Deviations from the Fundamental Plane and the Peculiar Velocities of Clusters

Details Deviations from the Fundamental Plane and the Peculiar Velocities of Clusters Deviations from the Fundamental Plane and the Peculiar Velocities of Clusters

1999-03-24

arxiv.org/abs/astro-ph/9903380v2

Astronomy and Astrophysics

Astrophysics

20 pages, including 7 figures, revised and lengthened

Scientific paper

We have fit the Fundamental Plane of Ellipticals (FP) to over 400 early-type galaxies in 20 nearby clusters (4000 < cz < 11000 km/s), using our own photometry and spectroscopy as well as measurements culled from the literature. We find that the quality-of-fit, r.m.s.[log(sigma)], to the average fundamental plane varies substantially among these clusters. A statistically significant gap in r.m.s.[log(sigma)] roughly separates the clusters which fit well from those that do not. In addition, these two groups of clusters show distinctly different behavior in their peculiar velocity (PV) distributions. Assuming galaxies are drawn from a single underlying population, cluster PV should not be correlated with r.m.s.[log(sigma)]. Instead, the clusters with below average scatter display no motion with respect to the cosmic microwave background (CMB) within our measurement errors (~250 km/s), while clusters in the poor-fit group typically show large PVs. Furthermore, we find that all X-ray bright clusters in our sample fit the well, suggesting that early-type galaxies in the most massive, virialized clusters form a more uniform population than do cluster ellipticals as a whole, and that these clusters participate in a quiet Hubble flow.

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