ADS BibCode:
2010Msngr.141....2K
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Kenworthy, M.; Quanz, S.; Meyer, M.; Kasper, M.; Girard, J.; Lenzen, R.; Codona, J.; Hinz, P.
AA(Leiden Observatory, the Netherlands) AB(ETH Zurich, Switzerland) AC(ETH Zurich, Switzerland) AD(ESO) AE(ESO) AF(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AG(University of Arizona, USA) AH(University of Arizona, USA)
Abstract:
In April 2010, a new coronagraphic optical element, called an Apodising Phase Plate (APP), was installed in NAOS–CONICA (NACO). The APP coronagraph is optimised for use at 4.05 µm with both narrow- and broadband filters. Unlike other types of coronagraph, it requires no alignment overhead and can be used immediately after switching from direct imaging for observing targets of interest where high contrast is required.
References:
Brandl, B. et al. 2010, The Messenger, 140, 30; Codona, J. & Angel, J. R. P. 2004, ApJL, 604, 117; Codona, J. et al. 2006, SPIE, 6269, 55; Guyon, O. et al. 2006, ApJS, 167, 81; Heinze, A. et al. 2010, ApJ, 714, 1570; Hinz, P. et al. 2006, ApJ, 653, 1486; Kasper, M. et al. 2007, A&A, 472, 32; Kasper, M. et al. 2009, The Messenger, 137, 8; Kenworthy, M. et al. 2007, ApJ, 660, 762; Kenworthy, M. et al. 2010, SPIE, 7735, arXiv:1007.3448; Lagrange, A.-M. et al. 2010, Science, 329, 57; Lenzen, R. et al. 2003, SPIE, 4841, 944; Quanz, S. et al. 2010, ApJL, submitted Rousset, G. et al. 2003, SPIE, 4839, 140

ADS BibCode:
2010Msngr.141....5M
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Martinez, P.; Kolb, J.; Sarazin, M.; Tokovinin, A.
AA(ESO) AB(ESO) AC(ESO) AD(Cerro-Tololo Inter American Observatory, Chile)
Abstract:
We attempt to clarify the frequent confusion between seeing and image quality for large telescopes. The full width at half maximum of a stellar image is commonly considered to be equal to the atmospheric seeing. However the outer scale of the turbulence, which corresponds to a reduction in the low frequency content of the phase perturbation spectrum, plays a significant role in the improvement of image quality at the focus of a telescope. The image quality is therefore different (and in some cases by a large factor) from the atmospheric seeing that can be measured by dedicated seeing monitors, such as a differential image motion monitor.
References:
Sarazin, M. & Roddier, F. 1990, A&A, 227, 294; Tokovinin, A. 2002, PASP, 114, 1156; Tokovinin, A. et al. 2007, MNRAS, 378, 701; Sarazin, M. et al. 2008, The Messenger, 132, 11; Martinez, P. et al. 2010, A&A, 516, A90; Floyd, D. J. E. et al. 2010, PASP, 122, 731; Dali Ali, W. et al. 2010, A&A, submitted

ADS BibCode:
2010Msngr.141....9K
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Kerber, F.; Querel, R.; Hanuschik, R.; Chacón, A.; Sarazin, M.; on behalf of the project team
AA(ESO) AB(Institute for Space Imaging Science (ISIS), Lethbridge, Canada) AC(ESO) AD(Grupo Astrometeorología, Universidad de Valparaíso, Chile) AE(ESO) AF on behalf of the project team*)
Abstract:
Precipitable water vapour (PWV) in the atmosphere is one of several key properties required to characterise overall quality of an astronomical site for observations at infrared wavelengths. Through analysis of archival data and by mounting a series of dedicated PWV measurement campaigns, we achieved our goal of establishing the Paranal Observatory as a reference site for evaluation of locations for the European Extremely Large Telescope (E-ELT) project. For the first time in an astronomical study, all measurement methods have been successfully validated with respect to balloon-borne radiosondes, the accepted standard in atmospheric research.
References:
Chacón, A. et al. 2010, Proc. SPIE Astronomical Instrumentation, in press Kerber, F. et al. 2010, Proc. SPIE Astronomical Instrumentation, in press Naylor, D. A. et al. 2008, Int. J. of Infrared & Millimeter waves, DOI 10.1007/210762-008-9421-2; Otárola, A. et al. 2010, PASP, 122, 470; Querel, R. R. et al. 2008, SPIE, 7014, 701457; Querel, R. R. et al. 2010, Proc. SPIE Astronomical Instrumentation, in press Schneider, M. et al. 2010, Atmos. Meas. Tech., 3, 323; Smette, A. et al. 2008, The 2007; ESO Instrument Calibration Workshop, eds. A. Kaufer & F. Kerber, Springer, 433; Thomas-Osip, J. et al. 2007, PASP, 119, 697

ADS BibCode:
2010Msngr.141...15B
Section:
Astronomical Science
Author(s)/Affiliation(s):
Barucci, M.A.; Alvarez-Candal, A.; Belskaya, I.; de Bergh, C.; DeMeo, F.; Dotto, E.; Fornasier, S.; Merlin, F.; Perna, D.
AA(Observatoire de Paris, LESIA, France) AB(ESO) AC(Observatoire de Paris, LESIA, France; Institute of Astronomy, Kharkiv University, Ukraine) AD(Observatoire de Paris, LESIA, France) AE(Observatoire de Paris, LESIA, France) AF(INAF–Osservatorio di Roma, Italy) AG(Observatoire de Paris, LESIA, France; Université de Paris VII–Diderot, France) AH(Observatoire de Paris, LESIA, France; Université de Paris VII–Diderot, France) AI(INAF–Osservatorio di Roma, Italy)
Abstract:
The icy bodies in orbit beyond Neptune and known as Trans-Neptunian objects (TNOs), or Kuiper Belt objects, are the most distant objects of the Solar System accessible to direct investigation from the ground. The study of these objects, containing the least processed material of the Solar System, can help in understanding the still-puzzling accretion/evolution processes that governed planetary formation in our Solar System as well as in other dusty star discs. An ESO large programme has been devoted to obtaining simultaneous high quality visible and near-infrared spectroscopy and photometry of about forty objects with various dynamical properties. A few selected objects have also been observed with polarimetry to define their surface characteristics better and with detailed photometry to determine their rotational properties. The results provide a unique insight into the physical and surface properties of these remote objects.
References:
Bagnulo, S. et al. 2008, A&A, 491, L33; Barucci, M. A. et al. 2005, AJ, 130, 1291; Barucci, M. A. et al. 2008, A&A, 479, L13; Belskaya, I. et al. 2008, A&A, 479, 265; Dalle Ore, C. M. et al. 2009, A&A, 501, 349; DeMeo, F. et al. 2009, A&A, 493, 283; Guilbert, A. et al. 2009, A&A, 501, 777; Fornasier, S. et al. 2009, A&A, 508, 457; Merlin, F. et al. 2009, AJ, 137, 315; Perna, D. et al. 2010, A&A, 508, 457

ADS BibCode:
2010Msngr.141...20S
Section:
Astronomical Science
Author(s)/Affiliation(s):
Schuller, F.; Beuther, H.; Bontemps, S.; Bronfman, L.; Carlhoff, P.; Cesaroni, R.; Contreras, Y.; Csengari, T.; Deharveng, L.; Garay, G.; Henning, T.; Herpin, F.; Immer, K.; Lefloch, B.; Linz, H.; Mardones, D.; Menten, K.; Minier, V.; Molinari, S.; Motte, F.; Nguyen Luong, Q.; Nyman, L.-Å.; Rathborne, J.; Reveret, V.; Risacher, C.; Russeil, D.; Schilke, P.; Schneider, N.; Tackenberg, J.; Testi, L.; Troost, T.; Vasyunina, T.; Walmsley, M.; Wienen, M.; Wyrowski, F.; Zavagno, A.
AA(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AB(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AC(Laboratoire d’Astrophysique de Bordeaux, France) AD(Universidad de Chile, Santiago, Chile) AE(University of Cologne, Germany) AF(Osservatorio Astrofisico di Arcetri, Firenze, Italy) AG(Universidad de Chile, Santiago, Chile) AH(IRFU/SAp, Commissariat à l’énergie atomique, Saclay, France) AI(Laboratoire d’Astrophysique de Marseille, France) AJ(Universidad de Chile, Santiago, Chile) AK(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AL(Laboratoire d’Astrophysique de Bordeaux, France) AM(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AN(Laboratoire d’Astrophysique de l’Observatoire de Grenoble, France) AO(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AP(Universidad de Chile, Santiago, Chile) AQ(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AR(IRFU/SAp, Commissariat à l’énergie atomique, Saclay, France) AS(INAF–Instituto di Fisica dello Spazio Interplanetario, Roma, Italy) AT(IRFU/SAp, Commissariat à l’énergie atomique, Saclay, France) AU(IRFU/SAp, Commissariat à l’énergie atomique, Saclay, France) AV(ALMA, Santiago, Chile) AW(Universidad de Chile, Santiago, Chile) AX(IRFU/SAp, Commissariat à l’énergie atomique, Saclay, France) AY(SRON, Groningen, Netherlands) AZ(Laboratoire d’Astrophysique de Marseille, France) BA(University of Cologne, Germany) BB(IRFU/SAp, Commissariat à l’énergie atomique, Saclay, France) BC(Max-Planck-Institut für Astronomie, Heidelberg, Germany) BD(ESO) BE(Max-Planck-Institut für Radioastronomie, Bonn, Germany) BF(Max-Planck-Institut für Astronomie, Heidelberg, Germany) BG(Osservatorio Astrofisico di Arcetri, Firenze, Italy) BH(Max-Planck-Institut für Radioastronomie, Bonn, Germany) BI(Max-Planck-Institut für Radioastronomie, Bonn, Germany) BJ(Laboratoire d’Astrophysique de Marseille, France)
Abstract:
Thermal emission from dust at submillimetre wavelengths is a direct tracer of high column densities and, thus, of dense cloud regions in which new stars are forming. Surveys of the Galactic Plane in thermal dust emission have the potential to deliver an unbiased view of high-mass star formation throughout the Milky Way. The Atacama Pathfinder Experiment (APEX) telescope is ideally located for mapping the inner Galaxy. Using the Large APEX Bolometer Camera (LABOCA), we have recently completed the APEX Telescope Large Area Survey of the Galaxy (ATLASGAL). This survey, which covers 360 square degrees at 870 µm, provides the first unbiased sample of cold dusty clumps in the Galaxy at submillimetre wavelengths and reveals the clumpy structure of the cold interstellar medium over very large scales that have previously been little explored.
References:
Beuther, H. et al. 2007, A&A, 466, 1065; Churchwell, E. et al. 2006, ApJ, 649, 759; Churchwell, E. et al. 2007, ApJ, 670, 428; Deharveng, L. et al. 2010, A&A, accepted, arXiv:1008.0926; Güsten, R. et al. 2006, A&A, 454, L13; Enoch, M. L. et al. 2006, ApJ, 638, 293; Johnstone, D. et al. 2004, ApJ, 611, L45; Molinari, S. et al. 2010, A&A, 518, L100; Motte, F. et al. 2007, A&A, 476, 1243; Rosolowsky, E. et al. 2010, ApJS, 188, 123; Schuller, F. et al. 2009, A&A, 504, 415; Siringo, G. et al. 2007, The Messenger, 129, 2; Siringo, G. et al. 2009, A&A, 497, 945; Siringo, G. et al. 2010, The Messenger, 139, 20

ADS BibCode:
2010Msngr.141...24S
Section:
Astronomical Science
Author(s)/Affiliation(s):
Saito, R.; Hempel, M.; Alonso-García, J.; Toledo, I.; Borissova, J.; González, O.; Beamin, J.C.; Minniti, D.; Lucas, P.; Emerson, J.; Ahumada, A.; Aigrain, S.; Alonso, M.V.; Amôres, E.; Angeloni, R.; Arias, J.; Bandyopadhyay, R.; Barbá, R.; Barbuy, B.; Baume, G.; Bedin, L.; Bica, E.; Bronfman, L.; Carraro, G.; Catelan, M.; Clariá, J.; Contreras, C.; Cross, N.; Davis, C.; de Grijs, R.; Dékány, I.; Drew, J.; Fariña, C.; Feinstein, C.; Fernández Lajús, E.; Folkes, S.; Gamen, R.; Geisler, D.; Gieren, W.; Goldman, B.; Gosling, A.; Gunthardt, G.; Gurovich, S.; Hambly, N.; Hanson, M.; Hoare, M.; Irwin, M.; Ivanov, V.; Jordán, A.; Kerins, E.; Kinemuchi, K.; Kurtev, R.; Longmore, A.; López-Corredoira, M.; Maccarone, T.; Martín, E.; Masetti, N.; Mennickent, R.; Merlo, D.; Messineo, M.; Mirabel, F.; Monaco, L.; Moni Bidin, C.; Morelli, L.; Padilla, N.; Palma, T.; Parisi, M.C.; Parker, Q.; Pavani, D.; Pietrukowicz, P.; Pietrzynski, G.; Pignata, G.; Rejkuba, M.; Rojas, A.; Roman-Lopes, A.; Ruiz, M.T.; Sale, S.; Saviane, I.; Schreiber, M.; Schröder, A.; Sharma, S.; Smith, M.; Sodré Jr., L.; Soto, M.; Stephens, A.; Tamura, M.; Tappert, C.; Thompson, M.; Valenti, E.; Vanzi, L.; Weidmann, W.; Zoccali, M.
AA(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile) AB(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile) AC(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile) AD(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile) AE(Departamento de Física y Astronomía, Universidad de Valparaíso, Chile) AF(ESO) AG(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile) AH(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile; Vatican Observatory, Italy) AI(Centre for Astrophysics Research, University of Hertfordshire, Hatfield, UK) AJ(School of Mathematical Sciences, Queen Mary, University of London, UK) AK(Observatorio Astronómico de Córdoba, Argentina; ESO; Consejo Nacional de Investigaciones Científicas y Técnicas, Buenos Aires, Argentina) AL(School of Physics, University of Exeter, UK; Department of Astrophysics, University of Oxford, UK) AM(Observatorio Astronómico de Córdoba, Argentina) AN(SIM, Faculdade de Ciências da Universidade de Lisboa, Portugal) AO(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile) AP(Departamento de Física, Universidad de La Serena, Chile) AQ(Department of Astronomy, University of Florida, USA) AR(Departamento de Física, Universidad de La Serena, Chile) AS(Universidade de São Paulo, Brazil) AT(Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Argentina) AU(Space Telescope Science Institute, Baltimore, USA) AV(Universidade Federal do Rio Grande do Sul, Porto Alegre, Brazil) AW(Departamento de Astronomía, Universidad de Chile, Santiago, Chile) AX(ESO) AY(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile) AZ(Observatorio Astronómico de Córdoba, Argentina) BA(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile) BB(Institute for Astronomy, The University of Edinburgh, UK) BC(Joint Astronomy Centre, Hilo, USA) BD(Kavli Institute for Astronomy and Astrophysics, Peking University, China) BE(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile) BF(Centre for Astrophysics Research, University of Hertfordshire, Hatfield, UK; Astrophysics Group, Imperial College London, UK) BG(Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Argentina) BH(Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Argentina) BI(Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Argentina) BJ(Departamento de Física y Astronomía, Universidad de Valparaíso, Chile) BK(Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Argentina) BL(Departmento de Astronomía, Universidad de Concepción, Chile) BM(Departmento de Astronomía, Universidad de Concepción, Chile) BN(Max-Planck Institute for Astronomy, Heidelberg, Germany) BO(Department of Astrophysics, University of Oxford, UK) BP(Departamento de Física, Universidad de La Serena, Chile) BQ(Observatorio Astronómico de Córdoba, Argentina) BR(Institute for Astronomy, The University of Edinburgh, UK) BS(Department of Physics, University of Cincinnati, USA) BT(School of Physics & Astronomy, University of Leeds, UK) BU(Institute of Astronomy, University of Cambridge, UK) BV(ESO) BW(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile) BX(Jodrell Bank Centre for Astrophysics, The University of Manchester, UK) BY(NASA–Ames Research Center, Moffett Field, USA) BZ(Departamento de Física y Astronomía, Universidad de Valparaíso, Chile) CA(Institute for Astronomy, The University of Edinburgh, UK) CB(Instituto de Astrofísica de Canarias, Tenerife, Spain) CC(School of Physics and Astronomy, University of Southampton, UK) CD(Instituto de Astrofísica de Canarias, Tenerife, Spain) CE(Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, Italy) CF(Departmento de Astronomía, Universidad de Concepción, Chile) CG(Observatorio Astronómico de Córdoba, Argentina) CH(ESTEC, Noordwijk, the Netherlands) CI(Service d’Astrophysique — IRFU, CEA–Saclay, France; Instituto de Astronomía y Física del Espacio, Buenos Aires, Argentina) CJ(ESO) CK(Departmento de Astronomía, Universidad de Concepción, Chile) CL(Dipartimento di Astronomia, Universitá di Padova, Italy) CM(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile) CN(Observatorio Astronómico de Córdoba, Argentina) CO(Observatorio Astronómico de Córdoba, Argentina) CP(Department of Physics, Macquarie University, Sydney, Australia; Australian Astronomical Observatory, Epping, Australia) CQ(Universidade Federal do Rio Grande do Sul, Porto Alegre, Brazil) CR(Nicolaus Copernicus Astronomical Center, Warsaw, Poland) CS(Departmento de Astronomía, Universidad de Concepción, Chile; Warsaw University Observatory, Poland) CT(Departamento de Ciencias Físicas, Universidad Andres Bello, Santiago, Chile) CU(ESO) CV(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile) CW(Departamento de Física, Universidad de La Serena, Chile) CX(Departamento de Astronomía, Universidad de Chile, Santiago, Chile) CY(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile; Departamento de Física y Astronomía, Universidad de Valparaíso, Chile) CZ(ESO) DA(Departamento de Física y Astronomía, Universidad de Valparaíso, Chile) DB(SKA/KAT, Cape Town, South Africa; Hartebeesthoek Radio Astronomy Observatory, South Africa) DC(Departamento de Física y Astronomía, Universidad de Valparaíso, Chile) DD(The University of Kent, Canterbury, UK) DE(Universidade de São Paulo, Brazil) DF(Departamento de Física, Universidad de La Serena, Chile) DG(National Astronomical Observatory of Japan, Tokyo, Japan) DH(Gemini Observatory, Hawaii, USA) DI(Departamento de Física y Astronomía, Universidad de Valparaíso, Chile) DJ(Centre for Astrophysics Research, University of Hertfordshire, Hatfield, UK) DK(ESO) DL(Departamento de Ingeniería Eléctrica, Pontificia Universidad Católica de Chile, Santiago, Chile) DM(Observatorio Astronómico de Córdoba, Argentina) DN(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile)
Abstract:
VISTA Variables in the Vía Láctea (VVV) is a public ESO near-IR variability survey aimed at scanning the Milky Way Bulge and an adjacent section of the mid-plane. VVV observations started in October 2009 during ESO science verification. Regular observations for the first year of the survey have been conducted since February 2010 and will cover a total area of 520 square degrees in five passbands and five epochs. Here we address the first results obtained from the VVV Survey as well as the current status of the observations.
References:
Arnaboldi, M. et al. 2010, The Messenger, 139, 6; Bertin, E. et al. 2002, ADASS XI, 281, 228; Churchwell, E. et al. 2009, PASP, 121, 213; Collinge, M. J. et al. 2006, ApJ, 651, 197; Emerson, J. & Sutherland, W. 2010, The Messenger, 139, 2; Debosscher, J. et al. 2007, A&A, 475, 1159; Debosscher, J. et al. 2009, A&A, 506, 519; Hodgkin, S. T. et al. 2009, MNRAS, 394, 675; Longmore, S. N. & Burton, M. G. 2009, PASA, 26, 439; Minniti, D. et al. 2010, New Astronomy, 15, 433; Skrutskie, M. F. et al. 2006, AJ, 131, 1163

ADS BibCode:
2010Msngr.141...29G
Section:
Astronomical Science
Author(s)/Affiliation(s):
Giuffrida, G.; Sbordone, L.; Zaggia, S.; Marconi, G.; Bonifacio, P.; Izzo, C.; Szeifert, T.; Buonanno, R.
AA(ASI Science Data Center, Frascati, Italy) AB(Max-Planck-Institut für Astrophysik, Garching, Germany; GEPI, Observatoire de Paris, Meudon, France) AC(INAF–Osservatorio Astronomico di Padova, Italy) AD(ESO) AE(GEPI, Observatoire de Paris, Meudon, France; Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Trieste, Italy) AF(ESO) AG(ESO) AH(ASI Science Data Center, Frascati, Italy; Università di Roma, Italy)
Abstract:
Using VIMOS in imaging and spectroscopy modes and FLAMES spectroscopy data, we have mapped the Sagittarius dwarf spheroidal galaxy (Sgr dSph) photometrically and spectroscopically over eight fields along the galaxy minor and major axes. We have found, for the first time, striking evidence of multiple populations in the peripheral zones of this near companion of the Milky Way. These data, together with previous analyses of the Sgr dSph core and streams, supply a detailed picture of this galaxy, and will give us the opportunity to reconstruct the history of this object and its influence on the evolution of the Milky Way.
References:
Bellazzini, M. et al. 2008, ApJ, 136, 1147; Eggen, O. J., Lynden-Bell, D. & Sandage, A. R. 1962, ApJ, 13, 748; Giuffrida, G. et al. 2010, A&A, 513, 62; Ibata, R. A. et al. 2001, ApJ, 551, 294; Ibata, R. A. et al. 1997, AJ, 113, 634; Ibata, R. A. et al. 1995, MNRAS, 277, 781; Ibata, R. A. et al. 1994, Nature, 370, 194; Majewski, S. R. et al. 2003, ApJ, 599, 1082; Mottini, M. et al. 2008, AJ, 136, 614; Searle, L. & Zinn, R. 1978, ApJ, 225, 357; Sbordone, L. et al. 2007, A&A, 465, 815

ADS BibCode:
2010Msngr.141...32B
Section:
Astronomical Science
Author(s)/Affiliation(s):
Bremer, M.; Lehnert, M.; Douglas, L.; Stanway, E.; Davies, L.; Clowe, D.; Milvang-Jensen, B.; Birkinshaw, M.
AA(H. H. Wills Physics Laboratory, University of Bristol, UK) AB(GEPI, Observatoire de Paris Meudon, France) AC(H. H. Wills Physics Laboratory, University of Bristol, UK; GEPI, Observatoire de Paris Meudon, France) AD(H. H. Wills Physics Laboratory, University of Bristol, UK) AE(H. H. Wills Physics Laboratory, University of Bristol, UK) AF(Ohio University, USA) AG(Dark Cosmology Centre, University of Copenhagen, Denmark) AH(H. H. Wills Physics Laboratory, University of Bristol, UK)
Abstract:
We present a discussion of and results from the ESO Remote Galaxy Survey (ERGS), a spectroscopic survey of Lyman-break galaxies with z ~ 5 and above. The survey directly explores the properties of these early star-forming galaxies, increasing the observational detail in our picture of early galaxy evolution. The survey provides a sample of galaxies ideally matched in spatial distribution to the capabilities of current and imminently available instrumentation. We discuss the results of the first follow-on studies of the sample in the mm/sub-mm that signpost the potential of these facilities for exploring early galaxy evolution.
References:
Davies, L. J. M. et al. 2010, MNRAS, in press, arXiv:1007.3989; Douglas, L. S. et al. 2007, MNRAS, 376, 1393; Douglas, L. S. et al. 2009, MNRAS, 400, 561; Douglas, L. S. et al. 2010, MNRAS, in press, arXiv:1007.2847; Lehnert, M. D. & Bremer, M. N. 2003, ApJ, 593, 630; Poggianti, B. et al. 2009, The Messenger, 136, 54; Stanway, E. R. et al. 2004, ApJ, 607, 704; Stanway, E. R. et al. 2008, ApJ, 687, L1; Stanway, E. R. et al. 2010, MNRAS, in press, arXiv:1007.0440; Verma, A. et al. 2007, MNRAS, 377, 1024; White, S. D. M. et al. 2005, A&A, 444, 365

ADS BibCode:
2010Msngr.141...37N
Section:
Astronomical News
Author(s)/Affiliation(s):
Neumayer, N.; Emsellem, E.
AA(ESO) AB(ESO)
Abstract:
An overview of the ESO workshop on black holes and nuclear star clusters is presented. The meeting reviewed the status of our observational and theoretical understanding of central massive objects, as well as the search for intermediate mass black holes in globular clusters. There will be no published proceedings, but presentations are available at http://www.eso.org/sci/meetings/cmo2010/program.html.
References:
Anderson, J. & van der Marel, R. P. 2010, ApJ, 710, 1032; Gillessen, S. et al. 2009, ApJL, 707, L114; Greene, J. E. et al. 2010, arXiv:1007.2851; Noyola, E. et al. 2008, ApJ, 676, 1008; Noyola, E. et al. 2010, ApJ, 719, L6

ADS BibCode:
2010Msngr.141...40C
Section:
Astronomical News
Author(s)/Affiliation(s):
Casali, M.
AA(ESO, SPIE Symposium co-chair)
Abstract:
A brief overview of the 2010 SPIE Symposium on Astronomical Telescopes and Instrumentation, with emphasis on the ESO contributions, is presented.

ADS BibCode:
2010Msngr.141...41L
Section:
Astronomical News
Author(s)/Affiliation(s):
Laing, R.; Maiolino, R.; Rykaczewski, H.; Testi, L.
AA(ESO) AB(INAF–Osservatorio Astronomico di Roma, Italy) AC(ESO) AD(ESO)
Abstract:
A small complement of receivers for the ALMA Band 5 (163–211 GHz) is under construction. This workshop was devoted to the scientific potential and goals of a full set of Band 5 receivers for ALMA, with emphasis on the detection of water in the local Universe and the 158 µm emission line of C⁺ from high redshift galaxies.

ADS BibCode:
2010Msngr.141...43F
Section:
Astronomical News
Author(s)/Affiliation(s):
Fosbury, R.; Trygg, T.
AA(Space Telescope European Co-ordinating Facility, ESO) AB(Aalto University School of Art and Design, Helsinki, Finland)
Abstract:
The recently developed technique of simple pinhole camera “solargraphy” enables images of the path of the Sun to be recorded over long periods. Solargraphy cameras have been installed at the three ESO observatory sites in Chile and at ESO Headquarters in Garching. These intriguing images are presented and described. They illustrate, in a very direct way, the clear skies at the observatories.

ADS BibCode:
2010Msngr.141...46S
Section:
Astronomical News
Author(s)/Affiliation(s):
Sartori, L.; Pelloni, C.
AA(Liceo Lugano 2, Savosa, Switzerland) AB(Liceo Lugano 2, Savosa, Switzerland)
Abstract:
As a project for diploma work at the end of Swiss high school, long-slit kinematic data for two giant elliptical galaxies, observed with the FORS1 spectrograph at the ESO VLT, were reduced by two students. The reduction of these data was our first research experience. The preparation and reduction of the long-slit data is outlined. We also describe our impressions of this first encounter with the scientific research world.
References:
Cappellari, M. & Emsellem, E. 2004, PASP, 116, 138; Carollo, C. M. et al. 1995, ApJ, 441, 25; Carollo, C. M. & Danziger, I. J. 1994a, MNRAS, 270, 523; Carollo, C. M. & Danziger, I. J. 1994b, MNRAS, 270, 743 (CD94b) Emsellem, E. 2006, in Mapping the Galaxy and nearby galaxies, eds. Wada, K. & Combes, F. Massey, P. 1997, A User’s Guide to CCD Reductions with IRAF, NOAO Massey, P. et al. 1992, A User’s Guide to Reducing Slit Spectra with IRAF, NOAO Rothberg, B. & Joseph, R. D. 2006, AJ, 132, 976

ADS BibCode:
2010Msngr.141...50P
Section:
Astronomical News
Author(s)/Affiliation(s):
Primas, F.; Casali, M.; Walsh, J.
AA(ESO) AB(ESO) AC(ESO)
Abstract:
In May and June 2010, Sandro D’Odorico and Alan Moorwood, both driving forces behind many ESO instruments and very active in research, retired after three decades at ESO. The ESO Director General, Tim de Zeeuw, elevated both to the newly inaugurated position of ESO Astronomer Emeritus. Celebrations on their transition to these esteemed positions were held and are briefly described.
References:
Moorwood, A. 2009, The Messenger, 136, 8

ADS BibCode:
2010Msngr.141...51.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2010Msngr.141...53.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2010Msngr.141...54.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2010Msngr.141Q..55.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2010Msngr.141R..55.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)