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Galaxy morphologies and star-formation rates depend on environment. Galaxiesin under-dense regions are generally star-forming and disky whereas galaxies inoverdense regions tend to be early-type and not actively forming stars. Themechanism(s) responsible for star-formation quenching and morphologicaltransformation remain unclear, although many processes have been proposed. Westudy the dependence of star-formation and morphology on X-ray luminosity forgalaxies in Sloan Digital Sky Survey Data Release 7 (SDSS-DR7) groups andclusters. While controlling for stellar and halo mass dependencies, we findthat galaxies in X-ray strong groups and clusters have preferentially lowstar-forming and disk fractions -- with the differences being strongest at lowstellar masses. The trends that we observe do not change when considering onlygalaxies found within or outside of the X-ray radius of the host group. Whenconsidering central and satellite galaxies separately we find that thisdependence on X-ray luminosity is only present for satellites, and we show thatour results are consistent with "galaxy stangulation" as a mechanism forquenching these satellites. We investigate the dynamics of the groups andclusters in the sample, and find that the velocity distributions of galaxiesbeyond the virial radius in low X-ray luminosity halos tend to be less Gaussianin nature than the rest of the data set. This may be indicative of low X-rayluminosity groups and clusters having enhanced populations of star-forming anddisk galaxies as a result of recent accretion.

Comparing galaxy disk and star-formation properties in X-ray bright and faint groups and clusters