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http://inaoe.repositorioinstitucional.mx/jspui/handle/1009/2044| On the formation of cD galaxies and their parent clusters | |
| Tovmassian Hrant | |
| Acceso Abierto | |
| Atribución-NoComercial-SinDerivadas | |
| Galaxies: clusters Clusters: general Galaxies: formation Galaxies: cD galaxies | |
| In order to study the mechanism of formation of cDgalaxies we search for possible dependencies between the K-band luminosity of cDs and the parameters of their host clusters which we select to have a dominant cD galaxy, corresponding to a cluster morphology of Bautz-Morgan (BM) type I. As a comparison sample we use cD galaxies in clusters where they are not dominant, which we define here as non-BMI (NBMI) type clusters. We find that for 71 BMI clusters the absolute K-band luminosity of cDsdepends on the cluster richness, but less strongly on the cluster velocity dispersion. Meanwhile, for 35 NBMI clusters the correlation between cD luminosity and cluster richness is weaker, and is absent between cD In order to study the mechanism of formation of cDgalaxies we search for possible dependencies between the K-band luminosity of cDs and the parameters of their host clusters which we select to have a dominant cD galaxy, corresponding to a cluster morphology of Bautz-Morgan (BM) type I. As a comparison sample we use cD galaxies in clusters where they are not dominant, which we define here as non-BMI (NBMI) type clusters. We find that for 71 BMI clusters the absolute K-band luminosity of cDsdepends on the cluster richness, but less strongly on the cluster velocity dispersion. Meanwhile, for 35 NBMI clusters the correlation between cD luminosity and cluster richness is weaker, and is absent between cD luminosity and velocity dispersion. In addition, we find that the luminosity of the cD galaxy hosted in BMI clusters tends to increase with the cD’s peculiar velocity with respect to the cluster mean velocity. In contrast, for NBMI clusters the cD luminosity decreases with increasing peculiar velocity. Also, the X-ray luminosity of BMI clusters depends on the cluster velocity dispersion, while in NBMI clusters such a correlation is absent. These findings favourthe cannibalism scenario for the formation of cD galaxies. WesuggestthatcDs inclusters of BMI type were formed and evolved preferentially in one and the same cluster. In contrast, cDs in NBMI type clusters were either originally formed in clusters that later merged with groups or clusters to form the current cluster, or are now in the process of merging. | |
| Monthly notices of the royal astronomical society | |
| 2012-12 | |
| Artículo | |
| Inglés | |
| Estudiantes Investigadores Público en general | |
| Tovmassian, Hrant M. and Andernach, Heinz, (2012), On the Formation of cD Galaxies and their Parent Cluster, Monthly notices of the royal astronomical society, Vol. 427(3):1-12 | |
| ASTRONOMÍA Y ASTROFÍSICA | |
| Versión aceptada | |
| acceptedVersion - Versión aceptada | |
| Aparece en las colecciones: | Artículos de Astrofísica |
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