ADS BibCode:
2011Msngr.143....2Z
Section:
The Organisation
Author(s)/Affiliation(s):
de Zeeuw, T.; Pottasch, S.; Wilson, R.
AA(ESO) AB(Kapteyn Laboratorium, Groningen, the Netherlands) AC(Rohrbach/Ilm, Germany)
Abstract:
In the last issue of The Messenger (142, p. 51) only a brief obituary of Adriaan Blaauw, the second Director General of ESO, could be included at the time of going to press. There follow three tributes to Adriaan Blaauw: by Tim de Zeeuw, current ESO Director General; by his long-term colleague at the Kapteyn Institute, Stuart Pottasch; and by Raymond Wilson, who led the Optics Group during his tenure as Director General.
References:
Blaauw, A. 2004, ARAA, 42, 1; Pottasch, S. R. 1994, The Messenger, 76, 62

ADS BibCode:
2011Msngr.143....5Z
Section:
The Organisation
Author(s)/Affiliation(s):
de Zeeuw, T.
AA(ESO)

ADS BibCode:
2011Msngr.143....7P
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Piskunov, N.; Snik, F.; Dolgopolov, A.; Kochukhov, O.; Rodenhuis, M.; Valenti, J.; Jeffers, S.; Makaganiuk, V.; Johns-Krull, C.; Stempels, E.; Keller, C.
AA(Department of Physics and Astronomy, Uppsala University, Sweden) AB(Sterrekundig Instituut Utrecht, Utrecht University, the Netherlands) AC(Crimean Astrophysical Observatory, Crimea, Ukraine) AD(Department of Physics and Astronomy, Uppsala University, Sweden) AE(Sterrekundig Instituut Utrecht, Utrecht University, the Netherlands) AF(STScI, Baltimore, USA) AG(Sterrekundig Instituut Utrecht, Utrecht University, the Netherlands) AH(Department of Physics and Astronomy, Uppsala University, Sweden) AI(Rice University, Houston, USA) AJ(Department of Physics and Astronomy, Uppsala University, Sweden) AK(Sterrekundig Instituut Utrecht, Utrecht University, the Netherlands)
Abstract:
The HARPS spectrograph can now perform a full polarisation analysis of spectra. It has been equipped with a polarimetric unit, HARPSpol, which was jointly designed and produced by Uppsala, Utrecht and Rice Universities and by the STScI. Here we present the new instrument, demonstrate its polarisation capabilities and show the first scientific results.
References:
Bagnulo, S. et al. 2009, PASP, 121, 993; Donati, J.-F. et al. 1997, MNRAS, 291, 658; Donati, J.-F. et al. 2006, Solar Polarization 4, ASP Conf. Series, 358, 362; Kochukhov, O. et al. 2010, A&A, 524, 5; Kotov, V. A. et al. 1998, ApJ, 116, 103; Mayor, M. et al. 2003, The Messenger, 114, 20; Ramelli, R. et al. 2010, SPIE, 7735, 1; Semel, M. et al. 1993, A&A, 278, 231; Snik, F. et al. 2008, SPIE, 7014, 22; Snik, F. et al. 2010, arXiv: 1010.0397

ADS BibCode:
2011Msngr.143...11N
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Nikolic, B.; Richer, J.; Bolton, R.; Hills, R.
AA(Astrophysics Group, Cavendish Laboratory, University of Cambridge, United Kingdom) AB(Astrophysics Group, Cavendish Laboratory, University of Cambridge, United Kingdom) AC(Astrophysics Group, Cavendish Laboratory, University of Cambridge, United Kingdom) AD(Joint ALMA Observatory, Santiago, Chile)
Abstract:
Of the many challenges facing ALMA, one of the greatest is overcoming the natural seeing limit set by the atmosphere to achieve very high resolution images. Its longest antenna separations (baselines) permit ALMA to synthesise the effect of a single antenna with a diameter exceeding 15 km, but an accurate radio “adaptive optics” system is required to ensure ALMA’s images are diffraction limited. With initial test data now available from the first ALMA antennas in Chile, we describe current progress towards this goal.
References:
Evans, N. et al. 2003, Site properties and stringency, ALMA Memo Series, 471, The ALMA Project Laing, R. et al. 2010, The Messenger, 141, 41; Nikolic, B. et al. 2008, The Messenger, 131, 14

ADS BibCode:
2011Msngr.143...16E
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Eisenhauer, F.; Perrin, G.; Brandner, W.; Straubmeier, C.; Perraut, K.; Amorim, A.; Schöller, M.; Gillessen, S.; Kervella, P.; Benisty, M.; Araujo-Hauck, C.; Jocou, L.; Lima, J.; Jakob, G.; Haug, M.; Clénet, Y.; Henning, T.; Eckart, A.; Berger, J.-P.; Garcia, P.; Abuter, R.; Kellner, S.; Paumard, T.; Hippler, S.; Fischer, S.; Moulin, T.; Villate, J.; Avila, G.; Gräter, A.; Lacour, S.; Huber, A.; Wiest, M.; Nolot, A.; Carvas, P.; Dorn, R.; Pfuhl, O.; Gendron, E.; Kendrew, S.; Yazici, S.; Anton, S.; Jung, Y.; Thiel, M.; Choquet, É; Klein, R.; Teixeira, P.; Gitton, P.; Moch, D.; Vincent, F.; Kudryavtseva, N.; Ströbele, S.; Sturm, S.; Fédou, P.; Lenzen, R.; Jolley, P.; Kister, C.; Lapeyrère, V.; Naranjo, V.; Lucuix, C.; Hofmann, R.; Chapron, F.; Neumann, U.; Mehrgan, L.; Hans, O.; Rousset, G.; Ramos, J.; Suarez, M.; Lederer, R.; Reess, J.-M.; Rohloff, R.-R.; Haguenauer, P.; Bartko, H.; Sevin, A.; Wagner, K.; Lizon, J.-L.; Rabien, S.; Collin, C.; Finger, G.; Davies, R.; Rouan, D.; Wittkowski, M.; Dodds-Eden, K.; Ziegler, D.; Cassaing, F.; Bonnet, H.; Casali, M.; Genzel, R.; Lena, P.
AA(Max-Planck Institute for Extraterrestrial Physics, Garching, Germany) AB(LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, Meudon, France; Groupement d’Intérêt Scientifique PHASE (Partenariat Haute résolution Angulaire Sol Espace) between ONERA, Observatoire de Paris, CNRS and Université Paris Diderot) AC(Max-Planck Institute for Astronomy, Heidelberg, Germany) AD(Physikalisches Institut, University of Cologne, Germany) AE(UJF–Grenoble 1/CNRS-INSU, Institut de Planétologie et d’Astrophysique de Grenoble, France) AF(Laboratório de Sistemas, Instrumentação e Modelação em Ciências e Tecnologias do Ambiente e do Espaço (SIM), Lisbon and Porto, Portugal) AG(ESO) AH(Max-Planck Institute for Extraterrestrial Physics, Garching, Germany) AI(LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, Meudon, France; Groupement d’Intérêt Scientifique PHASE (Partenariat Haute résolution Angulaire Sol Espace) between ONERA, Observatoire de Paris, CNRS and Université Paris Diderot) AJ(Max-Planck Institute for Astronomy, Heidelberg, Germany) AK(Physikalisches Institut, University of Cologne, Germany) AL(UJF–Grenoble 1/CNRS-INSU, Institut de Planétologie et d’Astrophysique de Grenoble, France) AM(Laboratório de Sistemas, Instrumentação e Modelação em Ciências e Tecnologias do Ambiente e do Espaço (SIM), Lisbon and Porto, Portugal) AN(ESO) AO(Max-Planck Institute for Extraterrestrial Physics, Garching, Germany) AP(LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, Meudon, France; Groupement d’Intérêt Scientifique PHASE (Partenariat Haute résolution Angulaire Sol Espace) between ONERA, Observatoire de Paris, CNRS and Université Paris Diderot) AQ(Max-Planck Institute for Astronomy, Heidelberg, Germany) AR(Physikalisches Institut, University of Cologne, Germany) AS(UJF–Grenoble 1/CNRS-INSU, Institut de Planétologie et d’Astrophysique de Grenoble, France; ESO) AT(Laboratório de Sistemas, Instrumentação e Modelação em Ciências e Tecnologias do Ambiente e do Espaço (SIM), Lisbon and Porto, Portugal) AU(ESO) AV(Max-Planck Institute for Extraterrestrial Physics, Garching, Germany) AW(LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, Meudon, France; Groupement d’Intérêt Scientifique PHASE (Partenariat Haute résolution Angulaire Sol Espace) between ONERA, Observatoire de Paris, CNRS and Université Paris Diderot) AX(Max-Planck Institute for Astronomy, Heidelberg, Germany) AY(Physikalisches Institut, University of Cologne, Germany) AZ(UJF–Grenoble 1/CNRS-INSU, Institut de Planétologie et d’Astrophysique de Grenoble, France) BA(Laboratório de Sistemas, Instrumentação e Modelação em Ciências e Tecnologias do Ambiente e do Espaço (SIM), Lisbon and Porto, Portugal) BB(ESO) BC(Max-Planck Institute for Extraterrestrial Physics, Garching, Germany) BD(LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, Meudon, France; Groupement d’Intérêt Scientifique PHASE (Partenariat Haute résolution Angulaire Sol Espace) between ONERA, Observatoire de Paris, CNRS and Université Paris Diderot) BE(Max-Planck Institute for Astronomy, Heidelberg, Germany) BF(Physikalisches Institut, University of Cologne, Germany) BG(UJF–Grenoble 1/CNRS-INSU, Institut de Planétologie et d’Astrophysique de Grenoble, France) BH(Laboratório de Sistemas, Instrumentação e Modelação em Ciências e Tecnologias do Ambiente e do Espaço (SIM), Lisbon and Porto, Portugal) BI(ESO) BJ(Max-Planck Institute for Extraterrestrial Physics, Garching, Germany) BK(LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, Meudon, France; Groupement d’Intérêt Scientifique PHASE (Partenariat Haute résolution Angulaire Sol Espace) between ONERA, Observatoire de Paris, CNRS and Université Paris Diderot) BL(Max-Planck Institute for Astronomy, Heidelberg, Germany) BM(Physikalisches Institut, University of Cologne, Germany) BN(Laboratório de Sistemas, Instrumentação e Modelação em Ciências e Tecnologias do Ambiente e do Espaço (SIM), Lisbon and Porto, Portugal; Centro de Investigação em Ciências Geo-Espaciais, Porto, Portugal) BO(ESO) BP(Max-Planck Institute for Extraterrestrial Physics, Garching, Germany) BQ(LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, Meudon, France; Groupement d’Intérêt Scientifique PHASE (Partenariat Haute résolution Angulaire Sol Espace) between ONERA, Observatoire de Paris, CNRS and Université Paris Diderot) BR(Max-Planck Institute for Astronomy, Heidelberg, Germany) BS(Laboratório de Sistemas, Instrumentação e Modelação em Ciências e Tecnologias do Ambiente e do Espaço (SIM), Lisbon and Porto, Portugal; ESO) BT(ESO) BU(Max-Planck Institute for Extraterrestrial Physics, Garching, Germany) BV(LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, Meudon, France; Groupement d’Intérêt Scientifique PHASE (Partenariat Haute résolution Angulaire Sol Espace) between ONERA, Observatoire de Paris, CNRS and Université Paris Diderot) BW(Max-Planck Institute for Astronomy, Heidelberg, Germany) BX(ESO) BY(Max-Planck Institute for Extraterrestrial Physics, Garching, Germany) BZ(LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, Meudon, France; Groupement d’Intérêt Scientifique PHASE (Partenariat Haute résolution Angulaire Sol Espace) between ONERA, Observatoire de Paris, CNRS and Université Paris Diderot) CA(Max-Planck Institute for Astronomy, Heidelberg, Germany) CB(ESO) CC(Max-Planck Institute for Extraterrestrial Physics, Garching, Germany) CD(LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, Meudon, France; Groupement d’Intérêt Scientifique PHASE (Partenariat Haute résolution Angulaire Sol Espace) between ONERA, Observatoire de Paris, CNRS and Université Paris Diderot) CE(Max-Planck Institute for Astronomy, Heidelberg, Germany) CF(ESO) CG(Max-Planck Institute for Extraterrestrial Physics, Garching, Germany) CH(LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, Meudon, France; Groupement d’Intérêt Scientifique PHASE (Partenariat Haute résolution Angulaire Sol Espace) between ONERA, Observatoire de Paris, CNRS and Université Paris Diderot) CI(Max-Planck Institute for Astronomy, Heidelberg, Germany) CJ(ESO) CK(Max-Planck Institute for Extraterrestrial Physics, Garching, Germany) CL(LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, Meudon, France; Groupement d’Intérêt Scientifique PHASE (Partenariat Haute résolution Angulaire Sol Espace) between ONERA, Observatoire de Paris, CNRS and Université Paris Diderot) CM(Max-Planck Institute for Astronomy, Heidelberg, Germany) CN(ESO) CO(Max-Planck Institute for Extraterrestrial Physics, Garching, Germany) CP(LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, Meudon, France; Groupement d’Intérêt Scientifique PHASE (Partenariat Haute résolution Angulaire Sol Espace) between ONERA, Observatoire de Paris, CNRS and Université Paris Diderot) CQ(Max-Planck Institute for Astronomy, Heidelberg, Germany) CR(ESO) CS(Max-Planck Institute for Extraterrestrial Physics, Garching, Germany) CT(LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, Meudon, France; Groupement d’Intérêt Scientifique PHASE (Partenariat Haute résolution Angulaire Sol Espace) between ONERA, Observatoire de Paris, CNRS and Université Paris Diderot) CU(Max-Planck Institute for Astronomy, Heidelberg, Germany) CV(ESO) CW(Max-Planck Institute for Extraterrestrial Physics, Garching, Germany) CX(LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, Meudon, France; Groupement d’Intérêt Scientifique PHASE (Partenariat Haute résolution Angulaire Sol Espace) between ONERA, Observatoire de Paris, CNRS and Université Paris Diderot) CY(ESO) CZ(Max-Planck Institute for Extraterrestrial Physics, Garching, Germany) DA(LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, Meudon, France; Groupement d’Intérêt Scientifique PHASE (Partenariat Haute résolution Angulaire Sol Espace) between ONERA, Observatoire de Paris, CNRS and Université Paris Diderot) DB(ESO) DC(Max-Planck Institute for Extraterrestrial Physics, Garching, Germany) DD(LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, Meudon, France; Groupement d’Intérêt Scientifique PHASE (Partenariat Haute résolution Angulaire Sol Espace) between ONERA, Observatoire de Paris, CNRS and Université Paris Diderot) DE(ONERA, Optics Department (DOTA), Châtillon, France; Groupement d’Intérêt Scientifique PHASE (Partenariat Haute résolution Angulaire Sol Espace) between ONERA, Observatoire de Paris, CNRS and Université Paris Diderot) DF(ESO) DG(ESO) DH(Max-Planck Institute for Extraterrestrial Physics, Garching, Germany) DI(LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, Meudon, France)
Abstract:
GRAVITY is the second generation Very Large Telescope Interferometer instrument for precision narrow-angle astrometry and interferometric imaging. With its fibre-fed integrated optics, wavefront sensors, fringe tracker, beam stabilisation and a novel metrology concept, GRAVITY will push the sensitivity and accuracy of astrometry and interferometric imaging far beyond what is offered today. Providing precision astrometry of order 10 microarcseconds, and imaging with 4-milliarcsecond resolution, GRAVITY will revolutionise dynamical measurements of celestial objects: it will probe physics close to the event horizon of the Galactic Centre black hole; unambiguously detect and measure the masses of black holes in massive star clusters throughout the Milky Way; uncover the details of mass accretion and jets in young stellar objects and active galactic nuclei; and probe the motion of binary stars, exoplanets and young stellar discs. The instrument capabilities of GRAVITY are outlined and the science opportunities that will open up are summarised.
References:
Amorim, A. et al. 2010, Proc. SPIE, 7734, 773415; Anderson, J. et al. 2010, ApJ, 710, 1032; Bartko, H. et al. 2010, Proc. SPIE, 7734, 773421; van Belle, G. 2008, PASP, 120, 617; Choquet, E. et al. 2010, Proc. SPIE, 7734, 77341Z Clénet, Y. et al. 2010, Proc. SPIE, 7736, 77364A Delplancke, F. 2008, NewAR, 52, 199; Eckart, A. et al. 2010, Proc. SPIE, 7734, 77340X Eisenhauer, F. et al. 2008, The Power of Optical/IR Interferometry: Recent Scientific Results and 2nd Generation Instrumentation, ed. Richichi, A. et al., ESO Astrophysics Symposia, 41, 431; Genzel, R. et al. 2010, RvMP, 82, 3121; Gillessen, S. et al. 2010, Proc. SPIE, 7734, 77340Y Gillessen, S. et al. 2009, ApJ, 692, 1075; Jocou, L. et al. 2010, Proc. SPIE, 7734, 773430; Paumard, T. et al. 2008, The Power of Optical/IR Interferometry: Recent Scientific Results and 2nd Generation Instrumentation, ed. Richichi, A. et al., ESO Astrophysics Symposia, 41, 431; Pfuhl, O. et al. 2010, Proc. SPIE, 7734, 77342A Raban, S. et al. 2009, MNRAS, 394, 1325; Staff, J. E. et al. 2010, ApJS, 722, 1325; Straubmeier, C. et al. 2010, Proc. SPIE, 7734, 773432; Will, C. M. 2008, ApJL, 674, 25

ADS BibCode:
2011Msngr.143...25G
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Gilmozzi, R.; Kissler-Patig, M.
AA(ESO) AB(ESO)

ADS BibCode:
2011Msngr.143...27F
Section:
Astronomical Science
Author(s)/Affiliation(s):
Fosbury, R.; Koch, G.; Koch, J.
AA(ESO) AB(Lycée Français Jean Renoir, München, Germany) AC(Lycée Français Jean Renoir, München, Germany)
Abstract:
Although only a trace constituent gas in the Earth’s atmosphere, ozone plays a critical role in protecting the Earth’s surface from receiving a damaging flux of solar ultraviolet radiation. What is not generally appreciated, however, is that the intrinsically weak, visible Chappuis absorption band becomes an important influence on the colour of the entire sky when the Sun is low or just below the horizon. This effect has been explored using spectra of the sunset and also of the eclipsed Moon; phenomena that involve a similar passage of sunlight tangential to the Earth’s surface. This geometry will also be relevant in future attempts to perform transit spectroscopy of exo-Earths.
References:
Allen, C. W. 1973, Astrophysical Quantities, 3rd Edition, (London: Athlone Press) Hulbert, E. O. 1953, JOSA, 43, 113; Pallé, E. et al. 2009, Nature, 459, 814; Perryman, M. et al. 2005, ESA–ESO Working Group Report No. 1, Extra-Solar Planets, Space- Telescope – European Coordinating Facility Pesic, P. 2005, Sky in a Bottle, (Cambridge, MA: The MIT Press) Vázquez, M., Pallé, E. & Montañés Rodríguez, P. 2010, The Earth as a Distant Planet, (New York: Springer)

ADS BibCode:
2011Msngr.143...32P
Section:
Astronomical Science
Author(s)/Affiliation(s):
Pontoppidan, K.M.; van Dishoeck, E.; Blake, G.A.; Smith, R.; Brown, J.; Herczeg, G.J.; Bast, J.; Mandell, A.; Smette, A.; Thi, W.-F.; Young, E.D.; Morris, M.R.; Dent, W.; Käufl, H.U.
AA(Space Telescope Science Institute, Baltimore, USA) AB(Leiden University, the Netherlands; Max Planck Institute for Extraterrestrial Physics, Garching, Germany) AC(California Institute of Technology, Pasadena, USA) AD(University of California at Los Angeles, USA) AE(Harvard-Smithsonian Center for Astrophysics, Cambridge, USA; Max Planck Institute for Extraterrestrial Physics, Garching, Germany) AF(Max Planck Institute for Extraterrestrial Physics, Garching, Germany) AG(Leiden University, the Netherlands) AH(NASA Goddard Space Flight Center, Greenbelt, USA) AI(ESO) AJ(University of Edinburgh, Scotland, United Kingdom; University of Grenoble, France) AK(University of California at Los Angeles, USA) AL(University of California at Los Angeles, USA) AM(University of Edinburgh, Scotland, United Kingdom) AN(ESO)
Abstract:
The inner regions (< 10 AU) of discs surrounding young pre-main sequence stars are thought to be places of active planet formation. The disc surfaces are traced by molecular emission lines in the infrared. We have carried out a spectroscopic 3–5 μm survey at the highest spectral resolution (as high as R = 100000) using CRIRES on the VLT, and have used the data to map the dynamics and chemistry of molecular gas, with the aims of constraining disc evolution and learning more about the process of planet formation. In this paper, we provide a brief overview of our CRIRES observing campaign and discuss the results obtained.
References:
Bast, J. et al. 2011, A&A, in press Brandl, B. et al. 2010, The Messenger, 140, 30; Brown, J. M. et al. 2011, ApJ, in preparation Herczeg, G. et al. 2011, A&A, submitted Clayton, R. 2002, Nature, 415, 860; Mandell, A. et al. 2011, ApJ, in preparation Monnier, J. et al. 2005, ApJ, 624, 832; Pontoppidan, K. M. et al. 2008, ApJ, 684, 1323; ESO Press Release 0827, Mind the Gap Pontoppidan, K. M. et al. 2010, ApJ, 720, 887; Pontoppidan, K. M. et al. 2011, ApJ, submitted Shu, F. et al. 1994, ApJ, 429, 781; Smith, R. L. et al. 2009, ApJ, 701, 163; Smith, R. L. et al. 2011, in preparation Thi, W.-F. et al. 2010, MNRAS, 406, 1409; Young, E. D. et al. 2011, ApJ, in press

ADS BibCode:
2011Msngr.143...37P
Section:
Astronomical Science
Author(s)/Affiliation(s):
Péroux, C.; Bouché, N.; Kulkarni, V.; York, D.; Vladilo, G.
AA(Laboratoire d’Astrophysique de Marseille, OAMP, Université Aix- Marseille & CNRS, France) AB(Department of Physics, University of California, Santa Barbara, USA; Laboratoire d’Astrophysique de Toulouse–Tarbes, CNRS, Observatoire Midi-Pyrénnées, France) AC(Department of Physics and Astronomy, University of South Carolina, Columbia, USA) AD(Department of Astronomy and Astrophysics and The Enrico Fermi Institute, University of Chicago, USA) AE(INAF–Osservatorio Astronomico di Trieste, Italy)
Abstract:
A complete picture of galaxy formation can only be obtained by detailed study of the processes by which galaxies convert their gas into stars. One approach is to relate the H I gas and the stars in galaxies. Damped and sub-damped Lyman-α systems (DLAs), which are galaxies probed by the absorption they produce in the spectra of background quasars, are purely selected on H I gas, but identifying the galaxy responsible for the absorber with more traditional methods remains challenging. Integral field spectroscopy provides an efficient way of detecting faint galaxies near bright quasars, further providing immediate redshift confirmation. Here, we report on the detection of DLA and sub-DLA systems identified in Hα emission with VLT/SINFONI at near-infrared wavelengths.
References:
Bouché, N. et al. 2007, ApJ, 669, L5; Bouché, N. et al. 2011, MNRAS, submitted Cresci, G. et al. 2010, Nature, 467, 811; Le Brun, V. et al. 1997, A&A, 321, 733; Noterdaeme, P. et al. 2009, A&A, 505, 1087; Pettini, M. & Pagel, B. E. J. 2004, MNRAS, 348L, 59; Péroux, C. et al. 2005, MNRAS, 363, 479; Péroux, C. et al. 2011a, MNRAS, 410, 2237; Péroux, C. et al. 2011b, MNRAS, 410, 2251; Péroux, C. et al. 2011c, MNRAS, submitted

ADS BibCode:
2011Msngr.143...42S
Section:
Astronomical Science
Author(s)/Affiliation(s):
Shanks, T.; Bielby, R.; Infante, L.
AA(Department of Physics, Durham University, United Kingdom) AB(Department of Physics, Durham University, United Kingdom) AC(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile)
Abstract:
We have completed the largest spectroscopic survey of Lyman-break galaxies (LBGs) at z ≈ 3, using the uniquely wide field of the VLT VIMOS multi-object spectrograph. The survey now contains about 2100 galaxy redshifts over the range 2 < z < 3.5 and is being used to investigate gas outflows from galaxies and large-scale structures at z ≈ 3. These results are having an immediate impact on theories of galaxy formation and producing new tests of the standard cosmological model. In particular, we find: further evidence from their clustering that LBGs may be the progenitors of spiral galaxies; new evidence for gas outflows from star-forming galaxies as required by theoretical galaxy formation models; and new evidence for gravitational infall of galaxies into clusters at a rate that is consistent with the standard cosmology.
References:
Adelberger, K. L. et al. 2003, ApJ, 584, 45; Adelberger, K. L. et al. 2005, ApJ, 629, 636; Bielby, R. et al. 2011, MNRAS, accepted, arXiv:1005.3028; Crighton, N. et al. 2011, MNRAS, accepted, arXiv:1006.4385; Guhathakurta, P. et al. 1990, ApJ, 357, 9; Metcalfe, N. et al. 1991, MNRAS, 249, 498; Metcalfe, N. et al. 1996, Nature, 383, 236; Shanks, T. et al. 1983, Nature, 303, 156; Shapley, A. E. et al. 2003, ApJ, 588, 65; Steidel, C. C. & Hamilton, D. 1993, AJ, 105, 2017; Steidel, C. C. et al. 1996, ApJL, 462, L17; Steidel, C. C. et al. 2003, ApJ, 592, 78

ADS BibCode:
2011Msngr.143...47G
Section:
Astronomical News
Author(s)/Affiliation(s):
Grosbøl, P.; Carraro, G.; Beletsky, Y.
AA(ESO) AB(ESO) AC(ESO)
Abstract:
The main objectives of the workshop were to review current observational evidence for spiral arms in our Galaxy and confront them with models of spiral structure in order to arrive at a consistent picture. Of primary importance was to understand just what additional information is required to resolve outstanding issues related to the spiral structure in the Milky Way, especially as new survey instruments (e.g., ALMA, VISTA and VST) are coming online and major space missions like GAIA will be launched in the near future.

ADS BibCode:
2011Msngr.143...49R
Section:
Astronomical News
Author(s)/Affiliation(s):
Randich, S.; Covino, S.; Cristiani, S.
AA(INAF–Osservatorio Astrofisico di Arcetri, Italy) AB(INAF–Osservatorio Astronomico di Brera, Italy) AC(INAF–Osservatorio Astronomico di Trieste, Italy)
Abstract:
The workshop was held with the aim of bringing together X-shooter users to discuss scientific results, performance and technical aspects, after the first year of successful operations of the instrument. The workshop was also organised to commemorate Roberto Pallavicini, whose scientific and human contribution to the development of X-shooter was invaluable and a source of continuous inspiration for all of us. A touching presentation focusing on the scientific personality of Roberto was given by Luca Pasquini on the second day of the workshop.
References:
Proceedings will be published in Astronomische Nachrichten in 2011.

ADS BibCode:
2011Msngr.143...52T
Section:
Astronomical News
Author(s)/Affiliation(s):
Testi, L.; Pilbratt, G.; Andreani, P.
AA(ESO) AB(ESA Research and Scientific Support Department, ESTEC, Noordwijk, the Netherlands) AC(ESO)
Abstract:
The ESA Herschel Space Observatory is currently producing new and exciting results, thanks to its unprecedented sensitivity, spectral resolution and wide-area surveying capabilities at far-infrared and submillimetre wavelengths. Many of the new discoveries by Herschel will require high angular resolution follow-up observations with ALMA. The goal of the workshop was to discuss the priorities for ALMA Early Science follow-up of the Herschel photometric and spectroscopic surveys. The possibility, or need for, simultaneous observing programmes with ALMA and Herschel was also discussed.
References:
André, P. et al. 2010, A&A, 518, L102; Cernicharo, J. et al. 2010, A&A, 518, L136; Maiolino, R. et al. 2009, A&A, 500, L1; Negrello, M. et al. 2010, Science, 330, 800; Testi, L. et al. 2010, The Messenger, 142, 17

ADS BibCode:
2011Msngr.143...56S
Section:
Astronomical News
Author(s)/Affiliation(s):
Sarazin, M.
AA(ESO)
Abstract:
As the site surveys for the Extremely Large Telescopes are nearing completion, two workshops gathered site testing specialists and atmospheric physicists to discuss the instrumental and data analysis issues. The two workshops are briefly reported.
References:
Masciadri, E. 2008, The Messenger, 134, 53

ADS BibCode:
2011Msngr.143...57H
Section:
Astronomical News
Author(s)/Affiliation(s):
Hainaut, O.; Sandu, O.; Christensen, L.L.
AA(ESO) AB(ESO) AC(ESO)
Abstract:
ESO’s Hidden Treasures astrophotography competition gave amateur astronomers the opportunity to search ESO’s Science Archive for a well-hidden cosmic gem. The competition attracted nearly one hundred entries and the winners were announced in January 2011. Astronomy enthusiast Igor Chekalin from Russia won the first prize — a trip to the Very Large Telescope at Paranal — in this difficult but rewarding challenge.
References:
Haines, C. P. et al. 2006, MNRAS, 371, 55; Patat, F. et al. 2010, A&A, in press, arXiv:1011.6156

ADS BibCode:
2011Msngr.143...59.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2011Msngr.143...60.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2011Msngr.143...61.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2011Msngr.143Q..62.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2011Msngr.143R..62.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2011Msngr.143...63.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2011Msngr.143...64.
Section:
Annual Index
Author(s)/Affiliation(s):
ESO
AA(ESO)