J/MNRAS/448/2644 REXCESS sample optical and X-ray profiles (Holland+, 2015)
Optical and X-ray profiles in the REXCESS sample of galaxy clusters.
Holland J.G., Bohringer H., Chon G., Pierini D.
<Mon. Not. R. Astron. Soc., 448, 2644-2664 (2015)>
=2015MNRAS.448.2644H 2015MNRAS.448.2644H (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; X-ray sources
Keywords: galaxies: clusters: general -
galaxies: clusters: intracluster medium - dark matter -
X-rays: galaxies: clusters
Abstract:
Galaxy clusters' structure, dominated by dark matter, is traced by
member galaxies in the optical and hot intracluster medium (ICM) in
X-rays. We compare the radial distribution of these components and
determine the mass-to-light ratio versus system mass relation. We use
14 clusters from the REXCESS sample which is representative of
clusters detected in X-ray surveys. Photometric observations with the
Wide Field Imager on the 2.2m Max-Planck-Gesellschaft/European
Southern Observatory telescope are used to determine the number
density profiles of the galaxy distribution out to r200. These
are compared to electron density profiles of the ICM obtained using
XMM-Newton, and dark matter profiles inferred from scaling
relations and a Navarro-Frenk-White model. While red sequence galaxies
trace the total matter profile, the blue galaxy distribution is much
shallower. We see a deficit of faint galaxies in the central regions
of massive and regular clusters, and strong suppression of bright and
faint blue galaxies in the centres of cool-core clusters, attributable
to ram pressure stripping of gas from blue galaxies in high-density
regions of ICM and disruption of faint galaxies due to galaxy
interactions. We find a mass-to-light ratio versus mass relation
within r200 of (3.0±0.4)x102hM☉/L_☉ at 1015M☉
with slope 0.16±0.14, consistent with most previous results.
Description:
The REXCESS sample has been compiled as a galaxy cluster sample,
representative of clusters detected by their X-ray luminosity and
independent of their morphology. The sample selection is described in
Bohringer et al. (2007A&A...469..363B 2007A&A...469..363B).
The X-ray observations are described in Bohringer et al.
(2007A&A...469..363B 2007A&A...469..363B). Each cluster was observed using all three
detectors (MOS1, MOS2 and PN).
We used the Wide Field Imager (WFI) on the Max-Planck-Gesellschaft
(MPG)/European Southern Observatory (ESO) 2.2m Telescope at La Silla,
which is well suited to XMM-Newton follow-up as it has a similar
field of view (34-arcminx33-arcmin). Each set of optical data
cover the cluster and a region outside r200 which we use for the
background assessment.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 79 14 Overview of the REXCESS clusters analysed in
this paper
tableb1.dat 76 56 NFW fitting results
tablec1.dat 69 56 Background count density measurements
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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- 3 A3 --- --- [RXC]
5- 16 A12 --- RXC RXC designation
18- 22 A5 --- Abell Abell cluster name (1)
24- 25 I2 h RAh Right ascension (J2000) (1)
27- 28 I2 min RAm Right ascension (J2000)
30- 33 F4.1 s RAs Right ascension (J2000)
35 A1 --- DE- Declination sign (J2000) (1)
36- 37 I2 deg DEd Declination (J2000)
39- 40 I2 arcmin DEm Declination (J2000)
42- 45 F4.1 arcsec DEs Declination (J2000)
47- 52 F6.4 --- z Redshift (1)
54- 58 F5.3 10+37W LX X-ray luminosity (1)
60- 65 F6.1 kpc r500 Radius at which the mean mass density is
500 times the critical density at the
cluster redshift (2)
67- 70 F4.2 10+14Msun M500 Mass within r500 (3)
72 A1 --- D [D] D for disturbed (2)
74- 75 A2 --- CC [CC ] CC for cool-core (2)
77 A1 --- M [M] M for massive
79 A1 --- ID ID used in figures in Section 3.9.4 to
distinguish between the clusters in the sample
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Note (1): from table 3 in Bohringer et al. (2007A&A...469..363B 2007A&A...469..363B).
Note (2): r500, CC and D are from table 1 in Pratt et al. (2009A&A...498..361P 2009A&A...498..361P).
Note (3): M500 was derived from r500 and z using the fiducial cosmology.
Massive objects are those with M500 above the median of the entire REXCESS
population, 2.95x1014M☉.
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Byte-by-byte Description of file: tableb1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 A3 --- --- [RXC]
5- 16 A12 --- RXC RXC designation (JHHMM.m+DDMM)
18- 29 A12 --- Filt Filter
31- 35 F5.2 --- beta Outer slope
37- 42 F6.2 --- e_beta rms uncertainty on beta
44- 50 F7.3 --- S0 Surface density (in R500-3)
52- 62 F11.3 --- e_S0 rms uncertainty on S0
65- 70 F6.2 --- SbgNFW Constant density component from an NFW fit
(in R500-2)
72- 76 F5.2 --- e_SbgNFW rms uncertainty on SbgNFW
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Byte-by-byte Description of file: tablec1.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- --- [RXC]
5- 16 A12 --- RXC RXC designation (JHHMM.m+DDMM)
18- 29 A12 --- Filt Filter
33- 37 F5.3 arcmin-2 Sbgs Simple count density (Sbg-simple)
39- 43 F5.3 arcmin-2 e_Sbgs rms uncertainty on Sbgs
45- 48 F4.2 arcmin-2 alpha Standard error measured from
sectors (αSbg-sector)
50- 55 F6.4 arcmin-2 SbgNFW Constant density component from an NFW fit
57- 62 F6.4 arcmin-2 e_SbgNFW rms uncertainty on SbgNFW
64- 68 F5.2 --- Sbgs/SbgNFW Simple count density to constant density
component ratio
69 A1 --- Note [*] Note on RXC J2023.0-2056 bright blue
filter (1)
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Note (1): In the case of the RXC J2023.0-2056 bright blue filter, no objects are
detected in the region used for measuring Sbgs.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 10-Sep-2015