Distinguishing Local and Global Influences on Galaxy Morphology: An HST Comparison of High and Low X-ray Luminosity Clusters

Details Distinguishing Local and Global Influences on Galaxy Morphology: An HST Comparison of High and Low X-ray Luminosity Clusters Distinguishing Local and Global Influences on Galaxy Morphology: An HST Comparison of High and Low X-ray Luminosity Clusters

2001-10-15

arxiv.org/abs/astro-ph/0110326v1

Astronomy and Astrophysics

Astrophysics

Astrophysical Journal, accepted (tent. Feb 10 2002, vol 566) 13 pages, emulateapj style with 9 in-line figures

Scientific paper

10.1086/338056

(Abridged) We present a morphological analysis of 17 X-ray selected clusters at z~0.25, imaged uniformly with HST WFPC2. Eight of these clusters have low X-ray luminosities (<10^{44} erg/s), while the remaining nine clusters have L_x>10^{45} ergs/s. The clusters cover a relatively small range in redshift and the data are homogeneous in terms of depth, resolution and rest wavelength observed. We use GIM2D to fit the two dimensional surface brightness profiles of galaxies down to M(702)<=-18.2 (Ho=50; roughly 0.01 L*) with parametric models, and quantify their morphologies using the fractional bulge luminosity (B/T). Within a single WFPC2 image we find that the Low-Lx clusters are dominated by galaxies with low B/T (~0), while the High-Lx clusters are dominated by galaxies with intermediate B/T (~0.4). We test whether this difference could arise from a universal morphology-density relation due to differences in the typical galaxy densities in the two samples. We find that small differences in the B/T distributions of the two samples persist with marginal statistical significance even when we restrict the comparison to galaxies in environments with similar projected local galaxy densities. From the correlations with the bulge and disk luminosity functions, we argue that the global environment affects the population of bulges, over and above trends seen with local density. We conclude that the destruction of disks through ram pressure stripping or harassment is not solely responsible for the morphology-density relation, and that bulge formation is less efficient in low mass clusters.

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