J/ApJ/801/44 HST lensing analysis of the CLASH sample (Zitrin+, 2015)
Hubble Space Telescope combined strong and weak lensing analysis of the CLASH
sample: mass and magnification models and systematic uncertainties.
Zitrin A., Fabris A., Merten J., Melchior P., Meneghetti M., Koekemoer A.,
Coe D., Maturi M., Bartelmann M., Postman M., Umetsu K., Seidel G.,
Sendra I., Broadhurst T., Balestra I., Biviano A., Grillo C., Mercurio A.,
Nonino M., Rosati P., Bradley L., Carrasco M., Donahue M., Ford H.,
Frye B.L., Moustakas J.
<Astrophys. J., 801, 44 (2015)>
=2015ApJ...801...44Z 2015ApJ...801...44Z
ADC_Keywords: Clusters, galaxy ; Gravitational lensing ; X-ray sources ;
Redshifts ; Models
Keywords: galaxies: clusters: general; galaxies: high-redshift;
gravitational lensing: strong; gravitational lensing: weak
Abstract:
We present results from a comprehensive lensing analysis in Hubble
Space Telescope (HST) data of the complete Cluster Lensing And
Supernova survey with Hubble cluster sample (CLASH). We identify
previously undiscovered multiple images, allowing improved or first
constraints on the cluster inner mass distributions and profiles. We
combine these strong lensing constraints with weak lensing shape
measurements within the HST field of view (FOV) to jointly constrain
the mass distributions. The analysis is performed in two different
common parameterizations (one adopts light-traces-mass (LTM) for both
galaxies and dark matter while the other adopts an analytical,
elliptical Navarro-Frenk-White (NFW) form for the dark matter) to
provide a better assessment of the underlying systematics--which is
most important for deep, cluster-lensing surveys, especially when
studying magnified high-redshift objects. We find that the typical
(median), relative systematic differences throughout the central FOV
are ∼40% in the (dimensionless) mass density, κ, and ∼20% in the
magnification, µ. We show maps of these differences for each
cluster, as well as the mass distributions, critical curves, and
two-dimensional (2D)-integrated mass profiles. For the Einstein radii
(zs=2) we find that all typically agree within 10% between the two
models, and Einstein masses agree, typically, within ∼15%. At larger
radii, the total projected, 2D-integrated mass profiles of the two
models, within r∼2', differ by ∼30%. Stacking the surface-density
profiles of the sample from the two methods together, we obtain an
average slope of dlog(Σ)/dlog(r)~-0.64±0.1, in the radial
range [5350]kpc. Last, we also characterize the behavior of the
average magnification, surface density, and shear differences between
the two models as a function of both the radius from the center and
the best-fit values of these quantities.
Description:
Each of the 25 CLASH clusters was observed with HST, generally in 16
filters ranging from the UVIS, through the optical into the near-IR,
using the Wide Field Camera 3 and Advanced Camera for Surveys (ACS)
cameras. Each cluster was observed to a depth of ∼15-20 orbits during
HST's cycles 18, 19, or 20, often supplementing some existing
observations. For full details, we refer the reader to Postman et al.
(2012, J/ApJS/199/25).
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 120 579 Multiple images and candidates
table3.dat 84 25 The CLASH cluster sample and HST observing plan
from Postman et al., 2012, J/ApJS/199/25
table4.dat 68 25 X-ray properties of the CLASH cluster sample
from Postman et al., 2012, J/ApJS/199/25
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See also:
B/hst : HST Archived Exposures Catalog (STScI, 2007)
VII/110 : Rich Clusters of Galaxies (Abell+ 1989)
J/ApJ/800/18 : HST/WFC3 obs. of z∼7-8 galaxies in A2744 (Atek+, 2015)
J/A+A/579/A4 : MCS J1206.2-0847 gal. spectral classif. (Girardi+, 2015)
J/MNRAS/443/1549 : MACSJ0416.1-2403 strong-lensing analysis (Jauzac+, 2014)
J/A+A/562/A86 : CLASH. Photometric + photo-z catalog (Jouvel+, 2014)
J/MNRAS/437/1858 : Galaxies in the RX J1347.5-1145 cluster (Kohlinger+, 2014)
J/ApJ/762/L30 : CLASH: MCS J0416.1-2403 lensing analysis (Zitrin+, 2013)
J/ApJ/757/22 : Strong and weak lensing analysis of A2261 (Coe+, 2012)
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/ApJ/723/1678 : LensPerfect A1689 analysis (Coe+, 2010)
J/MNRAS/404/325 : Massive galaxy clusters lensing analyse (Richard+, 2010)
J/MNRAS/395/1213 : galaxies in the field of MACS J1206.2-0847 (Ebeling+, 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/AJ/132/926 : Galaxies in the Hubble Ultra Deep Field (Coe+, 2006)
J/ApJ/621/53 : Multiple arc systems in A1689 (Broadhurst+, 2005)
http://www.stsci.edu/hst/campaigns/frontier-fields/ : HST frontier fields
http://archive.stsci.edu/prepds/clash/ : CLASH home page on MAST
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- ID Cluster abbreviated name
9- 19 A11 --- Arc Arc identifier (1)
21- 30 F10.6 deg RAdeg Right Ascension in decimal degrees (J2000)
32- 41 F10.6 deg DEdeg Declination in decimal degrees (J2000)
43- 46 F4.2 --- zph [0.02/7.7]? Photometric redshift (2)
48- 51 F4.2 --- b_zph ? Lower 95% confidence limit for zph
53- 56 F4.2 --- B_zph ? Upper 95% confidence limit for zph
58- 63 F6.3 --- z.in [-6.1/7.2]? Adopted input redshift (3)
65- 68 F4.2 --- zLTM [0.7/4.7]? Predicted LTM model redshift
70- 73 F4.2 --- b_zLTM ? Lower 95% confidence limit for zLTM
75- 78 F4.2 --- B_zLTM ? Upper 95% confidence limit for zLTM
80 A1 --- f_zLTM [u] Indicates zLTM is underconstrained
82- 85 F4.2 --- zNFW [0.6/6.3]? Predicted PIEMDeNFW model redshift
87- 90 F4.2 --- b_zNFW ? Lower 95% confidence limit for zNFW
92- 95 F4.2 --- B_zNFW ? Upper 95% confidence limit for zNFW
97 A1 --- f_zNFW [u] Indicates zNFW is underconstrained
99-120 A22 --- Com Additional comments and/or references (4)
--------------------------------------------------------------------------------
Note (1): In arc identifier, letters are:
c = candidate (for candidates the photo-z distribution, or
identification was ambiguous).
p = stands for predicted location for notably missing counter images
(so that absence of "p" does not necessarily mean that no other
images are predicted)
? = indicates that various candidates are seen nearby and the detection
is thus even more ambiguous, or that a candidate counter image is
seen but not necessarily predicted by the model.
Note (2): From the automated CLASH catalogs (best option among the IR and
optical+IR catalogs automatically generated by CLASH).
Note (3): If a spectroscopic redshift is available we list it with a minus sign,
along with its references in the "Com" column. Also, note that there
may be some discrepancy between the best adopted redshift per
system (which was more carefully chosen) and the mean photometric
redshift from its multiple images given in the automated CLASH
catalog.
Note (4): References as follows:
Ba13 = Balestra et al. (2013A&A...559L...9B 2013A&A...559L...9B)
Be13 = Belli et al. (2013ApJ...772..141B 2013ApJ...772..141B)
Br08 = Bradac et al. (2008ApJ...681..187B 2008ApJ...681..187B)
Ch12 = Christensen et al. (2012MNRAS.427.1953C 2012MNRAS.427.1953C)
Eb09 = Ebeling et al. (2009MNRAS.395.1213E 2009MNRAS.395.1213E)
Ha08 = Halkola et al. (2008A&A...481...65H 2008A&A...481...65H)
Li10 = Limousin et al. (2010MNRAS.405..777L 2010MNRAS.405..777L)
Li12 = Limousin et al. (2012A&A...544A..71L 2012A&A...544A..71L)
Mo14 = Monna et al. (2014MNRAS.438.1417M 2014MNRAS.438.1417M)
Ne11 = Newman et al. (2011ApJ...728L..39N 2011ApJ...728L..39N)
Ne13 = Newman et al. (2013ApJ...765...24N 2013ApJ...765...24N)
Ri11 = Richard et al. (2011MNRAS.414L..31R 2011MNRAS.414L..31R)
Sm01 = Smith et al. (2001ApJ...552..493S 2001ApJ...552..493S)
Sm09 = Smith et al. (2009ApJ...707L.163S 2009ApJ...707L.163S)
Zi12 = Zitrin et al. (2012, J/ApJ/749/97)
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1 A1 --- Set Cluster sample: X-ray or High magnification (1)
3- 17 A15 --- Name Cluster name
19 A1 --- n_Name [op] individual remarks on Cluster (2)
21- 22 I2 h RAh Hour of right ascension (J2000)
24- 25 I2 min RAm Minute of right ascension (J2000)
27- 31 F5.2 s RAs Second of right ascension (J2000)
33 A1 --- DE- Sign of declination (J2000)
34- 35 I2 deg DEd Degree of declination (J2000)
37- 38 I2 arcmin DEm Arcminute of declination (J2000)
40- 43 F4.1 arcsec DEs Arcsecond of declination (J2000)
45 A1 --- pos [a] position from optical image (3)
47- 51 F5.3 --- z [0.18/0.9] Cluster redshift
52 A1 --- f_z [b] Redshift from X-ray spectrum (4)
54- 55 I2 --- HST [18/20] HST cycle
57- 58 I2 --- CLASH [15/20] CLASH orbits
60- 64 I5 --- PID [12065/12791] Program ID
66- 74 A9 --- Orb Archival ACS orbits unless flagged (5)
76 A1 --- f_Orb [w] WFPC2 image (5)
78- 84 A7 --- ID Internal abbreviated cluster name as in
table 2; column added by CDS
--------------------------------------------------------------------------------
Note (1): the set is:
X = X-ray selected cluster
H = High magnification cluster
Note (2): Flag as follows:
o = RXJ2248.7-4431 is also Abell 1063S
p = RXJ1532.9+3021 is also referred to as MACS J1532.9+3021
(Ebeling et al. 2010MNRAS.407...83E 2010MNRAS.407...83E);
see section 4.18 of this work (Zitrin et al. 2015ApJ...801...44Z 2015ApJ...801...44Z)
Note (3):
a = Central cluster coordinates derived from optical image instead of
X-ray image.
Note (4):
b = Cluster redshift for MACS0416.1-2403 is based on Chandra X-ray spectrum
(Postman et al., 2012, J/ApJS/199/25). Uncertainty on this value is
±0.02. For this fit, the core was not excluded. To maximize the counts,
an aperture of 714kpc was used, binned to achieve a minimum of 20 counts
per energy bin. The background in the 0.7-7.0keV range was fitted from
the Chandra deep fields.
Note (5): Archival ACS images, when available, are used in conjunction with
new CLASH data to achieve the desired depths in all filters. The "w"
flag indicates a WFPC2 orbit (for the second value if two are given).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 A15 --- Name Cluster name
17- 20 F4.1 keV kT [5.5/15.5] Temperature
22- 25 F4.2 keV e_kT [0.2/3] kT uncertainty
27- 30 F4.1 10+37W Lbol [6.7/91] Bolometric luminosity in 1044erg/s (6)
32- 34 F3.1 10+37W e_Lbol [0.1/3] Lbol uncertainty
36- 39 F4.2 [Sun] Fe/H [0.1/0.6] Cluster to solar [Fe/H] ratio (7)
41- 44 F4.2 [Sun] e_Fe/H [0.06/0.3] Fe/H uncertainty
46- 49 F4.2 --- ell [0/1]? Ellipticity ε (8)
51- 54 F4.2 --- e_ell [0.01/0.03]? ell uncertainty
56- 59 F4.2 --- shift [0.07/2.2]? Centroid shift ((10-2R500)) (8)
61- 64 F4.2 --- e_shift [0.01/0.2]? shift uncertainty
66- 68 A3 --- Ref X-ray morphology reference(s) (9)
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Note (6): The X-ray bolometric luminosity covers the energy range 0.1-100keV.
Note (7): The solar abundance reference values used here are from
Anders & Grevesse (1989GeCoA..53..197A 1989GeCoA..53..197A).
Note (8): The X-ray ellipticity ε, and centroid shift ,
are from Maughan et al. (2008, J/ApJS/174/117).
Note (9): References as follows:
1 = Maughan et al. (2008, J/ApJS/174/117);
2 = Allen et al. (2008MNRAS.383..879A 2008MNRAS.383..879A);
3 = Ebeling et al. (2007ApJ...661L..33E 2007ApJ...661L..33E);
4 = Cavagnolo et al. (2008, J/ApJ/682/821);
5 = Mantz et al. (2010MNRAS.406.1759M 2010MNRAS.406.1759M);
6 = CLASH team selected cluster.
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Acknowledgements:
Adi Zitrin [California Institute of Technology] for a complete version
of table 2 (MACS J0744.9+3927 was missing in the original version of the
online paper).
History:
From electronic version of the journal (see Acknowledgements)
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 15-Jul-2015