Scaling relations in early-type galaxies belonging to groups

Details Scaling relations in early-type galaxies belonging to groups Scaling relations in early-type galaxies belonging to groups

2003-12-11

arxiv.org/abs/astro-ph/0312292v1

Mon.Not.Roy.Astron.Soc. 349 (2004) 527

Astronomy and Astrophysics

Astrophysics

Accepted for publication in MNRAS, 8 pages, 8 postscript figures

Scientific paper

10.1111/j.1365-2966.2004.07517.x

We present a photometric analysis of a large sample of early-type galaxies in 16 nearby groups, imaged with the Wide-Field Camera on the Isaac Newton Telescope. Using a two-dimensional surface brightness decomposition routine, we fit Sersic (r^{1/n}) and exponential models to their bulge and disk components respectively. Dividing the galaxies into three subsamples according to the X-ray luminosities of their parent groups, we compare their photometric properties. Galaxies in X-ray luminous groups tend to be larger and more luminous than those in groups with undetected or low X-ray luminosities, but no significant differences in n are seen. Both normal and dwarf elliptical galaxies in the central regions of groups are found to have cuspier profiles than their counterparts in group outskirts. Structural differences between dwarf and normal elliptical galaxies are apparent in terms of an offset between their ``Photometric Planes'' in the space of n, r_e and mu_0. Dwarf ellipticals are found to populate a surface, with remarkably low scatter, in this space with significant curvature, somewhat similar to the surfaces of constant entropy proposed by Marquez etal (2001). Normal ellipticals are offset from this distribution in a direction of higher specific entropy. This may indicate that the two populations are distinguished by the action of galaxy merging on larger galaxies.

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