J/ApJ/757/22 Strong and weak lensing analysis of A2261 (Coe+, 2012)
CLASH: precise new constraints on the mass profile of the galaxy cluster A2261.
Coe D., Umetsu K., Zitrin A., Donahue M., Medezinski E., Postman M.,
Carrasco M., Anguita T., Geller M.J., Rines K.J., Diaferio A., Kurtz M.J.,
Bradley L., Koekemoer A., Zheng W., Nonino M., Molino A., Mahdavi A.,
Lemze D., Infante L., Ogaz S., Melchior P., Host O., Ford H., Grillo C.,
Rosati P., Jimenez-Teja Y., Moustakas J., Broadhurst T., Ascaso B.,
Lahav O., Bartelmann M., Benitez N., Bouwens R., Graur O., Graves G.,
Jha S., Jouvel S., Kelson D., Moustakas L., Maoz D., Meneghetti M.,
Merten J., Riess A., Rodney S., Seitz S.
<Astrophys. J., 757, 22 (2012)>
=2012ApJ...757...22C 2012ApJ...757...22C
ADC_Keywords: Clusters, galaxy ; Spectroscopy ; Redshifts ; Galaxies, optical ;
Gravitational lensing ; Photometry, HST
Keywords: dark energy; dark matter; galaxies: clusters: individual: Abell 2261;
galaxies: evolution; gravitational lensing: strong;
gravitational lensing: weak
Abstract:
We precisely constrain the inner mass profile of A2261 (z=0.225) for
the first time and determine that this cluster is not
"overconcentrated" as found previously, implying a formation time in
agreement with ΛCDM expectations. These results are based on
multiple strong-lensing analyses of new 16-band Hubble Space Telescope
imaging obtained as part of the Cluster Lensing and Supernova survey
with Hubble (CLASH; Postman et al. 2012, Cat. J/ApJS/199/25).
Combining this with revised weak-lensing analyses of Subaru wide-field
imaging with five-band Subaru + KPNO photometry, we place tight new
constraints on the halo virial mass
Mvir=(2.2±0.2)x1015M☉h-170 (within
rvir~3Mpc.h-170) and concentration cvir=6.2±0.3 when
assuming a spherical halo. This agrees broadly with average c(M, z)
predictions from recent ΛCDM simulations, which span 5≲≲8.
Our most significant systematic uncertainty is halo elongation along
the line of sight (LOS). To estimate this, we also derive a mass
profile based on archival Chandra X-ray observations and find it to be
∼35% lower than our lensing-derived profile at r2500∼600kpc.
Agreement can be achieved by a halo elongated with a ∼2:1 axis ratio
along our LOS. For this elongated halo model, we find
Mvir=(1.7±0.2)x1015M☉h-170 and cvir=4.6±0.2,
placing rough lower limits on these values. The need for halo
elongation can be partially obviated by non-thermal pressure support
and, perhaps entirely, by systematic errors in the X-ray mass
measurements. We estimate the effect of background structures based on
MMT/Hectospec spectroscopic redshifts and find that these tend to
lower Mvir further by ∼7% and increase cvirby ∼5%.
Description:
We observed A2261 (17:22:27.2+32:07:57 (J2000) for the BCG, brightest
cluster galaxy) as part of the CLASH program in HST cycle 18 between
2011 March 9 and May 21 to a total depth of 20 orbits in 16 WFC3 and
ACS filters, spanning ∼2000-17000Å (GO 12066; PI: Postman). The
full 20-orbit, 16-filter depth is achieved over a central area of
3.9arcmin2, comfortably including all the strongly lensed galaxies.
We targeted probable A2261 cluster members based on their proximity to
the expected cluster red sequence and proximity to the BCG (K. Rines
et al. 2013, Cat. J/ApJ/767/15) with the Hectospec instrument mounted
on the 6.5m MMT. In addition, all targets were sufficiently bright
with magnitudes 16<r'<21 in Sloan Digital Sky Survey (SDSS) DR7.
Our weak-lensing analysis is based on archival BJVJRC imaging obtained
with the 34'x27' FOV Suprime-Cam on the Subaru 8.2m telescope and
NOAO archival MOSAIC1 i'z' imaging obtained with the Mayall 4m
telescope at KPNO (program 2008A-0356, PI. Mandelbaum).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 36 308 MMT/Hectospec spectroscopic redshifts for galaxies
within the Subaru FOV
table3.dat 64 30 Multiple images of galaxies strongly lensed by A2261
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See also:
B/hst : HST Archived Exposures Catalog (STScI, 2007)
II/294 : The SDSS Photometric Catalog, Release 7 (Adelman-McCarthy+, 2009)
VII/110 : Rich Clusters of Galaxies (Abell+ 1989)
J/A+A/562/A86 : CLASH. Photometric + photo-z catalog (Jouvel+, 2014)
J/ApJ/767/15 : Hectospec Cluster Survey (HeCS) (Rines+, 2013)
J/ApJS/199/25 : CLASH sources for MACS1149.6+2223 (Postman+, 2012)
J/ApJ/749/97 : Multiple lensed images in MCS J1206.2-0847 (Zitrin+, 2012)
J/A+A/535/A4 : X-ray galaxy clusters study (Reichert+, 2011)
J/ApJ/723/1678 : LensPerfect A1689 analysis (Coe+, 2010)
J/ApJ/690/670 : The Sloan lens ACS Survey. VIII. (Treu+, 2009)
J/ApJS/174/117 : Properties and metal abundances of clusters (Maughan+, 2008)
J/ApJ/668/643 : Multiply imaged gravitational lens systems (Limousin+, 2007)
J/ApJ/665/921 : Redshift survey in the field of A1689 (Frye+, 2007)
J/MNRAS/376/1073 : Sunyaev-Zel'dovich effect in galaxy clusters (Zemcov+, 2007)
J/ApJ/641/169 : Spectroscopy in lens fields (Momcheva+, 2006)
J/ApJ/621/53 : Multiple arc systems in A1689 (Broadhurst+, 2005)
J/AJ/109/14 : Optical spectroscopy of Abell clusters. I. (Owen+ 1995)
http://www.stsci.edu/~postman/CLASH/ : CLASH home page
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 9 F9.5 deg RAdeg [260.2/261] Right ascension (J2000)
11- 18 F8.5 deg DEdeg [31.8/32.5] Declination (J2000)
20- 26 F7.5 --- z [0.01/0.6] Spectroscopic redshift
28- 34 F7.5 --- e_z [0/0.002] Uncertainty in z
36 I1 --- Mm ? Cluster member code (0=non-member) (1)
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Note (1): Membership code as follows:
0 = not a member;
1 = cluster member from dynamical analysis.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- ID [1/12] Main image identification
(<[CUZ2012] NNa> in Simbad)
3 A1 --- m_ID [a-d] multiplicity index of image
5- 6 I2 h RAh Hour of right ascension (J2000)
8- 9 I2 min RAm Minute of right ascension (J2000)
11- 16 F6.3 s RAs Second of right ascension (J2000)
18 A1 --- DE- Sign of declination (J2000)
19- 20 I2 deg DEd Degree of declination (J2000)
22- 23 I2 arcmin DEm Arcminute of declination (J2000)
25- 29 F5.2 arcsec DEs Arcsecond of declination (J2000)
31- 35 F5.2 mag F775W [21.7/27.7] HST F775W AB magnitude
37- 40 F4.2 mag e_F775W [0.01/0.4] HST F775W uncertainty
41 A1 --- f_F775W [cd] continuous arc, or other filter (1)
43 A1 --- n_z [*] *: best-isolated arc (2)
45- 48 F4.2 --- z [0.2/5] Photometric redshift (2)
50- 53 F4.2 --- E_z [0.01/4] Positive error on z
55- 58 F4.2 --- e_z [0.01/3] Negative error on z
59 A1 --- f_z [c] continuous arc (1)
61- 64 F4.2 --- zLens Lens model redshift (from LensPerfect)
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Note (1): Flag as follows:
c = Continuous arcs were analyzed with a single photometric aperture for
more robust photometric redshift estimates.
d = F814W.
Note (2):
* = The best-isolated, least-contaminated arcs chosen to provide the input
redshift for each system. These are then optimized by the lens model.
Note that robust photometric redshifts are not expected for arcs fainter
than ∼26th magnitude. Uncertainties are formally 95% C.L. Broad,
asymmetric error bars generally indicate a bimodal solution.
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Nomenclature Notes:
In table 2, galaxies are <[CUZ2012] DDD.ddddd+DD.ddddd> in Simbad.
History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 20-May-2014