ADS BibCode:
2011Msngr.145....2J
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Jehin, E.; Gillon, M.; Queloz, D.; Magain, P.; Manfroid, J.; Chantry, V.; Lendl, M.; Hutsemékers, D.; Udry, S.
AA(Institut d’Astrophysique de l’Université de Liège, Belgium) AB(Institut d’Astrophysique de l’Université de Liège, Belgium) AC(Observatoire de l’Université de Genève, Switzerland) AD(Institut d’Astrophysique de l’Université de Liège, Belgium) AE(Institut d’Astrophysique de l’Université de Liège, Belgium) AF(Institut d’Astrophysique de l’Université de Liège, Belgium) AG(Observatoire de l’Université de Genève, Switzerland) AH(Institut d’Astrophysique de l’Université de Liège, Belgium) AI(Observatoire de l’Université de Genève, Switzerland)
Abstract:
TRAPPIST is a 60-cm robotic telescope that was installed in April 2010 at the ESO La Silla Observatory. The project is led by the Astrophysics and Image Processing group (AIP) at the Department of Astrophysics, Geophysics and Oceanography (AGO) of the University of Liège, in close collaboration with the Geneva Observatory, and has been funded by the Belgian Fund for Scientific Research (F.R.S.-FNRS) and the Swiss National Science Foundation (SNF). It is devoted to the detection and characterisation of exoplanets and to the study of comets and other small bodies in the Solar System. We describe here the goals of the project and the hardware and present some results obtained during the first six months of operation.
References:
Csizmadia, Sz. et al. 2011, A&A, 531, 41; Deming, D. & Seager, S. 2009, Nature, 462, 301; Farnham, T. L. et al. 2000, Icarus, 147, 180; Gillon, M. et al. 2011, A&A (accepted) Gillon, M. et al. 2007, A&A, 466, 743; Gillon, M. et al. 2009, A&A, 496, 259; Hsieh, H. & Jewitt D. 2006, Science 312, 561; Jehin, E. et al. 2010, CBET #2589; Jehin, E. et al. 2010, CBET, #2632; Mayor, M. et al. 2003, The Messenger, 114, 20; Meech, K. et al. 2011, ApJL, 734, L1; Queloz, D. et al. 2000, A&A, 354, 99; Sicardy, B. et al. 2011, Nature, accepted Triaud, A. et al. 2011, A&A, 513, A24

ADS BibCode:
2011Msngr.145....7W
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Wittkowski, M.; Ballester, P.; Bonneau, D.; Chelli, A.; Chesneau, O.; Cruzalèbes, P.; Duvert, G.; Hummel, C.; Lafrasse, S.; Mella, G.; Melnick, J.; Mérand, A.; Mourard, D.; Percheron, I.; Sacuto, S.; Shabun, K.; Stefl, S.; Vinther, J.
AA(ESO) AB(ESO) AC(Jean-Marie Mariotti Center, France; Université Nice Sophia Antipolis, CNRS, Observatoire de la Côte d’ Azur, Nice, France) AD(Jean-Marie Mariotti Center, France; Université Joseph Fourier 1/CNRS-INSU, Institut de Planetologie et d’Astrophysique de Grenoble, France) AE(Jean-Marie Mariotti Center, France; Université Nice Sophia Antipolis, CNRS, Observatoire de la Côte d’ Azur, Nice, France) AF(Jean-Marie Mariotti Center, France; Université Nice Sophia Antipolis, CNRS, Observatoire de la Côte d’ Azur, Nice, France) AG(Jean-Marie Mariotti Center, France; Université Joseph Fourier 1/CNRS-INSU, Institut de Planetologie et d’Astrophysique de Grenoble, France) AH(ESO) AI(Jean-Marie Mariotti Center, France; Université Joseph Fourier 1/CNRS-INSU, Institut de Planetologie et d’Astrophysique de Grenoble, France) AJ(Jean-Marie Mariotti Center, France; Université Joseph Fourier 1/CNRS-INSU, Institut de Planetologie et d’Astrophysique de Grenoble, France) AK(ESO) AL(ESO) AM(Jean-Marie Mariotti Center, France; Université Nice Sophia Antipolis, CNRS, Observatoire de la Côte d’ Azur, Nice, France) AN(ESO) AO(Jean-Marie Mariotti Center, France; Department of Physics and Astronomy, Uppsala University, Sweden) AP(ESO) AQ(ESO) AR(ESO)
Abstract:
Interferometric observations require frequent measurements of calibration stars of known diameter to estimate the instrumental transfer function. ESO offers the preparation tool CalVin to select suitable calibrators from an underlying list of calibrators. The latest version 3, first released in January 2011, offers major improvements in the number of available calibrators, the functionality of the search tool, as well as in terms of performance and ease of use. It has been developed in a collaboration between ESO and the French Jean-Marie Mariotti Center (JMMC).
References:
Beust, H. et al. 2011, MNRAS, 414, 108; Bonneau, D. et al. 2006, A&A, 456, 789; Bonneau, D. et al. 2011, to appear in A&A Bordé, P. et al. 2002, A&A, 393, 183; Cruzalèbes, P. et al. 2010, A&A, 515, A6; Ishihara, D. et al. 2010, A&A, 514, A1; Lafrasse, S. et al. 2010, VizieR Online Data Catalog, 2300; Mérand, A. et al. 2006, A&A, 447, 783; Verhoelst, T. 2005, PhD thesis K. U. Leuven, Belgium Wittkowski, M. et al. 2005, The Messenger, 119, 14

ADS BibCode:
2011Msngr.145...10R
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Ramsay, S.; Hammersley, P.; Pasquini, L.
AA(ESO) AB(ESO) AC(ESO)
Abstract:
With the advent of many large-area imaging surveys in recent years, the need for a new facility for spectroscopic surveys has become apparent. Following a recommendation from the Science and Technical Committee, ESO made a call in 2010 for wide field spectroscopic instrument proposals among its community. Two of the ten proposals were selected for a competitive Phase A study. This article describes the selection process and two associated articles present the instrument concepts.
References:
Arnaboldi, M. et al. 2007, The Messenger, 127, 28; Bode, M. F., Cruz, M. J. & Molster, F. J. 2008., The ASTRONET Infrastructure Roadmap, Astronet

ADS BibCode:
2011Msngr.145...11C
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Cirasuolo, M.; Afonso, J.; Bender, R.; Bonifacio, P.; Evans, C.; Kaper, L.; Oliva, E.; Vanzi, L.
AA(STFC United Kingdom Astronomy Technology Centre, Edinburgh, United Kingdom; Institute for Astronomy, University of Edinburgh, United Kingdom) AB(Observatorio Astronomico de Lisboa, Portugal) AC(Universitäts-Sternwarte, München, Germany; Max-Planck-Institut für extraterrestrische Physik, München, Germany) AD(GEPI, Observatoire de Paris, CNRS, Univ. Paris Diderot, France) AE(STFC United Kingdom Astronomy Technology Centre, Edinburgh, United Kingdom) AF(Astronomical Institute Anton Pannekoek, Amsterdam, the Netherlands) AG(INAF–Osservatorio Astrofisico di Arcetri, Italy) AH(Centre for Astro-Engineering at Universidad Catolica, Santiago, Chile)
Abstract:
MOONS (Multi-Object Optical and Near-infrared Spectrograph) is a large field (500 square arcminutes), multi-object (500 object + 500 sky fibres) instrument with spectral resolution of 5000 and 20000 proposed for the VLT Nasmyth focus. The science case for MOONS, covering Galactic structure and galaxy evolution up to the epoch of re-ionisation, is briefly outlined.
References:
Peacock, J. et al. 2001, Nature, 410, 169; Recio-Blanco, A., Hill, V. & Bienaymé, O. 2009, Proc. French Society of Astron. & Astrophys. SF2A-2009

ADS BibCode:
2011Msngr.145...14J
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
de Jong, R.
AA(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany)
Abstract:
4MOST (4-metre Multi-Object Spectroscopic Telescope) is a very large field (goal > 5 square degrees) multi-object spectrograph with up to 3000 fibres and spectral resolutions of 5000 and 20000, proposed for the New Technology Telescope (NTT) or the VISTA survey telescope. The science cases covering Gaia follow-up for chemistry and kinematics of the Galaxy and redshift surveys of targets from the eROSITA X-ray mission are briefly outlined.
References:
Akiyama, M. et al. 2008, SPIE, 7018, 94; Bode, M., Cruz, M. & Molster, F. 2008, The ASTRONET Infrastructure Roadmap Cooper, A. P. et al. 2010, MNRAS, 406, 744; de Zeeuw, P. & Molster, F. 2007, A Science Vision for European Astronomy (ASTRONET) Drew, J. et al. 2010, Report by the European telescope strategic review committee on Europe’s 2–4m telescopes over the decade to 2020 (ASTRONET) Helmi, A. et al. 2011, ApJL, 733, L7; Hu, H. et al. 2004, SPIE, 5492, 574; Mühlegger, M. 2010, Ph.D. thesis, Technische Universität München Predehl, P. et al. 2010, SPIE, 7732, 23; Turon, C. et al. 2008, Report by the ESA-ESO Working Group on Galactic populations, chemistry and dynamics, ST-ECF, ESO

ADS BibCode:
2011Msngr.145...17T
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Testi, L.; Zwaan, M.
AA(ESO) AB(ESO)
Abstract:
ALMA is rapidly progressing towards the end of the construction phase. At the beginning of August 2011, 17 antennas were interferometrically linked on the Chajnantor plateau at an altitude of 5000 metres. Twelve-metre antennas from all the vendors were used in this experiment, which is a major milestone towards the first Early Science guest observer observations, currently planned to begin soon. In the meantime, ALMA Science Verification datasets are becoming available on the ALMA webpages for users to download and gain familiarity with ALMA data reduction and analysis procedures.
References:
Hughes, A. M. et al. 2011, ApJ, 727, 85; Qi, C. et al. 2008, ApJ, 681, 1396; Randall, S. & Testi, L. 2011, The Messenger, 144, 39; Sakamoto, K., Ho, P. T. P. & Peck, A. B. 2006, ApJ, 644, 862; Testi, L. 2010, The Messenger, 139, 52; Testi, L. et al. 2010, The Messenger, 142, 17

ADS BibCode:
2011Msngr.145...20L
Section:
Astronomical Science
Author(s)/Affiliation(s):
Lellouch, E.; de Bergh, C.; Sicardy, B.; Käufl, H.-U.; Smette, A.
AA(LESIA-Observatoire de Paris, CNRS, UPMC Univ. Paris 06, Univ. Paris-Diderot, France) AB(LESIA-Observatoire de Paris, CNRS, UPMC Univ. Paris 06, Univ. Paris-Diderot, France) AC(LESIA-Observatoire de Paris, CNRS, UPMC Univ. Paris 06, Univ. Paris-Diderot, France) AD(ESO) AE(ESO)
Abstract:
The dwarf planet Pluto and Neptune's largest satellite, Triton, are two small icy bodies surrounded by tenuous and poorly known atmospheres. The high spectral resolution and high sensitivity of CRIRES on the VLT have permitted a major step forward in the study of these atmospheres, and especially of their composition. Absorptions due to methane and carbon monoxide in these atmospheres have been detected at 1.66 and 2.35 µm, providing an insight into the way in which these atmospheres are maintained, the surface-atmosphere interactions, their seasonal evolution and thermal balance.
References:
Barucci, M. A. et al. 2010, The Messenger, 141, 15; Buie, M. W. et al. 2010, AJ, 139, 1128; Douté, S. et al. 1999, Icarus, 142, 421; Greaves, J. S., Helling, C. & Friberg, P. 2011, MNRAS, 414, L36; Lellouch, E. et al. 2009, A & A, 495, L17. See also ESO PR-0809. Lellouch, E. et al. 2010, A & A, 512, L8. See also ESO PR-1015. Lellouch, E. et al. 2011, A & A, 511, L4; Origlia, L. & Oliva, E. 2009, Earth, Moon & Planets, 105, 123; Origlia, L., Oliva, E. & Maiolino, R. 2010, The Messenger, 140, 38; Schaller, E. L. & Brown, M. E. 2007, ApJ, 659, L61; Trafton, L. M., Matson, D.L. & Stansberry, J. A. 1998. In Solar System Ices, Kluwer Academic Publishers, 773; Young, L. et al. 1997, Icarus, 153, 148

ADS BibCode:
2011Msngr.145...24W
Section:
Astronomical Science
Author(s)/Affiliation(s):
Wittkowski, M.; Karovicova, I.; Boboltz, D. A.; Fossat, E.; Ireland, M.; Ohnaka, K.; Scholz, M.; van Wyk, F.; Whitelock, P.; Wood, P. R.; Zijlstra, A. A.
AA(ESO) AB(ESO) AC(United States Naval Observatory, Washington, DC, USA) AD(Laboratoire d’Université d’Astrophysique de Nice, France) AE(Dept. of Physics and Astronomy, Macquarie University, Sydney, Australia; Australian Astronomical Observatory, Epping, Australia) AF(Max-Planck Institut für Radioastronomie, Bonn, Germany) AG(Zentrum für Astronomie, University of Heidelberg, Germany; School of Physics, University of Sydney, Australia) AH(South African Astronomical Observatory, Cape Town, South Africa) AI(South African Astronomical Observatory, Cape Town, South Africa; Astronomy Dept., University of Cape Town, Rondebusch, South Africa) AJ(Australian National University, Canberra, Australia) AK(Jodrell Bank Centre for Astrophysics, University of Manchester, United Kingdom)
Abstract:
Mass loss from asymptotic giant branch (AGB) stars is the most important driver for the evolution of low to intermediate mass stars towards planetary nebulae. It is also one of the most important sources of chemical enrichment of the interstellar medium. The mass-loss process originates in the extended atmosphere, whose structure is affected by stellar pulsations, and where molecular and dusty layers are formed. Optical interferometry resolves the extended atmospheres of AGB stars and thereby enables us to obtain measurements of the intensity profile across this region. We present an overview of recent results from our spectro-interferometric observations of AGB stars using the near- and mid-infrared instruments AMBER and MIDI of the VLT Interferometer.
References:
Decin, L. et al. 2010, Nature, 467, 64; Habing, H. J & Olofsson, H. 2003, Astronomy and astrophysics library, New York, (Berlin: Springer) Ireland, M. et al. 2008, MNRAS, 391, 1994; Ireland, M. et al. 2011, MNRAS, in press (arXiv 1107.3619) Karovicova, I. et al. 2011, A&A, 532, A134; Ohnaka, K. et al. 2005, A&A, 429, 1057; Wittkowski, M. et al. 2008, A&A, 479, L21; Wittkowski, M. et al. 2011, A&A, 532, L7

ADS BibCode:
2011Msngr.145...29P
Section:
Astronomical Science
Author(s)/Affiliation(s):
Petr-Gotzens, M.; Alcalá, J. M.; Briceño, C.; González-Solares, E.; Spezzi, L.; Teixeira, P.; Osorio, M. R. Z.; Comerón, F.; Emerson, J.; Hodgkin, S.; Hussain, G.; McCaughrean, M.; Melnick, J.; Oliveira, J.; Ramsay, S.; Stanke, T.; Winston, E.; Zinnecker, H.
AA(ESO) AB(INAF–Osservatorio di Capodimonte, Napoli, Italy) AC(Centro de Investigaciones de Astronomía (CIDA), Mérida, Venezuela) AD(Institute of Astronomy, Cambridge, United Kingdom) AE(European Space Agency (ESTEC), Noordwijk, the Netherlands) AF(ESO) AG(Centro de Astrobiología, Instituto Nacional de Técnica Aerospacial (CSIC-INTA), Madrid, Spain) AH(ESO) AI(Astronomy Unit, Queen Mary, University of London, United Kingdom) AJ(Institute of Astronomy, Cambridge, United Kingdom) AK(ESO) AL(European Space Agency (ESTEC), Noordwijk, the Netherlands) AM(ESO) AN(Astrophysics Group, Keele University, United Kingdom) AO(ESO) AP(ESO) AQ(School of Physics, University of Exeter, United Kingdom) AR(SOFIA Science Center, NASA-Ames, Moffett Field, USA)
Abstract:
As part of the VISTA Science Verification programme, a large set of images in Orion was obtained at five near-infrared wavelength bands, from 0.9 to 2.2 μm. The resulting multi-band catalogue contains approximately three million sources, allowing investigation of various issues concerning star and brown dwarf formation, such as a) the difference in the shape of the substellar mass function in a cluster vs. non-clustered environment, b) the influence of massive OB stars on the process of brown dwarf formation, c) the size and morphology of dust envelopes around protostars, and d) the comparative role of mass and environment on the evolution of circumstellar discs. The data from the VISTA Orion Survey, including catalogues, are available to the community. In this article we present an overview of selected science results that have emerged so far from this survey.
References:
Allard, F. et al. 2001, ApJ, 556, 357; Allen, L. et al. 2007, in Protostars and Planets V. Eds. B. Reipurth, D. Jewitt, & K. Keil, Univ. Arizona Press, Tucson, p.361; Andreuzzi, G. et al. 2011, MNRAS, 412, 1265; Arnaboldi, M. et al. 2010, The Messenger, 139, 6; Bally, J. 2008, in Handbook of Star Forming Regions Vol. I, ed. B. Reipurth, ASP, p. 459; Baraffe, I. et al. 2003, A&A, 402, 701; Briceño, C. et al. 2005, AJ, 129, 907; Briceño, C. et al. 2007, ApJ, 661, 1119; Briceño, C. 2008, in Handbook of Star Forming Regions Vol. I, ed. B. Reipurth, ASP, p. 838; Briceño, C. et al. 2011, in preparation Caballero, J. A. & Solano, E. 2008, A&A, 485, 931; Chabrier, G. et al. 2000, ApJ, 542, 464; Emerson, J., McPherson, A. & Sutherland, W. 2006, The Messenger, 126, 41; Girardi, L. et al. 2002, A&A, 391, 195; Megeath, S. T. et al. 2005, IAUS, 227, 383; Peña Ramírez, K. et al. 2011, A&A, 532, 42; Scholz, A. & Eislöffel, J. 2005, A&A, 429, 1007; Sestito, P. et al. 2008, A&A, 488, 943

ADS BibCode:
2011Msngr.145...33E
Section:
Astronomical Science
Author(s)/Affiliation(s):
Evans, C.; Taylor, W.; Sana, H.; Hénault-Brunet, V.; Bagnoli, T.; Bastian, N.; Bestenlehner, J.; Bonanos, A.; Bressert, E.; Brott, I.; Campbell, M.; Cantiello, M.; Carraro, G.; Clark, S.; Costa, E.; Crowther, P.; de Koter, A.; de Mink, S.; Doran, E.; Dufton, P.; Dunstall, P.; Garcia, M.; Gieles, M.; Gräfener, G.; Herrero, A.; Howarth, I.; Izzard, R.; Köhler, K.; Langer, N.; Lennon, D.; Apellániz, J. M.; Markova, N.; Najarro, P.; Puls, J.; Ramirez, O.; Sabín-Sanjulián, C.; Simón-Díaz, S.; Smartt, S.; Stroud, V.; van Loon, J.; Vink, J. S.; Walborn, N.
AA(United Kingdom Astronomy Technology Centre, STFC, Royal Observatory, Edinburgh, United Kingdom) AB(Scottish Universities Physics Alliance, Institute for Astronomy, University of Edinburgh, United Kingdom) AC(Astronomical Institute Anton Pannekoek, University of Amsterdam, the Netherlands) AD(Scottish Universities Physics Alliance, Institute for Astronomy, University of Edinburgh, United Kingdom) AE(Astronomical Institute Anton Pannekoek, University of Amsterdam, the Netherlands) AF(Excellence Cluster Universe, Garching, Germany) AG(Armagh Observatory, Northern Ireland, United Kingdom) AH(National Observatory of Athens, Greece) AI(School of Physics, University of Exeter, United Kingdom; ESO; Harvard–Smithsonian Center for Astrophysics, Cambridge, USA) AJ(Department of Astronomy, University of Vienna, Austria) AK(Scottish Universities Physics Alliance, Institute for Astronomy, University of Edinburgh, United Kingdom) AL(Argelander-Institut für Astronomie der Universität Bonn, Germany) AM(ESO) AN(Department of Physics and Astronomy, The Open University, Milton Keynes, United Kingdom) AO(Departamento de Astronomia, Universidad de Chile, Santiago, Chile) AP(Department. of Physics & Astronomy, University of Sheffield, United Kingdom) AQ(Astronomical Institute Anton Pannekoek, University of Amsterdam, the Netherlands; University of Utrecht, the Netherlands) AR(Space Telescope Science Institute, Baltimore, USA; Hubble Fellow) AS(Department. of Physics & Astronomy, University of Sheffield, United Kingdom) AT(Department of Physics & Astronomy, Queen’s University Belfast, Northern Ireland, United Kingdom) AU(Department of Physics & Astronomy, Queen’s University Belfast, Northern Ireland, United Kingdom) AV(Instituto de Astrofísica de Canarias, La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, Tenerife, Spain) AW(Insitiute of Astronomy, University of Cambridge, United Kigdom) AX(Armagh Observatory, Northern Ireland, United Kingdom) AY(Instituto de Astrofísica de Canarias, La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, Tenerife, Spain) AZ(Department of Physics & Astronomy, University College London, United Kingdom) BA(Argelander-Institut für Astronomie der Universität Bonn, Germany) BB(Argelander-Institut für Astronomie der Universität Bonn, Germany) BC(Argelander-Institut für Astronomie der Universität Bonn, Germany) BD(European Space Agency, Space Telescope Science Institute, Baltimore, USA) BE(Instituto de Astrofísica de Andalucía-CSIC, Granada, Spain) BF(Institute of Astronomy with NAO, Smoljan, Bulgaria) BG(Centro de Astrobiología, CSIC-INTA, Madrid, Spain) BH(Universitäts-Sternwarte München, Germany) BI(Astronomical Institute Anton Pannekoek, University of Amsterdam, the Netherlands) BJ(Instituto de Astrofísica de Canarias, La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, Tenerife, Spain) BK(Instituto de Astrofísica de Canarias, La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, Tenerife, Spain) BL(Department of Physics & Astronomy, Queen’s University Belfast, Northern Ireland, United Kingdom) BM(Department of Physics and Astronomy, The Open University, Milton Keynes, United Kingdom; Faulkes Telescope Project, University of Glamorgan, Wales, United Kingdom) BN(School of Physical & Geographical Sciences, Keele University, United Kingdom) BO(Armagh Observatory, Northern Ireland, United Kingdom) BP(Space Telescope Science Institute, Baltimore, USA)
Abstract:
We introduce the VLT FLAMES Tarantula Survey, an ESO Large Programme from which we have obtained optical spectroscopy of over 800 massive stars in the spectacular 30 Doradus region of the Large Magellanic Cloud. A key feature is the use of multi-epoch observations to provide strong constraints on the binary fraction. This is the largest high quality survey of extragalactic massive stars ever assembled, and is already providing exciting new insights into their evolution, multiplicity and formation.
References:
Bestenlehner J. et al. 2011, A&A, 530, L14; Brott, I. et al. 2011, A&A, 530, A116; Cioni, M.-R. et al. 2011, A&A, 527, A116; Crowther, P. et al. 2010, MNRAS, 408, 731; de Mink, S., Langer, N. & Izzard, R. 2011, Bulletin Société Royale des Sciences de Liège, 80, 543; Evans, C. et al. 2008, The Messenger, 131, 25; Evans, C. et al. 2010, ApJ, 715, L74; Evans, C. et al. 2011, A&A, 530, A108; Niemela, V. 2002, Extragalactic Star Clusters, IAU Symp. 207, ASP, p202; Sana, H. & Evans, C. 2011, Active OB stars, IAU Symp. 272, arXiv:1009.4197; Taylor, W. et al. 2011, A&A, 530, L10

ADS BibCode:
2011Msngr.145...39S
Section:
Astronomical Science
Author(s)/Affiliation(s):
Förster Schreiber, N. M.; Genzel, R.; Renzini, A.; Tacconi, L. J.; Lilly, S. J.; Bouché, N.; Burkert, A.; Buschkamp, P.; Carollo, C. M.; Cresci, G.; Davies, R.; Eisenhauer, F.; Genel, S.; Gillessen, S.; Hicks, E. K. S.; Jones, T.; Kurk, J.; Lutz, D.; Mancini, C.; Naab, T.; Newman, S.; Peng, Y.; Shapiro, K. L.; Shapley, A. E.; Sternberg, A.; Vergani, D.; Wuyts, S.; Zamorani, G.; Arimoto, N.; Ceverino, D.; Cimatti, A.; Daddi, E.; Dekel, A.; Erb, D. K.; Kong, X.; Mainieri, V.; Maraston, C.; McCracken, H. J.; Mignoli, M.; Oesch, P.; Onodera, M.; Pozzetti, L.; Steidel, C. C.; Verma, A.
AA(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AB(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany; Dept. of Physics, University of California, Berkeley, USA) AC(INAF–Osservatorio Astronomico di Padova, Italy) AD(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AE(Institute of Astronomy, Eidgenössische Technische Hochschule Zürich, Switzerland) AF(Dept. of Physics, University of California, Santa Barbara, USA; CNRS Institut de Recherche en Astrophysique et Planetologie, Université de Toulouse, France; Université de Toulouse, UPS Observatoire Midi Pyrénées, Toulouse, France) AG(Universitäts Sternwarte München, Germany) AH(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AI(Institute of Astronomy, Eidgenössische Technische Hochschule Zürich, Switzerland) AJ(INAF–Osservatorio Astrofisico di Arcetri, Firenze, Italy) AK(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AL(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AM(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany; Sackler School of Physics & Astronomy, Tel Aviv University, Israel) AN(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AO(Dept. of Astronomy, University of Washington, Seattle, USA) AP(Dept. of Physics, University of California, Berkeley, USA) AQ(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AR(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AS(INAF–Osservatorio Astronomico di Padova, Italy) AT(Max-Planck-Institut für Astrophysik, Garching, Germany) AU(Dept. of Physics, University of California, Berkeley, USA) AV(Institute of Astronomy, Eidgenössische Technische Hochschule Zürich, Switzerland) AW(Northrop Grumman Aerospace Systems, Redondo Beach, USA) AX(Dept. of Physics and Astronomy, University of California, Los Angeles, USA) AY(Sackler School of Physics & Astronomy, Tel Aviv University, Israel) AZ(INAF–Osservatorio Astronomico di Bologna, Italy) BA(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) BB(INAF–Osservatorio Astronomico di Bologna, Italy) BC(National Astronomical Observatory of Japan, Tokyo, Japan) BD(Racah Institute of Physics, The Hebrew University, Jerusalem, Israel) BE(Dipt. di Astronomia, Universita di Bologna, Bologna, Italy) BF(CEA Saclay, DSM/DAPNIA/SAp, Gif-sur-Yvette, France) BG(Racah Institute of Physics, The Hebrew University, Jerusalem, Israel) BH(Dept. of Physics, University of Wisconsin, Milwaukee, USA) BI(Center for Astrophysics, University of Science and Technology of China, Heifei, China) BJ(ESO) BK(Institute of Cosmology and Gravitation, University of Portsmouth, United Kingdom) BL(Institut d’astrophysique de Paris, France) BM(INAF–Osservatorio Astronomico di Bologna, Italy) BN(University of California Observatory/Lick Observatory, University of California, Santa Cruz, USA) BO(Institute of Astronomy, Eidgenössische Technische Hochschule Zürich, Switzerland; CEA Saclay, DSM/DAPNIA/SAp, Gif-sur-Yvette, France) BP(INAF–Osservatorio Astronomico di Bologna, Italy) BQ(Caltech, Pasadena, USA) BR(Oxford Astrophysics, University of Oxford, United Kingdom)
Abstract:
In recent years, major advances have been made in our understanding of the early stages of galaxy formation and evolution. Remarkable progress has come from spatially- and spectrally-resolved studies of galaxies beyond z ~ 1 with SINFONI at the VLT, when the Universe was less than 40% of its present age. Here we report on key insights from our SINFONI observations of over 100 massive z ~ 2 star-forming galaxies, resolving the kinematics, physical, and star formation properties on scales of ~ 1-5 kiloparsecs.
References:
Daddi, E. et al. 2007, ApJ, 670, 156; Förster Schreiber, N. M. et al. 2009, ApJ, 706, 1364; Förster Schreiber, N. M. et al. 2011, ApJ, 739, 45; Genzel, R. et al. 2008, ApJ, 687, 59; Genzel, R. et al. 2011, ApJ, 733, 101; Lilly, S. J. et al. 2007, ApJS, 172, 70; Lilly, S. J. et al. 2008, The Messenger, 134, 35; Mancini, C. et al. 2011, ApJ, submitted Shapiro, K. L. et al. 2008, ApJ, 682, 231; Shapiro, K. L. et al. 2009, ApJ, 701, 955; Sharples, R. M. et al. 2010, The Messenger, 139, 24; Tacconi, L. J. et al. 2010, Nature, 463, 78

ADS BibCode:
2011Msngr.145...46W
Section:
Astronomical News
Author(s)/Affiliation(s):
Wagg, J.; De Breuck, C.
AA(ESO) AB(ESO)
Abstract:
Our knowledge of the formation and evolution of distant galaxies continues to advance dramatically with the advent of new facilities at most observable wavelengths. One of the outstanding questions related to this field is: How do galaxies get their gas? Over the next decade, radio and submillimetre facilities like the Expanded Very Large Array and the Atacama Large Millimeter/submillimeter Array will probe the chemistry, kinematics and obscured star formation properties of the interstellar medium in galaxies at high redshift, allowing this question to be addressed. We report on a timely workshop on the roles of theory and multi-wavelength observing facilities in furthering our understanding of interstellar medium physics in distant galaxies.

ADS BibCode:
2011Msngr.145...49Z
Section:
Astronomical News
Author(s)/Affiliation(s):
de Zeeuw, T.; Leibundgut, B.; Fosbury, R.; D’Odorico, S.
AA(ESO) AB(ESO) AC(ESO) AD(ESO)
Abstract:
Alan Moorwood died on 18 June 2011 at the age of 66 after a short illness. He had recently retired from ESO as Director of Programmes, having played a leading role in instrumentation for many years. There follows an obituary by Tim de Zeeuw and a joint tribute by three of his long-time ESO colleagues, Bruno Leibundgut, Bob Fosbury and Sandro D’Odorico.
References:
Primas, F., Casali, M. & Walsh, J. 2010, The Messenger, 141, 50

ADS BibCode:
2011Msngr.145...51Z
Section:
Astronomical News
Author(s)/Affiliation(s):
de Zeeuw, T.; Péron, M.
AA(ESO) AB(ESO)

ADS BibCode:
2011Msngr.145...52.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2011Msngr.145...53.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2011Msngr.145...55.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)