The Galaxy population of the Poor Cluster RXJ 1252.0-2920 ([VMF98] 124) at z ˜ 0.2

Details The Galaxy population of the Poor Cluster RXJ 1252.0-2920 ([VMF98] 124) at z ˜ 0.2 The Galaxy population of the Poor Cluster RXJ 1252.0-2920 ([VMF98] 124) at z ˜ 0.2

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006rmxac..26..199t&link_type=abstract

XI IAU Regional Latin American Meeting of Astronomy (Eds. L. Infante & M. Rubio) Revista Mexicana de Astronomía y Astrofísica (S

Astronomy and Astrophysics

Astronomy

Scientific paper

The majority of the galaxies in the Universe are concentrated in low-density environments. For intermediate redshift, z ˜ 0.2 - 0.5, while rich clusters of galaxies have been widely studied, the intermediate-mass systems, those between loose groups and rich clusters of galaxies have received comparatively little attention, either in the X-rays or in the optical. In the optical, many works have focused on the study of the galaxy population at intermediate redshifts, but mostly in rich cluster of galaxies.
In this work, we investigate the galaxy population in the poor cluster of galaxy RXJ 1252.0-2920 ([VMF98]124, Vikhlinin et al. 1998, ApJ, 502, 558). The analysis is based on deep imaging and spectroscopic observations obtained at Gemini South with the Gemini Multiobject Spectrograph. Located at z = 0.1853, the cluster has a low X-ray luminosity (L_X = 3.2×10^{43} erg s^{-1}) and a moderate velocity dispersion (578 km s^{-1}). We performed a galaxy classification by using the B/T ratio obtained with the GIM2D software (Simard et al. 2002, ApJS, 142, 1) and the break at 4000 Å endtex2html[d]eferred and the equivalent width of Hδ ``Balmer'' spectral indices, in order to study the morphological segregation in a low density environment. The results given by the Balogh's diagram (4000Å (Δ - W_0(Hδ) plane, Balogh et al. 1999, ApJ, 527, 54) show that the majority of the galaxies in this cluster are passive (no significant star formation is found). Also, there exist a correlation between the 4000 Å break and the B/T ratio that is in a good agreement with classification given by the Balogh's diagram (all galaxies with a reliable B/T measurement are passives). The morphological-radius relation shows a week correlation: the fraction of passive galaxies decrease at larger radius, as expected for this population of galaxies in clusters.

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