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Date and Time of the Query: 2019-07-15 T17:50:22 PDT
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For refcode 2002ApJ...566..123B:
Retrieve 17 NED objects in this reference.
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Copyright by American Astronomical Society. Reproduced by permission
2002ApJ...566..123B Distinguishing Local and Global Influences on Galaxy Morphology: A Hubble Space Telescope Comparison of High and Low X-Ray Luminosity Clusters Michael L. Balogh, Ian Smail, R. G. Bower, B. L. Ziegler, G. P. Smith, Roger L. Davies, A. Gaztelu, J.-P. Kneib, and H. Ebeling Received 2001 July 11; accepted 2001 September 12 ABSTRACT We present a morphological analysis of 17 X-ray-selected clusters at z ~ 0.25, imaged uniformly with the Hubble Space Telescope Wide Field Planetary Camera 2 (WFPC2). Eight of these clusters comprise a subsample selected for their low X-ray luminosities (<~10^44^ ergs s^-1^), called the low-L_X_ sample. The remaining nine clusters comprise a high-L_X_ subsample with L_X_ > 10^45^ ergs s^-1^. The two subsamples differ in their mean X-ray luminosity by a factor of 30 and span a range of more than 300. The clusters cover a relatively small range in redshift (z = 0.17-0.3, {sigma}_z_/z ~ 0.15), and the data are homogeneous in terms of depth, resolution (0.17" = 1 h_50_^-1^ kpc at z = 0.25), and rest wavelength observed, minimizing differential corrections from cluster to cluster. We fit the two-dimensional surface brightness profiles of galaxies down to very faint absolute magnitudes, M_702_ <= -18.2 + 5 log h_50_ (roughly 0.01L*_R_) with parametric models, and quantify their morphologies using the fractional bulge luminosity (B/T). Within a single WFPC2 image, covering a field of ~3' (1 h_50_^-1^ Mpc at z = 0.25) in the cluster center, we find that the low-L_X_ clusters are dominated by galaxies with low B/T (~0), while the high-L_X_ 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 (98% confidence based on a binned {chi}^2^ test) even when we restrict the comparison to galaxies in environments with similar projected local galaxy densities. A related difference (also of low statistical significance) is seen between the bulge-luminosity functions of the two cluster samples, while no difference is seen between the disk luminosity functions. From the correlations between these quantities, we argue that the global environment affects the population of bulges, over and above trends seen with local density. On the basis of this result, 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, perhaps reflecting a less rich merger history. Subject headings: galaxies: clusters: general - galaxies: evolution - galaxies: structure
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