approved with a large majority the Ex officio membership of the ALMA Board ommended to the Finance Committee and recommendations put forward to extend was confirmed for one year for Dr. Laurent Council. Changes to the Staff Rules and the Headquarters building.
ESO Annual Report 2008 99 Finance Committee
In 2008 the Finance Committee held two ordinary meetings and one extraordi Finance Committee nary meeting, which were chaired by 2008 Alain Heynen. The meetings took place at Chair Alain Heynen ESO Garching. Austria joined ESO as a member state on 1 July 2008. However, Austria Daniel Weselka (observer) until completion of the ratification proce Belgium Robert Renier dure, Austria maintained an observer sta tus on ESO Committees. Accordingly, Czech Republic Jaroslava Jeslínková an observer from Austria attended the last Jiri Toifl ordinary meeting of the Finance Commit Denmark Cecilie Tornøe tee in November. Finland Jaana Aalto The Finance Committee approved the awarding of 22 contracts exceeding France Patricia Laplaud €300000, 15 single-source procurements Germany Matthias Nagel exceeding € 150 000 and six amendments to existing contracts. Four contracts Italy Emanuela De Lauretis concerning the Headquarters extension The Netherlands Coen J. van Riel and the E-ELT have been approved by written procedure. Information was re Portugal Fernando Bello ceived concerning procurement statis tics, forthcoming calls for tenders and Spain Luis Ruiz López price enquiries exceeding € 150 000. The Sweden Johan Holmberg Finance Committee also dealt with finan cial issues (annual accounts, budget, Switzerland Jean-Pierre Ruder cash-flow situation, financial statements, United Kingdom Colin Vincent member state and Austrian contributions) and personnel subjects, concerning International and Local Staff as well as the Pension Fund. These themes were discussed in detail and recommendations were made to Council.
At its extraordinary meeting on 19 Febru ary 2008, the Finance Committee ap pointed the Finance Committee Working Group on the Financial Governance of ESO. The Working Group made sugges tions on procurement document struc ture and content, among other issues, as well as on the drafting of new Financial Rules and Regulations.
A meeting of the Finance Committee.
100 ESO Annual Report 2008 Scientific Technical Committee
STC-68 The STC was presented with upgrade The Scientific Technical Committee proposals for HARPS, which included a 2008 On 16 and 17 April the STC met for polarimetric unit, a laser comb for wave its 68th meeting in Garching. It discussed length calibration, a new Fabry–Pérot cal José Afonso (P) (ESAC Chair, ASAC) the new STC and subcommittee struc ibration unit, new fibres and a new ultra- Rafael Bachiller (ES) ture as proposed by the Council Science stable cryostat. The STC recommended Willy Benz (CH) Strategy Working Group. It welcomed that a single upgrade plan be presented, Joris Blommaert (B) (VLT/I) the new Terms of Reference and the which would outline the scientific priori Jean-Gabriel Cuby (F) (ESE) strengthening of the STC links to its sub ties, whether they would be compatible Raffaele Gratton (I) (ESE) committees by making sure that there with each other, and describe the re Lauri Haikala (FIN) are at least two STC members on each quired resources and a timescale for the Thomas Herbst (D) (ESE Chair) subcommittee. upgrade. The STC further supported Hans Kjeldsen (DK) (VLT/I Chair) the plans for continued operations of the Yannick Mellier (F) The STC was concerned about the diffi 2.2-metre telescope (with FEROS, WFI Dante Minniti (CH) culties in the operations of the Laser and GROND) and the NTT (SOFI, EFOSC2 Goran Olofsson (SE) (ESE) Guide Star Facility (LGSF) and urged ESO and visitor instruments). Michael Prouza (CZ) to devise a recovery plan to re-establish Patrick Roche (UK) nominal adaptive optics with laser guide The STC was pleased by the progress Linda Tacconi (D) (Chair) star operations at the VLT and bring the of PRIMA at the VLTI and with the con Huib Jan van Langevelde (NL) system to the same level of quality prevail tracts for the second generation VLTI in ing at Paranal. The STC felt that the struments, MATISSE and GRAVITY. It success of the current generation LGSF welcomed the news that ESO had issued is critical to the success of the many a Call for Proposals for the ultra-stable other laser guide star systems planned spectrograph at the combined VLT focus New STC structure in the ESO programme, starting with the as the first element in the overall instru Adaptive Optics Facility (AOF) and the mentation plan for the VLT in the ELT era. A new Scientific Technical Committee projects GRAAL and GALACSI on the VLT It encouraged a well-defined sequence (STC) structure has been implemented this and later the E-ELT, for which laser of calls for a wide-field, very high multiplex year to reflect the breadth of ESO’s activi guide star operation is critical. The STC spectrograph facility for a Nasmyth focus ties better and to improve interaction at further urged ESO to inform the astro and an additional concept for future in the technical level. Former ad hoc com nomical community about the limitations struments. In addition, ESO should inves mittees are now formally identified as ad on the availability of the LGSF in Calls tigate how it can upgrade or replace the visory to the STC. These include the VLTI for Proposals until normal operations can work horse instruments. The STC empha Implementation Committee, which has be recovered. sised that these new instrument concepts been expanded to become the La Silla are meant as long-term enhancements Paranal Committee, the ALMA European The STC further discussed strategies for and upgrades to the VLT in the era of the Science Advisory Committee (ESAC) ESO to secure the scientific eminence ELT and should not compromise the suite and the ELT Science and Engineering of the VLT into the ELT era. In particular, of approved second generation instru Committee (ESE). Council approved the upgrades of current VLT instruments mentation in the short- and mid-term. new Terms of Reference of the STC and La Silla facilities were evaluated. The and its subcommittees at its June 2008 STC welcomed the detailed and clear meeting. The member state representa upgrade plan for La Silla and Paranal pre STC-69 tion on the STC has been maintained, sented by ESO. It recommended that but membership of the subcommittees ESO look for cost-effective ways to enable At its 69th meeting on 21 and 22 October should reflect the necessary specific and maintain wide-field imaging and in Garching, the STC dealt with the Budget expertise. At its December meeting Coun spectroscopic facilities for the ESO com and Forward Look for 2008–2012, to cil approved the new members of the STC, munity without jeopardising the other gether with the upgrade plan for HARPS, who are replacing several long-serving major approved ESO projects. Comple giving its recommendation to both. STC members who had reached the end menting spectroscopic surveys would of their terms. significantly increase the scientific impact The budget document was delivered to of the new survey telescopes, VISTA and the STC only shortly before the meeting, the VST. Replacement of the four VIMOS but it was able to discuss its contents red detectors with CCDs of improved during several extended closed sessions. red sensitivity will enable spectroscopic The STC was pleased that the budget surveys to be carried out in an efficient provided for the highest priority compo manner, opening up new science oppor nents of the ESO programme, including tunities for the ESO community. The STC ranked the VIMOS upgrade as the highest priority.
ESO Annual Report 2008 101 the E-ELT design activities, the operation complicated laser guide star systems instruments for public wide-field spectro of the La Silla Paranal facilities, develop planned in the ESO programme, firstly for scopic surveys. The workshop would ment of the approved second generation the AOF and the projects GRAAL and also be an opportunity for the community instruments, the construction and early GALACSI, and later the E‑ELT. to propose new concepts for the next operation of ALMA, operation of APEX generation wide-field instruments on ESO and the commissioning and operation of Following the STC’s recommendation from telescopes consistent with the STC rec the survey telescopes. The STC was con the 68th meeting, the STC welcomed ommendations from STC-67 and STC- fident that this programme will keep ESO the single, coherent HARPS upgrade pro 68. Depending on the outcome of the at the forefront of world astronomy. posal from ESO, Geneva Observatory workshop, ESO could then call for Large and Uppsala University. The proposal in Programmes or Public Surveys so as The STC noted that the third VLTI instru cluded a three-part short-term upgrade to begin wide-field spectroscopic surveys ment, VSI, was not included in this plan, plan consisting of a new guiding system, as soon as the VIMOS upgrade is com in line with the priority set by the STC, a polarimeter and a wavelength calibra pleted successfully. and that the savings from the revised op tion unit. The STC recommended pro eration of La Silla begin in this period. ceeding with this short-term upgrade, The E-ELT site selection schedule is The STC regarded the provision of a new which would enable HARPS to maintain a concern of both the STC and the ESE. Headquarters building in Garching as its leading position in high precision As one of the advisory committees of especially important so as to co-locate all radial velocity studies and add new polar ESO, the STC needs to ensure that it has ESO Garching personnel and projects on imetric scientific capabilities. The pro sufficient information to evaluate whether a single site, and, in particular, to improve posal also outlined plans for a medium- the telescope and instrument designs communications between the optical/ term upgrade consisting of a new are optimal for the site that is ultimately infrared and ALMA science communities detector system and a fibre link. The STC selected. Both the ESE and the STC at ESO. and the consortium agreed to wait before requested clarification on the process of making a recommendation on this more instrument selection at the end of Phase Based on input from the La Silla Paranal expensive, invasive part of the upgrade B. Both committees acknowledged, how subcommittee report, the STC proceeded until experience with similar components ever, that it will not be possible to bring all with the strategic discussions for secur in HARPS-N has been gained. eight instrument studies forward to Phase ing and maintaining the scientific emi B immediately. nence of the VLT into the ELT era. The The STC was informed of progress on STC was pleased with the progress made the High Resolution Ultra-Stable Spec The STC welcomed the news of the ex on the implementation of the near-term trograph concept for the next generation cellent choices in the new ALMA Director upgrade plan for La Silla and Paranal in of VLT instrumentation. The STC strongly and Project Managers. It also received strumentation recommended in STC-68. supported ESO’s intent to maintain the significant input from the ESAC on the scientific eminence of the VLT. In this con ALMA project. Based on this input, the The STC and the La Silla Paranal sub nection, the STC noted the absence of STC found that, although there was sig committee were both satisfied that the progress on other aspects of the next nificant progress in all aspects of the pro installation of a recovery plan for the LGSF generation instrumentation. Specifically, it gramme, there were several areas that had led to a significant improvement repeated its recommendation to see a gave cause for concern. The STC and in the on-sky performance and reliability plan for further VLT instrumentation as for ESAC were worried by the continued lack of the system, but was concerned that mulated in the previous meeting. of a permanent solution to supplying when the atmospheric conditions are power to the ALMA sites, the delays in taken into consideration, the operational With the upgrades of GIRAFFE and the European Front End Integration efficiency of the LGSF will be insufficient VIMOS, ESO will provide a set of highly Centre, and concerns over the possible to eliminate the backlog of observations competitive facilities to run wide-field limitations of the current local oscillator still in the service queue. It encouraged spectroscopic surveys. These instruments design to baselines of less than 5 km. ESO to continue to investigate ways to will be unique for the next five years and increase the laser guide star observing will clearly put the ESO community in a efficiency. The progress of the LGSF leading position in the field. The STC then and the positive outcome of the Multi- requested that a joint STC-ESO work conjugate Adaptive-optics Demonstrator shop be organised as early as possible to were considered encouraging signs of review the scientific potential of these a healthy AO programme at ESO. The STC reiterated that success of the present AO programme is a necessary stepping stone for the success of the other more
102 ESO Annual Report 2008 Observing Programmes Committee
For the third year in a row, Antu (VLT UT1) dedicated to studies of gamma-ray bursts The Observing Programmes Committee has been the telescope with the most (GRBs). Of these, about half involved 2008 requested time. The pressure factor on observations made in the Rapid Response this telescope, i.e. the ratio of the re Mode (RRM) of the VLT. With this mode, Danielle Alloin quested to the available time, reached observation of a transient phenomenon Svetlana Berdyugina (P82, Vice-chairperson) 6.6 in P82; this is an all-time record for can be started automatically within François Boulanger (P83) the VLT. Pressure on the other ESO tele minutes of its activation. Thanks to the Jan Brand (P82) scopes ranged between 2.5 and 5 in unique performance of the VLT in RRM, Elias Brinks 2008. Among the VLT instruments, FORS2 combined with ESO’s policy of overriding Enrico Cappellaro (P83) remains the most demanded, as it has both Visitor and Service Mode obser Francisco Castander (P83) been since 2004. In P83, the requested vations, the VLT and the GRB community Cathie Clarke (P83) amount of time on FORS2 was 2.5 to of the ESO member states remain at the Adriano Fontana 3.5 times larger than on any VLT instru forefront of this field of research. Roland Gredel (P82) ment, excluding VISIR, which is in low Leopoldo Infante demand (40% of the average of the VLT Mika Juvela instruments) due to the very specific type Calibration Programmes Leon Koopmans (P83) of scientific applications for which it Claes-Ingvar Lagerkvist can be used. Among La Silla instruments, As of P82, a new proposal type was John Landstreet HARPS (especially for Large Programmes) introduced, for Calibration Programmes Daniel Lennon (P83) and EFOSC2 are in high demand. Visi- (CP). Such programmes are aimed at Claudia Maraston (P82) tor instruments were scheduled at the complementing the existing coverage of Huub Röttgering NTT in both P82 and P83: AstraLux, the calibration of ESO instruments. In Sabine Schindler (P82) ULTRASPEC, and a visible-infrared cam the proposal evaluation, the OPC consid Monica Tosi (Chairperson) era of the Max-Planck-Institut für Radio ers the potential enhancement of the Esko Valtaoja astronomie. On APEX, the prototype bo outcome of future science programmes Sylvie Vauclair (P82) lometer camera P-Artemis was allocated that would be enabled by execution of Kim Venn (Vice-chairperson in P83) time in P83. the proposed CP against the immediate return of current period science propos Joint telescope time applications for als directly competing for use of the same coordinated observations with the VLT resources. In P82, three CP proposals and with the XMM-Newton X-ray observ were received; the OPC recommended In 2008, the Observing Programmes atory were invited again in P83. These two of them to be implemented. The OPC Committee (OPC) held its two semi- proposals fall within the framework of an also approved two of the ten CPs evalu annual meetings in May and in November. agreement between ESO and ESA for ated at its P83 meeting. It had to evaluate 925 proposals received a joint telescope time allocation scheme, for Period 82 (P82; 1 October 2008 to 31 which was in its fifth year in 2008. It aims March 2009), and 961 proposals for Pe to take full advantage of the complemen Large Programmes riod 83 (P83; 1 April 2009 to 30 Septem tarity of ground-based and space-borne ber 2009). The latter represents the high observing facilities. No joint applications Large Programmes (LPs) are projects re est number of proposals ever submitted were submitted to ESO in P83, but two quiring a minimum of 100 hours of ob to the OPC for a single period. Since the of the five applications evaluated by the serving time and that have the potential introduction in 2000 of the OPC scientific XMM Time Allocation Committee were al to lead to a major advance or break categories currently in use, the number located telescope time. through in the considered field of study. of proposals dealing with “Galactic” sci LP execution is spread over several entific areas — interstellar medium, star observing periods. Until P82, the maxi formation and planetary systems (OPC Targets of Opportunity mum duration of an LP was two years; as category C), and stellar evolution (OPC of P83, this limit was raised to four years category D) — has almost doubled. The An unprecedented number of 53 propos for programmes to be carried out on number of “extragalactic” proposals of als for observations of Targets of Oppor the La Silla NTT or 3.6-metre telescope. categories A (cosmology) and B (galaxies tunity (ToO) were submitted for evaluation Since the introduction by ESO in 2001 and galactic nuclei) has not significantly by the OPC in P83. The number of such of this type of programme, the number of changed over the same time interval. proposals that are received each period such proposals submitted each period is, on average, almost twice as high as it has steadily increased, reaching an all- was five years ago, and four times greater time record of 30 in P83. Of the 21 LP than ten years ago. In 2008, about 40% proposals that were evaluated by the OPC of the successful ToO proposals were
ESO Annual Report 2008 103 in P82, five were recommended for ESO/GTC programmes OPC procedures implementation and scheduled accord ingly. Six LP proposals were approved in The accession agreement of Spain into Over the past two years, four new advi P83, three of them with HARPS on the ESO includes the allocation of 122 clear sory panels have been added to the OPC, 3.6-metre telescope, taking advantage of nights with the new 10.4-metre Gran Tele so as to allow referees to cope with the increased maximum duration of LPs scopio Canarias (GTC) to proposals by the increasing number of proposals to be on La Silla. In total, between the start of Principal Investigators from ESO member evaluated while keeping their workload VLT science operation in 1999 and 2008 countries. The first Call for Proposals for manageable. The OPC now consists (P83), 90 LP proposals that were favoura these ESO/GTC programmes was issued of twelve panels, each with six members. bly evaluated by the OPC were allocated with the ESO P82 Call for Proposals. The number of meeting rooms available time on the La Silla Paranal Observatory Users were invited to submit proposals for at ESO Headquarters in Garching is no telescopes. They cover almost all current programmes whose execution required longer sufficient to accommodate all astronomical topics, from the Solar Sys at least 20 nights, spread over a maximum of them. Accordingly, as of P82, the panel tem to cosmological studies. Scientific duration of two years. Sixteen proposals meetings were transferred to a venue reports on the outcome of those LPs that were received. For their evaluation, which outside ESO Headquarters, offering ade were completed between 2003 and was carried out in the same way as for LP quate meeting rooms and allowing the 2007 were presented at a workshop that proposals requesting time on ESO tele participants to perform their work under took place at ESO in Garching in October scopes, two members-at-large appointed appropriate conditions. Before and 2008 upon the OPC’s request. The re by Spain joined the OPC. Following the after the panel meetings, the OPC itself ports given at this workshop illustrate the OPC recommendations and review of the continues to hold its sessions at the ESO success and usefulness of the LP pro technical and operational constraints by Headquarters. posal scheme. the Liaison Committee between ESO and Spain, two programmes were approved.
The VLT at sunset.
104 ESO Annual Report 2008 Users Committee
The annual meeting of the Users Com and web pages, and the prospects for fu The Users Committee mittee (UC) took place at the ESO Head ture development and distribution of data 2008 quarters in Garching on 14 and 15 April. reduction pipelines.
Belgium Griet Van de Steene Following an introductory talk by the Di As usual, the morning of the second day Czech Republic Jiří Grygar rector General on ESO’s long-term strate of the meeting was devoted to a special gies and priorities, presentations were topic, which this year was Advanced Denmark Johan Fynbo given by ESO on the La Silla Paranal Ob Data Products (ADP). After a brief intro servatory (with emphasis on the revised duction by ESO, three users who had Finland Merja Tornikoski model of operations of La Silla as of 2010), submitted ADPs gave an account of their France Vanessa Hill ALMA, the observing proposals handling experience. They commented on the and evaluation process, the data reduc submission procedure, explained the mo Germany Jochen Heidt tion pipelines, the ESO User Portal, and tivation behind their decision to submit Italy Bianca Poggianti the E-ELT project. The UC presented the an ADP, and reported on their interac feedback from the user community, on tions with colleagues who had actually The Netherlands Walter Jaffe the basis both of a global survey across all retrieved and used these ADPs for their (Chairperson) member states and of direct input from own research. Portugal Nuno Santos the astronomers in the countries to their respective representatives. In general, Spain Ignacio Negueruela users are very satisfied with the actual ex ecution of observations at the La Silla Sweden Nils Ryde Paranal Observatory, both in Service Switzerland Frédéric Courbin Mode and in Visitor Mode. Their main concerns rest with the proposal evaluation United Kingdom Jacco van Loon process and the feedback that they re (Vice-chairperson) ceive about it, the difficulties encountered Chile Wolfgang Gieren by certain categories of users to find needed information in ESO documents
The VLT control room.
ESO Annual Report 2008 105
La Silla Observatory International Relations The International Relations Office (IRO) The Signing Ceremony was established in early 2008 within the with Austria. Office of the Director General, bringing to gether activities previously handled by various departments and offices across the organisation. The growth of ESO, both in terms of the number of member states and projects, as well as the increasing in ternationalisation of research, called for the establishment of a dedicated office to deal with these matters. The IRO sup ports and works closely with the Directo rates in pursuit of ESO’s mission.
One of the most important developments for ESO in 2008 in international relations was the finalisation of the membership negotiations with Austria. This led to the signing of the accession agreement by (May) and in Prague (December). An event The International Relations Office has also the Austrian Minister for Science and Re in Berlin was in preparation for January kept abreast of the evolution of European search, Johannes Hahn and ESO’s Direc 2009 in connection with the opening of science policies, particularly with regard tor General at a ceremony in Vienna on the International Year of Astronomy. to research infrastructures and has en 30 June. Unfortunately, the ratification sured an ESO presence at relevant meet procedure was delayed by early elections On 1 July, ESO assumed the rotating ings and events, including conferences and the process of forming a new gov Chairmanship of the EIROforum collabora organised by the rotating EU Presidency. ernment, so that the formal conclusion of tion, the partnership of Europe’s seven the ratification was still pending at the intergovernmental research organisations At the 51st Session of the UN Committee end of the year, though with encouraging operating major infrastructures. The regu for Peaceful Uses of Outer Space, ESO signs for completion in early 2009. lar Autumn meeting of the EIROforum was granted the status as permanent ob Council (the Directors General of the part server, supported by several member The continued success of ESO and its ner organisations), which was held at states and Chile. The status was con exciting future plans continue to draw in Paranal, began a review of the partnership firmed in December by the UN General terest in many countries beyond the cur and its past activities as the first step in de Assembly. rent member states. The ESO Council re veloping a forward plan for EIROforum that sponded positively, adopting new policy builds on its solid achievements to date. guidelines making it possible to under Visit of the EIROforum Council to Paranal. take discussions with several countries — including some outside of Europe — who had expressed an interest either in full membership of ESO or in some form of collaboration in the E-ELT project.
ESO has continued its programme of in teraction with industries in the member states, organising further information days aimed at raising the awareness in industry of the opportunities offered by ESO projects and giving enterprises an oppor tunity to interact directly with ESO special ists. These events are organised in close collaboration between the IRO and the Contracts and Procurement Department. In 2008, events took place in Copenhagen
The Austrian Minister for Science and Research, Dr Johannes Hahn, Prof. Sabine Schindler (University of Innsbruck) and ESO’s Director General, Prof. Tim de Zeeuw at the press conference at the Vienna Observatory on 24 April, where the Austrian govern ment announced its decision to join ESO.
ESO Annual Report 2008 109 Chile Relations
Throughout the year, ESO continued its Director of Civil Aeronau close interaction with the Chilean authori tical Services, General José Huepe and the ties and Chilean society in several areas. ESO Representative, Felix Mirabel, sign the An important component of ESO’s Collaboration Agreement. Cooperation Programme with Chile, the ESO/Government of Chile Joint Com mittee, continued its work in 2008. This year, 28 proposals from universities and institutions were reviewed and fund ing of US$ 618 000 was allocated.
The Office of the ESO Representative started negotiations with the Rector of the Universidad Católica del Norte over a project involving a permanent astronomy exhibition at the Ruinas de Huanchaca, a national monument area in Antofagasta, which had been gradually abandoned over the years. This project is now under way and inauguration is expected in 2009. Delegation from Civil Aeronautical Services visit Paranal. The annual meeting at CONICYT to allo cate funding that is provided by ESO/ AUI and NAOJ on behalf of ALMA for as tronomy in Chile took place in October. US$ 504 000 was allocated by the Com mittee to Chilean universities who had presented their projects.
In August a Cooperation Agreement concerning the continued operation of the Laser Guide Star in Paranal was signed with the Chilean Aviation authorities (DGAC & DASA) during a visit by the Di rector of Civil Aeronautics, General José Huepe and the Director of Airport Services Hector Barrientos. This Agreement fore sees scientific and technological collabo ration and a mutual exchange of informa tion, allowing ESO to continue to operate the Laser Guide Star System safely in worked with other national authorities to Two officials from the Ministry of Foreign the future, and the DGAC to monitor the increase security, including the Carabin Affairs visited La Silla to see the problem safety of airborne operations adequately. eros and the Direction of Frontiers on this first-hand, particularly the La Esperanza issue. mine, and they followed up the issue with the Ministry’s Legal Department. The ALMA – Security issues Vice-Minister of Foreign Affairs asked La Silla the Ministry of Mines to close the mines In view of some security problems that operating within the protected area have been encountered on the Chajnantor Mining requests continued to be filed by around La Silla. Meanwhile, the Ministry Plateau, two officials from the Ministry of individuals and companies seeking to of Mines has taken legal action against Foreign Affairs were invited to the ALMA establish mining rights within the La Silla the owner of the La Esperanza mine. This OSF, providing the opportunity to see protected area. This year alone, 80 letters action will serve as a precedent to speed the site and giving some background to were sent opposing these claims and re up the resolution of other cases that may discussions of security plans for the area. porting each case to the Mining Authori arise in the future. As a result, the Ministry of Foreign Affairs ties in Region IV.
110 ESO Annual Report 2008 Light pollution Ventarrones – A possible site for the VIP visitors E-ELT On 11 July, a large workshop was held Also in 2008, ESO — and especially in Antofagasta, co-organised by ESO and The Ministry of National Assets signed the Paranal — hosted many important visitors, the Office Against Light Pollution, to concession for this land for five years. including the Chilean Under-Secretary increase awareness of this problem. The Procedures were initiated to ensure proper for Foreign Affairs, Ambassador Alberto workshop was attended by representa protection against mining rights claims. Van Klaveren (former Chilean Ambassador tives of the Intendencia Region II, the to the European Union) who visited Chilean Environmental Agency, CONAMA, Outreach Paranal. Also, officials from the Dirección Senator Carlos Cantero, Rector of Uni de Política Especial visited La Silla and versidad Católica del Norte and a repre On 12 July, the town of Taltal, neighbours Paranal. In December 2008, the President sentative from the Ministry of Foreign to the Paranal Observatory, celebrated of Switzerland and his delegation visited Affairs, amongst others. its 150th Anniversary. The ESO Repre the ESO Vitacura Office. Finally, as in sentative participated in the celebrations, the previous years, several ambassadors A meeting was held between the Repre along with the main regional and local from ESO member state countries visited sentatives of the Observatories in Chile, authorities. The Mayor emphasised ESO’s Paranal. to discuss joint actions and in support scholarship programme for school chil of the Light Pollution Office. ESO will in dren and university students in his speech. crease its funding to cover more activities A detailed account of ESO’s public out in Region II. reach activities is given on page 22 of the Annual Report.
The President of Switzerland and his delegation visited the ESO Vitacura Office.
ESO Annual Report 2008 111 Four Seasons at a Glance
January An ESO workshop on “Star Formation A four-day ALMA Board meeting is held across the Milky Way Galaxy” is held at in Santiago de Chile. The two-year FP7 E-ELT Preparatory ESO Santiago. phase programme starts. The European ALMA Science Advisory ESO participates in NAM, Belfast, UK. Committee meets in Garching. ESO is present at the winter AAS meeting in Austin, USA. James Bond filming at Paranal, including ESO is present at FEST in Trieste, Italy. international and Chilean press events. The European ALMA Science Advisory Committee meets in Garching. May April ESO is present at the Galway Astronomy ESO celebrates 10 years since First Light Festival, Galway, Ireland. VISTA mirror arrives at Paranal. at the VLT.
Start of science operation of HAWK-I at VLT makes the most precise measure February UT4, AMBER + FINITO at the UTs, ment of the temperature of the Universe EFOSC2 at NTT. as it was less than three billion years The NTT is used to measure, at the 1% after Big Bang. precision level, the distance of a Cepheid EMMI and SUSI2 decommissioned at the star. NTT. The NEON 3D Spectra School, “The First Practical Workshop on IFU Observations A new multi-fuel power generator is Upgrade of the GIRAFFE CCD detector. and Data Reduction”, is held in Potsdam, installed at Paranal. Germany. 925 observing proposals are received for 121st meeting of the Finance Committee. Period 82. The ESO/EAAE Catch a Star competition awards prizes. A two-day meeting is held by the ALMA 32nd Meeting of the Users Committee. Science Advisory Committee in Santiago 122nd Finance Committee Meeting. de Chile. Scientific Technical Committee meets for its 68th session in Garching. ESO is present at the annual AAAS meeting in Boston, USA.
EIROforum participates in the MIT European Career Fair and Science Policy Meeting in Boston, USA.
March
GRB 080319B, the brightest explosion ever seen, is observed from La Silla.
A new observing proposal type for Calibration Programmes is introduced.
The first Band 7 and Band 9 receivers are delivered to the East Asian Front End Integration Centre.
VISTA primary mirror arrives in Chile.
First light of the laser comb calibration demonstrator on Tenerife.
Committee of Council meets in Stock holm, Sweden. VISTA primary mirror arrives in Chile in March.
112 ESO Annual Report 2008 82nd meeting of the Observing Programme Committee.
National Geographic Channel “World’s Toughest Fixes” series is filmed at Paranal.
First media training workshop for ESO Chile astronomers.
June
Austrian Minister for Science and Re search, Johannes Hahn and the ESO Director General, Tim de Zeeuw, sign the formal Accession Agreement between Austria and ESO.
A new agreement is signed between ESO and the Max-Planck-Institut für Astronomie for the continued operation of the MPG/ESO 2.2-metre telescope until 2013. Participants in the Euro-VO DCA European astronomers find a system of Workshop 2008. three super-Earths using HARPS.
ALMA antenna transporters are ready for July August operation at the ALMA Observatory. Austria becomes 14th ESO member The first front end assembly arrives at the The Technical Facilities at the ALMA state. ALMA Observatory in Chile. Operations Support Facilities at 2900 m altitude are accepted and ready for use. Start of direct data transfer from Paranal The Cooperation Agreement for the to the Science Archive in Garching. LGS system at Paranal is signed with The ESO workshop “Gas and Stars in the Chilean Aviation authorities. Galaxies: a Multi-Wavelength 3D Start of PRIMA installation and Perspective” and the Euro-VO DCA commissioning. The third NEON Archive Observing Workshop 2008 “How to Publish Data School is held in Garching. in the VO” take place in Garching. First ALMA antenna is transported at the ALMA Operations Support Facility. ESO is present at the Solar Eclipse Event The seventh NEON Observing School is in Oslo, Norway. held on La Palma, Spain. Light Pollution Workshop in Antofagasta, co-organised by ESO and the Chilean An international press event takes place ESO participates very actively in SPIE, Office Against Light Pollution. at Paranal with the History Channel for Marseille, France. the TV Series “The Universe”. The MPA/ESO/MPE/USM 2008 Joint ESO is present at Explore Science, Astronomy Conference, “Chemical Mannheim, Germany. Evolution of Dwarf Galaxies and Stellar Clusters” takes place in Garching. 112th Council Meeting in Prague in the Czech Republic. ESO takes over the chairmanship of EIROforum for one year. A three-day ALMA Board meeting is held in Marseille, France. EIROforum participates in ESOF, Barcelona, Spain.
ESO exhibition at Taltal for the 150th anniversary of the town.
ESO Annual Report 2008 113 September ESO is present at JENAM, Vienna, 83rd meeting of the Observing Pro Austria. gramme Committee. CRIRES probes in unsurpassed detail the inner regions of discs around infant stars, Inauguration of a new permanent astro where Earth-like planets may be forming. nomical exhibition at MIM Interactive November Museum in Santiago (Chile), supported First light of PRIMA on the VLTI at by the ESO-Chile Joint Committee. Professor Wolfgang Wild becomes the Paranal. Head of the ALMA Division and takes up duty as the new European ALMA Project Commissioning of SABOCA on APEX. October Manager. Dr. Richard Kurz takes up duty as the new ALMA Project Manager. Trial assembly of the first European ALMA MAD, on the VLT, produces the sharpest antenna is carried out in Spain. whole-planet picture ever taken from the ASTRONET presents the ASTRONET ground of Jupiter. Infrastructure Roadmap, a 20-year strat The European ALMA Science Advisory egy for the future of European astronomy, Committee meets in Garching. Professor Thijs de Graauw takes up duty identifying the E-ELT as a top priority. as the new ALMA Director. A two-day meeting is held by the ESO hosts the EIROforum Council at ALMA Science Advisory Committee The first amplitude calibration device is Paranal. in Charlottesville, USA. accepted and installed at the OSF. First light of X-shooter on Melipal. The ALMA Band 9 Cartridge Manufac 961 observing proposals are received for turing Readiness Review is held in Period 83. The Band 7 Pre-Production Review is Groningen in the Netherlands. held at IRAM in Grenoble, France. ESO workshop on “Large Programmes”, An ESO workshop on “Public Surveys” is Garching. The ALMA Band 9 Cartridge Pre- held in Garching. Production Review is held in Groningen, Committee of Council meets in Copenha the Netherlands, A workshop on “Future Ground based gen, Denmark. Solar System Research: Synergies with The ALMA water vapour radiometer Space Probes and Space Telescopes” is 69th meeting of the Scientific Technical Critical Design Review is held in held in Italy. Committee in Garching. Gothenburg, Sweden.
The PRIMA instrument of the ESO Very Large Telescope Interferometer.
114 ESO Annual Report 2008 A three-day ALMA board meeting is held First light of APE on the in San Pedro de Atacama. VLT.
123rd Meeting of the Finance Committee.
The 22nd James Bond adventure, Quantum of Solace, featuring the Paranal Residencia, is released.
A workshop on “Using the VLT Interfer ometer at the present time and in the near future” is held in Granada, Spain.
ESO, together with French partners, participates in the highly successful “Eu ropean City of Science”, Paris, France.
ESO organises a science expo at San Pedro de Atacama for the anniversary of the village. ESO informal meeting on “Six years of ESO exhibition at Quinta Normal Park, FLAMES operations” is held in Garching. Santiago, during the Chilean National Science Week. A three-day ALMA Annual External Review is held in San Pedro de Atacama.
December ESO participates in EU Presidency Conference on Research Infrastructures, ALMA observatory equipped with its first Versailles, France. antenna
SPHERE passes its Final Design Review. The first ALMA antenna to be handed over to the observatory. First light of APE on Melipal.
Visit by the President of Switzerland to the ESO Vitacura Office.
Three undergraduate students, from Leiden University in the Netherlands, dis cover an extrasolar planet using the VLT.
First production ALMA Band 9 Cartridge is ready for acceptance.
The Technical Building at the ALMA Array Operations Site at 5000 m altitude is accepted and ready for use.
Delivery of tunable filter boards for the ALMA correlator to the ALMA project is completed.
Closure of the Antenna Test Facility in Socorro (USA).
113th Council Meeting in Garching.
ESO Annual Report 2008 115 Credit: QUANTUM OF SOLACE / © 2008 Danjaq, United Artists, CPII., 007 TM and related James Bond Trademarks, TM Danjaq ESO’s Paranal Observatory was used as the key location for Quantum of Solace, the latest James Bond movie. A close up view of one of the VLT Unit Telescopes. Publications
Publications in refereed journals based on ESO data (2008)
Abia, C., de Laverny, P. & Wahlin, R. 2008, Chemical Alonso, R., Auvergne, M., Baglin, A., Ollivier, M., Antoniucci, S., Nisini, B., Giannini, T. & Lorenzetti, analysis of carbon stars in the Local Group. II. The Moutou, C., Rouan, D., Deeg, H. J., Aigrain, S., D. 2008, Accretion and ejection properties of Carina dwarf spheroidal galaxy, A&A, 481, 161 Almenara, J. M., Barbieri, M., Barge, P., Benz, W., embedded protostars: the case of HH26, HH34, Absil, O., di Folco, E., Mérand, A., Augereau, J. C., Bordé, P., Bouchy, F., de La Reza, R., Deleuil, M., and HH46 IRS, A&A, 479, 503 Coudé Du Foresto, V., Defrère, D., Kervella, P., Dvorak, R., Erikson, A., Fridlund, M., Gillon, M., Apai, D., Janson, M., Moro-Martín, A., Meyer, M. R., Aufdenberg, J. P., Desort, M., Ehrenreich, D., Gondoin, P., Guillot, T., Hatzes, A., Hébrard, G., Mamajek, E. E., Masciadri, E., Henning, T., Lagrange, A. M., Montagnier, G., Olofsson, J., Ten Kabath, P., Jorda, L., Lammer, H., Léger, A., Pascucci, I., Kim, J. S., Hillenbrand, L. A., Kasper, Brummelaar, T. A., McAlister, H. A., Sturmann, J., Llebaria, A., Loeillet, B., Magain, P., Mayor, M., M. & Biller, B. 2008, A Survey for Massive Giant Sturmann, L. & Turner, N. H. 2008, A near-infrared Mazeh, T., Pätzold, M., Pepe, F., Pont, F., Queloz, Planets in Debris Disks with Evacuated Inner interferometric survey of debris disc stars. II. D., Rauer, H., Shporer, A., Schneider, J., Steck Cavities, ApJ, 672, 1196 CHARA/FLUOR observations of six early-type lum, B., Udry, S. & Wuchterl, G. 2008, Transiting Arav, N., Moe, M., Costantini, E., Korista, K. T., Benn, dwarfs, A&A, 487, 1041 exoplanets from the CoRoT space mission. II. C. & Ellison, S. 2008, Measuring Column Densi- Acke, B., Verhoelst, T., van den Ancker, M. E., CoRoT-Exo-2b: a transiting planet around an ac- ties in Quasar Outflows: VLT Observations of QSO Deroo, P., Waelkens, C., Chesneau, O., Tatulli, E., tive G star, A&A, 482, L21 2359-1241, ApJ, 681, 954 Benisty, M., Puga, E., Waters, L. M., Verhoeff, A. & Alvarez-Candal, A., Fornasier, S., Barucci, M. A., de Aravena, M., Bertoldi, F., Schinnerer, E., Weiss, A., de Koter, A. 2008, MWC 297: a young high-mass Bergh, C. & Merlin, F. 2008, Visible spectroscopy Jahnke, K., Carilli, C. L., Frayer, D., Henkel, C., star rotating at critical velocity, A&A, 485, 209 of the new ESO large program on trans-Neptunian Brusa, M., Menten, K. M., Salvato, M. & Smolcic, Aguirre, A., Dow-Hygelund, C., Schaye, J. & Theuns, objects and Centaurs. Part 1, A&A, 487, 741 V. 2008, Properties of the molecular gas in a T. 2008, Metallicity of the Intergalactic Medium Ammler-von Eiff, M. & Santos, N. C. 2008, New starbursting QSO at z = 1.83 in the COSMOS field, using Pixel Statistics. IV. Oxygen, ApJ, 689, 851 constraints from the Hα line for the temperature A&A, 491, 173 Aharonian, F., Akhperjanian, A. G., Barres de of the transiting planet host star OGLE-TR-10, AN, Arentoft, T., Kjeldsen, H., Bedding, T. R., Bazot, M., Almeida, U., Bazer-Bachi, A. R., Behera, B., 329, 573 Christensen-Dalsgaard, J., Dall, T. H., Karoff, Beilicke, M., Benbow, W., Bernlöhr, K., Boisson, Andersen, D. R., Walcher, C. J., Böker, T., Ho, L. C., C., Carrier, F., Eggenberger, P., Sosnowska, D., C., Bolz, O., Borrel, V., Braun, I., Brion, E., Brown, van der Marel, R. P., Rix, H. W. & Shields, J. C. Wittenmyer, R. A., Endl, M., Metcalfe, T. S., A. M., Bühler, R., Bulik, T., Büsching, I., Boutelier, 2008, Caught in Formation: The Nuclear-Cluster- Hekker, S., Reffert, S., Butler, R. P., Bruntt, H., T., Carrigan, S., Chadwick, P. M., Chounet, L. to-Be in NGC 2139, ApJ, 688, 990 Kiss, L. L., O’Toole, S. J., Kambe, E., Ando, H., M., Clapson, A. C., Coignet, G., Cornils, R., Anderson, D. R., Gillon, M., Hellier, C., Maxted, P. Izumiura, H., Sato, B., Hartmann, M., Hatzes, A., Costamante, L., Dalton, M., Degrange, B., L., Pepe, F., Queloz, D., Wilson, D. M., Collier Bouchy, F., Mosser, B., Appourchaux, T., Barban, Dickinson, H. J., Djannati-Ataï, A., Domainko, W., Cameron, A., Smalley, B., Lister, T. A., Bentley, S. C., Berthomieu, G., Garcia, R. A., Michel, E., O’C. Drury, L., Dubois, F., Dubus, G., Dyks, J., J., Blecha, A., Christian, D. J., Enoch, B., Hebb, Provost, J., Turck-Chièze, S., Martić, M., Lebrun, Egberts, K., Emmanoulopoulos, D., Espigat, P., L., Horne, K., Irwin, J., Joshi, Y. C., Kane, S. R., J. C., Schmitt, J., Bertaux, J. L., Bonanno, A., Farnier, C., Feinstein, F., Fiasson, A., Förster, A., Marmier, M., Mayor, M., Parley, N. R., Pollacco, D. Benatti, S., Claudi, R. U., Cosentino, R., Leccia, Fontaine, G., Funk, S., Füßling, M., Gallant, Y. 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136 ESO Annual Report 2008 Additional peer-reviewed publications by ESO Scientists
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ESO Annual Report 2008 141 Glossary of Acronyms
4LGSF Four-Laser Guide Star Facility DASA Dirección de Aeródromos y Servicios FE Front End AAAS American Association for the Aeronáuticos (Chile) FEED Front -End Engineering Design (E-ELT) Advancement of Science DCA Euro-VO Data Centre Alliance FEIC Front-End Integration Centres (ALMA) A&A Journal Astronomy & Astrophysics DDL Differential Delay Line FEROS Fibre-fed, Extended Range, Échelle AAS American Astronomical Society DDL-PAOS Consortium (Geneva Observatory, Spectrograph (2.2-metre) ACD Amplitude Calibration Device Heidelberg Observatory and Max- FIERA CCD controller (VLT,optical) ACS ALMA Common Software Planck Institute for Astronomy in FINITO Fringe Tracking Instrument Nice Torino ACS Advanced Camera for Surveys Heidelberg) developing DDLs for (VLTI) (Hubble) PRIMA FITS Flexible Image Transport System ADE Archive Department DFO Data Flow Operations FLAMES Fibre Large Array Multi Element Admin Administration Division DGAC Dirección General de Aeronáutica Civil Spectrograph (VLT) ADP Advanced Data Products (Chile) FOAD Fibre Optic Amplifier/Demultiplexer ADS Astrophysics Data System DGCK Digitiser Clock Assemblies (ALMA) (ALMA) AGB Asymptotic Giant Branch DGP DGP gravity is a braneworld model FORS FOcal Reducer/low dispersion AGN Active Galactic Nucleus proposed by Dvali, Gabadadze and Spectrograph (VLT) AIDA Astronomical Infrastructure for Data Porrati in 2000 FORS1 FOcal Reducer/low dispersion Access DIPSI Diffraction Image Phase Sensing Spectrograph (VLT)-1 AIV Assembly, Integration and Verification Instrument FORS2 FOcal Reducer/low dispersion ALMA Atacama Large Millimeter/submillimeter DMO Data Management and Operations Spectrograph (VLT)-2 Array Division FP6 ELT-DS Sixth EC Framework Programme ELT AMBER Astronomical Multi-BEam combineR DOORS Requirement management software Design Study (VLTI Instrument) DPD Data Products Department FP7 Seventh EC Framework Programme AMOS AMOS Electronics Corporation DR1/2 Data Release 1/2 (Hubble Legacy GaBoDs Garching -Bonn Deep Survey Antu VLT Unit Telescope 1 Archive) Gaia Astrometric satellite (ESA) AO Adaptive Optics DRM Design Reference Mission (E-ELT) GALACSI Ground Atmospheric Layer Adaptive AOF Adaptive Optics Facility DRSP Design Reference Science Plan (E-ELT Optics for Spectroscopic Imaging AOS Array Operations Site (ALMA) & ALMA) GHz Gigahertz APE Active Phasing Experiment (E-ELT) DSM Deformable Secondary Mirror (AOF) GIRAFFE Spectrograph (VLT/FLAMES) APEX Atacama Pathfinder Experiment DTS Data Transmission System (ALMA) GOODS Great Observatories Optical Deep APLF Association of French-speaking E2V Electronics manufacturer Survey Planetariums EAAE European Association for Astronomy GRAAL GRound-layer Adaptive optics Assisted AQUARIUS Mid-infrared array Education by Lasers ARC ALMA Regional Centre EAGLE Multi -object NIR spectrograph (E-ELT) GRAVITY AO assisted, two-object, multiple- ASSIST Adaptive Secondary Setup and EC European Commission beam-combiner (VLTI) Instrument Simulator E-ELT European Extremely Large Telescope GRB Gamma-Ray Burst AstraLux Lucky Imaging camera for the Calar EFOSC2 ESO Faint Object Spectrograph and GROND Gamma-Ray burst Optical/Near- Alto 2.2-metre telescope Camera (v.2) infrared Detector ASTRONET Astronomy ERA-NET EIROforum Organisation consisting of the seven GTC Gran Telescopio Canarias AT Auxiliary Telescope for the VLTI largest scientific European international GUI Graphical User Interface ATF Antenna Test Facility (ALMA) organisations devoted to fostering HARMONI Single Field, Wide Band Spectrograph AUI Associated Universities Inc. (NRAO) mutual activities (E-ELT) aXeSIM Slitless spectroscopy data extraction ELT Extremely Large Telescope HARPS High Accuracy Radial Velocity software e-MERLIN Major project to upgrade the MERLIN Planetary Searcher (3.6-metre) BAL Broad Absorption Line array of radio telescopes HAWK-I High Acuity Wide field K-band Imager BE Back End EMMI ESO Multi-Mode Instrument (NTT) (VLT) BUS Back-Up Structure (ALMA) EPICS Planet imager and spectrograph HD High Definition CADC Canadian Astronomy Data Centre (E-ELT) HLA Hubble Legacy Archive CAPj Journal “Communicating Astronomy EPO Education and Public Outreach HR Human Resources with the Public” ePOD education and Public Outreach HST Hubble Space Telescope CASA Offline data reduction system (ALMA) Department IAC Instituto de Astrofisica de Canarias CCD Charge Coupled Device ERA-NET EU scheme to step up the cooperation IAU International Astronomical Union CDR Critical Design Review and coordination of research activities ICD Interface Control Document (ALMA) CERN European Organization for Nuclear carried out at national or regional level IFG Fast guiding controller (AMBER/VLTI) Research in the Member States and Associated INAF Istituto Nazionale di Astrofisica (Italy) CFRP Carbon Fibre Reinforced Plastic States IPS Intrusion Prevention System CMMS Computerised Maintenance ERP Administrative information system IPSAS International Public Sector Accounting Management System (ALMA) ESA European Space Agency Standards CMS Content Management System ESAC European Science Advisory Committee IPT Integrated Product Team (ALMA) CODEX High Resolution Optical Spectrograph (for ALMA) IQ Server system (E-ELT) ESE ELT Science and Engineering IQuEye Italian Quantum Eye COFUND FP7 Marie Curie Initiative ESFRI European Strategy Forum on Research IR InfraRed Co-I Co-Investigator Infrastructures IRACE InfraRed detector high speed Array CONAMA Chilean Environmental Agency ESO European Organisation for Control and processing Electronics CONICA COudé Near-Infrared CAmera (VLT) Astronomical Research in the Southern IRO International Relations Office CONICYT Comisión Nacional de Investigación Hemisphere IRAM Institut de Radioastronomie Científica y Tecnológica ESOF Euroscience Open Forum Millimétrique CODEX High stability high resolution optical EU European Union ISAAC Infrared Spectrometer And Array spectrograph (E-ELT) EU FEIC European Front-End Integration Centre Camera (VLT) COS Cosmic Origins Spectrograph (HST) (ALMA) ISM InterStellar Medium CP Calibration Programme EUCLID ESA dark energy mission IT Information Technology CRIRES Cryogenic InfraRed Echelle EUCYS EU Contest for Young Scientists ITUG IT User Group Spectrometer (VLT) EURO-VO European Virtual Observatory IVOA International Virtual Observatory CV Cataclysmic Variable EVLA Expanded Very Large Array Alliance CW Continuous Wave IYA2009 International Year of Astronomy 2009
142 ESO Annual Report 2008 JAAB Joint Advisory Appeals Board O&E WG Outreach and Education Working STFC Science and Technology Facilities JAO Joint ALMA Observatory Group Council (UK) JENAM Joint European and National OB Observation Block STIS Slit spectrograph (HST) Astronomy Meeting OCAM Test/controller camera for CCD220 STRAP Tip-tilt sensors (VLTI) JRA Joint Research Activity ODG Office of the Director General STScI Space Telescope Science Institute KIS-VTT Kiepenheuer -Institut für Sonnenphysik OmegaCAM Optical Camera for the VST (USA) Vacuum Tower Telescope (Canaries) OPC Observing Programmes Committee SUSI2 SUperb Seeing Imager-2 (NTT) KMOS K-band Multi-Object Spectrograph OPTICON Optical Infrared Coordination Network SWG Science Working Group (VLT) for Astronomy Swift NASA mission aimed at gamma-ray KONUS Gamma-ray detector on WIND satellite OPTIMOS Multi-object, optical and J-band burst studies Kueyan VLT Unit Telescope 2 spectrograph (E-ELT) TAROT Télescope à Action Rapide pour les LABOCA Large APEX Bolometer CAmera OSF ALMA Operations Support Facilities Objets Transitoires LAM Laboratoire d’Astrophysique de OT Observing Tool (ALMA) TB Terabyte Marseille P82 Observing Period 82 TFB Tunable Filter Bank LAOG Laboratoire d’Astrophysique de P83 Observing Period 83 THELI Software package for the reduction of l’Observatoire de Grenoble P84 Observing Period 84 astronomical imaging data LBO Lithium Triborate LiB3O5, nonlinear PA Product Assurance TinyTim Software for computing the camera optical crystal PARSEC Sodium line laser for VLT AO point spread functions LFC Laser Frequency Combs P-Artemis Prototype bolometer camera ToO Target of Opportunity LGS Laser Guide Star PB Petabyte TORTORA Telescopio Ottimizzato per la Ricerca LGSF Laser Guide Star Facility PI Principal Investigator dei Transiti Ottici RApidi LINER Low-ionisation nuclear emission-line PIO Public Information Officer TT Technology Transfer region galaxy PLC Programmable Logic Controllers UC Users Committee LMC Large Magellanic Cloud (E-ELT) UK United Kingdom LP Large Programme PLO Paranal La Silla Observatory UKIDSS UKIRT Infrared Deep Sky Survey LPG Liquefied Propane Gas PMS Pre-Main Sequence UKIRT UK Infrared Telescope LSP La Silla Paranal Committee PRIMA Phase -Referenced Imaging and Micro- ULTRASPEC High-speed, spectroscopic camera M4 Mirror #4 in E-ELT AO unit arcsecond Astrometry facility (VLTI) (ESO 3.6-metre) M5 Mirror #5 in E-ELT AO unit PROFISICA Chilean science foundation USD User Support Department MACAO Multi -Application Curvature Adaptive PR Press Release UT Unit Telescope of the VLT Otics (VLT/VLTI) PSD Pipeline Systems Department UT1–4 VLT Unit Telescopes 1–4: Antu, MAD Multi-conjugate Adaptive optics PYPS PYramid Phasing Sensor Kueyen, Melipal and Yepun Demonstrator QoS Quality of Service UV UltraViolet MARCEL PRIMA calibration source QSO Quasi Stellar Object UVES UV-Visual Echelle Spectrograph (VLT) MATISSE Multi AperTure mid-Infrared QSR Quasi-Stellar Radio-source VIMOS VIsible MultiObject Spectrograph (VLT) SpectroScopic Experiment (VLTI) R&D Research and Development VIPERS VIMOS Public Extragalactic Redshift MCAO Multi-Conjugate Adaptive Optics RadioNet Radio Astronomy Network in Europe Survey Melipal VLT Unit Telescope 3 RAL Rutherford Appleton Laboratory, VIRCAM VISTA IR Camera METIS Mid-infrared imager-spectrograph Didcot (UK) VirGO Visual Archive Browser (E-ELT) REM Rapid Eye Movement Telescope (La VISA VLTI Sub-Array MFPG Multi-Fuel Power Generator Silla) VISIR VLT Mid-Infrared Imager Spectrometer MICADO Diffraction-limited camera (E-ELT) RMN Reflective Memory Network VISTA Visible and Infrared Survey Telescope MIDI Mid-Infrared Interferometric Instrument rms Root mean square for Astronomy (VLTI) ROHS Restriction Of Hazardous Substances VLA Very Large Array MIMO Multiple Input/ Multiple Output RRM Rapid Response Mode VLT Very Large Telescope MPE Max -Planck-Institute for Extraterrestrial SABOCA Shortwave Apex BOlometer Camera VLTI Very Large Telescope Interferometer Physics (Germany) SAC EURO -VO Science Advisory VNR Video News Release MPIA Max-Planck-Institute for Astronomy Committee VO Virtual Observatory (Germany) SAM Sparse Aperture Mask (NACO) VOP Virtual Observatory Project Office MPIfR Max -Planck-Institute for SDD Software Development Division VOS Virtual Observatory Systems Radioastronomy (Germany) SED System Engineering Department VOTech EU FP6 funded design study for MPQ Max-Planck-Institut für Quantenoptik SEI System Engineering and Integration Euro-VO MUSE Multi Unit Spectroscopic Explorer (VLT) (ALMA) VPH Volume phase holographic, type of MUX Multiplexer (ALMA) SHAPS Shack-Hartmann sensor grating MVM Multi-resolution Vision Model (Archive) SHFI Swedish Heterodyne Facility VSI VLTI Spectro Imager NACO NAOS-CONICA (VLT) Instrument (APEX) VST VLT Survey Telescope NAOJ National Astronomical Observatory of SIMPLE High Spectral Resolution NIR VTK Vibration Tracking Japan Spectrograph WFC Wide Field Channel NAOS Nasmyth Adaptive Optics System (VLT) SINFONI Spectrograph for INtegral Field WFC3 Wide Field Camera 3 (Hubble) NASA National Aeronautics and Space Observations in the Near Infrared (VLT) WFCAM Infrared wide field camera for the UK Administration SM Service Mode Infrared Telescope on Mauna Kea NEON Network of European Observatories in SM4 Servicing Mission 4 (HST) WFI Wide Field Imager (2.2-metre) the North SNAP SuperNova Acceleration Probe WFPC2 Wide-Field Planetary Camera 2 (HST) NGC New General detector Controller SOFI SOn oF Isaac (NTT) Wind First of two NASA spacecraft in the NICMOS Near Infrared Camera and Multi-Object SPARTA Real-time computer platform for AOF Global Geospace Science initiative Spectrometer (Hubble) and SPHERE WVR Water Vapour Radiometer (ALMA) NIR Near-InfraRed spaxels Resolution scale for spectroscopy XMM-Newton X-ray Multi-Mirror satellite (ESA) NOVA Dutch Research School for Astronomy SPHERE Spectro-Polarimetric High-contrast X-shooter Wideband ultraviolet-infrared single (Nederlandse Onderzoekschool voor Exoplanet Research instrument target spectrograph (VLT) Astronomie) SSAC Site Selection Advisory Committee Yepun VLT Unit Telescope 4 NRI ESO quality control infrastructure STAC Standing Advisory Committee zCOSMOS VLT LP redshift survey NTT New Technology Telescope STC Scientific Technical Committee ZEUS Zernike Unit for Segment Phasing ST-ECF Space Telescope European Coordination Facility
ESO Annual Report 2008 143 ESO Europe Guest House Front cover: Part of the ESO VLT. Rey Gustavo Adolfo 4634 Headquarters Las Condes Back cover: Part of the globular cluster Omega Karl-Schwarzschild-Straße 2 Santiago de Chile Centauri, the brightest and largest globular cluster 85748 Garching bei München Chile in the sky. Germany Phone +5622084254 Phone +498932006-0 Fax +5622289333 Fax +49893202362 www.eso.org Antofagasta Office Avenida Balmaceda 2536 Office 504 ESO Chile Edificio ‘Don Guillermo’ Antofagasta Santiago Office Chile Alonso de Córdova 3107 Phone +5655260032 Vitacura Fax +5655260081 Casilla 19001 Santiago de Chile 19 Chile ESO is a partner in the international Phone +5624633100 ALMA project Fax +5624633101 ALMA Office Santiago La Silla Paranal Observatory El Golf 40, Piso 18 La Silla Site Las Condes IV Región Santiago de Chile Chile Chile Phone +5624644100 Phone +5624676100 Fax +5624644101 Fax +5624676101
La Silla Paranal Observatory ALMA Office San Pedro de Atacama Paranal Site Ayllo de Séquitor, Parcela 85 II Región II Región Chile Chile Phone +5655435100 Phone +5655448416 Fax +5655435101 Fax +5655448481
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La Serena Office All images are courtesy of ESO except Avenida El Santo 1538 where otherwise indicated. Casilla 567 La Serena Edited by the International Chile Relations Office Phone +5651225387 Fax +56 51215175 Produced by the education and Public Outreach Department
ESO 2009 ISSN 0531-4496