J/MNRAS/452/1437 Abell 2744 strong-lensing analysis (Jauzac+, 2015)
Hubble Frontier Fields: a high-precision strong-lensing analysis of the
massive galaxy cluster Abell 2744 using ∼ 180 multiple images.
Jauzac M., Richard J., Jullo E., Clement B., Limousin M., Kneib J.-P.,
Ebeling H., Natarajan P., Rodney S., Atek H., Massey R., Eckert D.,
Egami E., Rexroth M.
<Mon. Not. R. Astron. Soc., 452, 1437-1446 (2015)>
=2015MNRAS.452.1437J 2015MNRAS.452.1437J (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Gravitational lensing
Keywords: gravitational lensing: strong -
galaxies: clusters: individual: Abell 2744 - cosmology: observations
Abstract:
We present a high-precision mass model of galaxy cluster Abell 2744,
based on a strong gravitational-lensing analysis of the Hubble
Space Telescope Frontier Fields (HFF) imaging data, which now include
both Advanced Camera for Surveys and Wide Field Camera 3 observations
to the final depth. Taking advantage of the unprecedented depth of the
visible and near-infrared data, we identify 34 new multiply imaged
galaxies, bringing the total to 61, comprising 181 individual lensed
images. In the process, we correct previous erroneous identifications
and positions of multiple systems in the northern part of the cluster
core. With the lenstool software and the new sets of multiple images,
we model the cluster using two cluster-scale dark matter haloes plus
galaxy-scale haloes for the cluster members. Our best-fitting model
predicts image positions with an rms error of 0.79 arcsec, which
constitutes an improvement by almost a factor of 2 over previous
parametric models of this cluster. We measure the total projected mass
inside a 200kpc aperture as (2.162±0.005)x1014M☉, thus
reaching 1 percent level precision for the second time, following the
recent HFF measurement of MACSJ0416.1-2403. Importantly, the higher
quality of the mass model translates into an overall improvement by a
factor of 4 of the derived magnification factor. Together with our
previous HFF gravitational lensing analysis, this work demonstrates
that the HFF data enables high-precision mass measurements for massive
galaxy clusters and the derivation of robust magnification maps to
probe the early Universe.
Description:
The HFF observations of Abell 2744 (ID: 13495, P.I: J. Lotz) were
obtained with WFC3 between October 25th and November 28th 2013 in four
filters (F105W,F125W, F140W, and F160W) for total integration times
corresponding to 24.5, 12, 10, and 14.5 orbits, respectively. The HFF
ACS observations were obtained more recently, between May 14th and
July 1st 2014, in three filters (F435W, F606W, and F814W) for total
integration times corresponding to 24, 14, and 46 orbits,
respectively.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 64 173 Multiply imaged systems considered in this work
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See also:
J/ApJ/728/27 : Chandra and AAOmega observations of Abell 2744 (Owers+, 2011)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1 A1 --- n_ID [+*a] Note on ID (1)
2- 5 F4.1 --- ID Identification number, NN.N
7- 8 I2 h RAh Right ascension (J2000)
10- 11 I2 min RAm Right ascension (J2000)
13- 17 F5.2 s RAs Right ascension (J2000)
19 A1 --- DE- Declination sign (J2000)
20- 21 I2 deg DEd Declination (J2000)
23- 24 I2 arcmin DEm Declination (J2000)
26- 30 F5.2 arcsec DEs Declination (J2000)
32- 37 F6.3 --- z ? Redshift from model
39- 42 F4.2 --- e_z ? rms uncertainty on z
44- 48 F5.2 mag F814Wmag ? HST F814W magnitude (2)
50- 53 F4.2 mag e_F814Wmag ? rms uncertainty on F814Wmag
55 A1 --- l_mu Limit flag on mu
56- 60 F5.1 --- mu ? Magnification
62- 64 F3.1 --- e_mu ? rms uncertainty on mu
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Note (1): Flag as follows:
* = high-redshift candidate systems identified by Ishigaki et al.
(2015) not included in our model,
but for which we assumed z∼8 for the prediction of the magnification
+ = image identifications in which we are less confident, which are not
included in the optimization
a = system #46 is the high-redshift system identified by Zitrin et al.
(2014ApJ...793L..12Z 2014ApJ...793L..12Z) and system #60 is a new system discovered by
Wang et al. (2015, preprint, arXiv:1504.00240).
However, we include the predicted magnification given by our model.
Note (2): Some of the magnitudes are not quoted because we were facing
deblending issues that did not allow us to get reliable measurements.
The flux magnification factors come from our best-fitting mass model,
with errors derived from MCMC sampling.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 29-Jan-2016