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Spiral Galaxies and the Peculiar Velocity Field

Published online by Cambridge University Press:  25 May 2016

Riccardo Giovanelli ,
Martha P. Haynes ,
Pierre Chamaraux ,
Luiz N. Da Costa ,
Wolfram Freudling ,
John J. Salzer  and
Gary Wegner
Riccardo Giovanelli
Affiliation:
Cornell University, Ithaca, NY, USA
Martha P. Haynes
Affiliation:
Cornell University, Ithaca, NY, USA
Pierre Chamaraux
Affiliation:
Observatoire de Meudon, Meudon, France
Luiz N. Da Costa
Affiliation:
Observatorio Nacional, Rio de Janeiro, Brazil and Institut d'Astrophysique, Paris, France
Wolfram Freudling
Affiliation:
ESO ST–European Coordinating Facility, Garching, Germany
John J. Salzer
Affiliation:
Wesleyan University, Middletown, CT, USA
Gary Wegner
Affiliation:
Dartmouth College, Hanover, NH, USA

Abstract

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We report results of a redshift-independent distance measurement survey that extends to all sky and out to a redshift of approximately 7500 km s−1. Tully–Fisher (TF) distances for a homogeneous sample of 1600 late spiral galaxies are used to analyze the peculiar velocity field. We find large peculiar velocities in the neighborhood of superclusters, such as Perseus–Pisces (PP) and Hydra–Centaurus, but the main clusters embedded in those regions appear to be virtually at rest in the CMB reference frame. We find no compelling evidence for large-scale bulk flows, whereby the Local Group, Hydra–Cen and PP would share a motion of several hundred km s−1 with respect to the CMB. Denser sampling in the PP region allows a clear detection of infall and backflow motions, which can be used to map the mass distribution in the supercluster and to obtain an estimate of the cosmological density parameter.

Type
Part I: Invited Reviews
Information
Symposium - International Astronomical Union , Volume 168: Examining the Big Bang and the Diffuse Background Radiations , 1996 , pp. 183 - 191
Copyright
Copyright © Kluwer 1996 

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