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(Referência obtida automaticamente do Web of Science, por meio da informação sobre o financiamento pela FAPESP e o número do processo correspondente, incluída na publicação pelos autores.)

The mass density profile and star formation history of Gaussian and non-Gaussian clusters

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Autor(es):
de Carvalho, R. R. [1, 2] ; Costa, A. P. [3] ; Moura, T. C. [4] ; Ribeiro, A. L. B. [3]
Número total de Autores: 4
Afiliação do(s) autor(es):
[1] Univ Cidade Sao Paulo, Univ Cruzeiro Sul, NAT, BR-01506000 Sao Paulo - Brazil
[2] INPE, Div Astrofis, BR-12227010 Sao Jose Dos Campos - Brazil
[3] Univ Estadual Santa Cruz, Lab Astrofis Teor & Observac, BR-45650000 Ilheus, BA - Brazil
[4] Univ Sao Paulo, Inst Astrofis & Geofis, Dept Astron, BR-05508090 Sao Paulo, SP - Brazil
Número total de Afiliações: 4
Tipo de documento: Artigo Científico
Fonte: Monthly Notices of the Royal Astronomical Society; v. 487, n. 1, p. L86-L90, JUL 2019.
Citações Web of Science: 1
Resumo

This paper is the third of a series in which we investigate the discrimination between Gaussian (G) and Non-Gaussian (NG) clusters, based on the velocity distribution of the member galaxies. We study a sample of 177 groups from the Yang catalog in the redshift interval of 0.03 <= z <= 0.1 and masses >= 10(14) M-circle dot. Examining the projected stellar mass density distributions of G and NG groups, we find strong evidence of a higher infall rate in the outskirts of NG groups over the G ones. There is a 61 per cent excess of faint galaxies in NGs when contrasted with G groups, when integrating from 0.8 to 2.OR/R-200. The study of the star formation history (SFH) of ellipticals and spirals in the three main regions of the projected phase space reveals also that the star formation in faint spirals of NG groups is significantly different from their counterpart in the G groups. The assembled mass for faint spirals varies from 59 per cent at 12.7 Gyr to 75 per cent at 8.0 Gyr, while in G systems this variation is from 82 per cent to 91 per cent. This finding may also be interpreted as a higher in fall rate of gas-rich systems in NG groups. This accretion process through the filaments, disturbing the velocity distribution and modifying not only the stellar population of the incoming galaxies but also their SFH, should be seriously considered in modelling galaxy evolution. (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
Linha de fomento: Auxílio à Pesquisa - Temático
Processo FAPESP: 18/03480-7 - Modelamento de espectros integrados de aglomerados globulares e galáxias
Beneficiário:Tatiana Coelho de Moura Bastos
Linha de fomento: Bolsas no Brasil - Pós-Doutorado