Detalles de publicación

PP 010077

HerMES : SPIRE detection of high redshift massive compact galaxies in GOODS-N field

A. Cava,1,2; G. Rodighiero,3 I. Pérez-Fournon,1,2 F. Buitrago,4 I. Trujillo,1,2 B. Altieri,5 A. Amblard,6 R. Auld,7 J. Bock,8,9 D. Brisbin,10 D. Burgarella,11 N. Castro-Rodríguez,1,2 P. Chanial,12 M. Cirasuolo,13 D.L. Clements,12 C.J. Conselice,4 A. Cooray,6,8 S. Eales,7 D. Elbaz,14 P. Ferrero,1,2 A. Franceschini,3 J. Glenn,15 E.A. González Solares,16 M. Griffin,7 E. Ibar,13 R.J. Ivison,13,17 L. Marchetti,3 G.E. Morrison,18,19 A.M.J. Mortier,12 S.J. Oliver,20 M.J. Page,21 A. Papageorgiou,7 C.P. Pearson,22,23 M. Pohlen,7 J.I. Rawlings,21 G. Raymond,7 D. Rigopoulou,22,24 I.G. Roseboom,20 M. Rowan-Robinson,12 D. Scott,25 N. Seymour,21 A.J. Smith,20 M. Symeonidis,21 K.E. Tugwell,21 M. Vaccari,3 I. Valtchanov,5 J.D. Vieira,8 L. Vigroux,26 L. Wang20 and G. Wright13
1Instituto de Astrofísica de Canarias (IAC), E-38200 La Laguna, Tenerife, Spain 2Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38205 La Laguna, Tenerife, Spain 3Dipartimento di Astronomia, Universit`a di Padova, vicolo Osservatorio, 3, 35122 Padova, Italy 4School of Physics and Astronomy, University of Nottingham, NG7 2RD, UK 5Herschel Science Centre, European Space Astronomy Centre, Villanueva de la Ca˜nada, 28691 Madrid, Spain 6Dept. of Physics & Astronomy, University of California, Irvine, CA 92697, USA 7Cardiff School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff CF24 3AA, UK 8California Institute of Technology, 1200 E. California Blvd., Pasadena, CA 91125, USA 9Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USA 10Space Science Building, Cornell University, Ithaca, NY, 14853-6801, USA 11Laboratoire d’Astrophysique de Marseille, OAMP, Universit´e Aix-marseille, CNRS, 13388 Marseille cedex 13, France 12Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ, UK 13UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK 14Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu - CNRS - Universit´e Paris Diderot, CE-Saclay, F-91191 Gif-sur-Yvette, France 15Dept. of Astrophysical and Planetary Sciences, CASA 389-UCB, University of Colorado, Boulder, CO 80309, USA 16Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 17Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK 18Institute for Astronomy, University of Hawaii, Honolulu, HI 96822, USA 19Canada-France-Hawaii Telescope, Kamuela, HI, 96743, USA 20Astronomy Centre, Dept. of Physics & Astronomy, University of Sussex, Brighton BN1 9QH, UK 21Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey RH5 6NT, UK 22Space Science & Technology Department, Rutherford Appleton Laboratory, Chilton, Didcot, Oxfordshire OX11 0QX, UK 23Institute for Space Imaging Science, University of Lethbridge, Lethbridge, Alberta, T1K 3M4, Canada 24Astrophysics, Oxford University, Keble Road, Oxford OX1 3RH, UK 25Department of Physics & Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, Canada 26Institut d’Astrophysique de Paris, UMR 7095, CNRS, UPMC Univ. Paris 06, 98bis boulevard Arago, F-75014 Paris, France
ABSTRACT
We have analysed the rest-frame far infrared (FIR) properties of a sample of massive (Mstar > 10^11Msun) galaxies at 2 < z < 3 in the GOODS (Great Observatories Origins Deep Survey) North field using the Spectral and Photometric Imaging Receiver (SPIRE) instrument aboard the Herschel Space Observatory. To conduct this analysis we take advantage of the data from the HerMES key program. The sample comprises 45 massive galaxies with structural parameters characterised with HST NICMOS-3. We study detections at submm Herschel bands, together with Spitzer 24{\mu}m data, as a function of the morphological type, mass and size. We find that 26/45 sources are detected at MIPS-24{\mu}m and 15/45 (all MIPS-24{\mu}m detections) are detected at SPIRE-250{\mu}m, with disk-like galaxies more easily detected. We derive star formation rates (SFR) and specific star formation rates (sSFR) by fitting the spectral energy distribution (SED) of our sources, taking into account non-detections for SPIRE and systematic effects for MIPS derived quantities. We find that the mean SFR for the spheroidal galaxies (50-100 Msun*yr^-1) is substantially (a factor ~ 3) lower than the mean value presented by disk-like galaxies (250-300 Msun*yr^-1).

 
Aceptado para publicación en Herschel Special Issue | Enviado el 2010-11-05 | Proyecto 3E3207