ADS BibCode:
2009Msngr.136....2G
Section:
400 Years of the Telescope
Author(s)/Affiliation(s):
Gilmozzi, R.
AA(ESO)
Abstract:
The contributions of ESO to the art of telescope-making have come a long way since the early years, placing it, by the turn of the millennium, among the acknowledged leaders in the field. In this article I will give a brief history of what are, in my view, the highlights among these developments, from the 3.6-metre telescope through the NTT and VLT/I to the E-ELT.
References:
Cuby, J.-G. 2007, The Messenger, 127, 25; Cullum, M. 2008, The Messenger, 134, 63; Enard, D. 1987, The Messenger, 50, 29; Hook, I. 2007, The Messenger, 127, 20; Monnet, G. 2007, The Messenger, 127, 24; Spyromilio, J. et al. 2008, The Messenger, 133, 2; Tarenghi, M. et al. 1998, The Messenger, 93, 4 Wampler E. J. et al. 1990, ApJ, 362, L13

ADS BibCode:
2009Msngr.136....8M
Section:
400 Years of the Telescope
Author(s)/Affiliation(s):
Moorwood, A.
AA(ESO)
Abstract:
This is a brief account of the development of infrared instrumentation at ESO from the first single pixel photometers, built in the optically dominated late 1970s, through the revolution ushered in by the development of panoramic infrared detectors and the VLT, to a tiny glimpse of the 42-metre E-ELT, whose instruments will probably operate predominantly in the infrared, with the aid of adaptive optics. In support of my personal memories, I have combed The Messenger for facts and include here the most accurate timeline I could construct, together with references for those who wish to read more, and by way of acknowledging some of those who contributed to this story.

ADS BibCode:
2009Msngr.136...13D
Section:
400 Years of the Telescope
Author(s)/Affiliation(s):
Dekker, H.
AA(ESO)
Abstract:
The evolution of optical spectrograph design and its implementation at ESO since 1980 is sketched out from the point of view of the instrumentation with which I have been closely involved. The instruments range from the early days of EFOSC, EMMI, UVES, GIRAFFE to the present-day X-shooter and important optical design features, such as the use of focal reducers and the white light pupil principle, are highlighted.

ADS BibCode:
2009Msngr.136...18S
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Saviane, I.; Ihle, G.; Sterzik, M.; Kaufer, A.
AA(ESO) AB(ESO) AC(ESO) AD(ESO)
Abstract:
From October 2009, the La Silla Observatory will begin a new phase in its history, following implementation of a new operations model. We describe here the upcoming changes, how the visiting astronomers will interact with the Observatory and how they will carry out their observations from October 2009 (ESO Period 84).

ADS BibCode:
2009Msngr.136...20B
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Baade, D.; Balestra, A.; Cumani, C.; Eschbaumer, S.; Finger, G.; Geimer, C.; Mehrgan, L.; Meyer, M.; Stegmeier, J.; Reyes, J.; Todorovic, M.
AA(ESO) AB(ESO) AC(ESO) AD(ESO) AE(ESO) AF(ESO) AG(ESO) AH(ESO) AI(ESO) AJ(ESO) AK(ESO)
Abstract:
As the replacement for ESO’s standard infrared and optical detector controllers, IRACE and FIERA respectively, ESO has developed a new controller — the New General detector Controller — that will be the default detector controller for all new La Silla Paranal instruments in the next decade. The basics of its design and functionality are described, and first performance examples are given.
References:
Andolfato, L. & Karban, R. 2008, SPIE, 7019, 64; Beletic, J.W. et al. 1998, ASSL, 228, 103; Downing, M.D. et al. 2006, SPIE, 6276, 15; Fedrigo, E. et al. 2006, SPIE, 6272, 31; Finger, G., Meyer, M & Moorwood, A.F.M. 1987, SPIE, 782, 130; Finger, G. et al. 2009, in Astrophysics Detector Workshop, Nice, in press Gach, J.-L. et al. 2006, in Scientific Detectors for Astronomy, 639; Meyer, M. et al. 1998, SPIE, 3354, 134 Reiss, R. 1994, SPIE, 2198, 895

ADS BibCode:
2009Msngr.136...25G
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Gonté, F.; Araujo, C.; Bourtembourg, R.; Brast, R.; Derie, F.; Duhoux, P.; Dupuy, C.; Frank, C.; Karban, R.; Mazzoleni, R.; Noethe, L.; Sedghi, B.; Surdej, I.; Yaitskova, N.; Luong, B.; Chueca, S.; Reyes, M.; Esposito, S.; Pinna, E.; Puglisi, A.; Pacheco, F.Q.; Dohlen, K.; Vigan, A.
AA(ESO) AB(ESO) AC(ESO) AD(ESO) AE(ESO) AF(ESO) AG(ESO) AH(ESO) AI(ESO) AJ(ESO) AK(ESO) AL(ESO) AM(ESO) AN(ESO) AO(Fogale Nanotech, Nîmes, France) AP(Instituto de Astrofísica de Canarias, La Laguna, Teneriffe, Spain) AQ(Instituto de Astrofísica de Canarias, La Laguna, Teneriffe, Spain) AR(Osservatorio Astrofisico di Arcetri – INAF, Italy) AS(Osservatorio Astrofisico di Arcetri – INAF, Italy) AT(Osservatorio Astrofisico di Arcetri – INAF, Italy) AU(Osservatorio Astrofisico di Arcetri – INAF, Italy) AV(Laboratoire d’Astrophysique de Marseille, France) AW(Laboratoire d’Astrophysique de Marseille, France)
Abstract:
The Active Phasing Experiment (APE) has been used by ESO to gain experience in controlling segmented primary mirrors in preparation for the European Extremely Large Telescope. The experiment tested various phasing techniques and explored their advantages and limitations. Four optical phasing sensors were developed using different techniques — a curvature sensor, a pyramid sensor, a Shack–Hartmann sensor and a sensor based on a modified Mach–Zehnder interferometer. The design of the APE instrument is described. APE was installed at the VLT visitor focus for on-sky testing and a brief summary of the results of the experiment is given.
References:
Chanan, G. et al. 1998, Applied Optics, 37, 140; Chueca, S. et al. 2008, Proc. SPIE, 7012, 13; Dupuy, C. et al. 2008, Proc. SPIE, 7012, 127; Gonté, F. et al. 2007, The Messenger, 128, 23; Marchetti, E. et al. 2007, The Messenger, 129, 8; Mazzoleni, R. et al. 2008, Proc. SPIE, 7012, 124; Pinna, E. et al. 2008, Proc. SPIE, 7012, 116; Surdej, I. et al. 2008, Proc. SPIE, 7012, 34; Wilhelm, R. C. et al. 2008, Applied Optics, 47, 5473; Yaitskova, N. et al. 2005, Optical Society of America 22, 1093

ADS BibCode:
2009Msngr.136...32T
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Tan, G.H.; Ellison, B.; Lilley, P.; Patt, F.
AA(ESO) AB(Science and Technology Facilities Council, Rutherford Appleton Laboratory, Didcot, UK) AC(ESO) AD(ESO)
Abstract:
The ALMA Project has moved into the production phase, perhaps most notably for the advanced receiver systems, or Front Ends that are required by the project. This article provides a summary of the technical and production status of the various Front End subassemblies and some of their recent deliveries. The first complete Front End has been delivered by the European Front End Integration Centre to the ALMA Observatory in Chile.
References:
Barkhof, J. et al. 2009, Proc. 20th Int. Symp. on Space THz Technology, Charlottesville, USA, Emrich, A. et al. 2008, Proc. 19th Int. Symp. on Space THz Technology, Groningen, The Netherlands, 528. Emrich, A. et al. 2009, Proc. 20th Int. Symp. on Space THz Technology, Charlottesville, USA, Haupt, C. & Rykaczewski, H. 2007, The Messenger, 128, 2007; Jackson, B. D. et al. 2009, R. Proc. 20th Int. Symp. on Space THz Technology, Charlottesville, USA, Murk, A. et al. 2008, Proc. 19th Int. Symp. on Space THz Technology, Groningen, The Netherlands, 530; Nikolic, B. et al. 2008, The Messenger, 131, 14; Tan, G. H. et al. 2004, The Messenger, 118, 18

ADS BibCode:
2009Msngr.136...39K
Section:
Astronomical Science
Author(s)/Affiliation(s):
Kürster, M.; Zechmeister, M.; Endl, M.; Meyer, E.
AA(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AB(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AC(McDonald Observatory, University of Texas at Austin, USA) AD(Max-Planck-Institut für Astronomie, Heidelberg, Germany)
Abstract:
We present results from our search programme for extrasolar planets around M dwarfs carried out with UVES between 2000 and 2007 and enjoying ESO Large Programme status from April 2004 to March 2006. In our sample of 41 stars we have found one “brown dwarf desert” companion candidate, but no planetary mass companions. We have determined upper limits to the mass of possible companions, which, in the habitable zones of our better observed stars, reach the regime of a few Earth masses. Significant periodic variability observed in Barnard’s star is attributed to stellar activity.
References:
Endl M. et al. 2006, ApJ, 649, 436; Endl M. & Kürster M. 2008, A&A, 488, 1149 Hünsch M. et al. 1999, A&AS, 135, 319 Kasting, J. F. et al. 1993, Icarus, 101, 108 Kürster M. et al. 2003, A&A, 403, 1077 Kürster M., Endl M. & Rodler F. 2006, The Messenger, 123, 21 Kürster M., Endl M. & Reffert S. 2008, A&A, 483, 869 Meyer E., & Kürster M. 2008, in Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun, AIP Conf. Proc. 1094, 549 Nakajima T. et al. 1995, Nature, 378, 463 van Leeuwen F. 2007, A&A, 474, 653 Zechmeister M., Kürster M. & Endl M. 2009, A&A, submitted

ADS BibCode:
2009Msngr.136...44K
Section:
Astronomical Science
Author(s)/Affiliation(s):
Kraus, S.; Weigelt, G.; Balega, Y.; Docobo, J.; Hofmann, K.; Preibisch, T.; Schertl, D.; Tamazian, V.; Driebe, T.; Ohnaka, K.; Petrov, R.; Schöller, M.; Smith, M.
AA(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AB(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AC(Special Astrophysical Observatory, Russia) AD(University of Santiago de Compostela, Galicia, Spain) AE(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AF(Universitäts-Sternwarte, München, Germany) AG(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AH(University of Santiago de Compostela, Galicia, Spain) AI(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AJ(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AK(Observatoire de la Côte d’Azur, Nice, France) AL(ESO, Garching) AM(University of Kent, Canterbury, UK)
Abstract:
Located in the Orion Trapezium Cluster, θ1 Ori C is one of the youngest and nearest high-mass stars known. Besides its unique properties as an oblique magnetic rotator, the star happens to be a close (~20 milliarcseconds) binary system, which makes it an ideal laboratory to determine the fundamental parameters of young hot stars. In this article, we report on our 11-year interferometric monitoring campaign, which covers nearly the full dynamic orbit of the system and resulted in the first interferometric images obtained with the VLT interferometer (VLTI) in the infrared (~20 µm) and diffraction-limited bispectrum speckle interferometry at the ESO 3.6-metre telescope at visual (440 nm) wavelengths.
References:
Babel, J. & Montmerle, T. 1997, ApJ, 485, L29; Donati, J.-F. et al. 2002, MNRAS, 333, 55; Hofmann, K.-H. & Weigelt, G. 1993, A&A, 167, L15; Kraus, S. et al. 2007, A&A, 466, 649; Kraus, S. et al. 2009, A&A, 497, 195; Menten, K. M. et al. 2007, A&A, 474, 515; Patience, J. et al. 2008, ApJ, 674, L97; Petrov, R. G. et al. 2007, A&A, 464, 1; Schertl, D. et al. 2003, A&A, 402, 267; Stahl, O. et al. 2008, A&A, 487, 323; Tan, J. C. 2004, ApJ, 607, L47; Weigelt, G. et al. 1999, A&A, 347, L15

ADS BibCode:
2009Msngr.136...48Z
Section:
Astronomical Science
Author(s)/Affiliation(s):
Zoccali, M.; Hill, V.; Barbuy, B.; Lecureur, A.; Minniti, D.; Renzini, A.; Gonzalez, O.; Gómez, A.; Ortolani, S.
AA(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Chile) AB(CNRS, Observatoire de la Côte d’Azur, France) AC(Universidade de São Paulo, Brazil) AD(GEPI, Observatoire de Paris, France; Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Germany) AE(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Chile; Vatican Observatory, Italy) AF(INAF–Osservatorio Astronomico di Padova, Italy) AG(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Chile) AH(CNRS, Observatoire de la Côte d’Azur, France) AI(Università di Padova, Dipartimento di Astronomia, Italy)
Abstract:
VLT–FLAMES observations provide by far the largest sample of high dispersion spectra of Bulge red giants available. Five years of work on these 900 spectra have yielded the abundances of different elements in the Milky Way Bulge, and new results on its formation. The results so far include the Bulge metallicity distribution, the Bulge metallicity gradient, the metallicity dependence on kinematics, the history of enrichment with alpha-elements, as well as the lithium abundance. The evidence collected on Milky Way Bulge chemical enrichment supports a rapid early formation scenario, and the metallicity gradient argues against formation via secular bar evolution.
References:
Barbuy, B. et al. 2007, AJ, 134, 1613; Bensby, T., Feltzing, S. & Lundström, I. 2004, A&A, 421, 155; Clarkson, W. 2008, ApJ, 684, 1110; Cuhna, K. & Smith, V.V. 2006, ApJ, 651, 491; Fulbright, J.P., McWilliam, A. & Rich, R.M. 2007, ApJ, 661, 1152; González, O. et al. 2009, A&A, submitted Lecureur, A. et al. 2007, A&A, 465, 799; McWilliam, A. & Rich, R.M. 1994, ApJ, 91, 749; McWilliam, A. & Rich, R.M. 2003, in Origin and Evolution of the Elements Melendez, J. et al. 2008, A&A, 484, L21; Nordström, B. et al. 2004, A&A, 418, 989; Peletier, R. et al. 2007, MNRAS, 379, 445; Reddy, B.E., Lambert, D.L. & Allende Prieto, C. 2006, MNRAS, 367, 1329; Rich, R.M. & Origlia, L. 2005, ApJ, 634, 1293; Stetson, P., & Pancino, E. 2008, PASP, 120, 1332; Zoccali, M. et al. 2003, A&A, 399, 931; Zoccali, M. et al. 2006, A&A, 457, L1; Zoccali, M. et al. 2008, A&A, 486, 177

ADS BibCode:
2009Msngr.136...54P
Section:
Astronomical Science
Author(s)/Affiliation(s):
Poggianti, B.; Aragón-Salamanca, A.; Bamford, S.; Barazza, F.; Best, P.; Clowe, D.; Dalcanton, J.; De Lucia, G.; Desai, V.; Finn, R.; Halliday, C.; Jablonka, P.; Johnson, O.; Milvang-Jensen, B.; Moustakas, J.; Noll, S.; Nowak, N.; Pelló,R.; Poirier, S.; Rudnick, G.; Saglia, R.; Sánchez-Blázquez, P.; Simard, L.; Varela, J.; von der Linden, A.; Whiley, I.; White, S.; Zaritsky, D.
AA(INAF-Osservatorio Astronomico di Padova, Italy) AB(University of Nottingham, UK) AC(University of Nottingham, UK) AD(Ecole Polytechnique Federale de Lausanne, Switzerland) AE(Institute for Astronomy, Edimburgh, UK) AF(Ohio University, Athens, USA) AG(University of Washington, Seattle, USA) AH(INAF-Osservatorio Astronomico di Trieste, Italy) AI(Spitzer Science Center, California Institute of Technology, Pasadena, USA) AJ(Siena College, Loudonville, USA) AK(INAF-Osservatorio Astronomico di Padova, Italy) AL(Ecole Polytechnique Federale de Lausanne, Switzerland; Université de Geneve, Observatoire, Switzerland; GEPI, Observatoire de Paris, Meudon, France) AM(University of Nottingham, UK) AN(Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Denmark) AO(New York University, USA) AP(Observatoire Astronomique Marseille-Provence, France) AQ(Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany) AR(Universite de Toulouse, France) AS(GEPI, Observatoire de Paris, Meudon, France) AT(NOAO, Tucson, USA) AU(Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany) AV(University of Central Lancashire, Preston, UK) AW(Herzberg Institute of Astrophysics, Victoria, Canada) AX(INAF-Osservatorio Astronomico di Padova, Italy) AY(Max-Planck-Institut für Astrophysik, Garching, Germany) AZ(University of Nottingham, UK) BA(Max-Planck-Institut für Astrophysik, Garching, Germany) BB(Steward Observatory, Tucson, USA)
Abstract:
The ESO Distant Cluster Survey (EDisCS, P.I. Simon D.M. White, LP 166.A-0162) is an ESO Large Programme aimed at studying clusters and cluster galaxies at z = 0.4–1. How different is the evolution of the star formation activity in clusters, in groups and in the field? Does it depend on cluster mass and/or the local galaxy density? How relevant are starburst and post-starburst galaxies in the different environments? Is there an evolution in the galaxies’ structures, and if so, is this related to the changes in their star formation activity? These are some of the main questions that have been investigated using the EDisCS dataset.
References:
Barazza, F. et al. 2009, A&A, 497, 713; Clowe, D. et al. 2006, A&A, 451, 395; De Lucia, G. et al. 2004, ApJL, 610, L77; De Lucia, G. et al. 2007, MNRAS, 374, 809; Desai, V. et al. 2007, ApJ, 660, 1151; Finn, R. et al. 2005, ApJ, 630, 206; Gonzalez, A.H. et al. 2001, ApJS, 137, 117; Halliday, C. et al. 2004, A&A, 427, 397; Johnson, O. et al. 2006, MNRAS, 371, 1777; Milvang-Jensen, B. et al. 2008, A&A, 482, 419; Pello, R. et al. 2009, A&A in press Poggianti, B.M. et al. 2006, ApJ, 642, 188; Poggianti, B.M. et al. 2008, ApJ, 684, 888; Poggianti, B.M. et al. 2009a, ApJ, 693, 112; Poggianti, B.M. et al. 2009b, ApJL, 697, L137; Rudnick, G. et al. 2009, A&A in press Sánchez-Blázquez, P. et al. 2009, A&A, in press (arXiv:0902.3392) Whiley, I. et al. 2008, MNRAS, 387, 1253; White, S. et al. 2005, A&A, 444, 36

ADS BibCode:
2009Msngr.136...61V
Section:
Astronomical News
Author(s)/Affiliation(s):
van Loon, J.
AA(Astrophysics Group, Keele University, UK)
Abstract:
The European Southern Observatory is an international organisation serving a large scientific community. Financed by its member states, its facilities are open to all professional astronomers around the world. ESO and its users form a partnership, aimed at maximising scientific progress: ESO provides the infrastructure and logistical support, and the users carry out the most exciting measurements and publish these in a timely fashion in respectable journals.
References:
Wisotzki, L. 2001, The Messenger, 106, 46

ADS BibCode:
2009Msngr.136...64M
Section:
Astronomical News
Author(s)/Affiliation(s):
Melnick, J.; Mellier, Y.; Pasquini, L.; Leibundgut, B.
AA(ESO) AB(Institut d’Astrophysique de Paris, France) AC(ESO) AD(ESO)
Abstract:
The wide-field imaging surveys to be conducted with ESO VISTA and VST telescopes and with the ESA Gaia satellite demand spectroscopic follow-up. Presentations and discussions on the role of wide-field spectroscopic surveys with ESO telescopes at this dedicated workshop are summarised. The instrument requirements for spectroscopic surveys of large-scale galaxy structure, fundamental cosmology, and the structure of the Milky Way and its neighbourhood are presented.
References:
Benitez, N. et al. 2009, ApJ, 691, 241; Bode, M. F., Cruz, M. J. & Molster, F. 2008. The ASTRONET Infrastructure Roadmap: A Strategic Plan for European Astronomy Eisenstein, D. et al. 2005, ApJ, 633, 660; Guzzo, L. et al. 2008, Nature, 451, 541; Melo. C. et al. 2008, The Messenger, 133, 17 Moorwood, A. 2009, Science with the VLT in the ELT era, (Berlin: Springer) Peacock, J. et al. 2006, ESA–ESO Working Groups, Report No. 3, Fundamental Cosmology Tolstoy, E., Hill, V. & Tosi, M. 2009, ARAA, 47, in press Turon, C. et al. 2008, ESA–ESO Working Groups, Report No. 4, Galactic Populations, Chemistry and Dynamics

ADS BibCode:
2009Msngr.136...69K
Section:
Astronomical News
Author(s)/Affiliation(s):
Kissler-Patig, M.; Testi, L.
AA(ESO) AB(ESO)
Abstract:
The workshop explored the scientific synergies between ALMA and the extremely large telescopes that are being planned. The main goal of the workshop was to bring the ALMA and ELT communities together, to identify the common science cases and to outline instrumentation/upgrade priorities for the ALMA and ELT facilities. We provide a brief account of the scientific sessions and the wide-ranging discussions held during this very lively four-day meeting.

ADS BibCode:
2009Msngr.136...72L
Section:
Astronomical News
Author(s)/Affiliation(s):
Leibundgut, B.; Christensen, L.L.; Janssen, E.
AA(ESO) AB(ESO) AC(ESO)

ADS BibCode:
2009Msngr.136...73.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2009Msngr.136...74.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2009Msngr.136Q..75.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2009Msngr.136R..75.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2009Msngr.136...76.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2009Msngr.136...77.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2009Msngr.136...78.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2009Msngr.136...79.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)