J/A+A/570/A69 GALEX Ultraviolet Virgo Cluster Survey. IV. (Boselli+, 2014)
The GALEX Ultraviolet Virgo Cluster Survey (GUViCS).
IV: The role of the cluster environment on galaxy evolution.
Boselli A., Voyer E., Boissier S., Cucciati O., Consolandi G., Cortese L.,
Fumagalli M., Gavazzi G., Heines S., Roehlly Y., Toloba E.
<Astron. Astrophys. 570, A69 (2014)>
=2014A&A...570A..69B 2014A&A...570A..69B
ADC_Keywords: Clusters, galaxy ; Ultraviolet
Keywords: galaxies: clusters: general - galaxies: clusters: individual: Virgo -
galaxies: evolution - galaxies: interactions - galaxies: ISM -
galaxies: star formation
Abstract:
We study the role of the environment on galaxy evolution using a
sample of 868 galaxies in the Virgo cluster and in its surrounding
regions that are selected from the GALEX Ultraviolet Virgo Cluster
Survey (GUViCS) with the purpose of understanding the origin of the
red sequence in dense environments. The sample spans a wide range in
morphological types (from dwarf ellipticals to Im and BCD) and stellar
masses (107≤Mstar≤1011.5M☉). We collected multifrequency
data covering the whole electromagnetic spectrum for most of the
galaxies, including UV, optical, mid- and far-infrared imaging data,
as well as optical and HI spectroscopic data. We first identify the
different dynamical substructures that compose the Virgo cluster, and
we calculate the local density of galaxies using different methods. We
then study the distribution of galaxies belonging to the red sequence,
the green valley, and the blue cloud within the different cluster
substructures or as a function of galaxy density. Our analysis
indicates that all the most massive galaxies Mstar≥1011M☉)
are slow rotators and are the dominant galaxies of the different
cluster substructures, which are generally associated with a diffuse
X-ray emission. They are probably the result of major merging events
that occurred at early epochs, as also indicated by their very old
stellar populations. Slow rotators of lower stellar mass
(108.5≤Mstar≤1011M☉) are also preferentially located
within the different high-density substructures of the cluster. Their
position in the velocity space indicates that they are virialised
within the cluster; thus, they are Virgo members since its formation.
They have been shaped by gravitational perturbations occurring within
the infalling groups that later form the cluster (pre-processing). On
the contrary, low-mass star-forming systems are extremely rare in the
inner regions of the Virgo cluster A, where the density of the
intergalactic medium is at its maximum. Our ram pressure stripping
models consistently indicate that these star-forming systems can be
rapidly deprived of their interstellar medium during their interaction
with the intergalactic medium. The lack of gas quenches their
star-formation activity transforming them into quiescent dwarf
ellipticals. This mild transformation does not perturb the kinematic
properties of these galaxies, which still have rotation curves typical
of star-forming systems.
Description:
The sample analysed in this work has been extracted from the Extended
Source Catalogue of Voyer et al. (2014A&A...569A.124V 2014A&A...569A.124V, Cat.
J/A+A/569/A124), and it is composed of all galaxies detected by GALEX
in the near-ultraviolet (NUV) band in the Virgo cluster region and its
surroundings (12h≤RA≤13h; 0°≤Dec≤20°) with a recessional
velocity lower than 3500km/s.
Here, we present the WISE 22 micron flux densities of all the UV
extended sources and their uncertainties.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 66 1768 The WISE 22 micron data
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See also:
J/A+A/528/A107 : GALEX Ultraviolet Virgo Cluster Survey (Boselli+, 2011)
J/A+A/569/A124 : GUViCS. Ultraviolet Source Catalogs (Voyer+, 2014)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- Name Galaxy name
16- 24 F9.5 deg RAdeg Right Ascension (J2000.0)
26- 34 F9.5 deg DEdeg Declination (J2000.0)
36- 40 F5.1 arcsec a Aperture major axis radius
42- 46 F5.1 arcsec b Aperture minor axis radius
48- 50 I3 deg PA [0/360] Position angle measured from
north clockwise
52 I1 --- f_S22um [0/1] Flag indicating galaxy detected (1) or
undetected (0, S22um is an upper limit)
54- 60 F7.1 mJy S22um Flux density (or upper limit if no error)
at 22um
62- 66 F5.1 mJy e_S22um ? Uncertainty on the flux density
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Acknowledgements:
Alessandro Boselli, alessandro.boselli(at)lam.fr
References:
Boselli et al., Paper I 2011A&A...528A.107B 2011A&A...528A.107B, Cat. J/A+A/528/A107
Boissier et al., Paper II 2012A&A...545A.142B 2012A&A...545A.142B
(End) Patricia Vannier [CDS] 03-Sep-2014