ADS BibCode:
2013Msngr.154....2P
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Pasquini, L.; Casali, M.; Russell, A.
AA(ESO) AB(ESO) AC(ESO)
Abstract:
The development plan for instrumentation at the Paranal Observatory was presented to the ESO Scientific Technical Committee (STC) in April 2013. Its overall goal is to keep Paranal at the forefront of ground-based astronomy. In addition to the completion of the current second generation instruments, the installation of the Adaptive Optics Facility with the imager and spectrometer ERIS, and execution of the Very Large Telescope Interferometer (VLT/I) mid-term implementation plan, it will allow one new instrument, or instrument upgrade, to be initiated per year (provided current projects are completed). The plan is divided into two phases. Over 2013–2017, instruments are selected and developed with the criteria of filling the VLT capabilities and maintaining the balance between dedicated and general purpose facilities. Beyond 2018, the instruments will be deployed in the era of maturity of the European Extremely Large Telescope (E-ELT). The strategy for the second phase derives from analysis of VLT science in the E-ELT era, to be fully shaped in the coming five years. One new instrument is also proposed for the New Technology Telescope at La Silla, fully funded by the community.
References:
Cirasuolo, M. et al. 2011, The Messenger, 145, 11; de Jong, R. et al. 2011, The Messenger, 145, 14; Oliva, E. et al. 2012, Proc. SPIE, 84462N

ADS BibCode:
2013Msngr.154....7S
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Sánchez-Janssen, R.; Selman, F.; Mieske, S.; Bristow, P.; Hammersley, P.; Hilker, M.; Rejkuba, M.; Wolff, B.
AA(NRC Herzberg Institute of Astrophysics, Canada) AB(ESO) AC(ESO) AD(ESO) AE(ESO) AF(ESO) AG(ESO) AH(ESO)
Abstract:
Multi-object spectroscopic (MOS) observations with VIMOS have traditionally been limited to a narrow two-hour range from the meridian to minimise slit losses caused by atmospheric dispersion and differential refraction. We revisit the impact of these effects on the quality of VIMOS-MOS spectra through extensive simulations of slit losses. We show that MOS observations can be effectively extended to plus/minus three hours from the meridian for fields with zenith angles smaller than 20 degrees at culmination — provided a nonstandard rotator offset angle of 0 degrees is used. The increase in target observability will enhance the efficiency of operations, and hasten the completion of programmes — a particularly relevant aspect for the forthcoming spectroscopic public surveys with VIMOS.
References:
Bristow, P. et al. 2012, The Messenger, 148, 13; Cuby, J.-G. et al. 1998, Proc. SPIE Vol., 3355, 36; Hammersley, P. et al. 2012, The Messenger, 142, 8; Hammersley, P. et al. 2013, The Messenger, 151, 2; Le Fèvre, O. et al. 1998, Proc. SPIE Vol., 3355, 8

ADS BibCode:
2013Msngr.154...12M
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Mieske, S.; Baade, D.; Arnaboldi, M.; Carraro, G.; Dobrzycka, D.; Gabasch, A.; Gitton, Ph.; Haddad, N.; Hilker, M.; Holzlöhner, R.; Ivanov, V. D.; Morel, S.; Neeser, M.; Noethe, L.; Parra, R.; Parraguez, A.; Petr-Gotzens, M.; Rakich, A.; Rejkuba, M.; Riquelme, M.; Selman, F.; Schmutzer, R.; Szeifert, T.
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) AT(ESO) AU(ESO) AV(ESO) AW(ESO)
Abstract:
The science operations process of the VLT Survey Telescope (VST) camera, OmegaCAM, is described. OmegaCAM is a 267-megapixel CCD camera imaging a 1 × 1 degree field of view with a pixel scale of 0.21 arcseconds. It began operations in October 2011. The telescope and camera provide a survey speed that is five times greater than the now-decommissioned Wide Field Imager on the MPG/ESO 2.2-metre telescope at La Silla. OmegaCAM is currently used for three public surveys, guaranteed time observations for the OmegaCAM and VST consortia, and Chilean programmes. The execution of OmegaCAM observations, real-time quality control and the calibration plan are outlined.
References:
Baade, D. et al. 1999, The Messenger, 95, 15; Bierwirth, T. et al. 2010, SPIE, 7737E, 19; Capaccioli, M. & Schipani, P. 2011, The Messenger, 146, 2; Emerson, J. P. & Sutherland, W. 2010, SPIE, 7737E, 4; Hanuschik, R. W. et al. 2008, SPIE, 7016E, 22; Kuijken, K. 2002, The Messenger, 110, 15; Kuijken, K. 2011, The Messenger, 146, 8; Venemans, B. et al. 2013, ApJ, 779, 24; Wright, N. J. et al. 2013, MNRAS, in press, arXiv:1309.4086

ADS BibCode:
2013Msngr.154...18A
Section:
ESO Public Surveys
Author(s)/Affiliation(s):
Arnaboldi, M.; Rejkuba, M.; Retzlaff, J.; Delmotte, N.; Geier, S.; Hanuschik, R.; Hilker, M.; Hummel, W.; Hussain, G.; Ivanov, V. D.; Micol, A.; Mieske, S.; Neeser, M.; Petr-Gotzens, M.; Szeifert, T.
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)
Abstract:
In 2013 the eleven currently ongoing ESO public surveys successfully completed the submission and publication of their science data products via the ESO Science Archive Facility. An overview of the public survey projects in terms of telescope time allocation, observation progress and expected date of completion is presented. The science data products available in the ESO archive and their usage by the astronomical community are discussed with regard to the legacy value and scientific impact of these projects. This overview represents a natural introduction to the special section of the Messenger dedicated to the ESO public survey projects, in which the survey teams present their scientific aims and selected results in a series of dedicated articles.
References:
Arnaboldi, M. et al. 1998, The Messenger, 93, 30; Arnaboldi, M. et al. 2007, The Messenger, 127, 28; Arnaboldi, M. et al. 2011, The Messenger, 144, 17; Emerson, J., McPherson, A. & Sutherland, W. 2006, The Messenger, 126, 41; Kuijken, K. 2011, The Messenger, 146, 8

ADS BibCode:
2013Msngr.154...23C
Section:
ESO Public Surveys
Author(s)/Affiliation(s):
Cioni, M.-R. L.; Anders, P.; Bagheri, G.; Bekki, K.; Clementini, G.; Emerson, J.; Evans, C. J.; For, B.-Q.; de Grijs, R.; Gibson, B.; Girardi, L.; Groenewegen, M. A. T.; Guandalini, R.; Gullieuszik, M.; Ivanov, V. D.; Kamath, D.; Marconi, M.; Marquette, J.-B.; Miszalski, B.; Moore, B.; Moretti, M. I.; Muraveva, T.; Napiwotzki, R.; Oliveira, J. M.; Piatti, A. E.; Ripepi, V.; Romita, K.; Rubele, S.; Sturm, R.; Tatton, B.; van Loon, J. Th.; Wilkinson, M. I.; Wood, P. R.; Zaggia, S.
AA(University of Hertfordshire, United Kingdom; Leibniz-Institut für Astrophysik Potsdam, Germany) AB(National Astronomical Observatory of China, China) AC(University of Hertfordshire, United Kingdom) AD(ICRAR, University of Western Australia, Australia) AE(INAF, Osservatorio Astronomico di Bologna, Italy) AF(Queen Mary University London, United Kingdom) AG(Astronomy Technology Centre, Edinburgh, United Kingdom) AH(ICRAR, University of Western Australia, Australia) AI(Peking University, China) AJ(University of Central Lancashire, United Kingdom) AK(INAF, Osservatorio Astronomico di Padova, Italy) AL(Royal Observatory of Belgium, Belgium) AM(Institute of Astronomy, KU Leuven, Belgium) AN(INAF, Osservatorio Astronomico di Padova, Italy) AO(ESO) AP(Institute of Astronomy, KU Leuven, Belgium) AQ(INAF, Osservatorio Astronomico di Capodimonte, Italy) AR(Institut d’Astrophysique de Paris, France) AS(South African Astronomical Observatory, Cape Town, South Africa) AT(University of Zurich, Switzerland) AU(INAF, Osservatorio Astronomico di Capodimonte, Italy) AV(INAF, Osservatorio Astronomico di Bologna, Italy) AW(University of Hertfordshire, United Kingdom) AX(Lennard-Jones Laboratories, Keele University, United Kingdom) AY(Observatorio Astronómico, Universidad National de Córdoba, Argentina) AZ(INAF, Osservatorio Astronomico di Capodimonte, Italy) BA(University of Florida, USA) BB(INAF, Osservatorio Astronomico di Padova, Italy) BC(Max-Planck-Institut für extraterrestrische Physik, Germany) BD(Lennard-Jones Laboratories, Keele University, United Kingdom) BE(Lennard-Jones Laboratories, Keele University, United Kingdom) BF(University of Leicester, United Kingdom) BG(Australian National University, Australia) BH(INAF, Osservatorio Astronomico di Padova, Italy)
Abstract:
The VISTA near-infrared YJKs survey of the Magellanic Clouds system (VMC) has entered its core phase: about 50% of the observations across the Large and Small Magellanic Clouds (LMC, SMC), the Magellanic Bridge and Stream have already been secured and the data are processed and analysed regularly. The initial analyses, concentrated on the first two completed tiles in the LMC (including 30 Doradus and the South Ecliptic Pole), show the superior quality of the data. The photometric depth of the VMC survey allows the derivation of the star formation history (SFH) with unprecedented quality compared to previous wide-area surveys, while reddening maps of high angular resolution are constructed using red clump stars. The multi-epoch Ks-band data reveal tight period–luminosity relations for variable stars and permit the measurement of accurate proper motions of the stellar populations. The VMC survey continues to acquire data that will address many issues in the field of star and galaxy evolution.
References:
Cioni, M.-R. L. et al. 2011, A&A, 527, A116, Paper I Cioni, M.-R. L. et al. 2013a, A&A, 549, A29, Paper VI Cioni, M.-R. L. et al. 2013b, A&A, accepted, Paper IX Gullieuszik, M. et al. 2012, A&A, 537, A105, Paper III Miszalski, B. et al. 2011, A&A, 531, A157, Paper II Moretti, M. I. et al. 2013, A&A, accepted, Paper X Ripepi, V. et al. 2012, MNRAS, 424, 1807, Paper V Ripepi, V. et al. 2013, MNRAS, accepted, Paper VIII Rubele, S. et al. 2012, A&A, 537, A106, Paper IV Tatton, B. et al. 2013, A&A, 554, A33, Paper VII

ADS BibCode:
2013Msngr.154...26J
Section:
ESO Public Surveys
Author(s)/Affiliation(s):
Jarvis, M. J.; Häußler, B.; McAlpine, K.
AA(Astrophysics, Department of Physics, Oxford, United Kingdom; Physics Department, University of the Western Cape, Bellville, South Africa) AB(Astrophysics, Department of Physics, Oxford, United Kingdom; Centre for Astrophysics, Science & Technology Research Institute, University of Hertfordshire, Hatfield, United Kingdom) AC(Physics Department, University of the Western Cape, Bellville, South Africa)
Abstract:
The VIDEO survey is designed to answer key questions regarding the formation and evolution of galaxies, in particular the role of accretion onto black holes and how galaxy evolution may vary depending on environment. VIDEO undertakes deep near-infrared imaging over three well-observed extragalactic fields allowing in-depth study of galaxy evolution over 1 < z < 4, linking the shallower VST and VISTA surveys with the UltraVISTA survey. The area and depth of the VIDEO survey enables the detection of the bulk of the luminosity density arising from galaxies over 90% of the history of the Universe, as well as the most massive galaxies at all epochs and any associated accretion activity. A few scientific highlights from the early VIDEO data are provided.
References:
Ilbert, O. et al. 2006, A&A, 457, 841; Jarvis, M. J. 2012, African Skies, 16, 44; Jarvis, M. J. et al. 2013, MNRAS, 428, 1281; Karouzos, M., Jarvis, M. J. & Bonfield, D. G. 2013, MNRAS, submitted Le Fèvre, O. et al. 2013, A&A, 55, 14; Mauch, T. & Sadler, E. M. 2007, MNRAS, 375, 931; Mauduit, J.-C. et al. 2012, PASP, 124, 714; McAlpine, K., Jarvis, M. J. & Bonfield, D. G. 2013, MNRAS, 436, 1084; Oliver, S. et al. 2012, MNRAS, 424, 1614; Willott, C. J. et al. 2013, AJ, 145, 4

ADS BibCode:
2013Msngr.154...29M
Section:
ESO Public Surveys
Author(s)/Affiliation(s):
McCracken, H. J.; Milvang-Jensen, B.; Dunlop, J.; Franx, M.; Fynbo, J. P. U.; Le Fèvre, O.; Holt, J.; Caputi, K. I.; Goranova, Y.; Buitrago, F.; Emerson, J.; Freudling, W.; Herent, O.; Hudelot, P.; López-Sanjuan, C.; Magnard, F.; Muzzin, A.; Mellier, Y.; Møller, P.; Nilsson, K. K.; Sutherland, W.; Tasca, L.; Zabl, J.
AA(Institut d’Astrophysique de Paris, UMR7095 CNRS, Université Pierre et Marie Curie, Paris, France) AB(Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Denmark) AC(SUPA, Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, United Kingdom) AD(Leiden Observatory, Leiden University, the Netherlands) AE(Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Denmark) AF(Laboratoire d’Astrophysique de Marseille, Aix-Marseille Université, France) AG(Leiden Observatory, Leiden University, the Netherlands) AH(SUPA, Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, United Kingdom; Kapteyn Astronomical Institute, University of Groningen, the Netherlands) AI(Institut d’Astrophysique de Paris, UMR7095 CNRS, Université Pierre et Marie Curie, Paris, France) AJ(SUPA, Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, United Kingdom) AK(Astronomy Unit, School of Physics and Astronomy, Queen Mary University of London, United Kingdom) AL(ESO) AM(Institut d’Astrophysique de Paris, UMR7095 CNRS, Université Pierre et Marie Curie, Paris, France) AN(Institut d’Astrophysique de Paris, UMR7095 CNRS, Université Pierre et Marie Curie, Paris, France) AO(Laboratoire d’Astrophysique de Marseille, Aix-Marseille Université, France) AP(Institut d’Astrophysique de Paris, UMR7095 CNRS, Université Pierre et Marie Curie, Paris, France) AQ(Leiden Observatory, Leiden University, the Netherlands) AR(Institut d’Astrophysique de Paris, UMR7095 CNRS, Université Pierre et Marie Curie, Paris, France) AS(ESO) AT(Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Denmark) AU(Astronomy Unit, School of Physics and Astronomy, Queen Mary University of London, United Kingdom) AV(Laboratoire d’Astrophysique de Marseille, Aix-Marseille Université, France) AW(Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Denmark)
Abstract:
Large samples of distant galaxies covering degree-scale areas are an unparalleled source of information concerning the first sources that ionised the Universe and the origin of cosmic structures. The UltraVISTA public survey, using the unique capabilities of the VISTA telescope, aims to assemble a unique sample of remote, very high-redshift galaxies. The characteristics of the first UltraVISTA data release (DR1) and the upcoming DR2 data products are described. The DR1 data, comprising just a few months of observing time, already equals or exceeds in depth all previous wide-field near-infrared images taken on the COSMOS field in the last decade. The first scientific results from UltraVISTA are presented, including new measurements of the high redshift (z ~ 7) galaxy luminosity function and an accurate determination of the type-dependent galaxy stellar mass function from z ~ 0 to z ~ 4. DR2 will reach one to two magnitudes deeper in all bands and provide our clearest picture of the structure and composition of the Universe at high redshifts.
References:
Bowler, R. A. A. et al. 2012, MNRAS, 426, 2772; Ilbert, O. et al. 2013, A&A, 556, A55; McCracken, H. J. et al. 2012, A&A, 544, A156; Milvang-Jensen, B. et al. 2013, arXiv:1305.0262; Muzzin, A. et al. 2013, ApJ, in press, arXiv:1303.4409; Scoville, N. et al. 2007, ApJS, 172, 1

ADS BibCode:
2013Msngr.154...32E
Section:
ESO Public Surveys
Author(s)/Affiliation(s):
Edge, A.; Sutherland, W.; Kuijken, K.; Driver, S.; McMahon, R.; Eales, S.; Emerson, J. P.
AA(Deptartment of Physics, University of Durham, United Kingdom) AB(Astronomy Unit, School of Physics and Astronomy, Queen Mary University of London, United Kingdom) AC(Leiden Observatory, Leiden University, the Netherlands) AD(ICRAR, University of Western Australia, Crawley, Australia; SUPA — School of Physics and Astronomy, University of St. Andrews, United Kingdom) AE(Institute of Astronomy, University of Cambridge, United Kingdom) AF(School of Physics and Astronomy, Cardiff University, United Kingdom) AG(Astronomy Unit, School of Physics and Astronomy, Queen Mary University of London, United Kingdom)
Abstract:
VIKING is a medium-deep survey of 1500 square degrees over two areas of the extragalactic sky with VISTA in zYJHKs bands to sample the restframe optical for galaxies at z >~ 1. VIKING complements the two other surveys — VHS with its large area but shallower depth and VIDEO with its greater photometric depth and smaller spatial coverage. In addition to a 0.7 < z < 2 galaxy survey, the area and depth of VIKING enables other studies, such as detection of distant quasars and low-mass stars and many galaxy clusters and superclusters. The early results are summarised and future prospects presented.
References:
Andrews, S. K. et al. 2013, PASA, submitted Burton, C. S. et al. 2013, MNRAS, 433, 771; Eisenhardt, P. R. M. et al. 2012, ApJ, 755, 173; Eke, V. R., Cole, S. & Frenk, C. S. 1996, MNRAS, 282, 263; Fleuren, S. et al. 2012, MNRAS, 423, 2470; González-Nuevo, J. et al. 2012, ApJ, 749, 65; Kim, J.-W. et al. 2011, MNRAS, 410, 241; Marriage, T. A. et al. 2011, ApJ, 737, 61; Mehrtens, N. et al. 2012, MNRAS, 423, 1024; Mortlock, D. J. et al. 2011, Nature, 474, 616; Predehl, P. et al. 2009, AIPC, 1248, 543; Stanford, S. A. et al. 2012, ApJ, 753, 164; Venemans, B. et al. 2013, ApJ, 779, 24; Wilson, G. et al. 2009, ApJ, 698, 1943

ADS BibCode:
2013Msngr.154...35M
Section:
ESO Public Surveys
Author(s)/Affiliation(s):
McMahon, R. G.; Banerji, M.; Gonzalez, E.; Koposov, S. E.; Bejar, V. J.; Lodieu, N.; Rebolo, R.; and the VHS collaboration
AA(Institute of Astronomy, University of Cambridge, United Kingdom; Kavli Institute for Cosmology, University of Cambridge, United Kingdom) AB(Institute of Astronomy, University of Cambridge, United Kingdom; Department of Physics and Astronomy, University College London, United Kingdom) AC(Institute of Astronomy, University of Cambridge, United Kingdom) AD(Institute of Astronomy, University of Cambridge, United Kingdom) AE(Instituto de Astrofisica de Canarias, La Laguna, Tenerife, Spain; Departamento de Astrofisica, Universidad de La Laguna, Tenerife, Spain) AF(Instituto de Astrofisica de Canarias, La Laguna, Tenerife, Spain; Departamento de Astrofisica, Universidad de La Laguna, Tenerife, Spain) AG(Instituto de Astrofisica de Canarias, La Laguna, Tenerife, Spain; Departamento de Astrofisica, Universidad de La Laguna, Tenerife, Spain)
Abstract:
The first Galactic and extragalactic results from the VISTA Hemisphere Survey (VHS) are presented. The aim of the VHS is to carry out a near-infrared survey which, when combined with other VISTA public surveys, will result in coverage of the whole southern celestial hemisphere (~20 000 square degrees) to a depth 30 times fainter than the Two Micron All Sky Survey in at least two wavebands (J and Ks). The VHS vision includes a deep optical survey over the same area and this is now being realised with the VST surveys and the Dark Energy Survey, which has recently started. A summary of the survey progress is presented, with some follow-up results on low-mass stars and high-redshift quasars.
References:
Banerji, M. et al. 2013, MNRAS, 429, L55; Cross, N. J. et al. 2012, A&A, 548, A119; Gauza, B. et al. 2012, MNRAS, 427, 2457; Irwin, M. J. et al. 2004, SPIE, 5493, 411; Lewis, J. R., Irwin, M. J. & Bunclark, P. S. 2010, ASP Conf. Ser., 434, 91; Lodieu, N. et al. 2012, A&A, 548, A53; Roeser, S. et al. 2010, AJ, 139, 2440; Skrutskie, M. F. et al. 2006, AJ, 131, 1163; Wright, E. L. et al. 2010, AJ, 140, 1868

ADS BibCode:
2013Msngr.154...38S
Section:
ESO Public Surveys
Author(s)/Affiliation(s):
Shanks, T.; Belokurov, V.; Chehade, B.; Croom, S. M.; Findlay, J. R.; Gonzalez-Solares, E.; Irwin, M. J.; Koposov, S.; Mann, R. G.; Metcalfe, N.; Murphy, D. N. A.; Norberg, P. R.; Read, M. A.; Sutorius, E.; Worseck, G.
AA(Department of Physics, Durham University, United Kingdom) AB(Cambridge Astronomical Surveys Unit, Cambridge, United Kingdom) AC(Department of Physics, Durham University, United Kingdom) AD(School of Physics, University of Sydney, Australia) AE(Department of Physics, Durham University, United Kingdom) AF(Cambridge Astronomical Surveys Unit, Cambridge, United Kingdom) AG(Cambridge Astronomical Surveys Unit, Cambridge, United Kingdom) AH(Cambridge Astronomical Surveys Unit, Cambridge, United Kingdom) AI(Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, United Kingdom) AJ(Department of Physics, Durham University, United Kingdom) AK(Instituto de Astrofísica, Universidad Catolica de Chile, Chile) AL(ICC, Department of Physics, Durham University, United Kingdom) AM(Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, United Kingdom) AN(Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, United Kingdom) AO(Max-Planck-Institut für Astronomie, Heidelberg, Germany)
Abstract:
The VST ATLAS is a ugriz-imaging survey targeting ~ 4500 square degrees of the southern sky. It reaches similar magnitude limits to the Sloan Digital Sky Survey in the north, i.e., r ~ 22.5, but ATLAS has better median seeing of 1 arcsecond full width half maximum. ATLAS is a companion survey to the VISTA Hemisphere Survey, which supplies YJHK imaging over much of its area. In addition, the Wide-field Infrared Survey Explorer (WISE) satellite supplies a further four mid-infrared bands. Together these surveys complement each other and provide excellent multi-wavelength data for both Galactic and extragalactic science projects.
References:
Driver, S. P. et al. 2011, MNRAS, 413, 971; Geach, J. E., Murphy, D. N. A. & Bower, R. G. 2011, MNRAS, 413, 3059; Murphy, D. N. A., Geach, J. E. & Bower, R. G. 2012, MNRAS, 420, 1861; Robotham, A. S. G. et al. 2011, MNRAS, 416, 2640; Sawangwit, U. et al. 2010, MNRAS, 402, 2228; Worseck, G. & Prochaska, J. X. 2011, ApJ, 728, 23; Worseck, G. et al. 2011, ApJ, 733, L24

ADS BibCode:
2013Msngr.154...41D
Section:
ESO Public Surveys
Author(s)/Affiliation(s):
Drew, J. E.; Barentsen, G.; Fabregat, J.; Farnhill, H.; Mohr-Smith, M.; Wright, N. J.; Gonzalez-Solares, E.; Irwin, M. J.; Lewis, J.; Yoldas, A. K.; Greimel, R.; Eislöffel, J.; Groot, P.; Barlow, M. J.; Corradi, R.; Gänsicke, B. T.; Knigge, C.; Mampaso, A.; Morris, R.; Naylor, T.; Parker, Q. A.; Raddi, R.; Sale, S. E.; Steeghs, D.; Unruh, Y. C.; Vink, J. S.; Walsh, J. R.; Walton, N. A.; Wesson, R.; Zijlstra, A.
AA(School of Physics, Astronomy & Mathematics, University of Hertfordshire, Hatfield, United Kingdom) AB(School of Physics, Astronomy & Mathematics, University of Hertfordshire, Hatfield, United Kingdom) AC(Observatorio Astronómico, Universidad de Valencia, Paterna, Spain) AD(School of Physics, Astronomy & Mathematics, University of Hertfordshire, Hatfield, United Kingdom) AE(School of Physics, Astronomy & Mathematics, University of Hertfordshire, Hatfield, United Kingdom) AF(School of Physics, Astronomy & Mathematics, University of Hertfordshire, Hatfield, United Kingdom) AG(Institute of Astronomy, Cambridge University, United Kingdom) AH(Institute of Astronomy, Cambridge University, United Kingdom) AI(Institute of Astronomy, Cambridge University, United Kingdom) AJ(Institute of Astronomy, Cambridge University, United Kingdom) AK(IGAM, Institute of Physics, University of Graz, Austria) AL(Thüringer Landessternwarte, Tautenburg, Germany) AM(Afdeling Sterrenkunde, Radboud Universiteit Nijmegen, the Netherlands) AN(Department of Physics & Astronomy, University College London, United Kingdom) AO(Instituto de Astrofisica de Canarias, La Laguna, Tenerife, Spain) AP(Department of Physics, University of Warwick, Coventry, United Kingdom) AQ(School of Physics & Astronomy, University of Southampton, United Kingdom) AR(Instituto de Astrofisica de Canarias, La Laguna, Tenerife, Spain) AS(School of Physics, Bristol University, United Kingdom) AT(Department of Physics, University of Exeter, United Kingdom) AU(Department of Physics, Macquarie University, NSW 2109, Australia) AV(Department of Physics, University of Warwick, Coventry, United Kingdom) AW(Rudolf Peierls Centre for Theoretical Physics, Oxford University, United Kingdom) AX(Department of Physics, University of Warwick, Coventry, United Kingdom) AY(Department of Physics, Blackett Laboratory, Imperial College London, United Kingdom) AZ(Armagh Observatory, College Hill, Northern Ireland, United Kingdom) BA(ESO) BB(Institute of Astronomy, Cambridge University, United Kingdom) BC(ESO) BD(Jodrell Bank Centre for Astrophysics, School of Physics & Astronomy, University of Manchester, United Kingdom)
Abstract:
The VST Photometric H-alpha survey of the Southern Galactic Plane and Bulge (VPHAS+) is collecting single-epoch Sloan u, g, r, i and H-alpha narrowband photometry, at arcsecond resolution, down to point-source (Vega) magnitudes of ~ 21. The survey footprint encloses the entire southern Galactic Plane within the Galactic latitude range −5° < b < +5°, expanding to b = ±10° in the Galactic Bulge. This brief description of VPHAS+ includes sample data and examples of early science validation.
References:
Berry, M. et al. 2012, ApJ, 757, 166; Drew, J. E. et al. 2005, MNRAS, 362, 753; Groot, P. J. et al. 2009, MNRAS, 400, 1413; Guenther, E. W. et al. 2012, A&A, 543, A125; Parker, Q. A. et al. 2005, MNRAS, 362, 689; Sale, S. E. et al. 2009, MNRAS, 392, 497; Sale, S. E. 2012, MNRAS, 427, 2119; Sebastian, D. et al. 2012, A&A, 541, A34; Vargas Alvarez, C. A. et al. 2013, AJ, 145, 125

ADS BibCode:
2013Msngr.154...44J
Section:
ESO Public Surveys
Author(s)/Affiliation(s):
de Jong, J. T. A.; Kuijken, K.; Applegate, D.; Begeman, K.; Belikov, A.; Blake, C.; Bout, J.; Boxhoorn, D.; Buddelmeijer, H.; Buddendiek, A.; Cacciato, M.; Capaccioli, M.; Choi, A.; Cordes, O.; Covone, G.; Dall’Ora, M.; Edge, A.; Erben, T.; Franse, J.; Getman, F.; Grado, A.; Harnois-Deraps, J.; Helmich, E.; Herbonnet, R.; Heymans, C.; Hildebrandt, H.; Hoekstra, H.; Huang, Z.; Irisarri, N.; Joachimi, B.; Köhlinger, F.; Kitching, T.; La Barbera, F.; Lacerda, P.; McFarland, J.; Miller, L.; Nakajima, R.; Napolitano, N. R.; Paolillo, M.; Peacock, J.; Pila-Diez, B.; Puddu, E.; Radovich, M.; Rifatto, A.; Schneider, P.; Schrabback, T.; Sifon, C.; Sikkema, G.; Simon, P.; Sutherland, W.; Tudorica, A.; Valentijn, E.; van der Burg, R.; van Uitert, E.; van Waerbeke, L.; Velander, M.; Kleijn, G. V.; Viola, M.; Vriend, W.-J.
AA(Leiden Observatory, Leiden University, the Netherlands) AB(Leiden Observatory, Leiden University, the Netherlands) AC(Argelander Institute for Astronomy, University of Bonn, Germany) AD(OmegaCEN – University of Groningen, the Netherlands) AE(OmegaCEN – University of Groningen, the Netherlands) AF(Centre for Astrophysics & Supercomputing, Swinburne University, Hawthorn, Australia) AG(OmegaCEN – University of Groningen, the Netherlands) AH(OmegaCEN – University of Groningen, the Netherlands) AI(OmegaCEN – University of Groningen, the Netherlands) AJ(Argelander Institute for Astronomy, University of Bonn, Germany) AK(Leiden Observatory, Leiden University, the Netherlands) AL(Dept. of Physical Sciences, University Federico II, Naples, Italy) AM(SUPA, Institute for Astronomy, University of Edinburgh, United Kingdom) AN(Argelander Institute for Astronomy, University of Bonn, Germany) AO(Dept. of Physical Sciences, University Federico II, Naples, Italy) AP(INAF – Osservatorio Astronomico Capodimonte Napoli, Italy) AQ(Department of Physics, Durham University, United Kingdom) AR(Argelander Institute for Astronomy, University of Bonn, Germany) AS(Leiden Observatory, Leiden University, the Netherlands) AT(INAF – Osservatorio Astronomico Capodimonte Napoli, Italy) AU(INAF – Osservatorio Astronomico Capodimonte Napoli, Italy) AV(Department of Physics and Astronomy, University of British Columbia, Vancouver, Canada) AW(Leiden Observatory, Leiden University, the Netherlands) AX(Leiden Observatory, Leiden University, the Netherlands) AY(SUPA, Institute for Astronomy, University of Edinburgh, United Kingdom) AZ(Argelander Institute for Astronomy, University of Bonn, Germany) BA(Leiden Observatory, Leiden University, the Netherlands) BB(INAF – Osservatorio Astronomico Capodimonte Napoli, Italy) BC(Leiden Observatory, Leiden University, the Netherlands) BD(Department of Physics and Astronomy, University College London, United Kingdom) BE(Leiden Observatory, Leiden University, the Netherlands) BF(Mullard Space Science Laboratory, Holmbury St Mary, Dorking, United Kingdom) BG(INAF – Osservatorio Astronomico Capodimonte Napoli, Italy) BH(Queen’s University Belfast, United Kingdom) BI(OmegaCEN – University of Groningen, the Netherlands) BJ(Department of Physics, University of Oxford, United Kingdom) BK(Argelander Institute for Astronomy, University of Bonn, Germany) BL(INAF – Osservatorio Astronomico Capodimonte Napoli, Italy) BM(Dept. of Physical Sciences, University Federico II, Naples, Italy) BN(SUPA, Institute for Astronomy, University of Edinburgh, United Kingdom) BO(Leiden Observatory, Leiden University, the Netherlands) BP(INAF – Osservatorio Astronomico Capodimonte Napoli, Italy) BQ(INAF – Osservatorio Astronomico di Padova, Italy) BR(INAF – Osservatorio Astronomico Capodimonte Napoli, Italy) BS(Argelander Institute for Astronomy, University of Bonn, Germany) BT(Argelander Institute for Astronomy, University of Bonn, Germany) BU(Leiden Observatory, Leiden University, the Netherlands) BV(OmegaCEN – University of Groningen, the Netherlands) BW(Argelander Institute for Astronomy, University of Bonn, Germany) BX(Astronomy Unit, School of Physics and Astronomy, Queen Mary University of London, United Kingdom) BY(Argelander Institute for Astronomy, University of Bonn, Germany) BZ(OmegaCEN – University of Groningen, the Netherlands) CA(Leiden Observatory, Leiden University, the Netherlands) CB(Argelander Institute for Astronomy, University of Bonn, Germany) CC(Department of Physics and Astronomy, University of British Columbia, Vancouver, Canada) CD(Department of Physics, University of Oxford, United Kingdom) CE(OmegaCEN – University of Groningen, the Netherlands) CF(Leiden Observatory, Leiden University, the Netherlands) CG(OmegaCEN – University of Groningen, the Netherlands)
Abstract:
The Kilo-Degree Survey (KiDS), a 1500-square-degree optical imaging survey with the recently commissioned OmegaCAM wide-field imager on the VLT Survey Telescope (VST), is described. KiDS will image two fields in u-,g-,r- and i-bands and, together with the VIKING survey, produce nine-band (u- to K-band) coverage over two fields. For the foreseeable future the KiDS/VIKING combination of superb image quality with wide wavelength coverage will be unique for surveys of its size and depth. The survey has been designed to tackle some of the most fundamental questions of cosmology and galaxy formation of today. The main science driver is mapping the dark matter distribution in the Universe and putting constraints on the expansion of the Universe and the equation of state of dark energy, all through weak gravitational lensing. However, the deep and wide imaging data will facilitate a wide variety of science cases.
References:
Abazajian, K. et al. 2009, ApJS, 182, 543; Belokurov, V. et al. 2006, ApJ, 642, L137; de Jong, J. T. A. et al. 2013, ExA, 35, 25; Driver, S. P. et al. 2011, MNRAS, 413, 971; Erben, T. et al. 2013, MNRAS, 433, 2545; Heymans, C. et al. 2012, MNRAS, 427, 146; McFarland, J. P. et al. 2013, ExA, 35, 45; Peacock, J. A. et al. 2006, ESO/ESA Working Group Report No. 3; Fundamental Cosmology van Daalen, M. P. et al. 2011, MNRAS, 415, 3649; Venemans, B. et al. 2013, ApJ, 779, 24; Verdoes Kleijn, G. et al. 2013, ExA, 35, 103

ADS BibCode:
2013Msngr.154...47R
Section:
ESO Public Surveys
Author(s)/Affiliation(s):
Randich, S.; Gilmore, G.; on behalf of the Gaia–ESO Consortium
AA(INAF–Osservatorio Astrofisico di Arcetri, Italy) AB(Institute of Astronomy, University of Cambridge, United Kingdom)
Abstract:
The Gaia–ESO Public Spectroscopic Survey has completed about one third of the data taking and continues to acquire high-quality spectroscopy, with both Giraffe and UVES, of representative samples of all Galactic stellar populations, including open clusters — young and old, nearby and distant, interior and exterior to the Sun — and field stars in the Galactic Halo, the thick Disc, the thin Disc and the Galactic Bulge. A large sample of stars in the Solar Neighbourhood, selected to include all possible ages and metallicities, is also being observed with UVES. This will be the first such large internally homogeneous study of the Milky Way stellar populations. Besides the intrinsic range of exciting scientific results, the Gaia–ESO Survey is also a pathfinder for future massive Gaia follow-up. Equally importantly, we are building an ESO-wide community of stellar spectroscopists, sharing, optimising, refining and cross-calibrating complementary approaches, strengths and experience. Internal Science Verification (SV) has started with several results demonstrating the huge potential of the survey and the first release of spectra to ESO has occurred.
References:
De Silva, G. M. et al. 2007, AJ, 133, 1161; Gilmore, G. et al. 2012, The Messenger, 147, 25; Jofre, P. et al. 2013, arXiv:1309.1099; Magrini, L. et al. 2013, A&A, submitted Recio-Blanco, A. et al. 2013, A&A, submitted Yong, D., Carney, B. W. & Teixera de Almeida, M. L. 2005, AJ, 130, 597; Yong, D., Carney, B. W. & Friel, E. D. 2012, AJ, 144, 95

ADS BibCode:
2013Msngr.154...50S
Section:
ESO Public Surveys
Author(s)/Affiliation(s):
Smartt, S. J.; Valenti, S.; Fraser, M.; Inserra, C.; Young, D. R.; Sullivan, M.; Benetti, S.; Gal-Yam, A.; Knapic, C.; Molinaro, M.; Pastorello, A.; Smareglia, R.; Smith, K. W.; Taubenberger, S.; Yaron, O.
AA(Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, United Kingdom) AB(Osservatorio Astronomico di Padova, INAF, Italy; Las Cumbres Observatory Global Telescope Network, Goleta, USA; Department of Physics, University of California Santa Barbara, USA) AC(Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, United Kingdom; Institute of Astronomy, University of Cambridge, United Kingdom) AD(Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, United Kingdom) AE(Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, United Kingdom) AF(School of Physics and Astronomy, University of Southampton, United Kingdom) AG(Osservatorio Astronomico di Padova, INAF, Italy) AH(Benoziyo Center for Astrophysics, Weizmann Institute of Science, Rehovot, Israel) AI(INAF–Osservatorio Astronomico di Trieste, Italy) AJ(INAF–Osservatorio Astronomico di Trieste, Italy) AK(Osservatorio Astronomico di Padova, INAF, Italy) AL(INAF–Osservatorio Astronomico di Trieste, Italy) AM(Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, United Kingdom) AN(Max-Planck-Institut für Astrophysik, Garching, Germany) AO(Benoziyo Center for Astrophysics, Weizmann Institute of Science, Rehovot, Israel)
Abstract:
PESSTO, which began in April 2012 as one of two ESO public spectroscopic surveys, uses the EFOSC2 and SOFI instruments on the New Technology Telescope during ten nights a month for nine months of the year. Transients for PESSTO follow-up are provided by dedicated large-field 1–2-metre telescope imaging surveys. In its first year PESSTO classified 263 optical transients, publicly released the reduced spectra within 12 hours of the end of the night and identified 33 supernovae (SNe) for dedicated follow-up campaigns. Nine papers have been published or submitted on the topics of supernova progenitors, the origins of type ia SNe, the uncertain nature of faint optical transients and superluminous supernovae, and a definitive public dataset on a most intriguing supernova, the infamous SN2009ip.
References:
Benetti, S. et al. 2013, MNRAS, submitted, arXiv:1310.1311; Childress, M. J. et al. 2013, ApJ, 770, 29; Fraser, M. et al. 2013, MNRAS, 433, 1312; Inserra, C. et al. 2013, MNRAS, in press, arXiv:1307.1791; Maguire, K. et al. 2013, MNRAS, 436, 222; Maund, J. R. et al. 2013, MNRAS, 431, 102; Pastorello, A. et al. 2013, ApJ, 767, 1; Smartt, S. J. et al. 2013, A&A, in prep. Valenti, S. et al. 2013a, MNRAS, in press, arXiv:1302.2983; Valenti, S. et al. 2013b, MNRAS, in press, arXiv:1309.4269

ADS BibCode:
2013Msngr.154...54W
Section:
Astronomical Science
Author(s)/Affiliation(s):
Wegg, C.; Gerhard, O.
AA(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AB(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany)
Abstract:
A three-dimensional map of the density of red clump giant stars (RCGs) in the Galactic Bulge has been produced from the Data Release 1 of the ESO public survey VISTA Variables in the Via Lactea Survey (VVV). From the magnitude distributions of the RCGs we infer line-of-sight densities and, because the VVV survey has good Bulge coverage, we can combine many line-of-sight density measurements into a complete three-dimensional (3D) map. The 3D density shows a prominent peanut shape when viewed from the side, which appears very similar to simulations of barred galaxies after the bar has buckled, and some edge-on barred spiral galaxies.
References:
Alard, C. 2001, A&A, 379, L44; Böker, T. et al. 1999, ApJS, 124, 95; Combes, F. & Sanders, R. H. 1981, A&A, 96, 164; Gonzalez, O. A. et al. 2013, The Messenger, 152, 23; Lutticke, R., Dettmar, R. J. & Pohlen, M. 2000, ApJS, 145, 405; McWilliam, A. & Zoccali, M. 2010, ApJ, 724, 1491; Martinez-Valpuesta, I., Shlosman, I. & Heller, C. 2006, ApJ, 637, 214; Ness, M. et al. 2013, MNRAS, 432, 2092; Rich, R. M. 2013, in Planets, Stars and Stellar Systems. Volume 5: Galactic Structure and Stellar Populations, Springer Netherlands, Dordrecht, 271; Wegg, C. & Gerhard, O. 2013, MNRAS, 435, 1874

ADS BibCode:
2013Msngr.154...57B
Section:
Astronomical Science
Author(s)/Affiliation(s):
Birkby, J.; de Kok, R.; Brogi, M.; Schwarz, H.; Albrecht, S.; de Mooij, E.; Snellen, I.
AA(Leiden Observatory, the Netherlands) AB(SRON, Netherlands Institute for Space Research, Utrecht, the Netherlands) AC(Leiden Observatory, the Netherlands) AD(Leiden Observatory, the Netherlands) AE(Department of Physics, Massachusets Institute of Technology, Cambridge, USA) AF(Department of Astronomy and Astrophysics, University of Toronto, Canada) AG(Leiden Observatory, the Netherlands)
Abstract:
The search for signs of life elsewhere in the Universe requires the remote detection of molecules in the atmospheres of exoplanets. Recent progress with high-resolution infrared spectra obtained with CRIRES has led to the first ground-based detections of carbon monoxide and water in the atmospheres of hot giant exoplanets. This avenue of exoplanet characterisation has the potential to identify biomarkers in the atmospheres of Earth analogues with the European Extremely Large Telescope. The current detections not only provide evidence for how the composition of a hot giant planet atmosphere can affect its thermal structure and cloud formation processes, but also have the potential to constrain the universal mechanism for planet formation by pinpointing the birth location of the planet in its protoplanetary disc.
References:
Birkby, J. L. et al. 2013, MNRAS Letters, 436, 35; Brogi, M. et al. 2012, Nature, 486, 502; Brogi, M. et al. 2013, ApJ, 767, 27; Evans, T. et al. 2013, ApJL, 772, 16; Gibson, N. P. et al. 2011, MNRAS, 411, 2199; Knutson, H. et al. 2010, ApJ, 720, 1569; de Kok, R. J. et al. 2013a, A&A, 554, A82; de Kok, R. J. et al. 2013b, A&A, accepted Madhusudhan, N. et al. 2012, ApJ, 758, 36; Öberg, K. I. et al. 2011, ApJL, 743, L16; Pont, F. et al. 2013, MNRAS, 432, 2917; Snellen, I. A. G. et al. 2010, Nat, 465, 1049; Snellen, I. A. G. et al. 2013, ApJ, 764, 18

ADS BibCode:
2013Msngr.154...62B
Section:
Astronomical Science
Author(s)/Affiliation(s):
Burtscher, L.; Tristram, K. R. W.
AA(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AB(Max-Planck-Institut für Radioastronomie, Bonn, Germany)
Abstract:
The molecular gas and dust surrounding the central engine of active galactic nuclei (AGN) plays a fundamental role in understanding their physics. Due to the small angular size of this torus, direct studies of its properties require very high angular resolution. The VLTI/MIDI AGN Large Programme aims at characterising a statistical sample of AGN tori for the first time by resolving their dust emission in the mid-infrared interferometrically. Measurements of 23 sources show that most tori are very compact with sizes of 0.1 to 10 pc and emission from a two-component structure. The morphology of the torus differs significantly between individual objects and does not show the expected dependency on viewing angle (edge- on vs. face-on). The torus is thus significantly more complex than typically pictured, requiring new models and imaging interferometry on milliarcsecond scales to decipher the physics.
References:
Burtscher, L. et al. 2012, Proc. SPIE, 8445, 84451G Burtscher, L. et al. 2013, A&A, 558, A149; Kishimoto, M. et al. 2011, A&A, 536, A78; Meisenheimer, K. et al. 2008, The Messenger, 133, 36; Schartmann, M. et al. 2009, MNRAS, 393, 759; Schartmann, M. et al. 2010, MNRAS, 403, 1801; Tristram, K. R. W. et al. 2009, A&A, 502, 67

ADS BibCode:
2013Msngr.154...67P
Section:
Astronomical News
Author(s)/Affiliation(s):
Primas, F.; Hanowski, N.
AA(ESO) AB(ESA)
Abstract:
This first conference aimed at establishing closer communication and synergy of ground- and space-based operations for astronomy and Solar System science is summarised by the two chairs. The main topics covered the organisation and management of science operations, science and instrument planning, instrument handling and calibration, data processing and archiving, and support services.

ADS BibCode:
2013Msngr.154...69.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2013Msngr.154...701
Section:
Astronomical News
Author(s)/Affiliation(s):
Wesson, R.; Rahoui F.
AA(ESO) AB(ESO)

ADS BibCode:
2013Msngr.154...71.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)