J/MNRAS/441/203 Massive quiescent ETG in clusters (Delaye+ 2014)
Larger sizes of massive quiescent early-type galaxies in clusters than in the
field at 0.8 < z < 1.5.
Delaye L., Huertas-Company M., Mei S., Lidman C., Licitra R., Newman A.,
Raichoor A., Shankar F., Barrientos F., Bernardi M., Cerulo P., Couch W.,
Demarco R., Munoz R., Sanchez-Janssen R., Tanaka M.
<Mon. Not. R. Astron. Soc., 441, 203-223 (2014)>
=2014MNRAS.441..203D 2014MNRAS.441..203D
ADC_Keywords: Clusters, galaxy ; Galaxies, optical ; Morphology
Keywords: galaxies: clusters: general - galaxies: elliptical and lenticular -
galaxies: evolution
Abstract:
We analyse the mass-size relation of ∼400 quiescent massive ETGs
(M*/M☉>3x1010) hosted by massive clusters
(M200∼2-7x1014M☉) at 0.8<z<1.5, compared to those found in the
field at the same epoch. Size is parametrized using the
mass-normalized B-band rest-frame size, γ=Re/M110.57. We
find that the γ distributions in both environments peak at the
same position, but the distributions in clusters are more skewed
towards larger sizes. This tail induces average sizes ∼ 30-40 percent
larger for cluster galaxies than for field galaxies of similar stellar
mass, while the median sizes are statistically the same with a
difference of ∼10±10%. Since this size difference is not observed in
the local Universe, the evolution of average galaxy size at fixed
stellar mass from z∼1.5 for cluster galaxies is less steep at more
than 3σ(∝(1+z)-0.53±0.04) than the evolution of field
galaxies (∝(1+z)-0.92±0.04). The difference in evolution is
not measured when the median values of γ are considered:
∝(1+z)-0.84±0.04 in the field versus
∝(1+z)-0.71±0.05 in clusters. In our sample, the tail of
large galaxies is dominated by galaxies with
3x1010<M*/M☉<1011. At this low-mass end, the difference in
the average size is better explained by the accretion of new galaxies
that are quenched more efficiently in clusters and/or by different
morphological mixing in the cluster and field environments. If part of
the size evolution would be due to mergers, the difference that we see
between cluster and field galaxies could be caused by higher merger
rates in clusters at higher redshift, when galaxy velocities are
lower.
Description:
Our targets have been selected according to the following criteria:
(1) they cover a broad redshift range 0.84<z<1.45; (2) they have
been imaged with the HST/ACS in at least two bandpasses and have deep
ground-based images in the near-IR; (3) they have at least 10
spectroscopically confirmed cluster members.
All clusters have HST/ACS WFC (Wide Field Camera) images in at least
two bandpasses. The ACS WFC resolution is 0.05-arcsec/pix, and
its field of view is 210-arcsecx204-arcsec. The ACS/WFC PSF width
is around 0.11arcsec. Our ACS/WFC images were mostly obtained in a
programme designed to find Type Ia supernovae in distant galaxy
clusters (Dawson et al., 2009AJ....138.1271D 2009AJ....138.1271D). See Meyers et al.
(2012ApJ...750....1M 2012ApJ...750....1M) for a description of how these data were
processed. Three clusters (see below): RDCS J1252-2927, XMMU
J2235.3-2557 and RX J0152-1357 had been previously targeted with
the ACS camera on HST in the context of the ACS Intermediate Redshift
Cluster Survey (Ford 2004, HST Proposal ID 10327, ACS Imaging of a
High-Redshift Cluster of Galaxies; Postman et al. 2005ApJ...623..721P 2005ApJ...623..721P;
Mei et al. 2009ApJ...690...42M 2009ApJ...690...42M) and these data have been included.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableb1.dat 82 313 Catalogue of red sequence early-type galaxies
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See also:
J/AJ/125/1817 : SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)
J/MNRAS/422/494 : Optically selected ETGs X-ray properties (Danielson+, 2012)
Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- ID [157/4319] Galaxy Sequential number
6- 13 F8.4 deg RAdeg Right ascension (J2000)
15- 24 F10.6 deg DEdeg Declination (J2000)
26- 34 A9 --- Cluster Cluster short designation (1)
36- 40 F5.2 [Msun] logM [10.5/11.59] Mass of galaxy
42- 45 F4.2 [Msun] e_logM rms uncertainty on Mass
47- 51 F5.2 kpc Re [0.8/13] Effective radius of galaxy
53- 56 F4.2 kpc e_Re rms uncertainty on Re
58- 61 F4.2 --- n [0.7/8] Sersic index
63- 66 F4.2 --- e_n ?=- rms uncertainty on n
68- 71 F4.2 --- b/a [0/1] Axis ratio
73- 77 F5.3 --- e_b/a ?=- rms uncertainty on b/a
79- 82 F4.2 --- p(ETG) [0.5/1] Probability of early-type galaxy
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Note (1): Cluster names as follows:
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SName Name Simbad name
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RCS0220 = RCS 0220-0333 = RCS J0220.9-0333
RCS2319 = RCS 2319+0038 = RCS J2319+0038
RCS2345 = RCS 23454-3632 = RCS J2345.4-3632
RDCSJ1252 = RDCS J1252-2927 = RDCS J1252-2927
RXJ0152 = RX J0152-1357 = RX J0152.7-1357
XMMJ0223 = XMM J0223-0436 = XLSSU J022303.0-043622
XMMJ1229 = XMM J1229+0151 = NAME XMMU J1229.4+0151
XMMJ2215 = XMM J2215-1738 = XMMXCS J2215.9-1738
XMMU2235 = XMMU 2235-2557 = ClG J2235-2557
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 30-Jan-2015