THE ASTRONOMICAL JOURNAL    VOLUME 113, NUMBER 4, PAGE 1197         APRIL 1997

             21 cm H I LINE SPECTRA OF GALAXIES IN NEARBY CLUSTERS

                   MARTHA P. HAYNES AND RICCARDO GIOVANELLI

     Center for Radiophysics and Space Research and National Astronomy and
         Ionosphere Center, Cornell University, Ithaca, New York 14853

                        TERRY HERTER AND NICOLE P. VOGT

        Center for Radiophysics and Space Research, Cornell University,
                            Ithaca, New York 14853

                               WOLFRAM FREUDLING

     Space Telescope-European Coordinating Facility and European Southern
 Observatory, Karl Schwarzschild Str. 2, D-85748 Garching b. Munchen, Germany

                               MARCIO A. G. MAIA

      Departamento de Astronomia, Observatorio Nacional, Rua General Jose
     Cristino 77, Rio de Janeiro, 20921-030, Brazil National Astronomy and
         Ionosphere Center, Cornell University, Ithaca, New York 14853

                                 JOHN J. SALZER

                 Department of Astronomy, Wesleyan University,
                         Middletown, Connecticut 06459

                                  GARY WEGNER

            Department of Physics and Astronomy, Dartmouth College,
                          Hanover, New Hampshire 03755

    A compilation of H I line fluxes, systemic velocities and linewidths is
    presented for 840 detected galaxies, mostly in the vicinities of 30
    nearby rich clusters out to a redshift of z~.04, specifically for use
    in applications of the Tully-Fisher distance method. New 21 cm H I line
    profiles have been obtained for ~500 galaxies in 27 Abell clusters
    visible from Arecibo. Upper limits are also presented for 246 galaxies
    for which H I emission was not detected. In order to provide a
    homogeneous linewidth determination optimized for Tully-Fisher studies,
    these new data are supplemented by the reanalysis of previously
    published spectra obtained both at Arecibo and Green Bank that are
    available in a digital archive. Corrections for instrumental
    broadening, smoothing, signal-to-noise and profile shape are applied,
    and an estimate of the error on the width is given. When corrected for
    turbulent broadening and viewing angle, the corrected velocity widths
    presented here will provide the appropriate line width parameter needed
    to derive distances via the Tully-Fisher relation. (Copyright) 1997
    American Astronomical Society.