========================================================================== J/ApJ/669/821 CO Tully-Fisher relation for host galaxies of QSOs (Ho+, 2007) The following files can be converted to FITS (extension .fit or fit.gz) table1.dat table2.dat ========================================================================== Query from: http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/ApJ/669/821 ==========================================================================
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Beginning of ReadMe : J/ApJ/669/821 CO Tully-Fisher relation for host galaxies of QSOs (Ho+, 2007) ================================================================================ The CO Tully-Fisher relation and implications for the host galaxies of high-redshift quasars. Ho L.C. <Astrophys. J., 669, 821-829 (2007)> =2007ApJ...669..821H ================================================================================ ADC_Keywords: QSOs ; Active gal. nuclei ; Spectroscopy Keywords: galaxies: bulges - galaxies: ISM - galaxies: kinematics and dynamics - galaxies: nuclei - galaxies: Seyfert - quasars: general Abstract: The integrated line width derived from CO spectroscopy provides a powerful tool to study the internal kinematics of extragalactic objects, including quasars at high redshift, provided that the observed line width can be properly translated to more conventionally used kinematical parameters of galaxies. We show, through the construction of a Ks-band CO Tully-Fisher relation for nearby galaxies spanning a wide range in infrared luminosity, that the CO line width measured at 20% of the peak intensity, when corrected for inclination and other effects, successfully recovers the maximum rotation velocity of the disk. The line width at 50% of the peak intensity performs much more poorly, in large part because CO lines have a wide range of profiles, which are shown to vary systematically with infrared luminosity. We present a practical prescription for converting observed CO line widths into the stellar velocity dispersion of the bulge (sigma*) and then apply it to a sample of low-redshift (z< 0.2) and high-redshift (1.4< z< 6.4) quasars to study their host galaxies.