ADS BibCode:
2012Msngr.149....2C
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Lo Curto, G.; Pasquini, L.; Manescau, A.; Holzwarth, R.; Steinmetz, T.; Wilken, T.; Probst, R.; Udem, T.; Hänsch, T. W.; González Hernández, J.; Esposito, M.; Rebolo, R.; Canto Martins, B.; Renan de Medeiros, J.
AA(ESO) AB(ESO) AC(ESO) AD(Max-Planck-Institut für Quantenoptik, Garching, Germany; Menlo Systems GmbH, Martinsried, Germany) AE(Menlo Systems GmbH, Martinsried, Germany) AF(Menlo Systems GmbH, Martinsried, Germany) AG(Max-Planck-Institut für Quantenoptik, Garching, Germany) AH(Max-Planck-Institut für Quantenoptik, Garching, Germany) AI(Max-Planck-Institut für Quantenoptik, Garching, Germany) AJ(Instituto de Astrofisica de Canarias, La Laguna, Spain; Departamento de Astrofísica, Universidad de La Laguna, Tenerife, Spain) AK(Instituto de Astrofisica de Canarias, La Laguna, Spain; Departamento de Astrofísica, Universidad de La Laguna, Tenerife, Spain) AL(Instituto de Astrofisica de Canarias, La Laguna, Spain; Departamento de Astrofísica, Universidad de La Laguna, Tenerife, Spain) AM(Universidade Federal do Rio Grande de Norte, Natal, Brazil) AN(Universidade Federal do Rio Grande de Norte, Natal, Brazil)
Abstract:
Following the development of the laser frequency comb which led to the 2005 Nobel Prize in Physics, we began investigating the possibility of using this novel technology for precise and accurate spectrograph calibration. A programme was begun, aimed at demonstrating the capabilities of laser frequency combs (LFC) when coupled to an astronomical spectrograph. In the last three years we have tested an LFC connected to HARPS at the 3.6-metre telescope in La Silla, the most precise spectrograph available. Here we show the very promising results obtained so far, and outline future activities, including the provision of an LFC system for routine operation with HARPS, to be offered to the community in the near future.
References:
Araujo-Hauck, C. et al. 2007, The Messenger, 129, 24; Beringer, J. et al. 2012, Phys. Rev., D86, 010001; Liske, J. et al. 2008, MNRAS, 386, 1192; Lo Curto, G. et al. 2010, Proc. SPIE, 7735, 77350Z Lovis, C. et al. 2006, Nature, 441, 305; Mayor, M. et al. 2003, The Messenger, 114, 20; Murphy, M. et al. 2007, MNRAS, 380, 839; Palmer, B. & Engleman, R. 1983, Atlas of the Thorium spectrum, Los Alamos National Laboratory Steinmetz, T. et al. 2008, Science, 321, 1335; Wilken, T. et al. 2010, Proc. SPIE, 7735, 77350T Wilken, T. et al. 2010, MNRAS, 405, L16; Wilken, T. et al. 2012, Nature, 485, 611W

ADS BibCode:
2012Msngr.149....7A
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Arnaboldi, M.; Rejkuba, M.; Retzlaff, J.; Delmotte, N.; Hanuschik, R.; Hilker, M.; Hümmel, W.; Hussain, G.; Ivanov, V.; Micol, A.; Neeser, M.; Petr-Gotzens, M.; Szeifert, T.; Comeron, F.; Primas, F.; Romaniello, M.
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)
Abstract:
The ESO policies for public surveys include regular monitoring and reviews of the progress of the surveys to ensure their legacy value and scientific competitiveness. The review process is carried out on the basis of reports by the ESO survey team and the survey PIs submitted to the relevant Public Survey Panel (PSP) — the VISTA PSP in this case. A summary of the time allocation to VISTA surveys, the service mode observations and the current progress after two years of telescope operation is provided. Furthermore the content of the data products delivery by the survey teams to the ESO Science Archive Facility is described.
References:
Arnaboldi, M. et al. 2011, The Messenger, 144, 17; Arnaboldi, M. et al. 2008, The Messenger, 134, 42; Arnaboldi, M. et al. 2007, The Messenger, 127, 28; Bierwirth, T. et al. 2010, SPIE, 7737, 19; Emerson, J., McPherson, A. & Sutherland, W. 2006, The Messenger, 126, 41

ADS BibCode:
2012Msngr.149...12B
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Bramich, D.; Moehler, S.; Coccato, L.; Freudling, W.; Garcia-Dabó, C. E.; Møller, P.; Saviane, I.
AA(ESO) AB(ESO) AC(ESO) AD(ESO) AE(ESO) AF(ESO) AG(ESO)
Abstract:
An accurate absolute calibration of photometric data to place them on a standard magnitude scale is very important for many science goals. Absolute calibration requires the observation of photometric standard stars and analysis of the observations with an appropriate photometric model including all relevant effects. In the FORS Absolute Photometry (FAP) project, we have developed a standard star observing strategy and modelling procedure that enables calibration of science target photometry to better than 3% accuracy on photometrically stable nights given sufficient signal-to-noise. In the application of this photometric modelling to large photometric databases, we have investigated the Sloan Digital Sky Survey (SDSS) and found systematic trends in the published photometric data. The amplitudes of these trends are similar to the reported typical precision (~ 1% and ~ 2%) of the SDSS photometry in the griz- and u-bands, respectively.
References:
Bertin, E. & Arnouts, S. 1996, A&AS, 117, 393; Bramich, D. M. & Freudling, W. 2012, MNRAS, 424, 1584; Freudling, W. et al. 2007, The Messenger, 128, 13; Landolt, A. 1992, AJ, 104, 340; Moehler, S. et al. 2010, PASP, 122, 93; Padmanabhan, N. et al. 2008, ApJ, 674, 1217; Stetson, P. B. 2000, PASP, 112, 925; York, D. G. et al. 2000, AJ, 120, 1579

ADS BibCode:
2012Msngr.149...16R
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Ramsay, S.
AA(ESO)
Abstract:
The near-infrared, multi-integral-field unit spectrograph, KMOS, has passed an important milestone. The provisional acceptance of this instrument by ESO in summer 2012 was the first step towards the commissioning of this new Very Large Telescope facility on the VLT Unit Telescope 1 (UT1) at the end of November 2012.
References:
Sharples, R. et al. 2005, The Messenger, 122, 5; Sharples, R. et al. 2010, The Messenger, 139, 24

ADS BibCode:
2012Msngr.149...17K
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Kasper, M.; Beuzit, J.-L.; Feldt, M.; Dohlen, K.; Mouillet, D.; Puget, P.; Wildi, F.; Abe, L.; Baruffolo, A.; Baudoz, P.; Bazzon, A.; Boccaletti, A.; Brast, R.; Buey, T.; Chesneau, O.; Claudi, R.; Costille, A.; Delboulbé, A.; Desidera, S.; Dominik, C.; Dorn, R.; Downing, M.; Feautrier, P.; Fedrigo, E.; Fusco, T.; Girard, J.; Giro, E.; Gluck, L.; Gonte, F.; Gojak, D.; Gratton, R.; Henning, T.; Hubin, N.; Lagrange, A.-M.; Langlois, M.; Mignant, D.L.; Lizon, J.-L.; Lilley, P.; Madec, F.; Magnard, Y.; Martinez, P.; Mawet, D.; Mesa, D.; Möller-Nilsson, O.; Moulin, T.; Moutou, C.; O’Neal, J.; Pavlov, A.; Perret, D.; Petit, C.; Popovic, D.; Pragt, J.; Rabou, P.; Rochat, S.; Roelfsema, R.; Salasnich, B.; Sauvage, J.-F.; Schmid, H. M.; Schuhler, N.; Sevin, A.; Siebenmorgen, R.; Soenke, C.; Stadler, E.; Suarez, M.; Turatto, M.; Udry, S.; Vigan, A.; Zins, G.
AA(ESO) AB(Institut de Planétologie et d’Astrophysique de Grenoble, France) AC(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AD(Laboratoire d’Astrophysique de Marseille, France) AE(Institut de Planétologie et d’Astrophysique de Grenoble, France) AF(Institut de Planétologie et d’Astrophysique de Grenoble, France) AG(Observatoire de Genève, Switzerland) AH(Laboratoire Lagrange, Nice, France) AI(INAF – Osservatorio Astronomico di Padova, Italy) AJ(Laboratoire d’Etudes Spatiales et d’Instrumentation en Astrophysique, Paris, France) AK(Eidgenössische Technische Hochschule Zürich, Switzerland) AL(Laboratoire d’Etudes Spatiales et d’Instrumentation en Astrophysique, Paris, France) AM(ESO) AN(Laboratoire d’Etudes Spatiales et d’Instrumentation en Astrophysique, Paris, France) AO(Laboratoire Lagrange, Nice, France) AP(INAF – Osservatorio Astronomico di Padova, Italy) AQ(Institut de Planétologie et d’Astrophysique de Grenoble, France) AR(Institut de Planétologie et d’Astrophysique de Grenoble, France) AS(INAF – Osservatorio Astronomico di Padova, Italy) AT(Stichting ASTRonomisch Onderzoek in Nederland, the Netherlands) AU(ESO) AV(ESO) AW(Institut de Planétologie et d’Astrophysique de Grenoble, France) AX(ESO) AY(Office National d’Etudes et de Recherches Aérospatiales, Châtillon, France) AZ(ESO) BA(INAF – Osservatorio Astronomico di Padova, Italy) BB(Institut de Planétologie et d’Astrophysique de Grenoble, France) BC(ESO) BD(ESO) BE(INAF – Osservatorio Astronomico di Padova, Italy) BF(Max-Planck-Institut für Astronomie, Heidelberg, Germany) BG(ESO) BH(Institut de Planétologie et d’Astrophysique de Grenoble, France) BI(Laboratoire d’Astrophysique de Marseille, France) BJ(Laboratoire d’Astrophysique de Marseille, France) BK(ESO) BL(ESO) BM(Laboratoire d’Astrophysique de Marseille, France) BN(Institut de Planétologie et d’Astrophysique de Grenoble, France) BO(Institut de Planétologie et d’Astrophysique de Grenoble, France) BP(ESO) BQ(INAF – Osservatorio Astronomico di Padova, Italy) BR(Max-Planck-Institut für Astronomie, Heidelberg, Germany) BS(Institut de Planétologie et d’Astrophysique de Grenoble, France) BT(Laboratoire d’Astrophysique de Marseille, France) BU(ESO) BV(Max-Planck-Institut für Astronomie, Heidelberg, Germany) BW(Laboratoire d’Etudes Spatiales et d’Instrumentation en Astrophysique, Paris, France) BX(Office National d’Etudes et de Recherches Aérospatiales, Châtillon, France) BY(ESO) BZ(Stichting ASTRonomisch Onderzoek in Nederland, the Netherlands) CA(Institut de Planétologie et d’Astrophysique de Grenoble, France) CB(Institut de Planétologie et d’Astrophysique de Grenoble, France) CC(Stichting ASTRonomisch Onderzoek in Nederland, the Netherlands) CD(INAF – Osservatorio Astronomico di Padova, Italy) CE(Office National d’Etudes et de Recherches Aérospatiales, Châtillon, France) CF(Eidgenössische Technische Hochschule Zürich, Switzerland) CG(ESO) CH(Laboratoire d’Etudes Spatiales et d’Instrumentation en Astrophysique, Paris, France) CI(ESO) CJ(ESO) CK(Institut de Planétologie et d’Astrophysique de Grenoble, France) CL(ESO) CM(INAF – Osservatorio Astronomico di Padova, Italy) CN(Observatoire de Genève, Switzerland) CO(Laboratoire d’Astrophysique de Marseille, France) CP(Institut de Planétologie et d’Astrophysique de Grenoble, France)
Abstract:
Direct imaging and spectral characterisation of exoplanets is one of the most exciting, but also one of the most challenging areas, in modern astronomy. The challenge is to overcome the very large contrast between the host star and its planet seen at very small angular separations. This article reports on the progress made in the construction of the second generation VLT instrument SPHERE, the Spectro-Polarimetric High-contrast Exoplanet REsearch instrument. SPHERE is expected to be commissioned on the VLT in 2013.
References:
Beuzit, J.-L. et al. 2006, The Messenger, 125, 29; Beuzit, J.-L. et al. 2012, Proc. SPIE, 8446; Martinez, P., Aller-Carpentier, E. & Kasper, M. 2010, The Messenger, 140, 10; Mesa, D. et al. 2011, A&A, 529, 131

ADS BibCode:
2012Msngr.149...23S
Section:
Astronomical Science
Author(s)/Affiliation(s):
Saviane, I.; Held, E. V.; Da Costa, G. S.; Sommariva, V.; Gullieuszik, M.; Barbuy, B.; Ortolani, S.
AA(ESO) AB(INAF – Osservatorio Astronomico di Padova, Italy) AC(Australian National University, Mt. Stromlo Observatory, Australia) AD(INAF – Osservatorio Astrofisico di Arcetri, Italy) AE(INAF – Osservatorio Astronomico di Padova, Italy) AF(University of Sao Paulo, Brazil) AG(University of Padova, Italy)
Abstract:
Galactic globular clusters have a long and distinguished history as conspicuous providers of simple populations where models of low-mass stars can be tested. However their simplicity has been challenged several times and a few peculiar objects have been identified. Only recently has the case for extended star formation histories become really compelling, with the unprecedented quantity and quality of data from Hubble Space Telescope imagers and multiplexing spectrographs on large telescopes. With ages close to that of the Universe, globular clusters can also help us uncover the earliest phases in the formation of the Milky Way. In both areas, one of the major challenges is to have an abundance ranking of all clusters based on the same metallicity index, and for as many stars as possible inside each cluster; a homogeneous metallicity compilation is only available for about half of all globular clusters. A few years ago we began a project to help close this gap and we report on a few surprising results that are emerging.
References:
Anderson, J. 2002, ASP Conf. Series, 265, eds. F. van Leeuwen, J. D. Hughes, G. Piotto, 87; Arp, H. C., Baum, W. A. & Sandage, A. R. 1953, AJ, 58, 4; Bekki, K. & Freeman, K. C. 2003, MNRAS, 346, L11; Da Costa, G. S. et al. 2009, ApJ, 705, 1481; de Rossi, M. E. et al. 2009, MNRAS, 395, 210; Eggen, O. J., Lynden-Bell, D. & Sandage, A. R. 1962, ApJ, 136, 748; Gratton, R. G., Carretta, E. & Bragaglia, A. 2012, A&A Rev., 20, 50; Izzo, C. et al. 2010, Proc. SPIE, 7737, 773729; Marín-Franch, A. et al. 2009, ApJ, 694, 1498; Marino, A. F. et al. 2009, A&A, 505, 1099; Monaco, L. et al. 2009, A&A, 502, L9; Newberg, H. J., Yanny, B. & Willett, B. A. 2009, ApJ, 700, L61; Olszewski, E. W. et al. 2009, AJ, 138, 1570; Ortolani, S. et al. 1995, Nature, 377, 701; Paudel, S., Lisker, T. & Kuntschner, H. 2011, MNRAS, 413, 1764; Rey, S.-C. et al. 2001, AJ, 122, 3219; Rosenberg, A. et al. 1999, AJ, 118, 2306; Sandage, A. 1970, ApJ, 162, 841; Saviane, I. et al. 2012, A&A, 540, A27; Saviane, I., Rosenberg, A. & Piotto, G. 1997, in Stellar Ecology: Advances in Stellar Evolution, eds. R. T. Rood & A. Renzini, 65; Searle, L. & Zinn, R. 1978, ApJ, 225, 357; Stetson, P. B., van den Bergh, S. & Bolte, M. 1996, PASP, 108, 560; Wilson, R. N. 2004, Reflecting Telescope Optics I. Basic Design Theory and its Historical Development, 2nd edn. (Springer)

ADS BibCode:
2012Msngr.149...28M
Section:
Astronomical Science
Author(s)/Affiliation(s):
Morelli, L.; Corsini, E. M.; Pizzella, A.; Dalla Bontà, E.; Coccato, L.; Méndez-Abreu, J.; Cesetti, M.
AA(Dipartimento di Fisica e Astronomia, Università di Padova, Italy; INAF–Osservatorio Astronomico di Padova, Italy) AB(Dipartimento di Fisica e Astronomia, Università di Padova, Italy; INAF–Osservatorio Astronomico di Padova, Italy) AC(Dipartimento di Fisica e Astronomia, Università di Padova, Italy; INAF–Osservatorio Astronomico di Padova, Italy) AD(Dipartimento di Fisica e Astronomia, Università di Padova, Italy; INAF–Osservatorio Astronomico di Padova, Italy) AE(ESO) AF(Instituto Astrofísico de Canarias, La Laguna, Spain; Departamento de Astrofísica, Universidad de La Laguna, Spain) AG(Dipartimento di Fisica e Astronomia, Università di Padova, Italy; INAF–Osservatorio Astronomico di Padova, Italy)
Abstract:
The radial profiles of the age, metallicity and α/Fe enhancement of the stellar populations in the bulge-dominated region for a sample of eight spiral galaxies with low surface-brightness stellar discs and bulges are presented. Almost all the sample bulges are characterised by young stellar populations, solar α/Fe enhancements and metallicities spanning from high to sub-solar values. No significant gradient in age and α/Fe enhancement is measured, whereas a negative metallicity gradient is found in a few cases. The stellar populations of the bulges hosted by low surface-brightness discs share many properties with those of high surface-brightness galaxies and are therefore likely to have common formation scenarios and evolution histories.
References:
Annibali, F. et al. 2007, A&A, 463, 455; Arimoto, N. & Yoshii, Y. 1987, A&A, 173, 23; Beijersbergen, M., de Blok, W. J. G. & van der Hulst, J. M. 1999, A&A, 351, 903; Bekki, K. & Shioya, Y. 1999, ApJ, 513, 108; Bergmann, M. P., Jørgensen, I. & Hill, G. J. 2003, AJ, 125, 116; Bothun, G., Impey, C. & McGaugh, S. 1997, PASP, 109, 745; Coccato, L. et al. 2008, A&A, 490, 589; Galaz, G. et al. 2006, AJ, 131, 2035; Ganda, K. et al. 2007, MNRAS, 380, 506; Hopkins, P. F. et al. 2009, ApJS, 181, 135; McGaugh, S. S. et al. 1995, AJ, 109, 2019; Méndez-Abreu, J. et al. 2008, A&A, 478, 353; Moorthy, B. K. & Holtzman, J. A. 2006, MNRAS, 371, 583; Morelli, L. et al. 2004, MNRAS, 354, 753; Morelli, L. et al. 2008, MNRAS, 389, 341; Morelli, L. et al. 2012, MNRAS, 423, 962; Pipino, A., D’Ercole, A. & Matteucci, F. 2008, A&A, 484, 679; Sánchez-Blázquez, P. et al. 2006, A&A, 457, 809; Sarzi, M. et al. 2006, MNRAS, 366, 1151; Thomas, D., Maraston, C. & Bender, R. 2003, MNRAS, 339, 897; Thomas, D. & Davies, R. L. 2006, MNRAS, 366, 510

ADS BibCode:
2012Msngr.149...33K
Section:
Astronomical Science
Author(s)/Affiliation(s):
Koopmans, L.; Czoske, O.
AA(Kapteyn Astronomical Institute, Groningen, the Netherlands) AB(Institut für Astrophysik, Universität Wien, Austria)
Abstract:
Our understanding of the structure and formation of early-type galaxies (ETGs) is rapidly evolving, but our inability to disentangle stellar mass from dark matter often prevents direct comparison of galaxy formation models with observations without making strong assumptions, such as for the initial mass function (IMF) or dark matter mass fraction and density profile. As an example, the increase in mass-to-light ratio (M/L) along the Fundamental Plane could be partly due to changes in the structure of the ETGs, but also to a change in the ratio of dark versus stellar mass and even to a change in the stellar M/L with galaxy velocity dispersion (by a steepening of the IMF). We report on ongoing efforts to disentangle the structure of early-type galaxies using gravitational lensing, two-dimensional kinematics and stellar population analysis making use of high-resolution images from HST, integral field spectroscopy from VIMOS, and UVB/VIS spectra from X-shooter.
References:
Auger, M. et al. 2010, ApJ, 721, L163; Barnabè, M. & Koopmans, L. V. E. 2007, ApJ, 666, 726; Barnabè, M. et al. 2011, MNRAS, 415, 2215; Bolton, A. S. et al. 2006, ApJ, 638, 703; Bolton, A. S. et al. 2007, ApJ, 665, 105; Bolton, A. S. et al. 2012, arXiv:1201.2988; Czoske, O. et al. 2012, MNRAS, 419, 656; Gonzalez, J. J. 1993, PhD Thesis, Univ. California, Santa Cruz Hopkins, P. F. et al. 2006, ApJS, 163, 1; Hopkins, P. F. 2012, MNRAS, 423, 2037; Koopmans, L. V. E. & Treu, T. 2002, ApJ, 568, L5; Koopmans, L. V. E. et al. 2006, ApJ, 649, 599; Koopmans, L. V. E. et al. 2009, ApJL, 703, L51; Lagattuta, D. J. et al. 2012, MNRAS, 424, 2800; Spiniello, C. et al. 2011, MNRAS, 417, 3000; Spiniello, C. et al. 2012, ApJ, 753, 32; Treu, T. & Koopmans, L. V. E. 2002, ApJ, 575, 87; Treu, T. et al. 2010, ApJ, 709, 1195; van Dokkum, P. G. & Conroy, C. 2010, Nature, 468, 940; Vegetti, S. et al. 2012, Nature, 481, 341; Warren, S. J. et al. 1996, MNRAS, 278, 139

ADS BibCode:
2012Msngr.149...40S
Section:
Astronomical Science
Author(s)/Affiliation(s):
Swinbank, M.; Smail, I.; Karim, A.; Hodge, J.; Walter, F.; Alexander, D.; Bertoldi, F.; Biggs, A.; Brandt, N.; De Breuck, C.; Chapman, S.; Coppin, K.; Cox, P.; Danielson, A.; Dannerbauer, H.; Edge, A.; Ivison, R.; Greve, T.; Knudsen, K.; Menten, K.; Simpson, J.; Schinnerer, E.; Wardlow, J.; Weiss, A.; van der Werf, P.
AA(Institute for Computational Cosmology, University of Durham, United Kingdom) AB(Institute for Computational Cosmology, University of Durham, United Kingdom) AC(Institute for Computational Cosmology, University of Durham, United Kingdom) AD(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AE(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AF(Institute for Computational Cosmology, University of Durham, United Kingdom) AG(Argelander-Institut für Astronomie, Bonn, Germany) AH(ESO) AI(Pennsylvania State University, University Park, USA) AJ(ESO) AK(Institute for Astronomy, Cambridge, United Kingdom) AL(Dept. of Physics, McGill University, Montréal, Canada) AM(IRAM, Saint Martin d’Hères, France) AN(Institute for Computational Cosmology, University of Durham, United Kingdom) AO(Institut für Astronomie, Universität Wien, Austria) AP(Institute for Computational Cosmology, University of Durham, United Kingdom) AQ(UK Astronomy Technology Centre, Edinburgh, Scotland; Institute for Astronomy, University of Edinburgh, Scotland) AR(University College London, United Kingdom) AS(Onsala Space Observatory, Chalmers University, Sweden) AT(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AU(Institute for Computational Cosmology, University of Durham, United Kingdom) AV(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AW(Dept. of Physics and Astronomy, University of California Irvine, USA) AX(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AY(Leiden Observatory, the Netherlands)
Abstract:
Sensitive ALMA submillimetre maps of a sample of 122 870 μm selected submillimetre sources from our survey of the Extended Chandra Deep Field South are presented. The combination of sensitivity and resolution of ALMA allows us to precisely pinpoint the submillimetre emission from these galaxies to an accuracy of < 0.3 arcseconds. In two ALMA submillimetre galaxies (SMGs) we serendipitously detect bright [C II] 157.4 μm emission, yielding redshifts of 4.4. This blind detection rate within the 7.5 GHz bandpass of ALMA is consistent with the previously derived photometric redshift distribution of SMGs and suggests a modest, but not dominant (< 25%), tail of 870 μm selected SMGs at z > 4.
References:
Baugh, C. et al. 2005, MNRAS, 356, 1191; Brauher, J. et al. 2008, ApJS, 178, 280; Chapman, S. et al. 2005, ApJ, 622, 772; Genzel, R. et al. 2003, ApJ, 584, 633; Hodge, J. et al. 2012, MNRAS, in prep. Karim, A. et al. 2012, MNRAS, submitted Ivison, R. et al. 2007, MNRAS, 380, 199; Narayanan, R. et al. 2009, MNRAS, 400, 1919; Simpson, J. et al. 2012, MNRAS, in prep. Smail, I. et al. 1997, ApJ, 490, 5; Smail, I. et al. 2012, MNRAS, in prep. Smolčić, V. et al. 2012, ApJS, 200, 10; Swinbank, M. et al. 2006, MNRAS, 371, 465; Swinbank, M. et al. 2012, MNRAS, submitted Wardlow, J. et al. 2011, MNRAS, 415, 1479; Weiss, A. et al. 2009, ApJ, 707, 1201; Whitaker, K. E. et al. 2012, ApJ, 745, 179

ADS BibCode:
2012Msngr.149...44N
Section:
Astronomical Science
Author(s)/Affiliation(s):
Nagao, T.; Maiolino, R.; De Breuck, C.; Caselli, P.; Hatsukade, B.; Saigo, K.
AA(The Hakubi Center for Advanced Research, Kyoto University, Japan; Department of Astronomy, Kyoto University, Japan) AB(Cavendish Laboratory, University of Cambridge, United Kingdom) AC(ESO) AD(School of Physics and Astronomy, University of Leeds, United Kingdom) AE(Department of Astronomy, Kyoto University, Japan) AF(East Asian ALMA Regional Center, National Astronomical Observatory of Japan, Japan)
Abstract:
The chemical properties of galaxies provide strong constraints on galaxy evolutionary scenarios, but diagnosing the chemical properties of high-z dusty galaxies by means of optical and near-infrared spectroscopy has been challenging. We have therefore focussed on far-infrared fine-structure emission lines in high-z dusty galaxies, whose detection is feasible with ALMA. From ALMA Cycle 0 observations, we have detected [N II] 205 μm emission in a submillimetre galaxy at z = 4.76 whose [C II] 158 μm emission has been already detected in our previous APEX observations. The measured flux ratio of [N II] 205 μm/[C II] 158 μm implies solar metallicity in this galaxy, suggesting a significant chemical evolution even at z = 4.76 when the cosmic age was only ~1.3 billion years.
References:
Coppin, K. et al. 2009, MNRAS, 395, 1905; Cresci, G. et al. 2010, Nature, 467, 811; De Breuck, C. et al. 2011, A&A, 530, L8; Gilli, R. et al. 2011, ApJ, 730, L28; Maiolino, R. et al. 2008, A&A, 488, 463; Mannucci, F. et al. 2009, MNRAS, 398, 1915; Matsuoka, K. et al. 2011, A&A, 532, L10; Nagao, T. et al. 2006, A&A, 447, 157; Nagao, T. et al. 2006, A&A, 447, 863; Nagao, T. et al. 2011, A&A, 526, A149; Nagao, T. et al. 2012, A&A, 542, L34

ADS BibCode:
2012Msngr.149...47R
Section:
Astronomical News
Author(s)/Affiliation(s):
Randall, S.; Testi, L.; Hatziminaoglou, E.
AA(ESO) AB(ESO) AC(ESO)
Abstract:
Early Science operations began in September 2011 and ALMA is now more than half way through Cycle 0 and continues to gather data of remarkable quality. The first scientific results based on ALMA data include some very interesting findings and the number of ALMA publications is rapidly increasing. From the start of Cycle 1 at the beginning of 2013, the array will be offered to the astronomical community with enhanced science capabilities. The 2012 ALMA Community Days, summarised here, were held just a few weeks before the Cycle 1 proposal submission deadline and were designed to optimally prepare the European ALMA Community for Cycle 1 proposal submission.
References:
Randall, S. & Testi, L. 2011, The Messenger, 144, 39 Links 1 ALMA Science Portal: www.almascience.org 2 More information on the ARC at: http://www.eso.org/sci/facilities/alma/arc.html 3 Community Days 2012 website: http://www.eso.org/sci/meetings/2012/alma_es_2012/program.html

ADS BibCode:
2012Msngr.149...50F
Section:
Astronomical News
Author(s)/Affiliation(s):
Falcke, H.; Laing, R.; Testi, L.; Zensus, A.
AA(Radboud University Nijmegen and ASTRON, Dwingeloo, the Netherlands) AB(ESO) AC(ESO) AD(Max-Planck-Institut für Radioastronomie, Bonn, Germany)
Abstract:
Very long baseline interferometry at millimetre/submillimetre wavelengths (mm-VLBI) offers the highest achievable spatial resolution at any wavelength in astronomy and the inclusion of ALMA into a global network will bring unprecedented sensitivity. The workshop on mm-VLBI reviewed the broad range of science topics, from imaging the event horizon of the black hole at the centre of the Galaxy, through masers in the Milky Way and distant galaxies to jets in radio galaxies. Plans were laid to develop a science case and a European organisation to promote mm-VLBI including ALMA.
References:
Eisenhauer, F. et al. 2011, The Messenger, 143, 16; Falcke, H. et al. 2011, IAU Symp., 275, 68; Hada, K. et al. 2011, Nature, 477, 185; Maitra, D. 2011, IAU Symp., 275, 82; Krichbaum, T. et al. 2007, Exploring the Cosmic Frontier: Astrophysical Instruments for the 21st Century, 189; Mościbrodzka, M. et al. 2009, ApJ, 706, 497; Walker, R. C. et al. 2008, Extragalactic Jets: Theory and Observation from Radio to Gamma Ray, ASP Conference Series, 386, 87

ADS BibCode:
2012Msngr.149...54W
Section:
Astronomical News
Author(s)/Affiliation(s):
Walsh, J.
AA(ESO)
Abstract:
A very brief summary of the 2012 SPIE Symposium on Astronomical Telescopes + Instrumentation, held in July in Amsterdam, is presented from the viewpoint of ESO contributions.
References:
Casali, M. 2010, The Messenger, 141, 40

ADS BibCode:
2012Msngr.149...55M
Section:
Astronomical News
Author(s)/Affiliation(s):
Mainieri, V.
AA(ESO)
Abstract:
On 24 May 1982 Italy joined ESO, becoming the eighth Member State. In the past 30 years the participation of Italy in all of ESO’s endeavours has been substantial in all respects: people; fundamental industrial contributions in the construction of telescopes and infrastructures; collaboration of institutes in the development of instrument components; and science programmes. The aim of the symposium was to review critically these past achievements and discuss Italian participation in future ESO projects.

ADS BibCode:
2012Msngr.149...56.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2012Msngr.149...572
Section:
Astronomical News
Author(s)/Affiliation(s):
Rodrigues, M.; Sánchez-Janssen, R.; Spezzi, L.
AA(ESO) AB(ESO) AC(ESO)

ADS BibCode:
2012Msngr.149...59.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)