J/ApJ/750/93 Near-IR observations of XMM-LSS J02182-05102 (Papovich+, 2012)
CANDELS observations of the structural properties of cluster galaxies at
z=1.62.
Papovich C., Bassett R., Lotz J.M., van der Wel A., Tran K.-V.,
Finkelstein S.L., Bell E.F., Conselice C.J., Dekel A., Dunlop J.S., Guo Y.,
Faber S.M., Farrah D., Ferguson H.C., Finkelstein K.D., Haussler B.,
Kocevski D.D., Koekemoer A.M., Koo D.C., McGrath E.J., McLure R.J.,
McIntosh D.H., Momcheva I., Newman J.A., Rudnick G., Weiner B.,
Willmer C.N.A., Wuyts S.
<Astrophys. J., 750, 93 (2012)>
=2012ApJ...750...93P 2012ApJ...750...93P
ADC_Keywords: Clusters, galaxy ; Photometry, infrared ; Galaxies, IR ;
Redshifts
Keywords: galaxies: clusters: general - galaxies: high-redshift -
galaxies: clusters: individual: XMM-LSS02182-05102 -
galaxies: elliptical and lenticular, cD - galaxies: evolution
galaxies: structure
Abstract:
We discuss the structural and morphological properties of galaxies in
a z=1.62 proto-cluster using near-IR imaging data from Hubble Space
Telescope Wide Field Camera 3 data of the Cosmic Assembly Near-IR Deep
Extragalactic Legacy Survey (CANDELS). The cluster galaxies exhibit a
clear color-morphology relation: galaxies with colors of quiescent
stellar populations generally have morphologies consistent with
spheroids, and galaxies with colors consistent with ongoing star
formation have disk-like and irregular morphologies. The size
distribution of the quiescent cluster galaxies shows a deficit of
compact (≲1kpc), massive galaxies compared to CANDELS field galaxies
at z=1.6. As a result, the cluster quiescent galaxies have larger
average effective sizes compared to field galaxies at fixed mass at
greater than 90% significance. Combined with data from the literature,
the size evolution of quiescent cluster galaxies is relatively slow
from z≃1.6 to the present, growing as (1+z)-0.6±0.1. If this
result is generalizable, then it implies that physical processes
associated with the denser cluster region seem to have caused
accelerated size growth in quiescent galaxies prior to z=1.6 and
slower subsequent growth at z<1.6 compared to galaxies in the lower
density field. The quiescent cluster galaxies at z=1.6 have higher
ellipticities compared to lower redshift samples at fixed mass, and
their surface-brightness profiles suggest that they contain extended
stellar disks. We argue that the cluster galaxies require
dissipationless (i.e., gas-poor or "dry") mergers to reorganize the
disk material and to match the relations for ellipticity, stellar
mass, size, and color of early-type galaxies in z<1 clusters.
Description:
The z=1.62 cluster XMM-LSS J02182-05102 is located in the UKIRT IR
Deep Sky Survey (UKIDSS; Lawrence et al. 2007, Cat. II/319) Ultradeep
survey (UDS). This cluster received partial HST/WFC3 imaging in the
F125W and F160W bands as part of the Cosmic Assembly Near-IR Deep
Extragalactic Legacy Survey (CANDELS) program (PIs: S. Faber, H.
Ferguson) fully described in Grogin et al. (2011ApJS..197...35G 2011ApJS..197...35G) and
Koekemoer et al. (2011ApJS..197...36K 2011ApJS..197...36K).
In addition to the HST imaging, this field has deep BRiz imaging from
the Subaru-XMM Deep Survey (SXDF; Furusawa et al. 2008,
Cat. J/ApJS/176/1), JK imaging from UKIDSS (e.g., Williams et al.
2009ApJ...691.1879W 2009ApJ...691.1879W), Spitzer IRAC data in four bands probing
3.6-8.0um, and MIPS data at 24um.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 103 266 Properties of z=1.6 galaxy samples in the UDS
CANDELS field
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See also:
B/hst : HST Archived Exposures Catalog (STScI, 2007)
II/319 : UKIDSS-DR9 LAS, GCS and DXS Surveys (Lawrence+ 2012)
J/ApJS/206/10 : CANDELS multiwavelength catalog (Galametz+, 2013)
J/MNRAS/427/1666 : Massive galaxies in CANDELS-UDS field (Bruce+, 2012)
J/ApJS/203/24 : Structural parameters of CANDELS galaxies (van der Wel+, 2012)
J/ApJ/742/111 : Extreme emission-line galaxies in CANDELS (van der Wel+, 2011)
J/ApJS/176/1 : Subaru/XMM-Newton deep survey (SXDS). II. (Furusawa+, 2008)
http://candels.ucolick.org/data_access/UDS.html : CANDELS UDS Data Release
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 5 I5 --- ID [28489/45319] Object identification number
<[PBL2012] NNNNN> in Simbad
7- 14 F8.5 deg RAdeg [34.2/34.6] Right Ascension (J2000)
16- 23 F8.5 deg DEdeg [-5.3/-5.1] Declination (J2000)
25- 28 F4.2 --- zph [1.4/1.9] Photometric redshift
30- 33 F4.2 --- Pz [0/1] Integrated photometric redshift
probability distribution function (1)
35- 38 F4.2 mag z-J [0.4/2.4] (Suprime z-UKIDSS J) color index
40- 44 F5.2 mag J-3.6 [-0.7/3.2]? (UKIDSS J-Spitzer/IRAC 3.6um)
color index
46- 50 F5.2 mag Jmag [20.6/35.4] HST/WFC3 F125W band magnitude
measured from GALFIT
52- 55 F4.1 kpc Reff [0/41] Circularized effective radius
57- 60 F4.1 kpc e_Reff [0.1/33] Uncertainty in Reff
62- 65 F4.1 --- n [0/20] Sersic index
67- 69 F3.1 --- e_n [0.1/9] Uncertainty in n
71- 74 F4.2 --- Ell [0/0.83] Ellipticity (Ell=1-b/a)
76- 80 F5.2 [Msun] logM* [8.2/11.5]? Log of stellar mass
82- 85 F4.2 [Msun] E_logM* [0.03/0.7]? Uncertainty in logM*
87- 90 F4.2 [Msun] e_logM* [0.03/0.8]? Uncertainty in logM*
92 A1 --- l_logPhi Limit flag on logPhi
93- 97 F5.2 [Msun/yr] logPhi [-1/3.5]? Log star formation rate (2)
99-103 F5.2 Mpc Rproj [0.04/11.3] Projected distance (3)
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Note (1): Following Papovich et al. (2010ApJ...716.1503P 2010ApJ...716.1503P), we used the
multiwavelength photometry to derive photometric redshift probability
distribution functions, P(z), for each source using EAZY
(Brammer et al. 2008ApJ...686.1503B 2008ApJ...686.1503B). See section 2.1.
Note (2): From analysis of spectral energy distribution.
Note (3): From center of the z=1.62 cluster XMM-LSS J02182-05102.
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 05-Dec-2013