J/MNRAS/488/1704 Weak lensing measurements for galaxy clusters (Klein+, 2019)
Weak lensing measurements of the APEX-SZ galaxy cluster sample.
Klein M., Israel H., Nagarajan A., Bertoldi F., Pacaud F., Lee A.T.,
Sommer M., Basu K.
<Mon. Not. R. Astron. Soc., 488, 1704-1727 (2019)>
=2019MNRAS.488.1704K 2019MNRAS.488.1704K (SIMBAD/NED BibCode)
ADC_Keywords: Gravitational lensing ; Clusters, galaxy ; Optical
Keywords: gravitational lensing: weak - galaxies: clusters: general -
cosmology: observations
Abstract:
We present a weak lensing analysis for galaxy clusters from the
APEX-SZ survey. For 39 massive galaxy clusters that were observed via
the Sunyaev-Zel'dovich effect (SZE) with the APEX telescope, we
analyse deep optical imaging data from WFI(@2.2mMPG/ESO) and
Suprime-Cam(@SUBARU) in three bands. The masses obtained in this
study, including an X-ray selected sub-sample of 27 clusters, are
optimized for and used in studies constraining the mass to observable
scaling relations at fixed cosmology. A novel focus of our weak
lensing analysis is the multicolour background selection to suppress
effects of cosmic variance on the redshift distribution of source
galaxies. We investigate the effects of cluster member contamination
through galaxy density, shear profile, and recovered concentrations.
We quantify the impact of variance in source redshift distribution on
the mass estimate by studying nine sub-fields of the COSMOS survey for
different cluster redshift and magnitude limits. We measure a standard
deviation of ∼6 per cent on the mean angular diameter distance ratio
for a cluster at z=0.45 and shallow imaging data of R∼23mag. It falls
to ∼1 per cent for deep, R=26mag, observations. This corresponds to
8.4 per cent and 1.4 per cent scatter in M200. Our background
selection reduces this scatter by 20-40 per cent, depending on cluster
redshift and imaging depth. We derived cluster masses with and without
using a mass concentration relation and find consistent results, and
concentrations consistent with the used mass-concentration relation.
Description:
The galaxy clusters for the lensing follow-up observations were
selected based on their observations with APEX-SZ SZE detector. The
aim was to cover all SZE detections with z<1 using a combination of
dedicated observations with the Wide-Field Imager (WFI, Baade et al.
1999Msngr..95...15B 1999Msngr..95...15B) and archive data from the same instrument and
from Suprime-Cam(@Subaru) (Miyazaki et al. 2002PASJ...54..833M 2002PASJ...54..833M) with
at least three different filter bands. This goal was achieved with the
only exception of a cluster at z= 0.98, resulting in a complete sample
up to z=0.83.
The observation strategy with WFI was chosen to make optimal use of
archival data in order to minimize the need of additional
observations. For clusters where no archival existed, we observed with
WFI in the B-123, V-89, and RC-162 (here after B, V, R) bands. The
typical total exposure times for clusters at z=0.3 are 12000, 4500,
and 15000s. In case of existing archival data, we only observed the
missing bands or completed bands which had already some shallower
data.
Table 1 shows a summary of the data for the clusters presented in
this publication. In addition to the weak lensing measurements using
the default setting shown in Table 2, we present in Table A1 the
results without applying a prior on the concentration parameter. Table
A2 shows the results using the S/N -optimized background selection
without prior on the concentration.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 53 42 Cluster data sets
table2.dat 142 42 Lensing results
tablea1.dat 119 42 Weak lensing mass estimates for the conservative
background selection, for the overdensities
Δ=200 and Δ=500, without prior on
concentration
tablea2.dat 119 42 Weak lensing mass estimates for the
S/N-optimized background selection, for the
overdensities Δ=200 and Δ=500,
without prior on concentration
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- Name Cluster name
18- 22 F5.3 --- z Redshift as quoted in NED
24- 31 A8 --- Filter Filter used for observations (1)
33- 37 I5 s ExpTime Exposure time
39- 40 I2 --- N Number of coadded exposures
42- 45 F4.2 arcsec Seeing Seeing conditions in the lensing band
47- 53 A7 --- Inst Instrument used for observations (2)
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Note (1): The lensing band is denoted by *, and the s after the filter is used
to distinguish between Suprime-Cam and WFI-based data in case of
mixed data sets
Note (2): Intrument as follows:
WFI = Wide-Field Imager at the 2.2m MPG/ESO telescope
SUP = Suprime-Cam at the Subaru telescope
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 16 A16 --- Name Cluster name
18 A1 --- f_Name Flag on Name (G1)
20- 23 F4.2 --- bcut Detection-optimizing distance ratio cut (1)
25- 27 F3.1 --- pcut Detection-optimizing lower purity cut (2)
29- 32 F4.2 --- bgmean Detection-optimizing mean distance ratio
(1)
34- 37 F4.2 --- pgmean Detection-optimizing mean purity (2)
39- 42 F4.2 Mpc R200 Radius within which the enclosed mass
density equals 200 times the critical
density ρc(zd) at cluster
redshift zd
44- 47 F4.2 Mpc E_R200 Upper error on R200
49- 52 F4.2 Mpc e_R200 Lower error on R200
54- 57 F4.2 --- c200 Concentration parameter associated to R200
59- 62 F4.2 --- E_c200 Upper error on c200
64- 67 F4.2 --- e_c200 Lower error on c200
69- 73 F5.2 10+14Msun M200 Cluster mass within the R200 radius (G2)
75- 79 F5.2 10+14Msun E_M200 Upper error on M200
81- 85 F5.2 10+14Msun e_M200 Lower error on M200
87- 90 F4.2 Mpc R500 Radius within which the enclosed mass
density equals 500 times the critical
density ρc(zd) at cluster
redshift zd
92- 95 F4.2 Mpc E_R500 Upper error on R500
97-100 F4.2 Mpc e_R500 Lower error on R500
102-105 F4.2 --- c500 Concentration parameter associated to R500
107-110 F4.2 --- E_c500 Upper error on c500
112-115 F4.2 --- e_c500 Lower error on c500
117-121 F5.2 10+14Msun M500 Cluster mass within the R500 radius (G3)
123-127 F5.2 10+14Msun E_M500 Upper error on M500
129-133 F5.2 10+14Msun e_M500 Lower error on M500
135-137 I3 arcsec Thetamin Minimum separation from the assumed
cluster centre
139-142 I4 arcmin Thetamax Maximum separation from the assumed
cluster centre
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Note (1): β describes the strength of the light deflection in dependency
of the source distance and is usually referred to as angular diameter
ratio β=Dds/Ds, where Dds is the angular diameter distance
between the deflector and source and Ds is the angular diameter
distance between the observer and source
Note (2): Purity estimator p gives the probability of being a background galaxy
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Byte-by-byte Description of file: tablea1.dat tablea2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 16 A16 --- Name Cluster name
18 A1 --- f_Name Flag on Name (G1)
20- 23 F4.2 Mpc R200 Radius within which the enclosed mass density
equals 200 times the critical density
ρc(zd) at cluster redshift zd
25- 28 F4.2 Mpc E_R200 Upper error on R200
30- 33 F4.2 Mpc e_R200 Lower error on R200
35- 39 F5.2 --- c200 Concentration parameter associated to R200
41- 45 F5.2 --- E_c200 Upper error on R200
47- 51 F5.2 --- e_c200 Lower error on R200
53- 57 F5.2 10+14Msun M200 Cluster mass within the R200 radius (G2)
59- 63 F5.2 10+14Msun E_M200 Upper error on M200
65- 69 F5.2 10+14Msun e_M200 Lower error on M200
71- 74 F4.2 Mpc R500 Radius within which the enclosed mass density
equals 500 times the critical density
ρc(zd) at cluster redshift zd
76- 79 F4.2 Mpc E_R500 Upper error on R500
81- 84 F4.2 Mpc e_R500 Lower error on R500
86- 90 F5.2 --- c500 Concentration parameter associated to R500
92- 96 F5.2 --- E_c500 Upper error on c500
98-101 F4.2 --- e_c500 Lower error on c500
103-107 F5.2 10+14Msun M500 Cluster mass within the R500 radius (G3)
109-113 F5.2 10+14Msun E_M500 Upper error on R500
115-119 F5.2 10+14Msun e_M500 Lower error on R500
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Global Notes:
Note (G1): Flag as follows:
W = Results based on WFI
S = Results based on Suprime-Cam
Note (G2): The cluster mass within the R200 radius can be calculated as follows
M200=200x4π/3ρc(zd)R2003
Note (G3): The cluster mass within the R500 radius can be calculated as follows
M500=500x4π/3ρc(zd)R5003
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 05-Dec-2022