Galaxy Properties in Low X-Ray Luminosity Clusters at z=0.25

Details Galaxy Properties in Low X-Ray Luminosity Clusters at z=0.25 Galaxy Properties in Low X-Ray Luminosity Clusters at z=0.25

2002-07-17

arxiv.org/abs/astro-ph/0207360v1

Mon.Not.Roy.Astron.Soc. 337 (2002) 256

Astronomy and Astrophysics

Astrophysics

21 pages in MNRAS style, including 16 figures and 1 long (3 pages) table resubmitted to MNRAS July 16, after making changes re

Scientific paper

10.1046/j.1365-8711.2002.05909.x

We present the first spectroscopic survey of intrinsically low Lx clusters at z>>0, with HST WFPC2 imaging and ground-based spectroscopy. We study 172 confirmed cluster members in a sample of ten clusters at z=0.23-0.3, with Lx<4.E43 h^{-2} ergs/s. The core of each cluster is imaged with WFPC2 in the F702W filter, and the spectroscopic sample is statistically complete to Mr-19.0+5log(h), within an 11' field. The clusters are dynamically well-separated from the surrounding field and the velocity dispersions range from ~350-850 km/s. Emission line galaxies in these clusters are relatively rare, comprising only 22 +/- 4% of the sample. There is no evidence that these emission-line galaxies are dynamically distinct from the majority of the cluster population, though our sample is too small to rule out the ~30% difference that has been observed in more massive clusters. We find eleven galaxies, comprising 6% of the cluster members, which are disk-dominated but show no sign of emission in their spectrum. Most of these are relatively isolated, spiral galaxies with smooth disks. We find no cluster members with a starburst or post-starburst spectrum. The striking similarity between the spectral and morphological properties of galaxies in these clusters and those of galaxies in more massive systems at similar redshifts implies that the physical processes responsible for truncating star formation in galaxies are not restricted to the rare, rich cluster environment, but are viable in much more common environments. In particular, we conclude that ram pressure stripping or cluster-induced starbursts cannot be solely responsible for the low star formation rates in these systems.

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