@Article{RibeiroCaTrCaLaLoSc:2013:ClGaGr,
author = "Ribeiro, A. L. B. and Carvalho, Reinaldo Ramos de and Trevisan,
Marina and Capelato, Hugo Vicente and La Barbera, F. and Lopes, P.
A. A. and Schilling, A. C.",
affiliation = "Laborat{\'o}rio de Astrof{\'{\i}}sica Te{\'o}rica e
Observacional, Universidade Estadual de Santa Cruz-45650-000,
Ilh{\'e}us-BA, Brazil and {Instituto Nacional de Pesquisas
Espaciais (INPE)} and {Instituto Nacional de Pesquisas Espaciais
(INPE)} and {Instituto Nacional de Pesquisas Espaciais (INPE)} and
INAF-Osservatorio Astronomico di Capodimonte, Napoli, Italy and
Observat{\'o}rio do Valongo, Universidade Federal do Rio de
Janeiro, Brazil and Laborat{\'o}rio de Astrof{\'{\i}}sica
Te{\'o}rica e Observacional, Universidade Estadual de Santa
Cruz-45650-000, Ilh{\'e}us-BA, Brazil",
title = "SPIDER IX - Classifying galaxy groups according to their velocity
distribution",
journal = "Monthly Notices of the Royal Astronomical Society",
year = "2013",
volume = "434",
number = "1",
pages = "784--795",
keywords = "galaxies, groups, general.",
abstract = "We introduce a new method to study the velocity distribution of
galaxy systems, the Hellinger Distance (HD), designed for
detecting departures from a Gaussian velocity distribution.
Testing different approaches to measure normality of a
distribution, we conclude that HD is the least vulnerable method
to type I and II statistical errors. We define a relaxed galactic
system as the one with unimodal velocity distribution and a
normality deviation below a critical value (HD < 0.05). In this
work, we study the Gaussian nature of the velocity distribution of
the Berlind group sample, and of the FoF groups from the
Millennium simulation. For the Berlind group sample (z < 0.1), 67
per cent of the systems are classified as relaxed, while for the
Millennium sample we find 63 per cent (z = 0). We verify that in
multi-modal groups the average mass of modes in high-multiplicity
(N >= 20) systems are significantly larger than in
low-multiplicity ones (N < 20), suggesting that groups experience
a mass growth at an increasing virialization rate towards z = 0,
with larger systems accreting more massive subunits. We also
investigate the connection between galaxy properties ([Fe/H], Age,
eClass, g-r, Rpetro and <mu_petro>) and the Gaussianity of the
velocity distribution of the groups. Bright galaxies (Mr <=-20.7)
residing in the inner and outer regions of groups do not show
significant differences in the listed quantities regardless if the
group has a Gaussian (G) or a Non-Gaussian (NG) velocity
distribution. However, the situation is significantly different
when we examine the faint galaxies (-20.7 <Mr <=-17.9). In G
groups, there is a remarkable difference between the galaxy
properties of the inner and outer galaxy populations, testifying
how the environment is affecting the galaxies. Instead, in NG
groups there is no segregation between the properties of galaxies
in the inner and outer regions, showing that the properties of
these galaxies still reflect the physical processes prevailing in
the environment where they were found earlier.",
doi = "10.1093/mnras/stt1071",
url = "http://dx.doi.org/10.1093/mnras/stt1071",
issn = "0035-8711",
label = "scopus 2013-11",
language = "en",
targetfile = "1306.4722v2.pdf",
urlaccessdate = "27 abr. 2024"
}