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For refcode 1991ApJ...370...49C:
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Copyright by American Astronomical Society. Reproduced by permission
1991ApJ...370...49C THE JOINT FAR-INFRARED-OPTICAL LUMINOSITY FUNCTION FOR SPIRAL GALAXIES AND DATA FOR THE ABELL 400 AND CANCER CLUSTERS EDVIGE CORBELLI AND EDWIN E. SALPETER Center for Radiophysics and Space Research, Space Sciences Building, Cornell University, Ithaca, NY 14853 AND JOHN M. DICKEY Sterrewacht Leiden; and Department of Astronomy, Universtiy of Minnesota, Minneapolis, MN 55455 Received 1990 March 15; accepted 1990 September 6 ABSTRACT The joint far-infrared-optical luminosity function for late-type galaxies, {PSI}, is examined using an optically selected sample of 183 galaxies from the Revised Shapley-Ames Catalog and from the Virgo Cluster compilation of Helou and coworkers, including peculiar spirals but excluding Sa's. For each of these galaxies we have the far- infrared (FIR) flux at 60 microns, f_60_, and at 100 microns, f_100_ . We show that the distribution of the ratio of FIR to blue luminosity, r = L_FIR_/L_B_, depends weakly on L_B_, so that {PSI} can be approximated by a function of a single variable, {psi}(r'), where r' =r(L_B_/L_*_)^-{sigma}^ with {sigma} ~ 0.08 (~0 for large r) and L_*_ a constant. The function {psi}(r') is well fitted by a lognormal curve which peaks at r' = 0.35 and has a dispersion of 0.28. While an excess of galaxies, with respect to the lognormal curve, is visible for large r', our optically selected sample of nearby galaxies shows that a population of galaxies with very small values of r' is absent. This implies that spiral galaxies with a very low abundance of interstellar dust are rare. We also suggest an explanation for the positive correlation of both r and the FIR color c(c = f_100_/f_60_) with L_B_. By studying the FIR visibility function, we argue that the FIR luminosity function is proportional to @ for large r and that they both decline with a power law of index ~ -2. Using the Minnesota Automated Plate Scanner, we have an optical list of galaxies as faint as 17th magnitude in the blue in two more distant clusters: the Cancer Cluster and Abell 400. For groups of galaxies, optically similar but individually undetected in the FIR, we build up co-added "class average scans" which can give meaningful class average fluxes as small as 50 mJy at 60 microns. Using these, we are able to check the distribution function of r' at the faint FIR end, even in these more distant clusters. Subject headings: galaxies: clustering - galaxies: photometry - infrared: sources - luminosity function
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