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For refcode 1994AJ....107.1962B:
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1994AJ....107.1962B TESTS OF THE TULLY-FISHER RELATION. I. SCATTER IN INFRARED MAGNITUDE VERSUS 21 cm WIDTH GARY M. BERNSTEIN Bok Fellow, Steward Observatory, University of Arizona, Tucson, Arizona 85721 Electronic mail: gbernstein@as.artzona.edu PUPAGRA GUHATHAKURTA Hubble Fellow, Princeton University Observatory, Peyton Hall, Princeton, New Jersey 08544-1001 Electronic mail: raja@stsci.edu SOMAK RAYCHAUDHURY Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138 Electronic mail: somak@harlow.harvard.edu RICCARDO GIOVANELLI, MARTHA P. HAYNES, TERRY HERTER, AND NIOCOLE P. VOGT Cornell University, Center for Radiophysics and Space Research, Space Sciences Building, Ithaca, New York 14853 Electronic mail: haynes,riccardo,vogt,hetter@astrosun.tn.cornell.edu Received 1993 December 21; revised 1994 February 11 ABSTRACT We examine the precision of the Tully-Fisher relation (TFR) using a sample of galaxies in the Coma region of the sky, and find that it is good to 5% or better in measuring relative distances. Total magnitudes and disk axis ratios are derived from H and I band surface photometry, and Arecibo 21 cm profiles define the rotation speeds of the galaxies. Using 25 galaxies for which the disk inclination and 21 cm width are well defined, we find an rms deviation of 0.10 mag from a linear TFR with dI/d(log W_c_) = -5.6. Each galaxy is assumed to be at a distance proportional to its redshift, and an extinction correction of 1.4(1-b/a) mag is applied to the total I magnitude. The measured scatter is < 0.15 mag using milder extinction laws from the literature. The I band TFR scatter is consistent with measurement error, and the 95% CL limits on the intrinsic scatter are 0-0.10 mag. The rms scatter using H band magnitudes is 0.20 mag (N = 17). The low width galaxies have scatter in H significantly in excess of known measurement error, but the higher width half of the galaxies have scatter consistent with measurement error. The H band TFR slope may be as steep as the I band slope. As the first applications of this tight correlation, we note the following: (1) the data for the particular spirals commonly used to define the TFR distance to the Coma cluster are inconsistent with being at a common distance and are in fact in free Hubble expansion, with an upper limit of 300 km s^-1^ on the rms peculiar line-of-sight velocity of these gas-rich spirals; and (2) the gravitational potential in the disks of these galaxies has typical ellipticity <5%. The published data for three nearby spiral galaxies with Cepheid distance determinations are inconsistent with our Coma TFR, suggesting that these local calibrators are either ill-measured or peculiar relative to the Coma Supercluster spirals, or that the TFR has a varying form in different locales.
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