J/ApJ/961/186 Multiple images of Abell 2744 from JWST (Cha+, 2024)
Precision MARS mass reconstruction of A2744: synergizing the largest
strong-lensing and densest weak-lensing data sets from JWST.
Cha S., HyeongHan K., Scofield Z.P., Joo H., Jee M.J.
<Astrophys. J., 961, 186 (2024)>
=2024ApJ...961..186C 2024ApJ...961..186C
ADC_Keywords: Gravitational lensing; Infrared sources; Redshifts;
Clusters, galaxy
Keywords: Dark matter distribution ; Weak gravitational lensing ;
Strong gravitational lensing ; Galaxy clusters
Abstract:
We present a new high-resolution free-form mass model of A2744 that
combines both weak-lensing (WL) and strong-lensing (SL) data sets from
JWST. The SL data set comprises 286 multiple images, presenting the
most extensive SL constraint to date for a single cluster. The WL data
set, employing photo-z selection, yields a source density of
∼350arcmin-2, marking the densest WL constraint ever. The combined
mass reconstruction enables the highest-resolution mass map of A2744
within the ∼1.8Mpcx1.8Mpc reconstruction region to date, revealing an
isosceles triangular structure with two legs of ∼1Mpc and a base of
∼0.6Mpc. Although our algorithm, which is called MAximum-entropy
ReconStruction (MARS), is entirely blind to the cluster galaxy
distribution, the resulting mass reconstruction traces the brightest
cluster galaxies remarkably well. The five strongest mass peaks
coincide with the five most luminous cluster galaxies within ≲2". We
do not detect any unusual mass peaks that are not traced by the
cluster galaxies, unlike the findings in previous studies. Our mass
model shows the smallest scatter of SL multiple images in both source
(∼0.05") and image (∼0.1") planes, which is lower than in previous
studies by a factor of ∼4. Although MARS represents the mass field
with an extremely large number of free parameters (∼300000), it
converges to a solution within a few hours because we use a
deep-learning technique. We make our mass and magnification maps
publicly available.
Description:
Our weak-lensing and strong-lensing (WL+SL) analysis uses the publicly
available NIRcam mosaic images of A2744 processed by the Ultra-deep
NIRCam and NIRSpec ObserVations before the Epoch of Reionization
(UNCOVER) team, who combined the three JWST programs
(1) JWST-DD-ERS-1324 (PI: Treu T.; 2022ApJ...935..110T 2022ApJ...935..110T),
(2) JWST-GO-2561 (PIs: Labbe and Bezanson; 2024ApJ...974...92B 2024ApJ...974...92B), and
(3) JWST-DD-2756 (PI: Chen W.; 2022TNSAN.257....1C 2022TNSAN.257....1C). We created
color-composite images from the seven filter-imaging data (F115W,
F150W, F200W, F277W, F356W, F410M, and F444W) and identified
additional multiple images used for SL constraints based on their
morphological properties and colors.
Figure 1 shows the multiple-image distributions that we compiled for
the current study. In region A, we adopt the catalog of
Cha & Jee (2023ApJ...951..140C 2023ApJ...951..140C), who compiled the SL data from
Jauzac+ (2015, J/MNRAS/452/1437), Kawamata+ (2016, J/ApJ/819/114),
Mahler+ (2018, J/MNRAS/473/663), and Bergamini+ (2023, J/A+A/670/A60).
All multiple images in Bergamini+ (2023, J/A+A/670/A60) have
spectroscopic redshifts. In regions B and C, we adopt 79 multiple
images from Furtak+ (2023MNRAS.523.4568F 2023MNRAS.523.4568F) and 9 multiple images that
are knots (distinctive features such as star-forming regions in the
extended multiple images) of system 68 from
Bergamini+ (2023, J/ApJ/952/84).
See Section 2.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 54 286 Multiple image catalog of A2744
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See also:
J/ApJ/621/53 : Multiple arc systems in A1689 (Broadhurst+, 2005)
J/A+A/551/A24 : GMRT Radio Halo Cluster Survey sources (Venturi+, 2013)
J/A+A/564/A125 : AGN Torus model comparison of AGN in CDFS (Buchner+, 2014)
J/MNRAS/444/268 : HST Frontier Fields clusters (Richard+, 2014)
J/MNRAS/452/1437 : Abell 2744 strong-lensing analysis (Jauzac+, 2015)
J/ApJ/811/29 : GLASS. IV. Lensing cluster Abell 2744 (Wang+, 2015)
J/ApJ/801/44 : HST lensing analysis of the CLASH sample (Zitrin+, 2015)
J/ApJ/819/114 : Strong lensing mass modeling (Kawamata+, 2016)
J/MNRAS/473/663 : MUSE and HFFs Photometry of A2744 (Mahler+, 2018)
J/MNRAS/485/3738 : 3D structure in the A370 MUSE Mosaic (Lagattuta+, 2019)
J/A+A/646/A57 : VLT/MUSE MACS J0416.1-2403 redshift cat. (Vanzella+, 2021)
J/A+A/670/A60 : Abell 2744 members (Bergamini+, 2023)
J/ApJ/952/84 : GLASS-JWST ERSP. III. A2744 JWST & MUSE (Bergamini+, 2023)
J/ApJS/270/7 : UNCOVER phot. cat. of A2744 with HST+JWST (Weaver+, 2024)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- ID Identifier (<[CHS2024] A2744 NN.N.N> or
<[CHS2024] A2744 NNN.N> in Simbad (1)
9- 19 F11.9 deg RAdeg [3.54/3.61] Right Ascension (J2000)
21- 32 F12.8 deg DEdeg [-30.42/-30.35] Declination (J2000)
34- 45 F12.9 --- z [1/10.45] Redshift of image
47- 47 A1 --- f_z [*] *: photometric redshifts estimated
using MARS (2)
49- 54 A6 --- Class Class (3)
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Note (1): Identifiers follow the numbering scheme of
Furtak+ 2023MNRAS.523.4568F 2023MNRAS.523.4568F (<[FZW2023] A2744 NN.NN> in Simbad) for
the multiple images in regions B and C.
Note (2): We employ the algorithm called MAximum-entropy ReconStruction (MARS;
Cha & Jee 2022ApJ...931..127C 2022ApJ...931..127C & 2023ApJ...951..140C 2023ApJ...951..140C). MARS is a
free-form mass reconstruction method that uses cross entropy to
regularize its solution, which results in a quasi-unique solution even
though the number of free parameters greatly exceeds that of the
observables. In the current study, we extend the previous MARS
algorithm of Cha & Jee (2022) to accommodate weak-lensing (WL)
constraints as well.
See Section 3.2 for the MARS WL+SL mass reconstruction algorithm
explanations.
Note (3): Class as described in Section 2.2 as follows:
gold = images with spectroscopic redshifts (136 occurrences)
silver = images do not possess spectroscopic redshifts, but they
either have photometric redshifts or have been identified as
multiple images by various studies (150 occurrences)
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 10-Apr-2026