@Article{ProustYeSaIvBrSaCa:2015:StDyAC,
author = "Proust, Dominique and Yegorova, Irina and Saviane, Ivo and Ivanov,
Valentin D. and Bresolin, Fabio and Salzer, John J. and Capelato,
Hugo Vicente",
affiliation = "{Observatoire de Paris-Meudon} and {European Southern Observatory}
and {European Southern Observatory} and {European Southern
Observatory} and {Institute for Astronomy} and {Indiana
University} and {Instituto Nacional de Pesquisas Espaciais
(INPE)}",
title = "The structure and dynamics of the AC114 galaxy cluster revisited",
journal = "Monthly Notices of the Royal Astronomical Society",
year = "2015",
volume = "452",
number = "4",
pages = "3304--3318",
month = "July",
keywords = "Cosmology: observations, Distance scale, Galaxies: clusters:
general, Galaxies: distances and redshifts, Galaxies: evolution,
Large-scale structure of universe.",
abstract = "We present a dynamical analysis of the galaxy cluster AC114 based
on a catalogue of 524 velocities. Of these, 169 (32 per cent) are
newly obtained at European Southern Observatory (Chile) with the
Very Large Telescope and the VIsible MultiObject spectrograph.
Data on individual galaxies are presented and the accuracy of the
measured velocities is discussed. Dynamical properties of the
cluster are derived. We obtain an improvedmean redshift value z=
0.31665 ± 0.0008 and velocity dispersion \σ = 1893+73 -82 km
s-1. A large velocity dispersion within the core radius and the
shape of the infall pattern suggests that this part of the cluster
is in a radial phase of relaxation with a very elongated radial
filament spanning 12 000 km s-1. A radial foreground structure is
detected within the central 0.5 h-1 Mpc radius, recognizable as a
redshift group at the same central redshift value. We analyse the
colour distribution for this archetype Butcher-Oemler galaxy
cluster and identify the separate red and blue galaxy sequences.
The latter subset contains 44 per cent of confirmed members of the
cluster, reaching magnitudes as faint as Rf= 21.1 (1.0mag fainter
than previous studies). We derive a mass M200 = (4.3 ± 0.7) × 1015
M· h-1. In a subsequent paper, we will utilize the spectral data
presented here to explore the mass-metallicity relation for this
intermediate redshift cluster.",
doi = "10.1093/mnras/stv1558",
url = "http://dx.doi.org/10.1093/mnras/stv1558",
issn = "0035-8711 and 1365-2966",
language = "en",
targetfile = "proust_the structure.pdf",
urlaccessdate = "28 abr. 2024"
}