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Elliptical Galaxies and Large-Scale Velocity Flows

Published online by Cambridge University Press:  03 August 2017

S. M. Faber ,
David Burstein ,
Roger L. Davies ,
Alan Dressler ,
Donald Lynden-Bell ,
Roberto Terlevich  and
Gary Wegner
S. M. Faber
Affiliation:
Lick Observatory, U.C. Santa Cruz
David Burstein
Affiliation:
Dept. of Physics, Arizona State University
Roger L. Davies
Affiliation:
Kitt Peak National Observatory
Alan Dressler
Affiliation:
Mt. Wilson-Las Campanas Observatories
Donald Lynden-Bell
Affiliation:
Institute of Astronomy, Cambridge, England
Roberto Terlevich
Affiliation:
Royal Greenwich Observatory
Gary Wegner
Affiliation:
Dept. of Physics & Astronomy, Dartmouth College

Abstract

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Motions of nearby elliptical galaxies reveal a large-scale velocity flow relative to cosmic rest towards the point 1=307±10, b = 9±10. The data are fit best by a two-component flow model. The smaller component is due to Virgo, which induces a velocity at the Local Group of 250 km/s. The main flow is due to a more massive concentration located a distance of 4350±350 km/s towards 1=307, b=9, which induces a local velocity here of 570±60 km/s. This larger component falls off away from the mass concentration roughly as r−1. The Centaurus double cluster and its neighbors are in the direction of the mass concentration but are in the foreground and are falling into it. Galaxy counts, radial velocity surveys, and the motions of nearby spirals are consistent with the above model. The IRAS dipole results are less clear but may also be consistent. There is evidence that the distant mass concentration is non-spherical, with the Centaurus cloud a substantial sub-condensation in the foreground. The formal agreement of the large-scale flow with biased (b=2) cold dark matter is low, but the simple methods used so far to assess this are uncertain. The main weakness of the present data in comparing to theory is the fact that they do not penetrate far enough to show the velocity field on all sides of the mass concentration. Sphericity and total extent of the flow are therefore still unknown.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 130: Large Scale Structures of the Universe , 1988 , pp. 169 - 176
Copyright
Copyright © Reidel 1988 

References

Aaronson, M., Huchra, J., Mould, J., Schechter, P.L., and Tully, R.B. 1982, Ap. J., 258, 64.CrossRefGoogle Scholar
da Costa, L.N., Nunes, M.A., Pellegrini, P.S., and Willmer, C. 1986, A. J., 91, 6.Google Scholar
de Vaucouleurs, G., and Peters, W. L. 1985, Ap. J., 297, 27.CrossRefGoogle Scholar
Dressler, A., Faber, S. M., Burstein, D., Davies, R.L., Lynden-Bell, D., Terlevich, R., and Wegner, G. 1987, Ap. J., 313, 42.Google Scholar
Faber, S. M., Wegner, G. Burstein, D., Davies, R. L., Dressler, A., Lynden-Bell, D., and Terlevich, R. 1988, in preparation.Google Scholar
Lilje, P., Yahil, A., and Jones, B.J.T. 1986, Ap. J., 307, 91.Google Scholar
Lynden-Bell, D., Faber, S.M., Burstein, D., Davies, R. L., Dressler, A., Terlevich, R., and Wegner, G. 1988, Ap. J., in press.Google Scholar
Meiksin, A., and Davis, M. J. 1986, A. J., 91, 191.CrossRefGoogle Scholar
Shaya, E. J. 1984, Ap. J., 280, 470.Google Scholar
Tammann, G. A., and Sandage, A. 1985, Ap. J., 294, 81.Google Scholar
Yahil, A., Walker, D., and Rowan-Robinson, M. 1986, Ap. J. (Letters), 301, L1.CrossRefGoogle Scholar