J/ApJ/928/87 Strongest cluster lenses (Fox+, 2022)
The Strongest Cluster Lenses: an analysis of the relation between strong
gravitational lensing strength and the physical properties of galaxy clusters.
Fox C., Mahler G., Sharon K., Remolina Gonzalez J.D.
<Astrophys. J. 928, 87 (2022)>
=2022ApJ...928...87F 2022ApJ...928...87F (SIMBAD/NED BibCode)
ADC_Keywords: Gravitational lensing ; Clusters, galaxy
Keywords: galaxies: clusters - strong gravitational lensing
Abstract:
Strong gravitational lensing provides unique opportunities to
investigate the mass distribution at the cores of galaxy clusters and
to study high redshift galaxies. Using 110 strong lensing models of 74
cluster fields from the Hubble Frontier Fields (HFF), Reionization
Lensing Cluster Survey (RELICS), and Sloan Giant Arcs Survey (SGAS),
we evaluate the lensing strength of each cluster (area with |µ|≥3
for zs=9, normalized to a lens redshift of z=0.5). We assess how
large scale mass, projected inner core mass, and the inner slope of
the projected mass density profile relate to lensing strength. While
we do not identify a strong correlation between lensing strength and
large scale mass (Kendall τ=0.26 and Spearman r=0.36), we reveal
that the inner slope (50kpc≤r≤00kpc) of the projected mass
density profile is indicative of lensing strength and can set an upper
bound on the possible lensing strength of a cluster (Kendall
τ=0.53 and Spearman r=0.71). As anticipated, the effective
Einstein area strongly correlates with the lensing strength and a
large (≳30.0'') radial extent of lensing evidence is a strong
indicator of a powerful lens. We attribute the spread in the
correlation to the complexity of individual lensing clusters, which is
well captured by the lensing strength estimator. These results can
help to more efficiently design future observations to use clusters as
cosmic telescopes.
Description:
We gather a sample of strong lensing clusters with publicly available
models from the HFF (Lotz et al., 2017ApJ...837...97L 2017ApJ...837...97L), RELICS (Coe et
al., 2019ApJ...884...85C 2019ApJ...884...85C, Cat. J/ApJ/884/85), and Sloan Giant Arcs
Survey (SGAS; Sharon et al., 2020ApJS..247...12S 2020ApJS..247...12S, Cat. J/ApJS/247/12).
The final sample, which consists of 74 cluster fields with a total of
94 parametric lens models, spans a wide range in mass and redshift.
All clusters included in this table come from three programs: HFF,
RELICS, and SGAS. α and δ refer to the right ascension and
declination of the BCG selected in the analysis. zlens refers to the
redshift of the cluster. M500 and M200 are the large scale mass
estimates, measured independent of the lensing analyses. Alg. refers
to the modeling algorithm used: L=Lenstool, LTM=Light-Traces-Mass,
G=GLAFIC, GL=GRAVLENS, and GR=GRALE. For the HFF Lenstool models,
letters after the dash indicate the lens modeling team, where
L-S=Sharon, L-CATS=CATS, and L-Cam=Caminha. Spec-z indicates whether
or not the lens model employs a spectroscopic redshift constraint or
if it is unknown whether a spectroscopic constraint is used.
MSL(200kpc) refers to the mass within a 200kpc aperture from the BCG,
computed from the strong lens model. logS50-200 refers to the
logarithmic slope of the projected mass density profile in the range
of 50-200kpc from the BCG. rEe is the effective Einstein radius
for zs=9. Alens is the non-corrected lensing. strength and A0.5 is
the distance-corrected lensing strength, for zs=9.0 |µ|≥3.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 192 111 All clusters included in this paper, separated by
strong lensing programs (HFF, RELICS, and SGAS)
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See also:
J/ApJ/884/85 : RELICS: Reionization Lensing Cluster Survey (Coe+, 2019)
J/ApJS/247/12 : Strong lens models for 37 clusters from SGAS (Sharon+, 2020)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- Survey Survey (HFF, RELICS or SGAS) (1)
8- 27 A20 --- Cluster Cluster
28 A1 --- n_Cluster [ac] Note on Cluster (2)
30- 35 A6 --- Alg Algorithm used (3)
37- 38 A2 --- r_Alg [bdefghijkn ] References for Algorithm
used (4)
40- 46 F7.5 --- zlens Lens redshift
48- 56 F9.5 deg RAdeg BCG right ascension (J2000) (BCG_ra)
58- 66 F9.5 deg DEdeg BCG declination (J2000) (BCG_dec)
68- 72 F5.2 10+14Msun M500 ?=- Large-scale mass estimate M500,
measured independent of the of the BCG
selected in the analysis
74- 78 F5.2 10+14Msun e_M500 ?=- Error on M500 (lower value)
80- 84 F5.2 10+14Msun E_M500 ?=- Error on M500 (upper value)
86- 90 F5.2 10+14Msun M200 ?=- Large-scale mass estimate M200,
measured independent of the of the BCG
selected in the analysis
92- 96 F5.2 10+14Msun e_M200 ?=- Error on M200 (lower value)
98-102 F5.2 10+14Msun E_M200 ?=- Error on M200 (upper value)
104-110 A7 --- Spec-z [yes no unknown] indicates whether or not
the lens model employs a spectroscopic
redshift constraint or if it is unknown
whether a spectroscopic constraint is
used
112-117 F6.2 10+12Msun MSL200kpc Mass within a 200kpc aperture from the
BCG, computed from the strong lens model
119-123 F5.2 10+12Msun e_MSL200kpc Error on MSL200kpc (lower value)
125-129 F5.2 10+12Msun E_MSL200kpc Error on MSL200kpc (upper value)
131-135 F5.2 --- logS50-200 logarithmic slope of the projected mass
density profile in the range of 50-200kpc
from the BCG
137-140 F4.2 --- e_logS50-200 Error on logS50-200 (lower value)
142-145 F4.2 --- E_logS50-200 Error on logS50-200 (upper value)
147-151 F5.2 arcsec rEe Effective Einstein radius for zs=9
153-156 F4.2 arcsec e_rEe Error on rEe (lower value)
158-161 F4.2 arcsec E_rEe Error on rEe (upper value)
163-167 F5.2 arcmin+2 Alens Non-corrected lensing strength
(Alens|mu|≥3 )
169-172 F4.2 arcmin+2 e_Alens Error on Alens (lower value)
174-177 F4.2 arcmin+2 E_Alens Error on Alens (upper value)
179-182 F4.2 arcmin+2 A05 Distance-corrected lending strength for
zs=9 (A0.5|mu|≥3)
mu above 3 normed zs=0.5
184-187 F4.2 arcmin+2 e_A05 Error on A05 (lower value)
189-192 F4.2 arcmin+2 E_A05 Error on A05 (upper value)
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Note (1): Reference for HFF models: Johnson et al. (2014ApJ...797...48J 2014ApJ...797...48J).
Reference for SGAS models: Sharon et al. (2020ApJ...889..189S 2020ApJ...889..189S).
Note (2): Notes as follows:
a = Abell 1758a has two major components (Northwest and Southeast).
Although contained in one model, the amplification areas of the
lensing strength we compute (see section 3.1) for each component do
not intersect. We therefore split the model into Northwest and
Southeast components. RXS J060313.4+4212 has a Northern and Southern
component, modeled separately. Because they have been separated into
components, we do not include the Planck SZ M500 mass of these two
clusters in total mass comparisons.
c = PLCK G004.5-19.5 lens redshift was updated to z=0.519 in
Albert et al. (2017A&A...607A...4A 2017A&A...607A...4A, Cat. J/A+A/607/A4).
The cluster lens was modeled at the redshift reported in the table.
Note (3): Algorithm as follows:
G = GLAFIC
GL = GRAVLENS
GR = GRALE
L = Lenstool
L-CATS = CATS
L-Cam = Caminha
L-S = Sharon
LTM = Light-Traces-Mass
Note (4): References as follows:
b = Denotes the three GLAFIC models in which an additional 5% was added to
the upper error bar of the lensing strength to account for the
magnification map not including the entire |mu|≥3 region.
d = Cibirka et al. (2018ApJ...863..145C 2018ApJ...863..145C)
e = Cerny et al. (2018ApJ...859..159C 2018ApJ...859..159C)
f = Acebron et al. (2019ApJ...874..132A 2019ApJ...874..132A)
g = Acebron et al. (2018ApJ...858...42A 2018ApJ...858...42A)
h = Mahler et al. (2019ApJ...873...96M 2019ApJ...873...96M)
i = Acebron et al. (2020ApJ...898....6A 2020ApJ...898....6A)
j = Zitrin et al. (2017ApJ...839L..11Z 2017ApJ...839L..11Z)
k = Paterno-Mahler et al. (2018ApJ...863..154P 2018ApJ...863..154P)
n = The GLAFIC model of RXC J0600.1-2007 employs an updated redshift of
0.43 from more recent spectroscopy with the Multi Unit Spectroscopic
Explorer on the Very Large Telescope.
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Acknowledgements:
Guillaume Mahler, gmahler(at)umich.edu
(End) Patricia Vannier [CDS] 14-Jun-2021