J/ApJ/811/29 GLASS. IV. Lensing cluster Abell 2744 (Wang+, 2015)
The Grism Lens-Amplified Survey from Space (GLASS).
IV. Mass reconstruction of the lensing cluster Abell 2744 from Frontier Field
imaging and GLASS spectroscopy.
Wang X., Hoag A., Huang K.-H., Treu T., Bradac M., Schmidt K.B.,
Brammer G.B., Vulcani B., Jones T.A., Ryan R.E.JR, Amorin R.,
Castellano M., Fontana A., Merlin E., Trenti M.
<Astrophys. J., 811, 29 (2015)>
=2015ApJ...811...29W 2015ApJ...811...29W (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Gravitational lensing ; Redshifts ;
Photometry, HST ; Spectroscopy
Keywords: galaxies: clusters: individual: Abell 2744;
galaxies: evolution; galaxies: high-redshift
Abstract:
We present a strong and weak lensing reconstruction of the massive
cluster Abell 2744, the first cluster for which deep Hubble Frontier
Fields (HFF) images and spectroscopy from the Grism Lens-Amplified
Survey from Space (GLASS) are available. By performing a targeted
search for emission lines in multiply imaged sources using the GLASS
spectra, we obtain five high-confidence spectroscopic redshifts and
two tentative ones. We confirm one strongly lensed system by detecting
the same emission lines in all three multiple images. We also search
for additional line emitters blindly and use the full GLASS
spectroscopic catalog to test reliability of photometric redshifts for
faint line emitters. We see a reasonable agreement between our
photometric and spectroscopic redshift measurements, when including
nebular emission in photometric redshift estimations. We introduce a
stringent procedure to identify only secure multiple image sets based
on colors, morphology, and spectroscopy. By combining 7 multiple image
systems with secure spectroscopic redshifts (at 5 distinct redshift
planes) with 18 multiple image systems with secure photometric
redshifts, we reconstruct the gravitational potential of the cluster
pixellated on an adaptive grid, using a total of 72 images. The
resulting mass map is compared with a stellar mass map obtained from
the deep Spitzer Frontier Fields data to study the relative
distribution of stars and dark matter in the cluster. We find that the
stellar to total mass ratio varies substantially across the cluster
field, suggesting that stars do not trace exactly the total mass in
this interacting system. The maps of convergence, shear, and
magnification are made available in the standard HFF format.
Description:
The two position angles (P.A.s) of Grism Lens-Amplified Survey from
Space (GLASS) data analyzed in this study were taken on 2014 August 22
and 23 (P.A.=135) and 2014 October 24 and 25 (P.A.=233), respectively.
The Hubble Frontier Fields initiative (HFF, P.I. Lotz) is a Director's
Discretionary Time legacy program with HST devoting 840 orbits of HST
time to acquire optical ACS and NIR WFC3 imaging of six of the
strongest lensing galaxy clusters on the sky. All six HFF clusters are
included in the GLASS sample.
The Spitzer Frontier Fields program (P.I. Soifer) is a Director's
Discretionary Time program that images all six strong lensing galaxy
clusters targeted by the HFF in both warm IRAC channels (3.6 and 4.5um).
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 100 179 Multiply lensed arc systems identified in
the Abell 2744 field
table2.dat 137 114 Emission line detection results on multiply
and singly lensed sources (57 systems)
--------------------------------------------------------------------------------
See also:
J/ApJ/812/114 : Grism Lens-Amplified Survey from Space (GLASS) I. (Treu+, 2015)
J/MNRAS/452/1437 : Abell 2744 strong-lensing analysis (Jauzac+, 2015)
J/ApJ/800/18 : HST/WFC3 observations of z∼7-8 galaxies in A2744 (Atek+, 2015)
J/ApJS/207/24 : GOODS-S CANDELS multiwavelength catalog (Guo+, 2013)
J/ApJS/199/25 : CLASH sources for MACS1149.6+2223 (Postman+, 2012)
J/ApJ/728/27 : Chandra and AAOmega observations of Abell 2744 (Owers+, 2011)
J/A+A/500/947 : Spectroscopy and photometry in A2744 and A2537 (Braglia+, 2009)
J/A+A/449/461 : Radial velocities in A2744 (Boschin+, 2006)
J/ApJ/627/32 : Gravitationally lensed arcs in HST WFPC2 archive (Sand+, 2005)
J/AJ/112/1335 : Hubble Deep Field observations (Williams+ 1996)
http://glass.physics.ucsb.edu/ : GLASS home page
http://www.stsci.edu/~postman/CLASH : CLASH home page
http://www.stsci.edu/hst/campaigns/frontier-fields/ : HST FF home page
http://archive.stsci.edu/prepds/frontier/lensmodels/ : HFF lens models page
http://ssc.spitzer.caltech.edu/warmmission/scheduling/approvedprograms/ddt
/frontier/ : Spitzer FF
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 F4.1 --- ID [1.1/60.3] Arc identifier (1)
6 A1 --- f_ID [e] Flag on 2.2 (2)
8- 10 A3 --- r_ID Arc reference (3)
12- 20 F9.7 deg RAdeg Right ascension in decimal degrees (J2000)
22- 31 F10.6 deg DEdeg Declination in decimal degrees (J2000)
33- 37 F5.2 mag F140W [22.1/30.6]? HST/WFC3 NIR F140W magnitude (4)
39- 43 F5.2 --- z [1.2/10]? Spectroscopic redshift
45 A1 --- f_z [fgh] Flag on z for 46.1 (5)
47- 51 F5.2 --- zBayes [0.01/11.9]? Redshift obtained from
hierarchical Bayesian modeling (6)
53- 56 F4.2 --- b_zBayes [0.7/4.7]? 68% lower limit on zBayes
57 A1 --- --- [-]
58- 61 F4.2 --- B_zBayes [2/9.5]? 68% upper limit on zBayes
63 I1 --- q_zBayes [0/1]? zBayes quality (1=secure) (7)
65- 70 F6.3 --- CChi2 [0/16.6]? Color-χ2 value (see equation 1)
72 I1 --- Morph [0/8] Morphology criterion (8)
74 I1 --- Cont? [0/1] Contaminated? (9)
76 I1 --- Sys [0/1]? System pass flag
78 I1 --- Img [0/1] Image pass flag (10)
80- 87 F8.2 --- Magf [1.4/53874]? Flux Magnification µ (11)
89- 93 F5.2 --- b_Magf [1.4/61.7]? 68% lower limit on Magf
94 A1 --- --- [-]
95-100 F6.2 --- B_Magf [1.6/624]? 68% upper limit on Magf
--------------------------------------------------------------------------------
Note (1): Systems 15, 16, and 17 are not included in the table or the lens model
because they belong to northern subclumps with >1arcminute separation
from the cluster center shown in Figure 3. The coordinates of these
systems can be found in Richard et al. (2014MNRAS.444..268R 2014MNRAS.444..268R).
Note (2):
e = Due to the use of a fixed SExtractor detection image at F160W, 2.2 was
not detected with even the most aggressive SExtractor detection
settings, i.e., the "hot" mode settings. Upon visual inspection in other
HST bands; however, the object is clearly separated and unmistakably
belongs to system 2.
Note (3): References correspond to the most recent quote in the literature as
follows:
G = this work,
J = Jauzac et al. (2015MNRAS.452.1437J 2015MNRAS.452.1437J),
T = Johnson et al. (2014ApJ...797...48J 2014ApJ...797...48J),
R = Richard et al. (2014MNRAS.444..268R 2014MNRAS.444..268R),
C-B = Clement et al. (2015, in preparation),
Z = Zitrin et al. (2014ApJ...793L..12Z 2014ApJ...793L..12Z),
L = Lam et al. (2014ApJ...797...98L 2014ApJ...797...98L),
I = Ishigaki et al. (2015ApJ...799...12I 2015ApJ...799...12I)
System 60 is identified in this work for the first time.
Note (4): Objects for which F140 W magnitudes are not reported are not detected
by SExtractor.
Note (5): Flag on z as follows:
f = The redshift of this system comes from the geometric constraint
by Zitrin et al. (2014ApJ...793L..12Z 2014ApJ...793L..12Z).
g = Note that arc systems 1 and 55 have the same physical origin and
therefore have the same zspec through our identification of
arc 1.3 (object ID #336).
h = Systems 2 and 56 have also the same physical origin and zspec is
measured through arc 56.1 (object ID #888).
Note (6): This value is the mode of the combined posterior probability
distribution. For systems that fulfill the selection criteria and
do not have a spectroscopic redshift, this is the redshift assigned
to the system in the lens model.
Note that zBayes=0.01 is assigned if the posterior distribution
of photometric redshift declines monotonically from 0, and is thus
considered highly uncertain.
Note (7): Quality 0 indicates that zBayes is unreliable due to
zBayes<zcluster and/or there exists strong multi-modality in the
posterior probability distribution of photometric redshift and/or
only one image was used to compute zBayes.
Quality 1 indicates that zBayes is secure.
Note (8): The grading scheme based on morphological similarity is:
4 = Image is definitely part of the system.
3 = Image is very likely part of the system.
2 = Image is potentially part of the system.
1 = Image is very unlikely part of the system.
0 = Image is definitely not part of the system.
Two inspectors (A.H. and M.B.) independently assign a grade to each
image. The inspectors use several RGB images of the full HFF depth
that span the full HST spectral coverage to assign the grade for each
image. The two grades are then summed to get the reported morphology
grade. Examples of multiple images that receive high and low
morphology grades are shown in the Appendix.
See also section 4.1 for further explanations.
Note (9): Contaminated objects are only required to fulfill the morphology
criterion M>5, but they are not used to compute zBayes.
Note (10): Arc images with pass flag=1 fulfill Color+Morphology+Contamination
criteria and zBayes>zcluster and zBayes single-valued.
Note (11): Best-fit magnification derived from resampling the multiple image
systems themselves and their photometric redshifts from the
combined posterior distributions.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 I05 --- GLASS [00111/02400] GLASS identifier
7- 10 F4.1 --- ID [1.3/56.1]? Arc identifier
12- 22 F11.9 deg RAdeg Right ascension in decimal degrees (J2000)
24- 36 F13.9 deg DEdeg Declination in decimal degrees (J2000)
38- 42 F5.2 mag F140W [18.4/27.2] HST/WFC3 NIR F140W magnitude
44- 47 F4.2 mag e_F140W [0.01/0.2] F140W 1σ uncertainty
49- 52 F4.2 --- zph [0.01/3.7] Photometric redshift
54- 57 F4.2 --- E_zph [0.01/3.8] Positive 1σ uncertainty on zph
59- 62 F4.2 --- e_zph [0.01/3.3] Negative 1σ uncertainty on zph
64- 67 F4.2 --- zsp [0.3/4.9] Spectroscopic redshift
69 I1 --- Q [2/4] Quality (1)
71- 73 I3 deg PA [135/233] Position angle
75 I1 --- Nl [0/3]? Number of lines
77- 93 A17 --- Line Line(s)
95- 99 F5.1 --- Flux1 [0.2/112.4]? Line flux for first Line
101-104 F4.2 --- e_Flux1 [0.4/3]? Flux1 1σ uncertainty
106-109 F4.1 --- Flux2 [0.6/26.2]? Line flux for second Line
111-113 F3.1 --- e_Flux2 [0.5/1.1]? Flux2 1σ uncertainty
115-118 F4.1 --- Flux3 [1.5/14.8]? Line flux for third Line
120-122 F3.1 --- e_Flux3 [0.5/0.8]? Flux3 1σ uncertainty
124-127 F4.2 --- Magf [1.4/6.4]? Flux magnification µ (2)
129-132 F4.2 --- b_Magf [1.4/5.9]? 1σ lower limit on Magf
133 A1 --- --- [-]
134-137 F4.2 --- B_Magf [1.4/7.9]? 1σ upper limit on Magf
--------------------------------------------------------------------------------
Note (1): The first part of this table consists of emission line identifications
for the arcs of quality levels 4, 3, and 2, whereas the second part
is comprised of only high-confidence (quality 3 or 4) emission line
objects newly discovered during the blind search procedure, as
described in Section 4.3.
Note (2): Magnifications of multiply lensed objects are calculated assuming
redshift zspec, which was only used in the lens model for
quality >2 objects.
--------------------------------------------------------------------------------
History:
From electronic version of the journal
References:
Treu et al. Paper I. 2015ApJ...812..114T 2015ApJ...812..114T Cat. J/ApJ/812/114
Jones et al. Paper II. 2015AJ....149..107J 2015AJ....149..107J
Schmidt et al. Paper III. 2016ApJ...818...38S 2016ApJ...818...38S
Wang et al. Paper IV. 2015ApJ...811...29W 2015ApJ...811...29W This catalog.
Vulcani et al. Paper V. 2015ApJ...814..161V 2015ApJ...814..161V
Hoag et al. Paper VI. 2016ApJ...831..182H 2016ApJ...831..182H Cat. J/ApJ/831/182
Vulcani et al. Paper VII. 2016ApJ...833..178V 2016ApJ...833..178V Cat. J/ApJ/833/178
Vulcani et al. Paper VIII. 2017ApJ...837..126V 2017ApJ...837..126V
Morishita et al. Paper IX. 2017ApJ...835..254M 2017ApJ...835..254M Cat. J/ApJ/835/254
Wang et al. Paper X. 2017ApJ...837...89W 2017ApJ...837...89W
Schmidt et al. Paper XI. 2017ApJ...839...17S 2017ApJ...839...17S
(End) Emmanuelle Perret [CDS] 12-Feb-2016