Messenger No. 155 ( 2014)

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Telescopes and Instrumentation

2-5 (PDF)
J. Spyromilio et al.
ISAAC. An Appreciation

ADS BibCode:
2014Msngr.155....2S
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Spyromilio, J.; Cuby, J.; Lidman, C.; Johnson R.; Jaunsen, A. O.; Mason, E.; Ivanov, V. D.; Schmidtobreick, L.
AA(ESO) AB(Laboratoire d’astrophysique de Marseille, Université Aix-Marseille & CNRS, Marseille, France) AC(Australian Astronomical Observatory, Epping, Australia) AD(Institute of Astrophysics, University of Oslo, Norway) AE(INAF–Osservatorio Astronomico de Trieste, Italy) AF(ESO) AG(ESO)
Abstract:
ISAAC was switched off, almost certainly for the final time, on 12 December 2013. The last observing block executed was OB1030962, the target, Supernova 2013ct, for a programme whose principal investigator just happened to be the first instrument scientist for ISAAC. “All constraints were respected and spectra of the target detected” are the public comments in the log. A short history of ISAAC, from the instrument scientists’ viewpoint, is presented.
References:
Andersen, M. et al. 2004, A&A, 414, 969; de Zeeuw, P. T. 2011, The Messenger, 145, 49; Förster Schreiber, N. M. et al. 2006, AJ, 131, 1891; Leibundgut, B. et al. 2011, The Messenger, 145, 50; McLean, I. et al. 1986, SPIE, 627, 430; Pettini, M. et al. 2001, ApJ, 554, 981; Raynaud, E. et al. 2003, Icarus, 162, 344
6-11 (PDF)
S. Lewis et al.
Laser Guide Star Facility Upgrade

ADS BibCode:
2014Msngr.155....6L
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Lewis, S.; Calia, D. B.; Buzzoni, B.; Duhoux, P.; Fischer, G.; Guidolin, I.; Haimerl, A.; Hackenberg, W.; Hinterschuster, R.; Holzlöhner, R.; Jolley, P.; Pfrommer, T.; Popovic, D.; Alvarez, J.-L.; Beltran, J.; Girard, J.; Pallanca, L.; Riquelme, M.; Gonte, F.
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(ESO) AP(ESO) AQ(ESO) AR(ESO) AS(ESO)
Abstract:
The Laser Guide Star Facility is part of VLT Unit Telescope 4 and provides a single centre-launched sodium beacon for the two adaptive optics instruments SINFONI and NACO. The original facility, installed in 2006, employed a high-power dye laser source, PARSEC, producing an output beam that was delivered via a single-mode optical fibre to launch optics located behind the telescope secondary mirror. We recently installed a new prototype laser source, PARLA, based on Raman optical fibre technology. Requirements for the new laser include start-up times compatible with flexible observing, an output beam appropriate for the existing fibre-delivery system and an on-sky power of up to 7 watts. This is the first time that this type of laser has been deployed at a major observing facility, and it has a pathfinder role for future adaptive optics systems. Reported here are the main results of the development, deployment and early operation since the resumption of science operation in February 2013.
References:
Arsenault, R. et al. 2006, The Messenger, 123, 6; Bernard, R. 1939, ApJ, 89, 133; Bonaccini Calia, D. et al. 2006, SPIE, 6272, 627207; Bonaccini Calia, D. et al. 2010, SPIE, 7736, 77361U-1; Holzlöhner, R. et al. 2010, A&A, 510, A20; Kaenders, W. G. et al. 2010, SPIE, 7736, 773621; Rabien, S. et al. 2003, SPIE, 4839, 393; Simonich, D., Clemesha, B. & Kirchhoff, V. 1979, J. Geophys. Res.: Space Phys., 84, 1543; Slipher, V. M. 1929, PASP, 41, 262
12-16 (PDF)
S. Rengaswamy et al.
Speckle Imaging with VLT/NACO No-AO Mode

ADS BibCode:
2014Msngr.155...12R
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Rengaswamy, S.; Girard, J.; de Wit, W.-J.; Boffin, H.
AA(ESO) AB(ESO) AC(ESO) AD(ESO)
Abstract:
Long-exposure stellar images recorded with large ground-based telescopes are blurred due to the turbulent nature of the atmosphere. The VLT employs active and adaptive optics (AO) systems to compensate for the deleterious effects of the atmosphere in real time. The speckle imaging technique provides an alternative way to achieve diffraction-limited imaging by post-processing a series of short-exposure images. The use of speckle imaging with the no-AO mode of NACO at the VLT is demonstrated. Application of this technique is particularly suited to the J-band and it provides versatile high angular resolution imaging under mediocre conditions and/or in imaging extended objects. The implementation of this mode underlines the continuing attractiveness of NACO at the VLT.
References:
Allen, D. A., Harvey, P. M. & Swings, J. P. 1972, A&A, 20, 333; Girard, J. H. et al. 2010, SPIE, 7736, 77362N Jennison, R. 1958, MNRAS, 118, 276; Labeyrie, A. 1970, A&A, 6, 85; Lenzen, R. et al. 2003, SPIE, 4841, 944; Mason, B. D., Hartkopf, W. I. & Hurowitz, H. M. 2013, AJ, 146, 56; Monnier, J. D., Tuthill, P. G. & Danchi, W. C. 1999, ApJ, 525, L97; Rengaswamy, S., Girard, J. H. & Montagnier, G. 2010, SPIE, 7734, 77341B Rogstad, D. H. 1968, Appl. Opt., 7, 585; Rousset, G. et al. 2003, SPIE, 4839, 140; Schödel, R. & Girard, J. H. 2012, The Messenger, 150, 26; Schödel, R. et al. 2013, MNRAS, 429, 1367; Tuthill, P. G., Monnier, J. D. & Danchi, W. C. 1999, Nature, 398, 487; Weigelt, G. P. 1977, Optics Communications, 21, 55
17-18 (PDF)
F. Kerber et al.
Antarctic Air Visits Paranal — Opening New Science Windows

ADS BibCode:
2014Msngr.155...17K
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Kerber, F.; Kuntschner, H.; Querel, R. R.; van den Ancker, M.
AA(ESO) AB(ESO) AC(National Institute of Water & Atmospheric Research (NIWA), Lauder, New Zealand; Universidad de Chile, Santiago, Chile) AD(ESO)
Abstract:
Extremely low humidity (precipitable water vapour [PWV] of ~ 0.1 mm) in the atmosphere above Paranal has been measured by a water vapour radiometer over a period of about 12 hours. PWV values < 0.2 mm are usually only found at very high altitude or in Antarctica. In fact a pocket of Antarctic air has been shown to be responsible for this phenomenon and it may occur a few times per year at Paranal. We highlight the science opportunities — created by new atmospheric windows — that arise in such conditions. The community is invited to provide feedback on how to make best use of low PWV with the VLT.
References:
Kerber, F. et al. 2014, MNRAS, in press Kerber, F. et al. 2012, The Messenger, 148, 9; McLean, I. S. et al. 2012, Proc. SPIE, 8446, 844619; Motohara, K. et al. 2008, Proc. SPIE, 7014, 70142T Querel, R. R., Naylor, D. A. & Kerber, F. 2011, PASP, 123, 222; Sarazin, M., Kerber, F. & De Breuck, C. 2013, The Messenger, 152, 17
19-22 (PDF)
E. Fomalont et al.
The Calibration of ALMA using Radio Sources

ADS BibCode:
2014Msngr.155...19F
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Fomalont, E.; van Kempen, T.; Kneissl, R.; Marcelino, N.; Barkats, D.; Corder, S.; Cortes, P.; Hills, R.; Lucas, R.; Manning, A.; Peck, A.
AA(National Radio Astronomy Observatory, Santiago, Chile) AB(Leiden University, Leiden, the Netherlands) AC(ESO) AD(National Radio Astronomy Observatory, Charlottesville, VA, USA) AE(ESO) AF(National Radio Astronomy Observatory, Santiago, Chile) AG(National Radio Astronomy Observatory, Santiago, Chile) AH(Cavendish Laboratory, Cambridge, UK) AI(Institut d’Astrophysique de Grenoble, Grenoble, France) AJ(ESO) AK(National Radio Astronomy Observatory, Charlottesville, VA, USA)
Abstract:
For ALMA to produce high quality images of astronomical objects with sub-arcsecond resolution at frequencies above 85 GHz, the radio signals must be combined from up to 66 antennas spread over 15 km with a maximum path length delay difference of about 0.025 mm. This accuracy requires precise antenna structures, stable electronics, compensation for many temporal changes in the system and the measurement of the path-changing water vapour emission in the line of sight. The final stage of path length calibration is provided by frequent observations of relatively strong, point-like distant radio sources, quasars, that lie within a few degrees of the astronomical object. The ALMA Quasar Catalogue was implemented to provide a database that contains the essential parameters for hundreds of quasars and their brightness variations at several frequencies as a function of time. This paper describes the filling of the catalogue and the use of these quasar test signals to provide the path length accuracy needed for the imaging of radio sources.
References:
Antonucci, R. 1993, ARA&A, 31, 473; Nikolic, B. et al. 2008, The Messenger, 131, 14; Nikolic, B. et al. 2013, A&A, 552, A104

Astronomical Science

24-29 (PDF)
M. Hempel et al.
VISTA Variables in the Vía Láctea (VVV): Halfway Status and Results

ADS BibCode:
2014Msngr.155...29H
Section:
Astronomical Science
Author(s)/Affiliation(s):
Hempel, M.; Minniti, D.; Dékány, I.; Saito, R. K.; Lucas, P. W.; Emerson, J. P.; Ahumada, A. V.; Aigrain, S.; Alonso, M. V.; Alonso-García, J.; Amôres, E. B.; Angeloni, R.; Arias, J.; Bandyopadhyay, R.; Barbá, R. H.; Barbuy, B.; Baume, G.; Beamin, J. C.; Bedin, L.; Bica, E.; Borissova, J.; Bronfman, L.; Carraro, G.; Catelan, M.; Clariá, J. J.; Contreras, C.; Cross, N.; Davis, C.; de Grijs, R.; Drew, J. E.; Fariña, C.; Feinstein, C.; Lajús, E. F.; Folkes, S.; Gamen, R. C.; Geisler, D.; Gieren, W.; Goldman, B.; González, O.; Gosling, A.; Gunthardt, G.; Gurovich, S.; Hambly, N. C.; Hanson, M.; Hoare, M.; Irwin, M. J.; Ivanov, V. D.; Jordán, A.; Kerins, E.; Kinemuchi, K.; Kurtev, R.; Longmore, A.; López-Corredoira, M.; Maccarone, T.; Martín, E.; Masetti, N.; Mennickent, R. E.; Merlo, D.; Messineo, M.; Mirabel, I. 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. E.; Saviane, I.; Schreiber, M. R.; Schröder, A. C.; Sharma, S.; Smith, M.; Sodré Jr., L.; Soto, M.; Stephens, A. W.; Tamura, M.; Tappert, C.; Thompson, M. A.; Toledo, I.; Valenti, E.; Vanzi, L.; Weidmann, W.; Zoccali, M.
AA(Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Chile; The Milky Way Millennium Nucleus, Santiago, Chile) AB(Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Chile; Vatican Observatory, Italy) AC(Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Chile) AD(Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Chile; Universidade Federal de Sergipe, Departamento de Física, Cristóvão, Brazil) AE(Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield, UK) AF(Astronomy Unit, School of Physics and Astronomy, Queen Mary University of London, UK) AG(Observatorio Astronómico de Córdoba, Argentina; ESO; Consejo Nacional de Investigaciones Científicas y Técnicas, Buenos Aires, Argentina) AH(School of Physics, University of Exeter, UK) AI(Observatorio Astronómico de Córdoba, Argentina) AJ(Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Chile) AK(SIM, Faculdade de Ciências da Universidade de Lisboa, Portugal) AL(Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Chile) AM(Departamento de Física, Universidad de La Serena, Chile) AN(Department of Astronomy, University of Florida, Gainesville, USA) AO(Departamento de Física, Universidad de La Serena, Chile) AP(Universidade de São Paulo, Brazil) AQ(Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Argentina) AR(Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Chile) AS(Space Telescope Science Institute, Baltimore, USA) AT(Universidade Federal do Rio Grande do Sul, Porto Alegre, Brazil) AU(Departamento de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Chile) AV(Departamento de Astronomía, Universidad de Chile, Santiago, Chile) AW(ESO) AX(Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Chile) AY(Observatorio Astronómico de Córdoba, Argentina) AZ(Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Chile) BA(Institute for Astronomy, The University of Edinburgh, UK) BB(Joint Astronomy Centre, Hilo, USA) BC(Kavli Institute for Astronomy and Astrophysics, Peking University, China) BD(Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield, UK; Astrophysics Group, Imperial College London, UK) BE(Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Argentina) BF(Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Argentina) BG(Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Argentina) BH(Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield, UK; Departamento de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Chile) BI(Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Argentina) BJ(Departmento de Astronomía, Universidad de Concepción, Chile) BK(Departmento de Astronomía, Universidad de Concepción, Chile) BL(Max Planck Institute for Astronomy, Heidelberg, Germany) BM(ESO) BN(Department of Astrophysics, University of Oxford, UK) BO(Departamento de Física, Universidad de La Serena, Chile) BP(Observatorio Astronómico de Córdoba, Argentina) BQ(Institute for Astronomy, The University of Edinburgh, UK) BR(Department of Physics, University of Cincinnati, USA) BS(School of Physics & Astronomy, University of Leeds, UK) BT(Institute of Astronomy, University of Cambridge, UK) BU(ESO) BV(Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Chile) BW(Jodrell Bank Centre for Astrophysics, The University of Manchester, UK) BX(NASA-Ames Research Center, Moffett Field, USA) BY(Departamento de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Chile) BZ(Institute for Astronomy, The University of Edinburgh, UK) CA(Instituto de Astrofísica de Canarias, La Laguna, Tenerife, Spain) CB(Department of Physics, Texas Tech University, Lubbock, USA) CC(Instituto de Astrofísica de Canarias, La Laguna, Tenerife, Spain) CD(Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, Italy) CE(Departmento de Astronomía, Universidad de Concepción, Chile) CF(Observatorio Astronómico de Córdoba, Argentina) CG(Rochester Institute of Technology, Rochester, USA) CH(Service d’Astrophysique – IRFU, CEA-Saclay, Gif sur Yvette, France; Instituto de Astronomía y Física del Espacio, Buenos Aires, Argentina) CI(ESO) CJ(Instituto de Astronomía, Universidad Católica del Norte, Antofagasta, Chile) CK(Dipartimento di Astronomia, Universitá di Padova, Italy) CL(Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Chile) CM(Observatorio Astronómico de Córdoba, Argentina) CN(Observatorio Astronómico de Córdoba, Argentina) CO(Department of Physics, Macquarie University, Sydney, Australia; Australian Astronomical Observatory, Epping, Australia) CP(Universidade Federal do Rio Grande do Sul, Porto Alegre, Brazil) CQ(Nicolaus Copernicus Astronomical Center, Warsaw, Poland) CR(Departmento de Astronomía, Universidad de Concepción, Chile; Warsaw University Observatory, Warsaw, Poland) CS(Departamento de Ciencias Físicas, Universidad Andres Bello, Santiago, Chile) CT(ESO) CU(Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Chile) CV(Departamento de Física, Universidad de La Serena, Chile) CW(Departamento de Astronomía, Universidad de Chile, Santiago, Chile) CX(Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Chile; Departamento de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Chile; Rudolf Peierls Centre for Theoretical Physics, Oxford, UK) CY(ESO) CZ(Departamento de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Chile) DA(SKA/KAT, Cape Town, South Africa; Hartebeesthoek Radio Astronomy Observatory, Krugersdorp, South Africa) DB(Departamento de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Chile) DC(The University of Kent, Canterbury, UK) DD(Universidade de São Paulo, Brazil) DE(Departamento de Física, Universidad de La Serena, Chile) DF(Division of Optical and Infrared Astronomy, National Astronomical Observatory of Japan, Tokyo, Japan) DG(Gemini Observatory, Hawaii, USA) DH(Departamento de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Chile) DI(Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield, UK) DJ(ALMA Observatory, Santiago Chile) DK(ESO) DL(Departamento de Ingeniería Eléctrica, Pontificia Universidad Católica de Chile, Santiago, Chile) DM(Observatorio Astronómico de Córdoba, Argentina) DN(Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Chile)
Abstract:
The VISTA Variables in the Vía Láctea (VVV) survey is one of six near-infrared ESO public surveys, and is now in its fourth year of observing. Although far from being complete, the VVV survey has already delivered many results, some directly connected to the intended science goals (detection of variable stars, microlensing events, new star clusters), others concerning more exotic objects, e.g., novae. Now, at the end of the fourth observing period, and comprising roughly 50% of the proposed observations, the status of the survey, as well some of results based on the VVV data, are presented.
References:
Beamin, J. C. et al. 2013, ATel, 5215; Catelan, M. et al. 2011, Carnegie Observatories Astrophysics Series, Vol. 5; Dalton, G. B. et al. 2006, Proc. SPIE, 6269; Emerson, J. & Sutherland, W. 2010, The Messenger, 139, 2; Epchtein, N. 1994, A&SS, 217, 3; Gonzalez, O. A. et al. 2011, A&A, 543, L14; Gonzales, O. A. et al. 2013, The Messenger, 152, 23; Gromadzki, M. et al. 2013, Mem. S. A. It., 75, 282; Ivanov, V. D. et al. 2013, A&A, accepted, arXiv:1309.4301v1; Lépine, S. 2008, AJ, 135, 1247; Minniti, D. et al. 2010, New Astronomy, 15, 433; Minniti, D. et al. 2012, ATel, 4041; Nishiyama, S. et al. 2005, ApJ, 621, L105; Saito, R. K. et al. 2010, The Messenger, 141, 24; Saito, R. K. et al. 2012a, A&A, 544, 147; Saito, R. K. et al. 2012b, A&A, 537, 107; Saito, R. K. et al. 2013, A&A, 554, 123; Schlegel, D. et al. 1998, ApJ, 500, 525; Skrutski, M. F. et al. 2006, AJ, 131, 1163; Soto, M. et al. 2013, A&A, 552, 101
30-32 (PDF)
M. Miluzio
Search for Supernovae in Starburst Galaxies with HAWK-I

ADS BibCode:
2014Msngr.155...30M
Section:
Astronomical Science
Author(s)/Affiliation(s):
Miluzio, M.
AA(INAF–Osservatorio Astronomico di Padova, Italy)
Abstract:
With the aim of testing the relation between supernova (SN) rate and star formation rate, we conducted a SN search in a sample of local starburst galaxies (SBs) where both star formation rates and extinction are extremely high. The search was performed in the near-infrared, where the bias due to extinction is reduced using HAWK-I on the VLT. We discovered six SNe, in excellent agreement with expectations, when considering that, even in our search, about 60% of events remain hidden in the nuclear regions due to a combination of reduced search efficiency and very high extinction.
References:
Botticella, M. T. et al. 2008, A&A, 479, 49; Horiuchi, S. et al. 2011, ApJ, 738, 154; Hopkins, A. M. & Beacom, J. F. 2006, ApJ, 651, 142; Maiolino, R. et al. 2002, A&A, 389, 84; Mannucci, F. et al. 2003, A&A, 401, 519; Mannucci, F., Della Valle, M. & Panagia, N. 2006, MNRAS, 370, 773; Mattila, S. et al. 2007b, ApJ, 659, L9; Mattila, S. et al. 2012, ApJ, 756, 111; Melinder, J. et al. 2012, A&A, 545, A96; Miluzio, M. & Cappellaro, E. 2010, Central Bureau Electronic Telegrams, 2446, 1; Miluzio, M. et al. 2011, Central Bureau Electronic Telegrams, 2773, 1; Miluzio, M. et al. 2013, A&A, 554, A127; Richmond, M. W., Filippenko, A. V. & Galisky, J. 1998, PASP, 110, 553; Smartt, S. J. 2009, ARA&A, 47, 63
33-36 (PDF)
Le Fèvre O. et al.
The VIMOS VLT Deep Survey: Final Public Release of ~ 35 000 Galaxies and Active Galactic Nuclei Covering 13 Billion Years of Evolution

ADS BibCode:
2014Msngr.155...33F
Section:
Astronomical Science
Author(s)/Affiliation(s):
Le Fèvre O.; Adami C.; Arnouts, S.; Bardelli, S.; Bolzonella, M.; Bondi, M.; Bongiorno, A.; Bottini, D.; Cappi, A.; Cassata, P.; Charlot, S.; Ciliegi, P.; Contini, T.; Cucciati, O.; de la Torre, S; Foucaud, S.; Franzetti, P.; Garilli, B.; Gavignaud, I.; Guzzo, L.; Ilbert, O.; Iovino, A.; Le Brun, V.; Lemaux, B.; López-Sanjuan, C.; Maccagni, D.; McCracken, H. J.; Marano, B.; Marinoni, C.; Mazure, A.; Mellier, Y.; Merighi, R.; Merluzzi, P.; Moreau, C.; Paltani, S.; Pellò, R.; Pollo, A.; Pozzetti, L.; Scaramella, R.; Scodeggio, M.; Tasca, L.; Tresse, L.; Vergani, D.; Vettolani, G.; Zamorani, G.; Zanichelli, A.; Zucca, E.
AA(Aix–Marseille Université, CNRS, LAM–Laboratoire d’Astrophysique de Marseille, Marseille, France) AB(Aix–Marseille Université, CNRS, LAM–Laboratoire d’Astrophysique de Marseille, Marseille, France) AC(Aix–Marseille Université, CNRS, LAM–Laboratoire d’Astrophysique de Marseille, Marseille, France) AD(INAF–Osservatorio Astronomico di Bologna, Bologna, Italy) AE(INAF–Osservatorio Astronomico di Bologna, Bologna, Italy) AF(INAF–IRA, Bologna, Italy) AG(INAF–Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy) AH(INAF–IASF, Milano, Italy) AI(INAF–Osservatorio Astronomico di Bologna, Bologna, Italy) AJ(Aix–Marseille Université, CNRS, LAM–Laboratoire d’Astrophysique de Marseille, Marseille, France) AK(Institut d’Astrophysique de Paris, UMR) AL(INAF–Osservatorio Astronomico di Bologna, Bologna, Italy) AM(CNRS, Université Pierre et Marie Curie, Paris, France) AN(INAF–Osservatorio Astronomico di Bologna, Bologna, Italy) AO(Aix–Marseille Université, CNRS, LAM–Laboratoire d’Astrophysique de Marseille, Marseille, France) AP(Institut de Recherche en Astrophysique et Planétologie, Toulouse, France) AQ(INAF–IASF, Milano, Italy) AR(INAF–IASF, Milano, Italy) AS(Department of Physics & Astronomy, Shanghai JiaoTong University, Shanghai, China) AT(Departamento de CienciasFisicas, Universidad Andres Bello, Santiago, Chile) AU(Aix–Marseille Université, CNRS, LAM–Laboratoire d’Astrophysique de Marseille, Marseille, France) AV(Departamento de CienciasFisicas, Universidad Andres Bello, Santiago, Chile) AW(Aix–Marseille Université, CNRS, LAM–Laboratoire d’Astrophysique de Marseille, Marseille, France) AX(Aix–Marseille Université, CNRS, LAM–Laboratoire d’Astrophysique de Marseille, Marseille, France) AY(INAF–OsservatorioAstronomico di Brera, Milano, Italy) AZ(INAF–IRA, Bologna, Italy) BA(Institut d’Astrophysique de Paris, UMR) BB(Centro de Estudios de Físicadel Cosmos de Aragón, Teruel, Spain) BC(Università di Bologna, Dipartimento di Astronomia, Bologna, Italy) BD(Aix–Marseille Université, CNRS, LAM–Laboratoire d’Astrophysique de Marseille, Marseille, France) BE(Institut d’Astrophysique de Paris, UMR) BF(INAF–Osservatorio Astronomico di Bologna, Bologna, Italy) BG(INAF–IRA, Bologna, Italy) BH(Aix–Marseille Université, CNRS, LAM–Laboratoire d’Astrophysique de Marseille, Marseille, France) BI(Aix-Marseille Université, CNRS, Centre de Physique Théorique, Marseille, France; Integral Science Data Centre, Genève, Switzerland) BJ(CNRS, Université Pierre et Marie Curie, Paris, France) BK(Geneva Observatory, Genève, Switzerland; Astronomical Observatory of the Jagiellonian University, Kraków, Poland) BL(INAF–Osservatorio Astronomico di Bologna, Bologna, Italy) BM(INAF–Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy) BN(INAF–IASF, Milano, Italy) BO(Aix–Marseille Université, CNRS, LAM–Laboratoire d’Astrophysique de Marseille, Marseille, France) BP(Aix–Marseille Université, CNRS, LAM–Laboratoire d’Astrophysique de Marseille, Marseille, France) BQ(INAF–Osservatorio Astronomico di Bologna, Bologna, Italy) BR(INAF–IRA, Bologna, Italy) BS(INAF–Osservatorio Astronomico di Bologna, Bologna, Italy) BT(INAF–IRA, Bologna, Italy) BU(INAF–Osservatorio Astronomico di Bologna, Bologna, Italy)
Abstract:
The VIMOS VLT Deep Survey (VVDS) final and public data release offers an excellent opportunity to revisit galaxy evolution with a sample of 35 016 galaxies and active galactic nuclei covering the redshift range 0 < z < 6.7. The VVDS includes three tiered surveys, the wide, deep and ultra-deep surveys, covering up to 8.7 square degrees, and each magnitude-selected with limits iAB = 22.5, 24 and 24.75 respectively. The VVDS redshifts, spectra, and all associated multi-wavelength data are available at http://cesam.lam.fr/vvds. The highlights and scientific legacy of the VVDS are summarised.
References:
Abbas, U. et al. 2010, MNRAS, 406, 1306; Arnouts, S. et al. 2005, ApJ, 619, 43; Arnouts, S. et al. 2007, A&A, 476, 137; Baldry, I. K. et al. 2010, MNRAS, 404, 86; Bielby, R. et al. 2012, A&A, 545, 23; Bongiorno, A. et al. 2007, A&A, 472, 433; Cassata, P. et al. 2011, A&A, 525, 143; Cassata, P. et al. 2013, A&A, 556, 68; Ciliegi, P. et al. 2005, A&A, 441, 879; Contini, T. et al. 2012a, A&A, 539, 91; Contini, T. et al. 2012b, The Messenger, 147, 32; Cucciati, O. et al. 2006, A&A, 458, 39; Cucciati, O. et al. 2012, A&A, 539, 31; Cuillandre, J. C. et al. 2012, SPIE, 8448; Davis, M. et al. 2003, SPIE, 4834, 161; De la Torre, S. et al. 2011, A&A, 525, 125; De Ravel, L. et al. 2009, A&A, 498, 379; Gavignaud, I. et al. 2006, A&A, 457, 79; Guzzo, L. et al. 2008, Nature, 451, 541; Guzzo, L. 2013a, The Messenger, 151, 41; Guzzo, L. et al. 2013b, A&A, in press, arXiv:1303.2623; Ilbert, O. et al. 2005, A&A, 439, 863; Ilbert, O. et al. 2006, A&A, 457, 841; Laureijs, R. et al. 2011, arXiv:1110.3193; Le Fèvre, O. et al. 1995, ApJ, 455, 60; Le Fèvre, O. et al. 2003, SPIE, 4841, 1670; Le Fèvre, O. et al. 2004a, A&A, 428, 1043; Le Fèvre, O. et al. 2004b, A&A, 417, 839; Le Fèvre, O. et al. 2005a, A&A, 439, 845; Le Fèvre, O. et al. 2005b, Nature, 437, 519; Le Fèvre, O. et al. 2005c, A&A, 439, 877; Le Fèvre, O. et al. 2013a, A&A, 559, 14; Le Fèvre, O. et al. 2013b, A&A, submitted, arXiv:1307.6518; Lilly, S. J. et al. 2007, ApJS, 172, 70; Lemaux, B. et al. 2013, A&A, submitted, arXiv:1311.5228; Lonsdale, C. et al. 2003, PASP, 115, 897; Lopez-Sanjuan, C. et al. 2011, A&A, 530, 20; Marinoni, C. et al. 2005, A&A, 442, 801; McCracken, H. J. et al. 2003, A&A, 410, 17; Meneux, B. et al. 2006, A&A, 452, 387; Meneux, B. et al. 2008, A&A, 478, 299; Pollò, A. et al. 2006, A&A, 451, 409; Pozzetti, L. et al. 2007, A&A, 474, 443; Tresse, L. et al. 2007, A&A, 472, 403; Zucca, E. et al. 2006, A&A, 455, 879
37-41 (PDF)
Le Fèvre O. et al.
The VIMOS Ultra Deep Survey: 10 000 Galaxies to Study the Early Phases of Galaxy Assembly at 2 < z < 6+

ADS BibCode:
2014Msngr.155...38F
Section:
Astronomical Science
Author(s)/Affiliation(s):
Le Fèvre O.; Amorin, R.; Bardelli, S.; Capak, P.; Cassara, L.; Cassata, P.; Castellano, M.; Charlot, S.; Cimatti, A.; Contini, T.; Cuby, J.; Cucciati, O.; Durkalec, A.; de la Torre, S.; Fontana, A.; Fotopoulou, S.; Garilli, B.; Giavalisco, M.; Grazian, A.; Hathi, N.; Ilbert, O.; Le Brun, V.; Lemaux, B.; Lopez-Sanjuan, C.; Maccagni, D.; Mellier, Y.; Moreau, C.; Paltani, S.; Pentericci, L.; Ribeiro, B.; Salvato, M.; Schaerer, D.; Scodeggio, M.; Scoville, N.; Sommariva, V.; Talia, M.; Taniguchi, Y.; Tasca, L.; Thomas, R.; Tresse, L.; Vanzella, E.; Vergani, D.; Wang, P.; Zamorani, G.; Zucca, E.
AA(Aix–Marseille Université, CNRS, LAM – Laboratoire d’Astrophysique de Marseille, France) AB(INAF–Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy) AC(INAF–Osservatorio Astronomico di Bologna, Italy) Ad(Spitzer Science Center, California Institute of Technology, Pasadena, USA) AE(INAF–IASF, Milano, Italy) AF(Aix–Marseille Université, CNRS, LAM – Laboratoire d’Astrophysique de Marseille, France) AG(INAF–Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy) AH(Institut d’Astrophysique de Paris, UMR) AI(CNRS, Université Pierre et Marie Curie, Paris, France) AJ(Dipartimento di Astronomia, Università di Bologna, Italy) AK(Aix–Marseille Université, CNRS, LAM – Laboratoire d’Astrophysique de Marseille, France) AL(CNRS, Université Pierre et Marie Curie, Paris, France) AM(Aix–Marseille Université, CNRS, LAM – Laboratoire d’Astrophysique de Marseille, France) AN(Aix–Marseille Université, CNRS, LAM – Laboratoire d’Astrophysique de Marseille, France) AO(INAF–Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy) AP(Institut de Recherche en Astrophysique et Planétologie, Toulouse, France; ISDC Data Centre for Astrophysics, University of Geneva, Versoix, Switzerland) AQ(INAF–IASF, Milano, Italy) AR(Department of Astronomy, University of Geneva, Versoix, Switzerland) AS(INAF–Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy) AT(Aix–Marseille Université, CNRS, LAM – Laboratoire d’Astrophysique de Marseille, France) AU(Aix–Marseille Université, CNRS, LAM – Laboratoire d’Astrophysique de Marseille, France) AV(Aix–Marseille Université, CNRS, LAM – Laboratoire d’Astrophysique de Marseille, France) AW(Aix–Marseille Université, CNRS, LAM – Laboratoire d’Astrophysique de Marseille, France) AX(Department of Astronomy, University of Massachusetts, Amherst, USA) AY(INAF–IASF, Milano, Italy) AZ(Institut d’Astrophysique de Paris, UMR; Centro de Estudios de Físicadel Cosmos de Aragón, Teruel, Spain) BA(Aix–Marseille Université, CNRS, LAM – Laboratoire d’Astrophysique de Marseille, France) BB(Institut de Recherche en Astrophysique et Planétologie, Toulouse, France; ISDC Data Centre for Astrophysics, University of Geneva, Versoix, Switzerland) BC(INAF–Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy) BD(Aix–Marseille Université, CNRS, LAM – Laboratoire d’Astrophysique de Marseille, France) BE(CEA/Irfu/SAp Saclay, Laboratoire AIM, Gif-sur-Yvette, France) BF(ISDC Data Centre for Astrophysics, University of Geneva, Versoix, Switzerland) BG(INAF–IASF, Milano, Italy) BH(Max Planck Institut für extraterrestrische Physik, Garching, Germany) BI(INAF–Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy) BJ(INAF–Osservatorio Astronomico di Bologna, Italy) BK(California Institute of Technology, Pasadena, USA) BL(Aix–Marseille Université, CNRS, LAM – Laboratoire d’Astrophysique de Marseille, France) BM(Aix–Marseille Université, CNRS, LAM – Laboratoire d’Astrophysique de Marseille, France) BN(Aix–Marseille Université, CNRS, LAM – Laboratoire d’Astrophysique de Marseille, France) BO(CNRS, Université Pierre et Marie Curie, Paris, France) BP(Research Institute for Space and Cosmic Evolution, Ehime University, Matsuyama, Japan) BQ(Aix–Marseille Université, CNRS, LAM – Laboratoire d’Astrophysique de Marseille, France) BR(INAF–Osservatorio Astronomico di Bologna, Italy) BS(INAF–Osservatorio Astronomico di Bologna, Italy)
Abstract:
The VIMOS Ultra Deep Survey (VUDS) aims to study the early phases of galaxy assembly from a large, well-defined sample of ~ 10 000 galaxies with spectra obtained from very deep VIMOS observations. This sample is by far the largest to date, with spectroscopic redshifts covering a redshift range 2 <z < ~ 6 and it enables a range of fundamental studies to better understand the first major steps in galaxy evolution. The first results from the VUDS survey are summarised, including the discovery of a galaxy proto-cluster at z = 3.3.
References:
Amorin, R. et al. 2014, submitted, arXiv:1403.3692; Bielby, R. et al. 2011, MNRAS, 414, 2; Bouwens, R. et al. 2007, ApJ, 670, 928; Cardamone, C. et al. 2010, ApJS, 189, 270; Cassata, P. et al. 2014, submitted, arXiv:1403.3693; Cucciati, O. et al. 2014, submitted, arXiv:1403.3691; Garilli, B. et al. 2010, PASP, 122, 827; Guzzo, L. et al. 2013, The Messenger, 151, 41; Guzzo, L. et al. 2014, A&A, in press, arXiv:1303.2623; Ilbert, O. et al. 2013, A&A, 556, 55; Le Fèvre, O. et al. 2005, A&A, 439, 845; Le Fèvre, O. et al. 2013, A&A, 559, 14; Le Fèvre, O. et al. 2014a, A&A, submitted, arXiv:1307.6518; Le Fèvre, O. et al. 2014b, A&A, submitted, arXiv:1403.3938; Lemaux, B. et al. 2014, submitted, arXiv:1403.4230; Lilly, S. J. et al. 2007, ApJS, 172, 70; Moster, B. P. et al. 2011, ApJ, 731, 113; Ouchi, M. et al. 2008, ApJS, 176, 301; Scodeggio, M. et al. 2005, PASP, 117, 1284; Scodeggio, M. et al. 2009, The Messenger, 135, 13; Scoville, N. et al. 2007, ApJS, 172, 1; Stark, D. et al. 2010, MNRAS, 408, 1628; Steidel, C. C. et al. 2003, ApJ, 592, 728; Tasca, L. et al. 2014, A&A, in press, arXiv:1303.4400; Vanzella, E. et al. 2009, ApJ, 695, 1163
42-46 (PDF)
A. Fontana et al.
When VLT Meets HST: The HUGS Survey

ADS BibCode:
2014Msngr.155...42F
Section:
Astronomical Science
Author(s)/Affiliation(s):
Fontana, A.; Dunlop, J. S.; Paris, D.; Targett, T.; Boutsia, K.; Castellano, M.; Galametz, A.; Grazian, A.; McLure, R.; Merlin, E.; Pentericci, L.; Wuyts, S.; Almaini, O.; Caputi, K.; Chary, R.-R.; Cirasuolo, M.; Conselice, C.; Cooray, A.; Daddi, E.; Dickinson, M.; Faber, S. M.; Fazio, G.; Ferguson, H.; Giallongo, E.; Giavalisco, M.; Grogin, N.; Hathi, N.; Koekemoer, A.; Koo, D. C.; Lucas, R.; Nonino, M.; Rix, H.-W.; Renzini, A.; Rosario, D.; Santini, P.; Scarlata, C.; Sommariva, V.; Stark, D. P.; van der Wel, A.; Vanzella, E.; Wild, V.; Yan, H.; Zibetti, S.
AA(INAF–Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy) AB(Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, UK) AC(INAF–Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy) AD(Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, UK; Department of Physics and Astronomy, Sonoma State University, Rohnert Park, USA) AE(INAF–Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy) AF(INAF–Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy) AG(INAF–Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy) AH(INAF–Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy) AI(Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, UK) AJ(INAF–Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy) AK(INAF–Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy) AL(Max-Planck-Institut fur extraterrestrische Physik, Garching, Germany) AM(The School of Physics and Astronomy, University of Nottingham, UK) AN(Kapteyn Astronomical Institute, University of Groningen, the Netherlands) AO(Spitzer Science Center, California Institute of Technology, Pasadena, USA) AP(Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, UK) AQ(The School of Physics and Astronomy, University of Nottingham, UK) AR(Department of Physics and Astronomy, University of California, Irvine, USA) AS(CEA-Saclay/DSM/DAPNIA/Service d’Astrophysique, Gif-sur-Yvette, France) AT(National Optical Astronomy Observatories, Tucson, USA) AU(UCO/Lick Observatory, Department of Astronomy and Astrophysics, University of California, Santa Cruz, USA) AV(Harvard–Smithsonian Center for Astrophysics, Cambridge, USA) AW(Space Telescope Science Institute, Baltimore, USA) AX(INAF–Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy) AY(Department of Astronomy, University of Massachusetts, Amherst, USA) AZ(Space Telescope Science Institute, Baltimore, USA) BA(Aix–Marseille Université, CNRS, Laboratoire d’Astrophysique de Marseille UMR 7326, Marseille, France) BB(Space Telescope Science Institute, Baltimore, USA) BC(UCO/Lick Observatory, Department of Astronomy and Astrophysics, University of California, Santa Cruz, USA) BD(Space Telescope Science Institute, Baltimore, USA) BE(INAF–Osservatorio Astronomico di Trieste, Italy) BF(Max Planck Institute for Astronomy, Heidelberg, Germany) BG(INAF–Osservatorio Astronomico di Padova, Italy) BH(Max-Planck-Institut fur extraterrestrische Physik, Garching, Germany) BI(INAF–Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy) BJ(Minnesota Institute of Astrophysics and School of Physics and Astronomy, University of Minnesota, Minneapolis, USA) BK(INAF–Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy; INAF–Osservatorio Astronomico di Bologna, Italy) BL(Department of Astronomy, Steward Observatory, University of Arizona, Tucson, USA) BM(Max Planck Institute for Astronomy, Heidelberg, Germany) BN(INAF–Osservatorio Astronomico di Bologna, Italy) BO(School of Physics and Astronomy, University of St. Andrews, United Kingdom; Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, UK) BP(Department of Physics and Astronomy, University of Missouri, Columbia, USA) BQ(INAF–Osservatorio Astrofisico di Arcetri, Firenze, Italy)
Abstract:
A new ultra-deep near-infrared imaging survey has been completed using the HAWK-I imager at the VLT. It is named HUGS (HAWK-I Ultra Deep Survey and GOODS Survey) and delivers the deepest, highest quality images ever collected in the K-band. HUGS complements the data delivered by the HST CANDELS survey over two well-studied extragalactic fields, and promises to open up exciting new opportunities to explore the highest redshift Universe. The survey is outlined and faint galaxy number counts and the search for passive galaxies in the early Universe are highlighted. The HUGS data have been completely analysed and are being made public to the worldwide community.
References:
Bruzual, G. & Charlot, S. 2003, MNRAS, 344, 1000; Castellano, M. et al. 2010, A&A, 511, A20; Castellano, M. et al. 2014, A&A, in press, arXiv:1403.0743; Daddi, E. et al. 2004, ApJ, 617, 746; Fontana, A. et al. 1999, A&A, 343, 19; Fontana, A. et al. 2000, AJ, 120, 2206; Fontana, A. et al. 2006, A&A, 459, 745; Fontana, A. et al. 2014, A&A, in press Heidt, J. et al. 2003, A&A, 398, 49; Kissler-Patig, M. et al. 2008, A&A, 491, 941; Illingworth, G. D. et al. 2013, ApJS, 209, 6; Laidler, V. G. et al. 2007, PASP, 119, 1325; Menci, N. et al. 2005, ApJ, 632, 49; Merson, A. I. et al. 2012, arXiv:1206.4049; Retzlaff, J. et al. 2010, A&A, 511, A50; Somerville, R. S. et al. 2012, MNRAS, 423, 1992; Sommariva, V. et al. 2014, A&A, submitted

Astronomical News

48-50 (PDF)
F. Comerón, T. de Zeeuw
Celebrating Fifty Years of ESO in Chile

ADS BibCode:
2014Msngr.155...48C
Section:
Astronomical News
Author(s)/Affiliation(s):
Comerón, F.; de Zeeuw, T.
AA(ESO) AB(ESO)
Abstract:
The fiftieth anniversary of the signing of the agreement between the Government of Chile and ESO to set up a new observatory occurred on 6 November 2013. The anniversary was marked by a formal occasion in Santiago, more informal celebrations at all the ESO sites in Chile and by visits from two European astronauts. A round-up of the anniversary events is presented.
References:
Blaauw, A. 1991, ESO’s Early History – The European Southern Observatory from Concept to Reality, (Garching: ESO) Madsen, C. 2012, The Jewel on the Mountaintop – The European Southern Observatory through Fifty Years, (Weinheim: Wiley-VCH) Sirey, R. 2012, The Messenger, 150, 7
51-54 (PDF)
D. A. Gadotti, R. Sánchez-Janssen
Report on the Workshop ''Deconstructing Galaxies: Structure and Morphology in the Era of Large Surveys''

ADS BibCode:
2014Msngr.155...51G
Section:
Astronomical News
Author(s)/Affiliation(s):
Gadotti, D. A.; Sánchez-Janssen, R.
AA(ESO) AB(NRC Herzberg Institute of Astrophysics, Canada)
Abstract:
Over 120 researchers — observers and theoreticians — gathered to present new results and discuss ongoing investigations on the structure of galaxies. The study of the structure and morphology of galaxies is one of the major tools that astronomers have to address how galaxies form and evolve. Recent progress in the field has enabled a boost in our understanding of the properties of the different structural components in nearby galaxies, as well as in galaxies at intermediate redshifts (z ~ 1–2).
55-57 (PDF)
J. R. de Medeiros et al.
Report on the Workshop ''400 Years of Stellar Rotation''

ADS BibCode:
2014Msngr.155...55M
Section:
Astronomical News
Author(s)/Affiliation(s):
de Medeiros, J. R.; Melo, C.; Pasquini, L.
AA(Departamento de Fisica, Universidad Federal do Rio Grande do Norte, Natal, Brazil) AB(ESO) AC(ESO)
Abstract:
The workshop marked the 400th anniversary of the observation of sunspots by Galileo and his deduction of the rotation of the Sun. The topics covered extensively both the theoretical and observational aspects of stellar rotation for stars of all types, from pre-main sequence to evolved stages, and including binary stars and stars hosting planets. A summary of the selected themes is presented.
References:
Molaro, P. 2012, AN, 333, 186; Righini, A. 2008, Galileo. Tra scienza fede e politica, (Bologna: Editrice Compositori)
57-59 (PDF)
S. Randall et al.
Report on the ALMA Community Days: Preparing for Cycle 2

ADS BibCode:
2014Msngr.155...57R
Section:
Astronomical News
Author(s)/Affiliation(s):
Randall, S.; Biggs, A.; Davis, T.; Lagos, C.; Stanke, T.; Testi, L.; Zwaan, M.
AA(ESO) AB(ESO) AC(ESO) AD(ESO) AE(ESO) AF(ESO) AG(ESO)
Abstract:
ALMA has now been obtaining scientific observations for the astronomical community for over two years. While commissioning is still continuing, the upcoming Cycle 2 should allow for nearly 2000 hours of science observations. The Cycle 2 ALMA Community Days, summarised here, were designed to optimally prepare the European ALMA Community for proposal submission and were held just a couple of weeks before the Cycle 2 deadline.
References:
Randall, S. et al. 2011, The Messenger, 144, 39; Randall, S. et al. 2012, The Messenger, 149, 47
60-61 (PDF)
D. Jones, K. Muzic
Fellows at ESO

ADS BibCode:
2014Msngr.155...60.
Section:
Astronomical News
Author(s)/Affiliation(s):
Jones, D.; Muzic, K.
AA(ESO) AB(ESO)
61-61 (PDF)
ESO
Personnel Movements

ADS BibCode:
2014Msngr.155...61.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)
62-62 (PDF)
ESO
ESO Studentship Programme 2014

ADS BibCode:
2014Msngr.155...62.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

Annual Index

64-67 (PDF)
ESO
Annual Index 2013 (Nos. 151–154)

ADS BibCode:
2014Msngr.155...64.
Section:
Annual Index
Author(s)/Affiliation(s):
ESO
AA(ESO)