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For refcode 1997AJ....113.1197H:
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Copyright by American Astronomical Society. Reproduced by permission
1997AJ....113.1197H 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 Electronic mail: haynes@astrosun.tnycornell.edu. riccardo@astrosun.tn.cornell.edu. TERRY HERTER AND NICOLE P. VOGT Center for Radiophysics and Space Research, Cornell University, Ithaca, New York 14853 Electronic mail: herter@astrosrnn.tn.cornell.edu, nicole@lick.ucsc.edu WOLFRAM FREUDLlNG Space Telescope-European Coordinating Facility and European Southern Observatory, Karl Schwarzschild Str. 2, D-85748 Garching b. Munchen. Germany Electronic mail: wfreudli@eso.org MARCIO A. G. MAIA Departamento de Astronomia, Observatorio Nacional, Rua General Jose Cristino 77, Rio de Janeiro, 20921-030, Brazil, and National Astronomy and Ionosphere Center, Cornell University, Ithaca, New York 14853 Electronic mail: maia@on.br JOHN J. SALZER Department of Astronomy, Wesleyan University, Middletown, Connecticut 06459 Electronic mail: slaz@parcha.astro.wesleyan.edu GARY WEGNER Department of Physics and Astronomy, Dartmouth College, Hanover, New Hampshire 03755 Electronic mail: wegner@kayz.dartmouth.edu Received 1996 December 11; revised 1996 December 20 ABSTRACT 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 HI 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.
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