ADS BibCode:
2014Msngr.157....2.
Section:
The Organisation
Author(s)/Affiliation(s):
de Zeeuw, T.
AA(ESO)

ADS BibCode:
2014Msngr.157....5L
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Lopez, B.; Lagarde, S.; Jaffe, W.; Petrov, R.; Schöller, M.; Antonelli, P.; Beckmann, U.; Berio, P.; Bettonvil, F.; Glindemann, A.; Gonzalez, J.-C.; Graser, U.; Hofmann, K.-H.; Millour, F.; Robbe-Dubois, S.; Venema, L.; Wolf, S.; Henning, T.; Lanz, T.; Weigelt, G.; Agocs, T.; Bailet, C.; Bresson, Y.; Bristow, P.; Dugué, M.; Heininger, M.; Kroes, G.; Laun, .; Lehmitz, M.; Neumann, U.; Augereau, J.-C.; Avila, G.; Behrend, J.; van Belle, G.; Berger, J.-P.; van Boekel, R.; Bonhomme, S.; Bourget, P.; Brast, R.; Clausse, J.-M.; Connot, C.; Conzelmann, R.; Cruzalèbes, P.; Csepany, G.; Danchi, W.; Delbo, M.; Delplancke, F.; Dominik, C.; van Duin, A.; Elswijk, E.; Fantei, Y.; Finger, G.; Gabasch, A.; Gay, J.; Girard, P.; Girault, V.; Gitton, P.; Glazenborg, A.; Gonté, F.; Guitton, F.; Guniat, S.; De Haan, M.; Haguenauer, P.; Hanenburg, H.; Hogerheijde, M.; ter Horst, R.; Hron, J.; Hugues, Y.; Hummel, C.; Idserda, J.; Ives, D.; Jakob, G.; Jasko, A.; Jolley, P.; Kiraly, S.; Köhler, R.; Kragt, J.; Kroener, T.; Kuindersma, S.; Labadie, L.; Leinert, C.; Le Poole, R.; Lizon, J.-L.; Lucuix, C.; Marcotto, A.; Martinache, F.; Martinot-Lagarde, G.; Mathar, R.; Matter, A.; Mauclert, N.; Mehrgan, L.; Meilland, A.; Meisenheimer, K.; Meisner, J.; Mellein, M.; Menardi, S.; Menut, J.-L.; Merand, A.; Morel, S.; Mosoni, L.; Navarro, R.; Nussbaum, E.; Ottogalli, S.; Palsa, R.; Panduro, J.; Pantin, E.; Parra, T.; Percheron, I.; Duc, T. P.; Pott, J.-U.; Pozna, E.; Przygodda, F.; Rabbia, Y.; Richichi, A.; Rigal, F.; Roelfsema, R.; Rupprecht, G.; Schertl, D.; Schmidt, C.; Schuhler, N.; Schuil, M.; Spang, A.; Stegmeier, J.; Thiam, L.; Tromp, N.; Vakili, F.; Vannier, M.; Wagner, K.; Woillez, J.
AA(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) AB(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) AC(Leiden Observatory, Leiden University, the Netherlands) AD(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) AE(ESO) AF(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) AG(Max-Planck Institute for Radio Astronomy, Bonn, Germany) AH(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) AI(NOVA ASTRON, Dwingeloo, the Netherlands) AJ(ESO) AK(ESO) AL(Max-Planck Institute for Astronomy, Heidelberg, Germany) AM(Max-Planck Institute for Radio Astronomy, Bonn, Germany) AN(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) AO(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) AP(NOVA ASTRON, Dwingeloo, the Netherlands) AQ(Institute of Theoretical Physics and Astrophysics, Kiel University, Germany) AR(Max-Planck Institute for Astronomy, Heidelberg, Germany) AS(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) AT(Max-Planck Institute for Radio Astronomy, Bonn, Germany) AU(NOVA ASTRON, Dwingeloo, the Netherlands) AV(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) AW(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) AX(ESO) AY(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) AZ(Max-Planck Institute for Radio Astronomy, Bonn, Germany) BA(NOVA ASTRON, Dwingeloo, the Netherlands) BB(Max-Planck Institute for Astronomy, Heidelberg, Germany) BC(Max-Planck Institute for Astronomy, Heidelberg, Germany) BD(Max-Planck Institute for Astronomy, Heidelberg, Germany) BE(Université de Grenoble Alpes, CNRS, IPAG, Grenoble, France) BF(ESO) BG(Max-Planck Institute for Radio Astronomy, Bonn, Germany) BH(Lowell Observatory, Flagstaff, USA) BI(ESO) BJ(Max-Planck Institute for Astronomy, Heidelberg, Germany) BK(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) BL(ESO) BM(ESO) BN(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) BO(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) BP(Max-Planck Institute for Radio Astronomy, Bonn, Germany) BQ(ESO) BR(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) BS(MTA Research Centre for Astronomy and Earth Sciences, Konkoly Thege Miklos Astronomical Institute, Budapest, Hungary) BT(NASA/Goddard Space Flight Center, Greenbelt, USA) BU(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) BV(ESO) BW(Sterrenkundig Instituut “Anton Pannekoek”, University of Amsterdam, the Netherlands) BX(NOVA ASTRON, Dwingeloo, the Netherlands) BY(NOVA ASTRON, Dwingeloo, the Netherlands) BZ(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) CA(ESO) CB(ESO) CC(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) CD(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) CE(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) CF(ESO) CG(Kernfysisch Versneller Institute, Groningen, the Netherlands) CH(ESO) CI(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) CJ(ESO) CK(NOVA ASTRON, Dwingeloo, the Netherlands) CL(ESO) CM(NOVA ASTRON, Dwingeloo, the Netherlands) CN(Leiden Observatory, Leiden University, the Netherlands) CO(NOVA ASTRON, Dwingeloo, the Netherlands) CP(Institut für Astrophysik, University of Vienna, Austria) CQ(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) CR(ESO) CS(NOVA ASTRON, Dwingeloo, the Netherlands) CT(ESO) CU(ESO) CV(Lowell Observatory, Flagstaff, USA) CW(ESO) CX(Lowell Observatory, Flagstaff, USA) CY(Max-Planck Institute for Astronomy, Heidelberg, Germany) CZ(Max-Planck Institute for Radio Astronomy, Bonn, Germany) DA(Max-Planck Institute for Astronomy, Heidelberg, Germany) DB(NOVA ASTRON, Dwingeloo, the Netherlands) DC(I. Physics Institute, University of Cologne, Germany) DD(Max-Planck Institute for Astronomy, Heidelberg, Germany) DE(Leiden Observatory, Leiden University, the Netherlands) DF(ESO) DG(ESO) DH(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) DI(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) DJ(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) DK(Max-Planck Institute for Astronomy, Heidelberg, Germany) DL(Université de Grenoble Alpes, CNRS, IPAG, Grenoble, France) DM(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) DN(ESO) DO(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) DP(Max-Planck Institute for Astronomy, Heidelberg, Germany) DQ(Leiden Observatory, Leiden University, the Netherlands) DR(Max-Planck Institute for Astronomy, Heidelberg, Germany) DS(ESO) DT(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) DU(ESO) DV(ESO) DW(MTA Research Centre for Astronomy and Earth Sciences, Konkoly Thege Miklos Astronomical Institute, Budapest, Hungary) DX(NOVA ASTRON, Dwingeloo, the Netherlands) DY(Max-Planck Institute for Radio Astronomy, Bonn, Germany) DZ(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) EA(ESO) EB(Max-Planck Institute for Astronomy, Heidelberg, Germany) EC(Laboratoire AIM, CEA/DSM–CNRS–Université Paris Diderot, IRFU/Service d’Astrophysique, CEA-Saclay, Gif-sur-Yvette, France) ED(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) EE(ESO) EF(ESO) EG(Max-Planck Institute for Astronomy, Heidelberg, Germany) EH(ESO) EI(Deutsche Thomson OHG, Villingen-Schwenningen, Germany) EJ(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) EK(National Astronomical Research Institute of Thailand, Chiang Mai, Thailand) EL(NOVA ASTRON, Dwingeloo, the Netherlands) EM(NOVA ASTRON, Dwingeloo, the Netherlands) EN(ESO) EO(Max-Planck Institute for Radio Astronomy, Bonn, Germany) EP(ESO) EQ(ESO) ER(NOVA ASTRON, Dwingeloo, the Netherlands) ES(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) ET(ESO) EU(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) EV(NOVA ASTRON, Dwingeloo, the Netherlands) EW(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) EX(Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Nice, France) EY(Max-Planck Institute for Astronomy, Heidelberg, Germany) EZ(ESO)
Abstract:
MATISSE, a second generation Very Large Telescope Interferometer (VLTI) instrument, is a combined imager and spectrograph for interferometry in the 3–5 μm region (L- and M-bands) and the 8–13 μm window (N-band). MATISSE builds on the experience gained with the VLTI’s first generation instruments. It employs multi-axial beam combination while also providing wavelength differential visibility and phase, and closure-phase aperture-synthesis imaging at a range of spectral resolutions. MATISSE is designed for a broad range of science goals, and its potential for studies of the discs around young stars and active galactic nuclei are highlighted. The instrument concept and operating modes are described; construction is in progress towards installation at the VLTI in 2016.
References:
Burtscher, L. et al. 2013, A&A, 558, A149; Burtscher, L. & Tristram, K. R. W. 2013, The Messenger, 154, 62; Crida, A. et al. 2008, A&A, 483, 325; Eisenhauer, F. et al. 2011, The Messenger, 143, 16; Jaffe, W. et al. 2004, Nature, 429, 47; Kishimoto, M. et al. 2011, A&A, 536, 78; Lagarde, S. et al. 2012, SPIE, 8445-91; Lopez, B. et al. 2013, MATISSE Science Analysis Report, Issue 4; Lopez-Gonzaga, N. et al. 2014, A&A, 565, 71; Leinert, C. et al. 2004, A&A, 423, 537; Meisenheimer, K. et al. 2007, A&A, 471, 453; Menu, J. et al. 2014, A&A, 564, A93; Mosoni, L. et al. 2013, A&A, 552, A62; Petrov, R. G. et al. 2012, SPIE, 8445-0W Richichi, A. et al. (eds.) 2008, The Power of Optical/ IR Interferometry: Recent Scientific Results and 2nd Generation VLTI Instrumentation, Proc. ESO Workshop, Springer Schegerer, A. A. et al. 2009, A&A, 502, 367; Thiébaut, E. & Giovannelli, J. F. 2010, IEEE Signal Processing Magazine, 27, 97; Tristram, K. R. W. et al. 2014, A&A, 563, A82; van Boekel, R. et al. 2004, Nature, 432, 479; Weigelt, G. et al. 2011, A&A, 527, A103; Weigelt, G. et al. 2012, A&A, 541, L9; Wolf, S. et al. 2007, MATISSE Phase A Science Cases, Issue 1

ADS BibCode:
2014Msngr.157...13B
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Bacon, R.; Vernet, J.; Borisiva, E.; Bouché, N.; Brinchmann, J.; Carollo, M.; Carton, D.; Caruana, J.; Cerda, S.; Contini, T.; Franx, M.; Girard, M.; Guerou, A.; Haddad, N.; Hau, G.; Herenz, C.; Herrera, J. C.; Husemann, B.; Husser, T.-O.; Jarno, A.; Kamann, S.; Krajnovic, D.; Lilly, S.; Mainieri, V.; Martinsson, T.; Palsa, R.; Patricio, V.; Pécontal, A.; Pello, R.; Piqueras, L.; Richard, J.; Sandin, C.; Schroetter, I.; Selman, F.; Shirazi, M.; Smette, A.; Soto, K.; Streicher, O.; Urrutia, T.; Weilbacher, P.; Wisotzki, L.; Zins, G.
AA(CRAL, Observatoire de Lyon, Saint-Genis-Laval, France) AB(ESO) AC(Institute of Astronomy, ETH Zentrum, Zurich, Switzerland) AD(IRAP, Observatoire Midi Pyrénées, Toulouse, France) AE(Leiden Observatory, Leiden University, the Netherlands) AF(Institute of Astronomy, ETH Zentrum, Zurich, Switzerland) AG(Leiden Observatory, Leiden University, the Netherlands) AH(Leibniz Institut für Astrophysik Potsdam, AIP, Germany) AI(ESO) AJ(IRAP, Observatoire Midi Pyrénées, Toulouse, France) AK(Leiden Observatory, Leiden University, the Netherlands) AL(IRAP, Observatoire Midi Pyrénées, Toulouse, France) AM(IRAP, Observatoire Midi Pyrénées, Toulouse, France; ESO) AN(ESO) AO(ESO) AP(Leibniz Institut für Astrophysik Potsdam, AIP, Germany) AQ(ESO) AR(ESO) AS(Institute for Astrophysics Göttingen, Germany) AT(CRAL, Observatoire de Lyon, Saint-Genis-Laval, France) AU(Institute for Astrophysics Göttingen, Germany) AV(Leibniz Institut für Astrophysik Potsdam, AIP, Germany) AW(Institute of Astronomy, ETH Zentrum, Zurich, Switzerland) AX(ESO) AY(Leiden Observatory, Leiden University, the Netherlands) AZ(ESO) BA(CRAL, Observatoire de Lyon, Saint-Genis-Laval, France) BB(CRAL, Observatoire de Lyon, Saint-Genis-Laval, France) BC(IRAP, Observatoire Midi Pyrénées, Toulouse, France) BD(CRAL, Observatoire de Lyon, Saint-Genis-Laval, France) BE(CRAL, Observatoire de Lyon, Saint-Genis-Laval, France) BF(Leibniz Institut für Astrophysik Potsdam, AIP, Germany) BG(IRAP, Observatoire Midi Pyrénées, Toulouse, France) BH(ESO) BI(Institute of Astronomy, ETH Zentrum, Zurich, Switzerland) BJ(ESO) BK(Institute of Astronomy, ETH Zentrum, Zurich, Switzerland) BL(Leibniz Institut für Astrophysik Potsdam, AIP, Germany) BM(Leibniz Institut für Astrophysik Potsdam, AIP, Germany) BN(Leibniz Institut für Astrophysik Potsdam, AIP, Germany) BO(Leibniz Institut für Astrophysik Potsdam, AIP, Germany) BP(IPAG, Observatoire de Grenoble, France; ESO)
Abstract:
The Multi Unit Spectroscopic Explorer (MUSE) is now in Paranal and was installed on the VLT’s Unit Telescope 4 in January 2014. MUSE enters science operations in October. A short summary of the commissioning activities and Science Verification are presented. Some examples of the first results achieved during the two commissioning runs are highlighted.
References:
Arsenault, R. et al. 2006, The Messenger, 123, 6; Arsenault, R. et al. 2010, The Messenger, 142, 12; Bacon, R. 2006, The Messenger, 124, 5; Bacon, R. 2012, The Messenger, 147, 4

ADS BibCode:
2014Msngr.157...17G
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Gonté, F.; Smette, A.; Abadie, S.; Alvarez, J. L.; Baksai, P.; Beltran, J.; Boffin, H.; Bourget, P.; Carraro, G.; Castillo, R.; de Wit, W.-J.; Diaz, A.; Gadotti, D.; Girard, J.; Haddad, N.; Hau, G.; Ivanov, V.; Lizon, J.-L.; Mardones, P.; Mérand, A.; Mieske, S.; Monaco, L.; O’Neal, J.; Pallanca, L.; Pompei, E.; Ramirez, A.; Riquelme, M.; Rojas, C.; Schmitobreick, L.; Schmutzer, R.; Smoker, J.; Valenzuela, J. J.; Zins, G.
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) AX(ESO) AY(ESO) AZ(ESO) BA(ESO) BB(ESO) BC(ESO) BD(ESO) BE(ESO) BF(ESO) BG(ESO)
Abstract:
Instrumentation at the Paranal Observatory is currently composed of 18 scientific instruments (operational, in commissioning or on standby) and nine technical instruments (test camera, fringe trackers, adaptive optics modules, laser guide star facility, tip-tilt sensor). Over the 15 years since their first implementation and operation, enough information on their typical behaviour has been gathered to define a global plan for preventive maintenance and/or general refurbishment for each instrument in order to retain their reliability and performance. Several examples of monitoring of instrument performance are presented and reasons for failure are listed. We describe the range of activities undertaken to ensure efficient and reliable Paranal instrumentation.
References:
Dorn, R. et al. 2014, The Messenger, 156, 7; Follert, R. et al. 2014, SPIE, 9147-44; Hammersley, P. et al. 2010, The Messenger, 142, 8; Hammersley, P. et al. 2013, The Messenger, 151, 2; Kerber, F. et al. 2012, SPIE, 8446; Lewis, S. et al. 2014, The Messenger, 155, 6; Pasquini, L., Casali, M. & Russell, A. 2013, The Messenger, 154, 2; Rabien, S. et al. 2003, SPIE, 4839, 393; Rupprecht, G. et al. 2010, The Messenger, 140, 2; Spyromilio, J. et al. 2014, The Messenger, 155, 2

ADS BibCode:
2014Msngr.157...27M
Section:
Astronomical Science
Author(s)/Affiliation(s):
Morel, T.; Castro, N.; Fossati, L.; Hubrig, S.; Langer, N.; Przybilla, N.; Schöller, M.; Carroll, T.; Ilyin, I.; Irrgang, A.; Oskinova, L.; Schneider, F. R. N.; Díaz, S. S.; Briquet, M.; González, J. F.; Kharchenko, N.; Nieva, M.-F.; Scholz, R.-D.; de Koter, A.; Hamann, W.-R.; Herrero, A.; Apellániz, J. M.; Sana, H.; Arlt, R.; Barbá, R.; Dufton, P.; Kholtygin, A.; Mathys, G.; Piskunov, A.; Reisenegger, A.; Spruit, H.; Yoon, S.-C.
AA(Institut d’Astrophysique et de Géophysique, Liège, Belgium) AB(Argelander-Institut für Astronomie, Bonn, Germany) AC(Argelander-Institut für Astronomie, Bonn, Germany) AD(Leibniz-Institut für Astrophysik Potsdam (AIP), Potsdam, Germany) AE(Argelander-Institut für Astronomie, Bonn, Germany) AF(Institute for Astro- and Particle Physics, University of Innsbruck, Austria) AG(ESO) AH(Leibniz-Institut für Astrophysik Potsdam (AIP), Potsdam, Germany) AI(Leibniz-Institut für Astrophysik Potsdam (AIP), Potsdam, Germany) AJ(Dr. Remeis Observatory & ECAP, Bamberg, Germany) AK(Institut für Physik und Astronomie der Universität Potsdam, Germany) AL(Argelander-Institut für Astronomie, Bonn, Germany) AM(Instituto de Astrofísica de Canarias, La Laguna, Spain; Universidad de La Laguna, Dpto. de Astrofísica, La Laguna, Spain) AN(Institut d’Astrophysique et de Géophysique, Liège, Belgium) AO(Instituto de Ciencias Astronomicas, de la Tierra, y del Espacio (ICATE), San Juan, Argentina) AP(Main Astronomical Observatory, Kiev, Ukraine) AQ(Institute for Astro- and Particle Physics, University of Innsbruck, Austria; Dr. Remeis Observatory & ECAP, Bamberg, Germany) AR(Leibniz-Institut für Astrophysik Potsdam (AIP), Potsdam, Germany) AS(Astronomical Institute Anton Pannekoek, Amsterdam, the Netherlands; Instituut voor Sterrenkunde, Universiteit Leuven, Belgium) AT(Institut für Physik und Astronomie der Universität Potsdam, Germany) AU(Instituto de Astrofísica de Canarias, La Laguna, Spain; Universidad de La Laguna, Dpto. de Astrofísica, La Laguna, Spain) AV(Instituto de Astrofísica de Andalucía-CSIC, Granada, Spain) AW(ESA/Space Telescope Science Institute, Baltimore, USA) AX(Leibniz-Institut für Astrophysik Potsdam (AIP), Potsdam, Germany) AY(Departamento de Física, La Serena, Chile) AZ(Astrophysics Research Centre, Belfast, UK) BA(Chair of Astronomy, Saint-Petersburg State University, Russia) BB(ESO) BC(Institute of Astronomy of the Russian Acad. Sci., Moscow, Russia) BD(Pontificia Universidad Católica de Chile, Santiago, Chile) BE(Max-Planck-Institut für Astrophysik, Garching, Germany) BF(Department of Physics and Astronomy, Seoul National University, Republic of Korea)
Abstract:
The B fields in OB stars (BOB) survey is an ESO Large Programme collecting spectropolarimetric observations for a large number of early-type stars in order to study the occurrence rate, properties, and ultimately the origin of magnetic fields in massive stars. A total of 98 objects was observed over 20 nights with FORS2 and HARPSpol to July 2014. Preliminary results indicate that the fraction of magnetic OB stars with an organised, detectable field is low. This conclusion, now independently reached by two different surveys, has profound implications for any theoretical model attempting to explain the field formation in these stars. We also discuss some important issues addressed by our observations (e.g., the lower bound of the field strength) and the discovery of some remarkable objects.
References:
Bagnulo, S. et al. 2012, A&A, 538, A129; Braithwaite, J. & Spruit, H. C. 2004, Nature, 431, 819; Cantiello, M. & Braithwaite, J. 2011, A&A, 534, A140; Castro, N. et al., in preparation Fossati, L. et al. 2014, to be submitted to A&A Hubrig, S. et al. 2009a, The Messenger, 135, 21; Hubrig, S. et al. 2009b, AN, 330, 317; Hubrig, S. et al. 2014, A&A, 564, L10; Kohoutek, L. et al. 1999, A&AS, 134, 129; Landstreet, J. D. et al. 2008, A&A, 481, 465; Lignières, F. et al. 2014, in Proc. IAUS, 302, 338; Mikulášek, Z. et al. 2008, A&A, 485, 585; Neiner, C. et al. 2014, A&A, 562, A59; Przybilla, N. et al., in preparation Sana, H. et al. 2012, Science, 337, 444; Silvester, J. et al. 2009, MNRAS, 398, 1505; ud-Doula, A. et al. 2009, MNRAS, 392, 1022; Wade, G. A. et al. 2013, in Proc. IAUS, 302, 265; Wickramasinghe, D. T. et al. 2014, MNRAS, 437, 675

ADS BibCode:
2014Msngr.157...32R
Section:
Astronomical Science
Author(s)/Affiliation(s):
Ripepi, V.; Cignoni, M.; Tosi, M.; Marconi, M.; Musella, I.; Grado, A.; Limatola, L.; Clementini, G.; Brocato, E.; Cantiello, M.; Capaccioli, M.; Cappellaro, E.; Cioni, M.-R. L.; Cusano, F.; Dall’Ora, M.; Gallagher, J. S.; Grebel, E. K.; Nota, A.; Palla, F.; Romano, D.; Raimondo, G.; Sabbi, E.; Getman, F.; Napolitano, N. R.; Schipani, P.; Zaggia, S.
AA(INAF-Osservatorio Astronomico di Capodimonte, Naples, Italy) AB(Space Telescope Science Institute, Baltimore, USA; INAF-Osservatorio Astronomico di Bologna, Italy) AC(INAF-Osservatorio Astronomico di Bologna, Italy) AD(INAF-Osservatorio Astronomico di Capodimonte, Naples, Italy) AE(INAF-Osservatorio Astronomico di Capodimonte, Naples, Italy) AF(INAF-Osservatorio Astronomico di Capodimonte, Naples, Italy) AG(INAF-Osservatorio Astronomico di Capodimonte, Naples, Italy) AH(INAF-Osservatorio Astronomico di Bologna, Italy) AI(INAF-Osservatorio Astronomico di Roma, Italy) AJ(INAF-Osservatorio Astronomico di Teramo, Italy) AK(Università Federico II, Naples, Italy) AL(INAF-Osservatorio Astronomico di Padova, Italy) AM(University of Hertfordshire, Hatfield, United Kingdom; Leibnitz-Institut für Astrophysik Potsdam, Germany) AN(INAF-Osservatorio Astronomico di Bologna, Italy) AO(INAF-Osservatorio Astronomico di Capodimonte, Naples, Italy) AP(University of Wisconsin-Madison, USA) AQ(Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Germany) AR(Space Telescope Science Institute, Baltimore, USA; European Space Agency, Space Telescope Science Institute, Baltimore, USA) AS(INAF-Osservatorio Astrofisico di Arcetri, Firenze, Italy) AT(INAF-Osservatorio Astronomico di Bologna, Italy) AU(INAF-Osservatorio Astronomico di Teramo, Italy) AV(Space Telescope Science Institute, Baltimore, USA) AW(INAF-Osservatorio Astronomico di Capodimonte, Naples, Italy) AX(INAF-Osservatorio Astronomico di Capodimonte, Naples, Italy) AY(INAF-Osservatorio Astronomico di Capodimonte, Naples, Italy) AZ(INAF-Osservatorio Astronomico di Padova, Italy)
Abstract:
STEP (Small Magellanic Cloud in Time: Evolution of a Prototype interacting late-type dwarf galaxy) is a Guaranteed Time Observation survey being carried out at the VLT Survey Telescope. STEP will obtain homogeneous photometry in the g-, r-, i- and Hα-bands over an area of 74 square degrees covering the main body of the Small Magellanic Cloud (42 square degrees), the Bridge that connects it to the Large Magellanic Cloud (30 square degrees) and a small part of the Magellanic Stream (2 square degrees). Our photometry will allow us to detect and measure the magnitudes of individual stars well below the main sequence turnoff of the oldest populations. Here we describe the observing strategy, the photometric techniques, and the upcoming data products of the STEP survey. Preliminary results for the first two fields for which data acquisition is complete are also presented.
References:
Bica, E. et al. 2008, MNRAS, 389, 678; Capaccioli, M. & Schipani, P. 2011, The Messenger, 146, 2; Cignoni, M. et al. 2013, ApJ, 775, 83; Cignoni, M. et al. 2012, ApJ, 754, 130; Cioni, M. R. L. et al. 2011, The Messenger, 144, 25; Elson, R. A. W., Fall, S. M. & Freeman, K. C. 1987, ApJ, 323, 54; Glatt, K. et al. 2009, AJ, 138, 1403; Grado, A. et al. 2012, MemSAIT, 19, 362; Marigo, P. et al. 2008, A&A, 482, 883; Kuijken, K. 2011, The Messenger, 146, 8; Ripepi, V. et al. 2014, MNRAS, 442, 1897; Tolstoy, L., Hill, V. & Tosi, M. 2009, ARAA, 47, 371

ADS BibCode:
2014Msngr.157...38B
Section:
Astronomical Science
Author(s)/Affiliation(s):
Bower, R.; Bureau, M.
AA(Institute for Computational Cosmology, University of Durham, United Kingdom) AB(Sub-department of Astrophysics, University of Oxford, United Kingdom)
Abstract:
A brief overview of the first results from KROSS, a VLT/KMOS guaranteed time programme is presented. KROSS will spatially resolve the dynamics, metallicity and star formation of 1000 mass- and colour-selected galaxies at z ~ 1. These data will chart the formation of disc galaxies at the epoch of peak star formation density in the Universe.
References:
Abazajian, K. et al. 2009, ApJS, 182, 543; Alexander, D. M. & Hickox, R. C. 2012, NewAR, 56, 93; Colless, M. et al. 2001, MNRAS, 328, 1039; Dekel, A. et al. 2009, Nature, 457, 451; Forster-Schreiber, N. et al. 2009, ApJ, 806, 1364; Bower, R. et al. 2006, MNRAS, 370, 645; Behroozi, P. et al. 2013, ApJ, 762, 31; Contini, T. et al. 2012, A&A, 539, 91; Davies, R. et al. 2013, A&A, 558, 56; Gilmore, G. et al. 2002, ApJ, 574, 39; Karim, A. et al. 2011, ApJ, 730, 61; Lilly, S. et al. 1996, ApJ, 460, 1; Maiolino, R. et al. 2008, A&A, 488, 463; Miller, S. H. et al. 2013, ApJ, 762, 11; Pettini, M. et al. 2002, Ap&SS, 281, 461; Puech, M. et al. 2008, A&A, 484, 173; Shapiro, K. L. et al. 2008, ApJ, 682, 231; Sharples, R. et al. 2013, The Messenger, 151, 21; Sobral, D. et al. 2013, ApJ, 779, 139; Stott, J. et al. 2014, submitted, arXiv1407.1047; Swinbank, M. et al. 2010, MNRAS, 405, 234; Swinbank, M. et al. 2012, MNRAS, 436, 935; Tacconi, L. et al. 2013, ApJ, 768, 74; van de Voort, F. et al. 2011, MNRAS, 414, 2458

ADS BibCode:
2014Msngr.157...41S
Section:
Astronomical Science
Author(s)/Affiliation(s):
Smail, I.; Walter, F.
AA(Institute of Computational Cosmology, Durham University, United Kingdom) AB(Max-Planck-Institut für Astronomie, Heidelberg, Germany)
Abstract:
The ALESS survey is an ALMA Cycle 0 study of ~ 100 luminous high-redshift ultraluminous infrared galaxies in the Extended Chandra Deep Field South (ECDFS), one of the best-studied cosmological deep fields accessible from the southern hemisphere. These galaxies were originally selected based on their bright emission in the submillimetre continuum (so-called submillimetre galaxies, or SMGs) through observations using the APEX bolometer camera LABOCA. Compared to the single-dish LABOCA data, the interferometric ALMA data provide a positional accuracy that is nearly two orders of magnitude higher. The ALMA data thus enable galaxy identifications that were previously impossible, and so remove many of the biases inherent in previous studies of SMGs to give us our first unbiased view of a large sample of this important galaxy population.
References:
Biggs, A. J. et al. 2011, MNRAS, 413, 2314; Calvi, R. et al. 2013, MNRAS, 432, 3141; Chapman, S. C. et al. 2005, ApJ, 622, 772; Chen, C. C. et al. 2014, ApJ, submitted Coppin, K. E. K. et al. 2009, MNRAS, 395, 1905; da Cunha, E. et al. 2014, ApJ, submitted Decarli, R. et al. 2014, ApJ, 780, 115; Greve, T. R. et al. 2009, ApJ, 719, 483; Hickox, R. C. et al. 2012, MNRAS, 421, 284; Hodge, J. A. et al. 2013, ApJ, 768, 91; Ivison, R. J. et al. 2002, MNRAS, 337, 1; Ivison, R. J. et al. 2010, MNRAS, 402, 245; Karim, A. et al. 2013, MNRAS, 432, 2; Lee, N. et al. 2013, ApJ, 778, 131; Lutz, D. et al. 2010, ApJ, 712, 1287; Magnelli, B. et al. 2011, A&A, 539, 155; Simpson, J. M. et al. 2014, ApJ, 788, 125; Smolcic, V. et al. 2012, A&A, 548, A4; Swinbank, A. M. et al. 2012, MNRAS, 427, 1066; Swinbank, A. M. et al. 2014, MNRAS, 438, 1267; Thomson, A. P. et al. 2014, MNRAS, in press, arXiv:1404.7128; Walter, F. et al. 2012, Nature, 486, 233; Wang, S. X. et al. 2013, ApJ, 778, 179; Wardlow, J. L. et al. 2011, MNRAS, 415, 1479; Weiß, A. et al. 2009, ApJ, 707, 1201; Weiß, A. et al. 2013, ApJ, 767, 88

ADS BibCode:
2014Msngr.157...46V
Section:
Astronomical Science
Author(s)/Affiliation(s):
Vanzella, E.; Fontana, A.; Pentericci, L.; Castellano, M.; Grazian, A.; Giavalisco, M.; Nonino, M.; Cristiani, S.; Zamorani, G.; Vignali, C.
AA(INAF-Osservatorio Astronomico di Bologna, Italy) AB(INAF-Osservatorio Astronomico di Roma, Monteporzio, Italy) AC(INAF-Osservatorio Astronomico di Roma, Monteporzio, Italy) AD(INAF-Osservatorio Astronomico di Roma, Monteporzio, Italy) AE(INAF-Osservatorio Astronomico di Roma, Monteporzio, Italy) AF(Department of Astronomy, University of Massachusetts, Amherst, USA) AG(INAF-Osservatorio Astronomico di Trieste, Italy) AH(INAF-Osservatorio Astronomico di Trieste, Italy) AI(INAF-Osservatorio Astronomico di Bologna, Italy) AJ(Dipartimento di Fisica e Astronomia, Università degli Studi di Bologna, Italy)
Abstract:
GDS_1408, a relatively bright (F125W ~ 26 mag), solid z ~ 7 galaxy candidate in the Hubble Ultra Deep Field, has been the target of 52 hours of spectroscopic observations with FORS2 at the VLT. This is the deepest spectrum ever obtained for a galaxy at the epoch of reionisation. Neither emission lines nor a continuum were detected up to 10 100 Å, to a limiting equivalent width of 9 Å; a redshift of 6.82 ± 0.1 is determined, combining the superb HST photometry and the deep FORS2 spectrum. This increased redshift accuracy makes ALMA an interesting option for the confirmation of the redshift. The non-detection of Lyman-α in even the best z ~ 7 candidate demonstrates the limitations of the current generation of 8–10-metre-class telescopes for these spectroscopic confirmations; future facilities such as JWST and the E-ELT will be necessary to make decisive progress.
References:
de Breuck, C. et al. 2014, The Messenger, 156, 38; Caruana, J. et al. 2014, MNRAS, in press, arXiv/1311.0057; Castellano, M. et al. 2010, A&A, 511, 20; Fontana, A. et al. 2010, ApJ, 725, L205; Finkelstein, S. L. et al. 2013, Nature, 502, 524; Grazian, A. et al. 2011, A&A, 532, 33G Guo, Y. et al. 2013, ApJ, 207, 24; Inoue, A. et al. 2014, ApJ, 780, 18; Law, D. R. et al. 2007, ApJ, 656, 1; Miralda-Escudé, J., Haehnelt, M. & Rees, M. J. 2000, ApJ, 530, 1; Pentericci, L. et al. 2014, arXiv:1403.5466; Schenker, M. A. et al. 2014, arXiv:1404.4632; Vanzella, E. et al. 2009, ApJ, 695, 1163; Vanzella, E. et al. 2011, ApJ, 730, 35; Vanzella, E. et al. 2014a, ApJ, 783, 12; Vanzella, E. et al. 2014b, A&A, in press Verhamme, A. et al. 2008, A&A, 491, 89

ADS BibCode:
2014Msngr.157...50W
Section:
Astronomical News
Author(s)/Affiliation(s):
de Wit, W.-J.; Oudmaijer, R. D.; van den Ancker, M. E.; Calvet, N.
AA(ESO) AB(School of Physics & Astronomy, University of Leeds, UK) AC(ESO) AD(Department of Astronomy, University of Michigan, USA)
Abstract:
The workshop highlighted the many recent advances within the field of Herbig Ae/Be stars and the close links to star and planet formation. Topics such as magnetospheric accretion and the evolution of dust in discs, the structure of circumstellar discs and the role of walls and gaps and their links to planet formation from many observational aspects were covered. The workshop was dedicated to the life and works of George H. Herbig, who sadly passed away at the end of last year.
References:
Garufi, A. et al. 2013, A&A, 560, 105; Henning, T. & Semenov, D. 2013, ChRv, 113, 9016; Herbig, G. H. 1960, ApJS, 4, 337; Strom, S. E. et al. 1972, ApJ, 173, 353

ADS BibCode:
2014Msngr.157Q..54.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2014Msngr.157R..54.
Section:
Astronomical News
Author(s)/Affiliation(s):
Grunhut, J.; Geier, S.
AA(ESO) AB(ESO)

ADS BibCode:
2014Msngr.157...56.
Section:
Astronomical News
Author(s)/Affiliation(s):
Jiménez-Serra, I.
AA(ESO)

ADS BibCode:
2014Msngr.157...57.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2014Msngr.157Q..58.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2014Msngr.157R..58.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)