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arXiv:astro-ph/9602149 (astro-ph)
[Submitted on 28 Feb 1996]

Title:The Peculiar Velocity Function of Galaxy Clusters

Authors:Neta A. Bahcall, Siang Peng Oh (Princeton University Observatory)
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Abstract: The peculiar velocity function of clusters of galaxies is determined using an accurate sample of cluster velocities based on Tully-Fisher distances of Sc galaxies (Giovanelli et al 1995b). In contrast with previous results based on samples with considerably larger velocity uncertainties, the observed velocity function does not exhibit a tail of high velocity clusters. The results indicate a low probability of $\lesssim$\,5\% of finding clusters with one-dimensional velocities greater than $\sim$ 600 {\kms}. The root-mean-square one-dimensional cluster velocity is 293$\pm$28 {\kms}. The observed cluster velocity function is compared with expectations from different cosmological models. The absence of a high velocity tail in the observed function is most consistent with a low mass-density ($\Omega \sim$0.3) CDM model, and is inconsistent at $\gtrsim 3 \sigma$ level with $\Omega$= 1.0 CDM and HDM models. The root-mean-square one-dimensional cluster velocities in these models correspond, respectively, to 314, 516, and 632 {\kms} (when convolved with the observational uncertainties). Comparison with the observed RMS cluster velocity of 293$\pm$28 {\kms} further supports the low-density CDM model.
Comments: revised version accepted for publication in ApJ Letters, 18 pages, uuencoded PostScript with 3 figures included; complete paper available through WWW at this http URL
Subjects: Astrophysics (astro-ph)
Report number: POPe-658
Cite as: arXiv:astro-ph/9602149
  (or arXiv:astro-ph/9602149v1 for this version)
  https://doi.org/10.48550/arXiv.astro-ph/9602149
Related DOI: https://doi.org/10.1086/310041

Submission history

From: Siang Peng Oh [view email]
[v1] Wed, 28 Feb 1996 22:45:08 UTC (57 KB)
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