J/MNRAS/473/663 MUSE and HFFs Photometry of A2744 (Mahler+, 2018)
Strong-lensing analysis of A2744 with MUSE and Hubble Frontier Fields images.
Mahler G., Richard J., Clement B., Lagattuta D., Schmidt K., Patricio V.,
Soucail G., Bacon R., Pello R., Bouwens R., Maseda M., Martinez J.,
Carollo M., Inami H., Leclercq F., Wisotzki L.
<Mon. Not. R. Astron. Soc., 473, 663-692 (2018)>
=2018MNRAS.473..663M 2018MNRAS.473..663M (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Photometry, HST ; Spectroscopy
Keywords: gravitational lensing: strong - techniques: imaging spectroscopy -
galaxies: clusters: individual: Abell 2744 - galaxies: high redshift -
dark matter
Abstract:
We present an analysis of Multi Unit Spectroscopic Explorer (MUSE)
observations obtained on the massive Frontier Fields (FFs) cluster
A2744. This new data set covers the entire multiply imaged region
around the cluster core. The combined catalogue consists of 514
spectroscopic redshifts (with 414 new identifications). We use this
redshift information to perform a strong-lensing analysis revising
multiple images previously found in the deep FF images, and add three
new MUSE-detected multiply imaged systems with no obvious Hubble Space
Telescope counterpart. The combined strong-lensing constraints include
a total of 60 systems producing 188 images altogether, out of which 29
systems and 83 images are spectroscopically confirmed, making A2744
one of the most well-constrained clusters to date. Thanks to the large
amount of spectroscopic redshifts, we model the influence of
substructures at larger radii, using a parametrization including two
cluster-scale components in the cluster core and several group scale
in the outskirts. The resulting model accurately reproduces all the
spectroscopic multiple systems, reaching an rms of 0.67-arcsec in
the image plane. The large number of MUSE spectroscopic redshifts
gives us a robust model, which we estimate reduces the systematic
uncertainty on the 2D mass distribution by up to ∼2.5 times the
statistical uncertainty in the cluster core. In addition, from a
combination of the parametrization and the set of constraints, we
estimate the relative systematic uncertainty to be up to
9 per cent at 200kpc.
Description:
The HFF observations of A2744 (ID: 13495, PI: J. Lotz) were taken
between 2013 October 25 and 2014 July 1 in seven different filters,
three with the Advanced Camera for Surveys (ACS; F435W, F606W, F814W)
and four taken with the Wide Field Camera 3 (WFC3; F105W, F125W, F140W
and F160W). In total 280 orbits were devoted to A2744 reaching in each
filter a 5σ limiting magnitude AB∼29. The self-calibrated data
provided by Space Telescope Science Institute (STScI,
https://archive.stsci.edu/missions/hlsp/frontier/abell2744/images/hst/)
(version v1.0 for WFC3 and v1.0-epoch2 for ACS) with a pixel size of
60mas are used in this study.
A2744 was observed with the Multi Unit Spectrographic Explorer (MUSE)
between 2014 September and 2015 October as part of the GTO Program
094.A-0115 (PI: Richard). A 2x2 mosaic of MUSE pointings was designed
to cover the entire multiple image area, centred at RA=00:14:20.952
and DE=-30:23:53.88. The four quadrants were observed for a total of
3.5, 4, 4 and 5h, in addition to 2h at the centre of the cluster.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
catalog.dat 186 514 Redshift catalogue
tablea1.dat 110 185 Multiply imaged systems considered in this work
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See also:
http://muse-vlt.eu/science/a2744 : MUSE A2744 Home Page
Byte-by-byte Description of file: catalog.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- ID Identification number
7- 16 F10.8 deg RAdeg Right ascension (J2000)
18- 28 F11.7 deg DEdeg Declination (J2000)
30- 35 F6.4 --- z Redshift
37 I1 --- confid [1/3] Confidence level of the detection (G1)
39 I1 --- Type [0/6] Classification of the object (2)
41- 45 F5.1 --- MUL ? Multiple image ID if it is reported in our
strong-lensing analysis
47 A1 --- l_F435W [-] - for upper limit on F435W
48- 58 F11.8 mag F435W ? HST ACS F435W magnitude
60- 66 F7.4 mag e_F435W ? rms uncertainty on F435W
68 A1 --- l_F606W [-] - for upper limit on F606W
69- 79 F11.8 mag F606W ? HST ACS F606W magnitude
81- 86 E6.4 mag e_F606W ? rms uncertainty on F606W
88 A1 --- l_F814W [-] - for upper limit on F814W
89- 95 F7.4 mag F814W ? HST ACS F814W magnitude
97-102 E6.4 mag e_F814W ? rms uncertainty on F814W
104 A1 --- l_F105W [-] - for upper limit on F105W
105-111 F7.4 mag F105W ? HST WFC3 F105W magnitude
113-118 E6.4 mag e_F105W ? rms uncertainty on F105W
120 A1 --- l_F125W [-] - for upper limit on F125W
121-127 F7.4 mag F125W ? HST WFC3 F125W magnitude
129-134 E6.4 mag e_F125W ? rms uncertainty on F125W
136 A1 --- l_F140W [-] - for upper limit on F140W
137-143 F7.4 mag F140W ? HST WFC3 F140W magnitude
145-150 E6.4 mag e_F140W ? rms uncertainty on F140W
152 A1 --- l_F160W [-] - for upper limit on F160W
153-159 F7.4 mag F160W ? HST WFC3 F160W magnitude
161-166 E6.4 mag e_F160W ? rms uncertainty on F160W
168-175 F8.3 mag mu Magnification ratio computed from our
lensing mass model
177-186 F10.4 mag e_mu ?=66666 rms uncertainty on mu
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Note (2): based on the system used for the MUSE-UDF analysis (Bacon et al.,
in prep.) as follows:
0 = stars
1 = nearby emission line object
2 = [OII] emitters
3 = absorption line galaxies
4 = CIII] emitters
6 = Lyman-alpha emitters
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 5 F5.1 --- MUL Multiple image ID
7- 16 F10.8 deg RAdeg Right ascension (J2000)
18- 27 F10.6 deg DEdeg Declination (J2000)
29- 31 A3 --- zref Previous studies reporting spectroscopic
redshifts in agreement with our detection (1)
33- 38 F6.4 --- zspec ? Spectroscopic redshift
41 I1 --- confid [1/3]? Confidence level attached to the
spectroscopic identification of the
redshift (G1)
43- 48 F6.4 --- zmod ?=- Model redshift
49 A1 --- --- [+]
50- 55 F6.4 --- E_zmod ? Error on zmod (upper value)
56 A1 --- --- [-]
57- 62 F6.4 --- e_zmod ? Error on zmod (lower value)
65- 74 A10 --- absline Absorption lines detected in the spectrum
76- 85 A10 --- emline Emission lines detected in the spectrum
87- 90 F4.2 arcsec rmsg ?=- rms of the predicted image positions
according to models runs with the related set
of constraints (gold)
92- 95 F4.2 arcsec rmss ?=- rms of the predicted image positions
according to models runs with the related set
of constraints (silver)
97-100 F4.2 arcsec rmsb ?=- rms of the predicted image positions
according to models runs with the related set
of constraints (bronze)
102-105 F4.2 arcsec rmsc ?=- rms of the predicted image positions
according to models runs with the related set
of constraints (copper)
107-110 A4 ---- Cat Category of confidence level in which each
image belongs (2)
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Note (1): References as follows:
J = Johnson et al., 2014ApJ...797...48J 2014ApJ...797...48J
R = Richard et al., 2014, Cat. J/MNRAS/444/268
W = Wang et al., 2015, Cat. J/ApJ/811/29
M = this study
Note (2): Category of confidence level as follows:
g = most reliable constraints, gold
s = second set of constraints, silver
b = third set, bronze, includes less reliable constraints
c = fourth set, copper, include images 3.3, 8.3, 14.3, 36.3, 37.3 and 38.3
because they were previously in disagreement among previous studies
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Global notes:
Note (G1): Confidence level of the detection from 3 for very secure down
to 1 for less secure identifications according to our grading policy.
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History:
From electronic version of the journal and http://muse-vlt.eu/science/a2744/
(End) Patricia Vannier [CDS] 13-Sep-2019