The shape of velocity dispersion profiles and the dynamical state of galaxy clusters

Autor(es)

Costa, A. P. ^[1] ; Ribeiro, A. L. B. ^[1] ; de Carvalho, R. R. ^[2]

Afiliação do(s) autor(es)

^[1] Univ Estadual Santa Cruz, Lab Astrofis Teor & Observac, BR-45650000 Ilheus, BA - Brazil

^[2] Div Astrofis INPE MCT, BR-12227010 Sao Jose Dos Campos, SP - Brazil

• Tipo de documento: Artigo Científico
• Fonte: Monthly Notices of the Royal Astronomical Society; v. 473, n. 1, p. L31-L35, JAN 2018.
• Citações Web of Science: 5

Resumo

Motivated by the existence of the relationship between the dynamical state of clusters and the shape of the velocity dispersion profiles (VDPs), we study the VDPs for Gaussian (G) and non-Gaussian (NG) systems for a subsample of clusters from the Yang catalogue. The groups cover a redshift interval of 0.03 <= z <= 0.1 with halo mass >= 10(14) M-circle dot. We use a robust statistical method, Hellinger Distance, to classify the dynamical state of the systems according to their velocity distribution. The stacked VDP of each class, G and NG, is then determined using either Bright or Faint galaxies. The stacked VDP for G groups displays a central peak followed by a monotonically decreasing trend which indicates a predominance of radial orbits, with the Bright stacked VDP showing lower velocity dispersions in all radii. The distinct features we find in NG systems are manifested not only by the characteristic shape of VDP, with a depression in the central region, but also by a possible higher infall rate associated with galaxies in the Faint stacked VDP. (AU)

• Processo FAPESP: 14/11156-4 - O que determina o crescimento da massa estelar de galáxias elípticas? Intrínseco ou ambiente: a saga contínua
• Beneficiário: Reinaldo Ramos de Carvalho
• Modalidade de apoio: Auxílio à Pesquisa - Temático