========================================================================== J/ApJ/693/1840 The IR LFs of rich clusters (Bai+, 2009) The following files can be converted to FITS (extension .fit or fit.gz) table1.dat ========================================================================== Query from: http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/ApJ/693/1840 ==========================================================================
drwxr-xr-x 16 cats archive 4096 Jan 29 2012 [Up] drwxr-xr-x 2 cats archive 4096 May 12 10:00 [TAR file] -rw-r--r-- 1 cats archive 467 Dec 5 2011 .message -r--r--r-- 1 cats archive 4098 Apr 14 2011 ReadMe -rw-r--r-- 1 cats archive 607 Dec 5 2011 +footg5.gif -rw-r--r-- 1 cats archive 2159 Dec 5 2011 +footg8.gif -r--r--r-- 1 cats archive 5341 Mar 17 2011 table1.dat [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe : J/ApJ/693/1840 A3266 galaxies at 24um (Bai+, 2009) ================================================================================ The infrared luminosity functions of rich clusters. Bai L., Rieke G.H., Rieke M.J., Christlein D., Zabludoff A.I. <Astrophys. J., 693, 1840-1850 (2009)> =2009ApJ...693.1840B ================================================================================ ADC_Keywords: Clusters, galaxy ; Photometry, infrared ; Galaxies, IR Keywords: galaxies: clusters: individual (Abell 3266) - galaxies: luminosity function, mass function - infrared: galaxies Abstract: We present Multiband Imaging Photometer observations of the cluster A3266. About 100 spectroscopic cluster members have been detected at 24um. The infrared (IR) luminosity function (LF) in A3266 is very similar to that in the Coma cluster down to the detection limit LIR 10^43^erg/s, suggesting a universal form of the bright-end IR LF for local rich clusters with M 10^15^M_sun_. The shape of the bright end of the A3266-Coma composite IR LF is not significantly different from that of nearby field galaxies, but the fraction of IR-bright galaxies (star formation rate (SFR)>0.2M_sun_/yr) in both clusters increases with cluster-centric radius. The decrease of the blue galaxy fraction toward the high-density cores only accounts for part of the trend; the fraction of red galaxies with moderate SFRs (0.2M_sun_/yr<SFR<1M_sun/yr) also decreases with increasing galaxy density. These results suggest that for the IR-bright galaxies nearby rich clusters are distinguished from the field by a lower star forming galaxy fraction, but not by a change in L*_IR_. Description: The A3266 cluster was observed by the Multiband Imaging Photometer for Spitzer (MIPS) in medium scan map mode on 2005 June 28 at 24, 70, and 160um simultaneously. A rectangular 45'x60' region was mapped.
© UDS/CNRS