J/ApJ/890/148 Concentration-mass relation for XXL clusters (Umetsu+, 2020)
Weak-lensing analysis of X-ray-selected XXL galaxy groups and clusters with
Subaru HSC data.
Umetsu K., Sereno M., Lieu M., Miyatake H., Medezinski E., Nishizawa A.J.,
Giles P., Gastaldello F., McCarthy I.G., Kilbinger M., Birkinshaw M.,
Ettori S., Okabe N., Chiu I.-N., Coupon J., Eckert D., Fujita Y.,
Higuchi Y., Koulouridis E., Maughan B., Miyazaki S., Oguri M., Pacaud F.,
Pierre M., Rapetti D., Smith G.P.
<Astrophys. J., 890, 148 (2020)>
=2020ApJ...890..148U 2020ApJ...890..148U
ADC_Keywords: Clusters, galaxy; X-ray sources; Redshifts; Optical;
Gravitational lensing
Keywords: Weak gravitational lensing ; Observational cosmology ;
Gravitational lensing shear ; Dark matter distribution ;
Cold dark matter
Abstract:
We present a weak-lensing analysis of X-ray galaxy groups and clusters
selected from the XMM-XXL survey using the first-year data from the
Hyper Suprime-Cam (HSC) Subaru Strategic Program. Our joint
weak-lensing and X-ray analysis focuses on 136 spectroscopically
confirmed X-ray-selected systems at 0.031≤z≤1.033 detected in the
25deg2 XXL-N region, which largely overlaps with the HSC-XMM field.
With high-quality HSC weak-lensing data, we characterize the mass
distributions of individual clusters and establish the
concentration-mass (c-M) relation for the XXL sample, by accounting
for selection bias and statistical effects and marginalizing over the
remaining mass calibration uncertainty. We find the mass-trend
parameter of the c-M relation to be β=-0.07±0.28 and the
normalization to be c200=4.8±1.0(stat)±0.8(syst) at
M200=1014h-1M☉ and z=0.3. We find no statistical evidence
for redshift evolution. Our weak-lensing results are in excellent
agreement with dark-matter-only c-M relations calibrated for recent
ΛCDM cosmologies. The level of intrinsic scatter in c200 is
constrained as σ(lnc200)<24% (99.7% CL), which is smaller than
predicted for the full population of ΛCDM halos. This is likely
caused in part by the X-ray selection bias in terms of the cool-core
or relaxation state. We determine the temperature-mass (TX-M500)
relation for a subset of 105 XXL clusters that have both measured HSC
lensing masses and X-ray temperatures. The resulting TX-M500 relation
is consistent with the self-similar prediction. Our TX-M500 relation
agrees with the XXL DR1 results at group scales but has a slightly
steeper mass trend, implying a smaller mass scale in the cluster
regime. The overall offset in the TX-M500 relation is at the
∼1.5σ level, corresponding to a mean mass offset of 34%±20%.
We also provide bias-corrected, weak-lensing-calibrated M200 and M500
mass estimates of individual XXL clusters based on their measured
X-ray temperatures.
Description:
In the present study, we focus on spectroscopically confirmed
X-ray-selected systems of class C1 and C2 drawn from the XXL DR2
catalog presented in XXL Paper XX (Chiappetti+, 2018, IX/52).
See Section 2.1.
We use the Subaru HSC first-year shear catalog for our weak-lensing
analysis. Full details of the creation of the catalog are described in
Mandelbaum+ (2018MNRAS.481.3170M 2018MNRAS.481.3170M and 2018PASJ...70S..25M 2018PASJ...70S..25M).
The first-year shear catalog was produced using about 90 nights of
HSC-Wide data taken from 2014 March to 2016 April. This shear catalog
consists of six distinct patches of the sky covering a total of 137deg2.
See Section 2.2.
Throughout this paper, we assume a spatially flat ΛCDM
cosmology with Ωm=0.28, ΩΛ=0.72, and a Hubble
constant of H0=100h.km/s/Mpc with h=0.7. We adopt σ8=0.817
for the fiducial normalization of the matter power spectrum, with
σ8 the rms amplitude of linear mass fluctuations in a sphere
of comoving radius 8h-1Mpc. We denote the critical density of the
universe at a particular redshift z as ρc(z)=3H2(z)/(8πG),
with H(z) the redshift-dependent Hubble parameter.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 121 136 Cluster properties and weak-lensing measurements
--------------------------------------------------------------------------------
See also:
IX/49 : XXL Survey: First results (Pierre+, 2016)
IX/52 : XXL Survey. DR2 (Chiappetti+, 2018)
J/ApJ/690/1236 : COSMOS photometric redshift catalog (Ilbert+, 2009)
J/ApJS/199/25 : CLASH sources for MACS1149.6+2223 (Postman+, 2012)
J/MNRAS/444/147 : Richness of galaxy clusters (Oguri, 2014)
J/ApJS/216/27 : Galaxy clusters in the SPT-SZ survey (Bleem+, 2015)
J/A+A/581/A41 : OmegaWINGS BV phot. of galaxy clusters (Gullieuszik+, 2015)
J/MNRAS/450/3675 : CoMaLit. IV. Sigma Catalogue (Sereno+, 2015)
J/ApJS/224/24 : The COSMOS2015 catalog (Laigle+, 2016)
J/ApJS/224/1 : redMaPPer cluster catalog from DES data (Rykoff+, 2016)
J/A+A/607/A81 : Properties of the sample of clusters (Biviano+, 2017)
J/MNRAS/468/1917 : Concentration parameter of galaxy clusters (Rossetti+, 2017)
J/MNRAS/468/3322 : CoMaLit. V. Mass forecasting with proxies (Sereno+, 2017)
J/PASJ/70/S20 : HSC Wide S16A cluster catalog (Oguri+, 2018)
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- XLSSC [2/202] Identifier (1)
5- 10 F6.3 deg RAdeg [30.42/38.51] X-ray cluster right
ascension (J2000)
12- 17 F6.3 deg DEdeg [-6.21/-2.66] X-ray cluster
declination (J2000)
19- 23 F5.3 --- z [0.03/1.04] Redshift
25 I1 --- Cl [1/2] Object class (2)
27- 30 F4.2 keV T300kpc [0.63/6.03]? X-ray temperature, T300kpc
32- 35 F4.2 keV e_T300kpc [0.03/1.05]? T300kpc downwards uncertainty
37- 40 F4.2 keV E_T300kpc [0.04/1.14]? T300kpc upwards uncertainty
42- 44 F3.1 --- c200 [2/9.6] Concentration parameter
c200=r200/rs (section 4.1) (3)
46- 48 F3.1 --- e_c200 [1.2/5.6] C200 uncertainty
50- 52 F3.1 --- c200Med [1.9/9.3] Median value of c200
54- 57 F4.2 10+14Msun M200 [0.07/9.64] Mass enclosed within a sphere
of radius r200 (3)
59- 62 F4.2 10+14Msun e_M200 [0.08/7.94] M200 uncertainty
64- 67 F4.2 10+14Msun M200Med [0.07/9.45] Median value of M200
69- 72 F4.2 10+14Msun M500 [0.05/5.59] Mass, M500 (3)
74- 77 F4.2 10+14Msun e_M500 [0.05/5.5] M500 uncertainty
79- 82 F4.2 10+14Msun M500Med [0.05/5.53] Median value of M500
84- 87 F4.2 10+14Msun M200MT [0.2/6.8]? Bias-corrected,
weak-lensing-calibrated mass estimates,
M200,MT (4)
89- 92 F4.2 10+14Msun e_M200MT [0.1/2.2]? M200MT downwards uncertainty
94- 97 F4.2 10+14Msun E_M200MT [0.19/3.4]? M200MT upwards uncertainty
99- 102 F4.2 10+14Msun M500MT [0.16/4.72]? Bias-corrected,
weak-lensing-calibrated mass estimates,
M500,MT (4)
104- 107 F4.2 10+14Msun e_M500MT [0.08/1.35]? M500MT downwards uncertainty
109- 112 F4.2 10+14Msun E_M500MT [0.14/1.92]? M500MT upwards uncertainty
114- 117 F4.1 --- S/N [-2.1/6] Signal-to-noise ratio based on
the linear estimator (Equation (13))
119- 121 F3.1 --- SNRq [0.8/9.1] Signal-to-noise ratio based on
the quadratic estimator (Equation (15))
--------------------------------------------------------------------------------
Note (1): XLSSC cluster identifier (between 1 and 499 or between 500 and 999,
for XXL-N or XXL-S, respectively).
Note (2): Class of the spectroscopically confirmed X-ray-selected systems
from the XXL Paper (Pierre+, 2016, IX/49) as follows:
1 = free of contamination by spurious detections or blended point sources
2 = deeper population but its initial selection is about 50% contaminated
Note (3): These parameters have been constrained by fitting a spherical NFW
model to the weak-lensing ΔΣ(R) profile of each individual
cluster over the comoving radial range R in [0.3,3]h-1Mpc. These
cluster mass and concentration measurements are not corrected for mass
modeling bias, statistical bias, or selection effects. All the mass
estimates are subject to a systematic uncertainty of ±5%. Our
concentration estimates have a systematic uncertainty of ±16%.
Note (4): We provide bias-corrected, weak-lensing-calibrated mass estimates
M200,MT and M500,MT (median and 68% confidence intervals of the
posterior distribution) for each individual cluster based on the
measured X-ray temperature, T300kpc, where available (Section 5.5;
see Figure 10). We recommend using these statistically corrected
MΔ,MT as a weak-lensing mass estimate for a given individual
cluster.
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 02-Aug-2021