J/MNRAS/452/1171 Extended X-ray sources in CFHTLenS footprint (Wilcox+, 2015)
The XMM Cluster Survey:
testing chameleon gravity using the profiles of clusters.
Wilcox H., Bacon D., Nichol R.C., Rooney P.J., Terukina A., Romer A.K.,
Koyama K., Zhao G.-B., Hood R., Mann R.G., Hilton M., Manolopoulou M.,
Sahlen M., Collins C.A., Liddle A.R., Mayers J.A., Mehrtens N.,
Miller C.J., Stott J.P., Viana P.T.P.
<Mon. Not. R. Astron. Soc., 452, 1171-1183 (2015)>
=2015MNRAS.452.1171W 2015MNRAS.452.1171W (SIMBAD/NED BibCode)
ADC_Keywords: X-ray sources ; Redshifts
Keywords: gravitation - gravitational lensing: weak - X-rays: galaxies: clusters
Abstract:
The chameleon gravity model postulates the existence of a scalar field
that couples with matter to mediate a fifth force. If it exists, this
fifth force would influence the hot X-ray emitting gas filling the
potential wells of galaxy clusters. However, it would not influence
the clusters weak lensing signal. Therefore, by comparing X-ray and
weak lensing profiles, one can place upper limits on the strength of a
fifth force. This technique has been attempted before using a single,
nearby cluster (Coma, z=0.02). Here we apply the technique to the
stacked profiles of 58 clusters at higher redshifts (0.1<z<1.2),
including 12 new to the literature, using X-ray data from the XMM
Cluster Survey and weak lensing data from the
Canada-France-Hawaii-Telescope Lensing Survey. Using a multiparameter
Markov chain Monte Carlo analysis, we constrain the two chameleon
gravity parameters (β and φ{inf}). Our fits are consistent
with general relativity, not requiring a fifth force. In the special
case of fR gravity (where β=sqrt(1/6)), we set an upper limit
on the background field amplitude today of |fR0|<6x10-5 (95
percent CL). This is one of the strongest constraints to date on
|fR0| on cosmological scales. We hope to improve this constraint in
future by extending the study to hundreds of clusters using data from
the Dark Energy Survey.
Description:
In this paper, we used public weak lensing data (galaxy ellipticities
and photometric redshifts) provided by the CFHTLenS (Heymans et al.,
2012MNRAS.427..146H 2012MNRAS.427..146H). We also used public X-ray data taken from the
XMM-Newton archive and have collated a sample of X-ray clusters in
the CFHTLenS region using pipelines developed for the XCS
(Lloyd-Davies et al., 2011MNRAS.418...14L 2011MNRAS.418...14L).
We have examined 58 X-ray-selected galaxy clusters, which have both
good quality weak lensing data from CFHTlenS and X-ray data from XCS.
After binning our clusters by X-ray temperature, we have generated
weak lensing profiles and X-ray surface brightness profiles.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableb1.dat 32 118 Sample of the extended X-ray sources in
CFHTLenS footprint
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See also:
J/MNRAS/423/1024 : XCS-DR1 Cluster Catalogue (Mehrtens+, 2012)
J/MNRAS/424/2086 : LX-T relation in galaxy clusters (Hilton+, 2012)
Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- --- [XMMXCS]
8- 25 A18 --- XMMXCS XMMXCS name (JHHMMSS.s+DDMMSS.s)
27- 30 F4.2 --- z ? Redshift, when available
32 A1 --- Flag [0-3] Flag (1)
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Note (1): The clusters forming the sample used throughout this work have a flag
with the following meaning:
0 = in the T<2.5 keVbin
1 = in the T>2.5 keV bin
2 = source was discounted for having no measured redshift
3 = source was discounted for having no measured X-ray temperature
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 29-Jan-2016