ADS BibCode:
2011Msngr.144....2B
Section:
The Organisation
Author(s)/Affiliation(s):
Bruch, A.
AA(Laboratório Nacional de Astrofísica – LNA, Itajubá, Brazil)
Abstract:
On 29 December 2010, in a ceremony held at the Ministry of Science and Technology in Brazil´s capital, Brasília, the then Minister, Sergio Machado Rezende and the ESO Director General Tim de Zeeuw signed the accession agreement by which, pending ratification by the Brazilian Congress, Brazil becomes the 15th ESO Member State and the first non-European member. An overview of the historical background, the current state of astronomy in Brazil, and the motivation that made Brazil apply to become an ESO Member State is presented.
References:
de Zeeuw, P. T. 2011, The Messenger, 143, 5; Prazeres, A. 2004, Georg Marcgrave, e o desenvolvimento da astronomia moderna na América Latina, na cosmopolita Recife de Nassau, http://www.liada.net/NASSAU%20&%20GEORG%20MARCGRAVE.pdf Videira, A. A. P. 2007. História do Observatório Nacional: a persistente construção de uma identidade científica. Río de Janeiro: Observatorio Nacional

ADS BibCode:
2011Msngr.144....9S
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Siebenmorgen, R.; Carraro, G.; Valenti, E.; Petr-Gotzens, M.; Brammer, G.; Garcia, E.; Casali, M.
AA(ESO) AB(ESO) AC(ESO) AD(ESO) AE(ESO) AF(ESO) AG(ESO)
Abstract:
HAWK-I is ESO’s most efficient near-infrared camera, and after two and a half years of operations we review its science return and give some future directions in the context of the Adaptive Optics Facility. The instrument underwent major technical challenges in the early phase of its operations: there was a problem with the entrance window, which was replaced, and radioactive events occur in the material of two of the four detectors. A number of high quality science papers based on HAWK-I data have been published, indicating a good performance and scientific return. HAWK-I is well-suited for a variety of attractive science cases and a project is in development to provide a faster readout, which would improve the capabilities for Galactic observations. When combined with the laser-assisted ground layer adaptive optics system, HAWK-I will become an excellent facility for challenging follow-up observations of exoplanetary transits.
References:
Anderson, D. R. et al. 2010, A&A, 513, 3; Arsenault, R. et al. 2010, The Messenger, 142, 12; Bakos, G. A. et al. 2011, AAS Meeting 217, 253.02; Bouwens, R. J. et al. 2010, ApJ 725, 1587; Brasseur, C. A. et al. 2010, AJ, 140, 1672; Cameron, A. C. et al. 2009, IAU Symposium, Volume 253, 29; Castellano, M. et al. 2010a, A&A, 511, 20; Castellano, M. et al. 2010b, A&A, 524, 28; Coppin, K. E. K. et al. 2010, MNRAS, 407, L103; D’Avanzo, P. et al. 2010, A&A, 422, 20; Decarli, R. et al. 2009, ApJ, 703, L76; Finger, G. Reports on HAWK-I detectors available at: http://www.eso.org/~gfinger/marseille_08/AS08-AS12-9_H2RG_mosaic_gfi_final.pdf http://www.eso.org/~gfinger/hawaii_1Kx1K/crosstalk_rock/crosstalk.pdf Fontana, A. et al. 2010, ApJL, i725, 205; Galametz, A. et al. 2010, A&A, 522, 58; Gibson, N. P. et al. 2010, MNRAS, 404, L104; Gillon, M. et al. 2009, A&A, 506, 359; Gogus, E. et al. 2010, ApJ, 718, 331; Goobar, A. et al. 2009, A&A, 507, 71; Greiner, J. et al. 2009, ApJ, 693, 1610; Hayes, M. et al. 2010, Nature, 464, 562; Hayes, M. et al. 2010, A&A, 509, L5; Hickey, S. et al. 2010, MNRAS, 404, 212; Le Louarn, M. et al. 2010, SPIE, 7736, 111; Letawe, G. & Magain, P. 2010, A&A, 515, 84; Lidman, C. et al. 2008, A&A, 489, 981; Mattila, S. et al. 2008, ApJ, 688, L91; McLure, R. J. et al. 2010, MNRAS, 403, 960; Moutou, C. et al. 2008, A&A, 488, L47; Paufique, J. et al. 2010, SPIE, 7736, 57; Roxburgh, I. W. & Catala C. 2006, IAUJD, 17, 32; Snodgrass, C. et al. 2010, A&A, 511, 72; Stanishev, V. et al. 2009, A&A, 507, 61; Tanvir, N. R. et al. 2009, Nature, 461, 1254; Vanzella, L. et al. 2010, ApJL, 730, 35

ADS BibCode:
2011Msngr.144...13S
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Sandin, C.; Weilbacher, P.; Streicher, O.; Walcher, C. J.; Roth, M. M.
AA(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AB(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AC(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AD(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AE(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany)
Abstract:
The second release of the data reduction tool p3d now also supports the integral-field modes of the ESO VLT instruments VIMOS and FLAMES. This article describes the general capabilities of p3d and how its different tools can be invoked, with particular reference to its use with data from VIMOS and FLAMES.
References:
González-Lópezlira, R. A. et al. 2010, MNRAS, 403, 1213; Hammersley, P. et al. 2010, The Messenger, 142, 8; Markwardt, C. B. 2009, ASP Conf. Ser., 411, 251; Melo, C. et al. 2007, The Messenger, 133, 17; Monreal-Ibero, A. et al. 2005, ApJ, 628, L139; Pych, W. 2004, PASP, 116, 148; Roth, M. M. et al. 2004, ApJ, 603, 531; Sandin, C. et al. 2010, A&A, 515, A35; Walcher, C. J. et al. 2009, MNRAS, 398, 44

ADS BibCode:
2011Msngr.144...17A
Author(s)/Affiliation(s):
Arnaboldi, M.; Retzlaff, J.; Slijkhuis, R.; Forchí, V.; Nunes, P.; Sforna, D.; Zampieri, S.; Bierwirth, T.; Comerón, F.; Péron, M.; Romaniello, M.; Suchar, D.
AA(ESO) AB(ESO) AC(ESO) AD(ESO) AE(ESO) AF(ESO) AG(ESO) AH(ESO) AI(ESO) AJ(ESO) AK(ESO) AL(ESO)
Abstract:
Phase 3 represents the final step in the execution of ESO large programmes and public surveys, which starts with the submission of the letters of intent for public surveys and proposals for large programmes, i.e. Phase 1, and continues with the preparation and submission of observing blocks for service mode observations, i.e. Phase 2. In this paper we present the new Phase 3 infrastructure deployed on 10 March 2011. This infrastructure supports the reception, validation and publication of data products from the public survey projects and large programmes to the ESO Science Archive Facility.
References:
Arnaboldi, M. et al. 2007, The Messenger, 127, 28; Capaccioli, M., Mancini, D. & Sedmak, G. 2005, The Messenger, 120, 10; Emerson, J., McPherson, A. & Sutherland, W. 2006, The Messenger, 126, 41

ADS BibCode:
2011Msngr.144...21L
Section:
Astronomical Science
Author(s)/Affiliation(s):
Lagadec, E.; Verhoelst, T.; Mekarnia, D.; Suarez, O.; Zijlstra, A. A.; Bendjoya, P.; Szczerba, R.; Chesneau, O.; Van Winckel, H.; Barlow, M. J.; Matsuura, M.; Bowey, J. E.; Lorenz-Martins, S.; Gledhill, T.
AA(ESO) AB(Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Belgium) AC(Fizeau, OCA/UNS/CNRS, Nice, France) AD(Fizeau, OCA/UNS/CNRS, Nice, France; Instituto de Astrofisica de Andalucia, Granada, Spain) AE(Jodrell Bank Centre for Astrophysics, University of Manchester, United Kingdom) AF(Fizeau, OCA/UNS/CNRS, Nice, France) AG(N. Copernicus Astronomical Center, Torun, Poland) AH(Fizeau, OCA/UNS/CNRS, Nice, France) AI(Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Belgium) AJ(University College London, United Kingdom) AK(University College London, United Kingdom; Mullard Space Science Laboratory, Univerisity College London, United Kingdom) AL(University College London, United Kingdom) AM(Universidade Federal do Rio de Janeiro, Brazil) AN(University of Hertfordshire, United Kingdom)
Abstract:
Post asymptotic giant branch (AGB) stars are key objects for the study of the dramatic morphological changes that low- to intermediate-mass stars undergo during their evolution from the AGB towards the planetary nebula stage. There is growing evidence that binary interaction processes may play a determining role in shaping many objects, but so far direct evidence for binarity is still weak. We report on a systematic study of the dust distribution around a large sample of post-AGB stars that probes the symmetry-breaking in the nebulae around these systems.
References:
Balick, B. & Frank, A. 2002, ARA&A, 40, 439; Chesneau, O. et al. 2006, A&A, 455, 1009; Chesneau, O. et al. 2007, A&A, 473, L29; Corradi, R. L. M. & Schwarz, H. E. 1995, A&A, 293, 871; Guzman-Ramirez, L. et al. 2011, MNRAS Lagadec, E. et al. 2006, A&A, 448, 203; Lagadec, E. et al. 2011, MNRAS, in press Law, N. M. et al. 2006, MNRAS, 368, 1917; Matsuura, M. et al. 2006, ApJl, 646, L123; Meaburn, J. et al., 2008, MNRAS, 385, 269; Meixner, M. et al. 1999, ApJS, 122, 221; Stanghellini, L. et al. 2007, ApJ, 671, 1669; Soker, N. 1998, ApJ, 496, 833

ADS BibCode:
2011Msngr.144...25C
Section:
Astronomical Science
Author(s)/Affiliation(s):
M.-R., Cioni; Clementini, G.; Girardi, L.; Guandalini, R.; Gullieuszik, M.; Miszalski, B.; Moretti, M.-I.; Ripepi, V.; Rubele, S.; Bagheri, G.; Bekki, K.; Cross, N.; de Blok, E.; de Grijs, R.; Emerson, J.; Evans, C.; Gibson, B.; Gonzales-Solares, E.; Groenewegen, M.; Irwin, M.; Ivanov, V.; Lewis, J.; Marconi, M.; Marquette, J.-B.; Mastropietro, C.; Moore, B.; Napiwotzki, R.; Naylor, T.; Oliveira, J.; Read, M.; Sutorius, E.; van Loon, J.; Wilkinson, M.; Wood, P.
AA(University of Hertfordshire, Physics Astronomy and Mathematics, United Kingdom; University Observatory Munich, Germany) AB(INAF, Osservatorio Astronomico di Bologna, Italy) AC(INAF, Osservatorio Astronomico di Padova, Italy) AD(University of Hertfordshire, Physics Astronomy and Mathematics, United Kingdom) AE(Royal Observatory of Belgium, Belgium) AF(University of Hertfordshire, Physics Astronomy and Mathematics, United Kingdom) AG(University of Bologna, Department of Astronomy, Italy) AH(INAF, Osservatorio Astronomico di Capodimonte, Italy) AI(INAF, Osservatorio Astronomico di Padova, Italy) AJ(University of Hertfordshire, Physics Astronomy and Mathematics, United Kingdom) AK(ICRAR, University of Western Australia, Australia) AL(University of Edinburgh, Institute for Astronomy, United Kingdom) AM(University of Cape Town, South Africa) AN(Peking University, Kavli Institute for Astronomy and Astrophysics, China) AO(Queen Mary, University of London, United Kingdom) AP(UK Astronomy Technology Centre, United Kingdom) AQ(Centre for Astrophysics, University of Central Lancshire, United Kingdom) AR(University of Cambridge, Institute of Astronomy, United Kingdom) AS(Royal Observatory of Belgium, Belgium) AT(University of Cambridge, Institute of Astronomy, United Kingdom) AU(ESO) AV(University of Cambridge, Institute of Astronomy, United Kingdom) AW(INAF, Osservatorio Astronomico di Capodimonte, Italy) AX(UPMC, University of Paris, Institut d’Astrophysique de Paris, France; CNRS, Institut d’Astrophysique de Paris, France) AY(LERMA, Observatoire de Paris, France) AZ(University of Zurich, Institute of Theoretical Physics, Switzerland) BA(University of Hertfordshire, Physics Astronomy and Mathematics, United Kingdom) BB(University of Exeter, School of Physics, United Kingdom) BC(University of Keele, School of Physical and Geographical Sciences, United Kingdom) BD(University of Edinburgh, Institute for Astronomy, United Kingdom) BE(University of Edinburgh, Institute for Astronomy, United Kingdom) BF(University of Keele, School of Physical and Geographical Sciences, United Kingdom) BG(University of Leicester, United Kingdom) BH(Mount Stromlo Observatory, RSSA, Australia)
Abstract:
The VISTA public survey project VMC targets the Large Magellanic Cloud, the Small Magellanic Cloud, the Bridge and two fields in the Stream. The VMC survey is a uniform and homogeneous survey in the Y, J and Ks near-infrared filters. The main goals are the determination of the star formation history and the three-dimensional structure of the Magellanic system. The survey is therefore designed to reach stars as faint as the oldest main sequence turn-off point and to constrain the mean magnitude of pulsating variable stars such as RR Lyrae and Cepheids. We provide a brief overview of the survey strategy and first science results. Further details are given in Cioni et al. (2011).
References:
Arnaboldi, M. et al. 2010, The Messenger, 134, 42; Cappellaro, E. 2005, The Messenger, 120, 13; Cioni, M.-R. L. et al. 2011, A&A, 527, A116; Clementini, G. et al. 2000, AJ, 120, 2054; Emerson, J. et al. 2006, The Messenger, 126, 41; Emerson, J. et al. 2010, The Messenger, 139, 2; Hodgkin, S. T. et al. 2009, MNRAS, 394, 675; Irwin, M. 2009, UKIRT Newsletter, 25, 15; Irwin, M. 2010, UKIRT Newsletter, 26, 14; Kontizas, M. et al. 1990, A&A, 84, 527; McClure-Griffiths, N. et al. 2009, ApJS, 181, 398; Tisserand, P. et al. 2007, A&A, 469, 387

ADS BibCode:
2011Msngr.144...32S
Section:
Astronomical Science
Author(s)/Affiliation(s):
Stetson, P. B.; Monelli, M.; Fabrizio, M.; Walker, A.; Bono, G.; Buonanno, R.; Caputo, F.; Cassisi, S.; Corsi, C.; Dall’Ora, M.; Degl’Innocenti, S.; François, P.; Ferraro, I.; Gilmozzi, R.; Iannicola, G.; Merle, T.; Nonino, M.; Pietrinferni, A.; Moroni, P.P.; Pulone, L.; Romaniello, M.; Thévenin, F.
AA(DAO/HIA/NRC, Victoria, Canada) AB(IAC, Tenerife, Spain; Univ. La Laguna, Tenerife, Spain) AC(Univ. Tor Vergata, Roma, Italy) AD(NOAO/CTIO, La Serena, Chile) AE(Univ. Tor Vergata, Roma, Italy; INAF–OAR, Monte Porzio Catone, Italy; ESO) AF(Univ. Tor Vergata, Roma, Italy; ASDC. Frascati, Italy) AG(INAF–OAR, Monte Porzio Catone, Italy) AH(INAF–OACTe, Teramo, Italy) AI(INAF–OAR, Monte Porzio Catone, Italy) AJ(INAF–OAC, Napoli, Italy) AK(Univ. Pisa, Pisa, Italy; INFN, Pisa, Italy) AL(Obs. de Paris-Meudon, Paris, France) AM(INAF–OAR, Monte Porzio Catone, Italy) AN(ESO) AO(INAF–OAR, Monte Porzio Catone, Italy) AP(Obs. Côte d’Azur, Nice, France) AQ(INAF–OAT, Trieste, Italy) AR(INAF–OACTe, Teramo, Italy) AS(Univ. Pisa, Pisa, Italy; INFN, Pisa, Italy) AT(INAF–OAR, Monte Porzio Catone, Italy) AU(ESO) AV(Obs. Côte d’Azur, Nice, France)
Abstract:
We present deep and precise multiband (U, B, V, I) optical data for the Carina dwarf spheroidal galaxy. Data were collected using three different ground-based telescopes (4-metre Blanco CTIO, MPG/ESO 2.2-metre, 1.5-metre CTIO) and cover the entire body of the galaxy. We discuss the reliability of the absolute photometric zero-point calibrations of images collected with large-format and mosaic CCD cameras. The typical precision for the B- , V- and I-bands is better than 0.01 mag. The U-band is a little worse. A preliminary comparison with scaled-solar and alpha-enhanced evolutionary predictions covering a broad range of ages and chemical compositions seems to support previous photometric evidence that both the old (12 Gyr) and the intermediate-age (4–6 Gyr) subpopulations show a limited spread in chemical composition. The use of the Carina galaxy field as a possible standard stellar field is outlined.
References:
Balbinot, E. et al. 2010, MNRAS, 404, 1625; Bono, G. et al. 2010, PASP, 122, 651; Dall’Ora, M. et al. 2003, AJ, 126, 197; Fabrizio, M. et al. 2011, PASP accepted Graham, J. A. 1982, PASP, 94, 244; Helmi, A. et al. 2006, ApJL, 651, L121; Koch, A. et al. 2006, AJ, 131, 895; Koch, A. et al. 2008, AJ, 135, 1580; Kravtsov, A. 2010, Advances in Astronomy, 2010, Landolt, A. U. 1973, AJ, 78, 959; Landolt, A. U. 1983, AJ, 88, 439; Landolt, A. U. 1992, AJ, 104, 340; Mac Low, M. & Ferrara, A. 1999, ApJ, 513, 142; Madau, P. et al. 2008, ApJ, 679, 1260; Monelli, M. et al. 2003, AJ, 126, 218; Pietrinferni, A. et al. 2004, ApJ, 612, 168; Pietrinferni, A. et al. 2006, ApJ, 642, 797; Prada, F. & Burkert, A. 2002, ApJ, 564L, 73; Shetrone M. D., et al. 2003, AJ, 125, 684 Stetson, P. B. 1987, PASP, 99, 191; Stetson, P. B. 1994, PASP, 106, 250; Stetson, P. B. 2000, PASP, 112, 925; Stetson, P. B. 2005, PASP, 117, 563; Tolstoy, E., Hill, V. & Tosi, M. 2009, ARA&A, 47, 371; Woo, J., Courteau, S. & Dekel, A. 2008, MNRAS, 390, 1453

ADS BibCode:
2011Msngr.144...39R
Section:
Astronomical News
Author(s)/Affiliation(s):
Randall, S.; Testi, L.
AA(ESO) AB(ESO)
Abstract:
ALMA is rapidly approaching Early Science operations, and is scheduled to start the first observing projects for the astronomical community in the autumn of 2011. The Call for Proposals for ALMA Early Science Cycle 0 was published on 30 March, inviting the community to submit observing proposals by the deadline of 30 June 2011. Held just after the Call for Proposals was issued, the ALMA Community Days were designed to optimally prepare the European ALMA Community for Cycle 0 proposal submission. The workshop included a broad range of scientific and technical presentations as well as hands-on software tutorials for the ALMA simulators and the Observing Tool.
References:
Olofsson, H. et al. 2010, A&A, 515, 270

ADS BibCode:
2011Msngr.144...41L
Section:
Astronomical News
Author(s)/Affiliation(s):
Longmore, S.; Testi, L.; Klaassen, P.
AA(ESO) AB(ESO) AC(ESO)
Abstract:
With the deadline for ALMA Early Science Cycle 0 proposals fast approaching, a workshop was held for members of the European massive star formation community to discuss ideas for potential ALMA Early Science projects. The workshop began with short summary talks on the ALMA Early Science capabilities, the multi-wavelength large-area survey data available as ALMA source-finder charts and the modelling/analysis tools that are available to help interpret future ALMA data. The rest of the meeting was spent discussing science ideas and proposal strategies. There was general agreement on the main science questions to be addressed, the basic observing strategies required to achieve the goals and the future steps needed to develop the ideas into proposals.

ADS BibCode:
2011Msngr.144...44M
Section:
Astronomical News
Author(s)/Affiliation(s):
Mieske, S.; Gieles, M.
AA(ESO) AB(Institute of Astronomy, Cambridge, United Kingdom)
Abstract:
The dynamics of low-mass stellar systems is not only an interesting subject in its own right, but is also intimately linked to global theories of structure formation, the physics of gravity, and the shape of the stellar initial mass function. Given the wealth of new information gathered very recently in this field, the time was ripe to hold a dedicated meeting on this topic. The workshop brought together a mix of about 100 astronomers who work on both the observation and theory of the dynamics of dwarf galaxies and star clusters, and a total of around 60 oral presentations and about 25 posters were presented.
References:
for figures Frank, M. et al. 2011, MNRAS letters in press, arXiv:1104.2593; Misgeld, I. & Hilker, M. 2011, MNRAS in press, arXiv:1103.1628; Noyola, E. et al. 2010, ApJ, 719L, 60; Scarpa, R. & Fallomo, R. 2010, A&A 523, A43; Walker, M. et al. 2009, ApJ, 704, 1274

ADS BibCode:
2011Msngr.144...47S
Section:
Astronomical News
Author(s)/Affiliation(s):
Schmidtobreick, L.; Schreiber, M. R.
AA(ESO) AB(Departamento de Física y Astronomía, Universidad de Valparaíso, Chile)
Abstract:
The workshop, organised by ESO and the Universidad de Valparaíso, was held with the aim of bringing together people from different communities to concentrate on the specific problem of binary evolution. Compact binaries divide into many classes, but the evolution of all these objects is driven by a common mechanism: angular momentum loss. From the formation of compact binaries over the various phases of contact to their explosive deaths in a supernova Type Ia or gamma-ray burst, the measurement and understanding of the braking mechanisms was the main discussion point of the meeting.

ADS BibCode:
2011Msngr.144...49P
Section:
Astronomical News
Author(s)/Affiliation(s):
Pierce-Price, D.
AA(ESO)

ADS BibCode:
2011Msngr.144...49.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2011Msngr.144...51.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2011Msngr.144...52.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2011Msngr.144...53E
Section:
Astronomical News
Author(s)/Affiliation(s):
Emsellem, E.; Klaassen, P.; West, M.
AA(ESO) AB(ESO) AC(ESO)
Abstract:
For the first of the newly formatted ESO Fellow Days, a total of 25 fellows, including several ESO COFUND Fellows from Alma Regional Centres in Europe, and one fellow from Chile, gathered. All the fellows briefly introduced themselves and most presented recent research results and perspectives. ESO staff astronomers and students were also invited to these presentations, which beautifully demonstrated the excellence of the science being conducted by ESO Fellows.

ADS BibCode:
2011Msngr.144...55.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)