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1999AJ....117...75C - Astron. J., 117, 75-101 (1999/January-0)
Tides, interactions, and fine-scale substructures in galaxy clusters.
CONSELICE C.J. and GALLAGHER III J.S.
Abstract (from CDS):
Distorted, interacting, and fine-scale substructures have a range of colors extending from blue objects with B-R~0 to redder colors at B-R~2.5. We also find that the structures with the most disturbed morphology have the bluest colors. In addition, the relative number distributions of these structures suggest that two separate classes of galaxy clusters exist: one dominated by distorted structures and the other dominated by galaxy associations. The Coma and Perseus clusters, respectively, are proposed as models for these types of clusters. These structures avoid the deep potentials of the dominant D or cD galaxies in the Coma and Perseus clusters, and tend to clump together.
Possible mechanisms for the production of fine-scale substructure are reviewed and compared with observations of z~0.4 Butcher-Oemler clusters. We conclude, based on color, positional, and statistical data, that the most likely mechanism for the creation of these structures is through an interaction with the gravitational potential of the cluster, possibly coupled with effects of weak interactions with cluster ellipticals.
Abstract Copyright: ∼
Journal keyword(s): Galaxies: Clusters: Individual: Name: Coma - Galaxies: Clusters: Individual: Name: Abell 1656 - Galaxies: Clusters: Individual: Name: Perseus - Galaxies: Clusters: Individual: Name: Abell 2199 - galaxies: clusters: individual (AWM 3, AWM 5) - Galaxies: Evolution - Galaxies: Formation - Galaxies: Interactions
VizieR on-line data: <Available at CDS (J/AJ/117/75): table2.dat table3.dat table4.dat table5.dat table6.dat table10.dat>
Nomenclature: Table 2: [CG99] SA1656-NNN (Nos 1-116). Table 3: [CG99] SA426-NN (Nos 1-69). Table 4: [CG99] SA2199-NN (Nos 1-30). Table 5: [CG99] SAWM5-NN (Nos 1-23). Table 6: [CG99] SAWM3-NN (Nos 1-10).
Simbad objects: 267