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The Arecibo Galaxy Environment Survey – II. A H i view of the Abell cluster 1367 and its outskirts
Authors:L Cortese  R F Minchin  R R Auld  J I Davies  B Catinella  E Momjian  J L Rosenberg  R Taylor  G Gavazzi  K O'Neil  M Baes  A Boselli  G Bothun  B Koribalski  S Schneider  W van Driel
Institution:School of Physics and Astronomy, Cardiff University, Cardiff CF24 3AA;NAIC-Arecibo Observatory, HC3 Box 53995, Arecibo, PR 00612, USA;Max-Planck-Institut für Astrophysik, D-85748 Garching, Germany;Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS 65, Cambridge, MA 02138-1516, USA;Universitádegli Studi di Milano-Bicocca, Piazza della Scienza 3, 20126 Milano, Italy;National Radio Astronomy Observatory, Green Bank, WV 24944, USA;Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, B-900 Gent, Belgium;Laboratoire d'Astrophysique de Marseille, BP8, Traverse du Siphon, F-13376 Marseille, France;Physics Department, University of Oregon, 1371 East 13th Avenue, Eugene, OR 97403, USA;Australia Telescope National Facility, CSIRO, Epping, NSW, Australia;Department of Astronomy, University of Massachusetts, Amherst, MA 01003, USA;Observatoire de Meudon, 5 Place Jules Janssen, 92195 Meudon, France;NRAO, P.O. Box O, Socorro, NM 87801, USA
Abstract:We present 21 cm H  i line observations of 5 × 1 deg2 centred on the local Abell cluster 1367 obtained as part of the Arecibo Galaxy Environment Survey. One hundred sources are detected (79 new H  i measurements and 50 new redshifts), more than half belonging to the cluster core and its infalling region. Combining the H  i data with Sloan Digital Sky Survey (SDSS) optical imaging, we show that our H  i selected sample follows scaling relations similar to the ones usually observed in optically selected samples. Interestingly, all galaxies in our sample appear to have nearly the same baryon fraction independently of their size, surface brightness and luminosity. The most striking difference between H  i and optically selected samples resides in their large-scale distribution: whereas optical and X-ray observations trace the cluster core very well, in H  i there is almost no evidence of the presence of the cluster. Some implications on the determination of the cluster luminosity function and H  i distribution for samples selected at different wavelength are also discussed.
Keywords:surveys  galaxies: clusters: individual: A1367  galaxies: evolution  galaxies: peculiar  radio lines: galaxies
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