2014A&A...564A.129I


Query : 2014A&A...564A.129I

2014A&A...564A.129I - Astronomy and Astrophysics, volume 564A, 129-129 (2014/4-1)

The 400d Galaxy Cluster Survey weak lensing programme. III. Evidence for consistent WL and X-ray masses at z ≃ 0.5.

ISRAEL H., REIPRICH T.H., ERBEN T., MASSEY R.J., SARAZIN C.L., SCHNEIDER P. and VIKHLININ A.

Abstract (from CDS):

Scaling properties of galaxy cluster observables with cluster mass provide central insights into the processes shaping clusters. Calibrating proxies for cluster mass that are relatively cheap to observe will moreover be crucial to harvest the cosmological information available from the number and growth of clusters with upcoming surveys like eROSITA and Euclid. The recent Planck results led to suggestions that X-ray masses might be biased low by ∼40%, more than previously considered. We aim to extend knowledge of the weak lensing - X-ray mass scaling towards lower masses (as low as 1x1014M) in a sample representative of the z ∼0.4-0.5 population. Thus, we extend the direct calibration of cluster mass estimates to higher redshifts. We investigate the scaling behaviour of MMT/Megacam weak lensing (WL) masses for 8 clusters at 0.39≤z≤0.80 as part of the 400d WL programme with hydrostatic Chandra X-ray masses as well as those based on the proxies, e.g. YX=TXMgas. Overall, we find good agreement between WL and X-ray masses, with different mass bias estimators all consistent with zero. When subdividing the sample into a low-mass and a high-mass subsample, we find the high-mass subsample to show no significant mass bias while for the low-mass subsample, there is a bias towards overestimated X-ray masses at the ∼2σ level for some mass proxies. The overall scatter in the mass-mass scaling relations is surprisingly low. Investigating possible causes, we find that neither the greater range in WL than in X-ray masses nor the small scatter can be traced back to the parameter settings in the WL analysis. We do not find evidence for a strong (∼40%) underestimate in the X-ray masses, as suggested to reconcile recent Planck cluster counts and cosmological constraints. For high-mass clusters, our measurements are consistent with other studies in the literature. The mass dependent bias, significant at ∼2σ, may hint at a physically different cluster population (less relaxed clusters with more substructure and mergers); or it may be due to small number statistics. Further studies of low-mass high-z lensing clusters will elucidate their mass scaling behaviour.

Abstract Copyright:

Journal keyword(s): galaxies: clusters: general - cosmology: observations - gravitational lensing: weak - X-rays: galaxies: clusters

Simbad objects: 16

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Number of rows : 16
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 ClG J0030+2618 ClG 00 30 33.6 +26 18 16           ~ 58 0
2 ClG J0152-1358 ClG 01 52 41.3 -13 58 13           ~ 250 3
3 ClG J0159+0030 ClG 01 59 18.2 +00 30 09           ~ 28 0
4 ClG J0230+1836 ClG 02 30 26.6 +18 36 22           ~ 17 0
5 ZwCl 0806+2822 ClG 08 09 41.0 +28 11 58           ~ 22 0
6 ClG J1003+3253 ClG 10 03 04.1 +32 54 28           ~ 25 0
7 ClG J1120+4318 ClG 11 20 07.6 +43 18 07           ~ 57 0
8 ClG J1226+3332 ClG 12 26 57.7 +33 32 50           ~ 202 0
9 ClG J1357+6232 ClG 13 57 19.4 +62 32 42           ~ 17 0
10 ClG J1416+4446 ClG 14 16 28.1 +44 46 38           ~ 44 0
11 ClG J1524+0957 ClG 15 24 40.3 +09 57 35           ~ 58 0
12 ClG J1641+4001 ClG 16 41 52.3 +40 01 29           ~ 37 0
13 ClG J1701+6414 ClG 17 01 22.6 +64 14 09           ~ 67 0
14 SPT-CL J2022-6323 ClG 20 22 05.6 -63 23 50           ~ 14 0
15 SPT-CL J2030-5638 ClG 20 30 49.6 -56 38 07           ~ 14 0
16 SPT-CL J2135-5726 ClG 21 35 39.8 -57 26 29           ~ 21 0

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2022.09.26-08:52:59

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