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Large-scale motions in the universe: Using clusters of galaxies as tracersCan clusters of galaxies be used to trace the large-scale peculiar velocity field of the universe? We answer this question by using large-scale cosmological simulations to compare the motions of rich clusters of galaxies with the motion of the underlying matter distribution. Three models are investigated: Omega = 1 and Omega = 0.3 cold dark matter (CDM), and Omega = 0.3 primeval baryonic isocurvature (PBI) models, all normalized to the Cosmic Background Explorer (COBE) background fluctuations. We compare the cluster and mass distribution of peculiar velocities, bulk motions, velocity dispersions, and Mach numbers as a function of scale for R greater than or = 50/h Mpc. We also present the large-scale velocity and potential maps of clusters and of the matter. We find that clusters of galaxies trace well the large-scale velocity field and can serve as an efficient tool to constrain cosmological models. The recently reported bulk motion of clusters 689 +/- 178 km/s on approximately 150/h Mpc scale (Lauer & Postman 1994) is larger than expected in any of the models studied (less than or = 190 +/- 78 km/s).
Document ID
19950049044
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Gramann, Mirt
(Princeton Univ. Princeton, NJ, United States)
Bahcall, Neta A.
(Princeton Univ. Princeton, NJ, United States)
Cen, Renyue
(Princeton Univ. Princeton, NJ, United States)
Gott, J. Richard
(Princeton Univ. Princeton, NJ, United States)
Date Acquired
August 16, 2013
Publication Date
March 10, 1995
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 441
Issue: 2
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
95A80643
Funding Number(s)
CONTRACT_GRANT: NAGW-2448
CONTRACT_GRANT: NSF AST-91-08103
CONTRACT_GRANT: NSF ASC-93-18185
CONTRACT_GRANT: NSF AST-90-20506
Distribution Limits
Public
Copyright
Other

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