J/A+A/593/A2 Red-sequence early-type galaxies in clusters (Andreon+, 2016)
The size growth of red-sequence early-type galaxies in clusters in the
last 10 Gyr.
Andreon S., Dong H., Raichoor A.
<Astron. Astrophys. 593, A2 (2016)>
=2016A&A...593A...2A 2016A&A...593A...2A (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Stars, masses
Keywords: galaxies: clusters: general -
galaxies: elliptical and lenticular, cD - galaxies: evolution -
Abstract:
We carried out a photometric and structural analysis in the rest-frame
V band of a mass-selected (logM/M☉>10.7) sample of red sequence
galaxies in 14 galaxy clusters, six of which are at z>1.45, namely
JKCS041, IDCS J1426.5+3508, SpARCS104922.6+564032.5,
SpARCSJ022426-032330, XDCPJ0044.0-2033, and SPT-CLJ2040-4451. To this
aim, we reduced/analysed about 300 orbits of multicolor images taken
with the Advanced Camera for Survey and the Wide Field Camera 3 on
Hubble Space Telescope. We uniformly morphologically classified
galaxies from z=0.023 to z=1.803, and we homogeneously derived
sizes (effective radii) for the entire sample. Furthermore, our size
derivation allows, and therefore is not biased by, the presence of the
usual variety of morphological structures seen in early-type galaxies,
such as bulges, bars, disks, isophote twists, and ellipticity
gradients. By such a mass-selected sample, composed of 244
red-sequence early-type galaxies, we find that the log of the galaxy
size at a fixed stellar mass, logM/M☉=11 increases with time
with a rate of 0.023±0.002dex per Gyr in the last 10Gyr, in marked
contrast with the threefold increase found in literature for galaxies
in the general field over the same period. This suggests, at face
value, to exclude that secular processes are the primary drivers of
size evolution, because we observed and environmental environmental
dependent size growth. Using spectroscopic ages of Coma early-type
galaxies we also find that recently quenched early-type galaxies are a
numerically minor population not different in size enough to alter the
mean size at a given mass, which implies that the progenitor bias is
minor, i.e. that the evolution measured by selecting galaxies at the
redshift of observation is indistinguishable from the one that
compares ancestors and descendents.
Description:
Table 3 provides the cluster name (column 1), object identification
(column 2), position (column 3), stellar mass (column 4, assuming a
Bruzual & Charlot (2003MNRAS.344.1000B 2003MNRAS.344.1000B) stellar population synthesis
model with solar metallicity and Salpeter initial mass function),
log10 of half-light radius (column 5), and the adopted PSF correction
(column 6) of 158 galaxies in 13 galaxy clusters. Stellar mass and
radii assume ωm=0.3, ωλ=0.7, H0=70km/s/Mpc.
The 14th cluster is published in Andreon et al., Cats. J/A+AS/116/429
and J/A+AS/126/67.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
clusters.dat 49 13 List of studied clusters
table3.dat 66 158 Coordinates, mass and sizes
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See also:
J/A+AS/116/429 : Classification of Coma early galaxies (Andreon+ 1996)
J/A+AS/126/67 : Coma and Perseus clusters galaxies (Andreon+ 1997)
Byte-by-byte Description of file: clusters.dat
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Bytes Format Units Label Explanations
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1- 23 A23 --- Cluster Cluster name
26- 27 I2 --- NGal Number of galaxies in table3 for this cluster
29- 49 A21 --- SName Simbad name of the cluster
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 23 A23 --- Cluster Cluster name
25- 28 I4 --- ID Galaxy identification number within the cluster
30- 38 F9.5 deg RAdeg Right ascension (J2000.0)
40- 48 F9.5 deg DEdeg Declination (J2000)
50- 54 F5.2 [Msun] logM log10 of stellar mass (1)
56- 60 F5.2 [kpc] logre log10 of half-light radius
62- 66 F5.2 --- PSFcorr Applied correction to logre (in dex units)
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Note (1): assuming a Bruzual & Charlot (2003MNRAS.344.1000B 2003MNRAS.344.1000B) stellar population
synthesis model with solar metallicity and Salpeter initial mass function.
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Acknowledgements:
Stefano Andreon, stefano.andreon(at)brera.inaf.it
History:
* 29-Aug-2016: on-line version
* 18-May-2017: SpARCSJ021524-034331 corrected into SpARCSJ022426-032330,
from author
(End) Patricia Vannier [CDS] 31-May-2016