@Article{CarvalhoCostMourRibe:2019:MaDePr,
               author = "Carvalho, Reinaldo Ramos de and Costa, A. P. and Moura, T. C. and 
                         Ribeiro, A. L. B.",
          affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and 
                         {Universidade Estadual de Santa Cruz} and {Universidade de 
                         S{\~a}o Paulo (USP)} and {Universidade Estadual de Santa Cruz}",
                title = "The mass density profile and star formation history of Gaussian 
                         and non-Gaussian clusters",
              journal = "Monthly Notices of the Royal Astronomical Society",
                 year = "2019",
               volume = "487",
               number = "1",
                pages = "L86--L90",
                month = "July",
             keywords = "galaxies: clusters: general – galaxies:evolution – 
                         galaxies:formation – galaxies:star formation – galaxies:stellar 
                         content – galaxies: interactions.",
             abstract = "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.",
                  doi = "10.1093/mnrasl/slz084",
                  url = "http://dx.doi.org/10.1093/mnrasl/slz084",
                 issn = "0035-8711 and 1365-2966",
             language = "en",
           targetfile = "carvalho_mass.pdf",
        urlaccessdate = "27 abr. 2024"
}