J/ApJ/843/76 Cool-core clusters with Chandra obs. (Andrade-Santos+, 2017)
The fraction of cool-core clusters in X-ray versus SZ samples using Chandra
observations.
Andrade-Santos F., Jones C., Forman W.R., Lovisari L., Vikhlinin A.,
van Weeren R.J., Murray S.S., Arnaud M., Pratt G.W., Democles J., Kraft R.,
Mazzotta P., Bohringer H., Chon G., Giacintucci S., Clarke T.E., Borgani S.,
David L., Douspis M., Pointecouteau E., Dahle H., Brown S., Aghanim N.,
Rasia E.
<Astrophys. J., 843, 76 (2017)>
=2017ApJ...843...76A 2017ApJ...843...76A
ADC_Keywords: Clusters, galaxy ; X-ray sources ; Redshifts
Keywords: galaxies: clusters: general ; large-structure of universe
Abstract:
We derive and compare the fractions of cool-core clusters in the
Planck Early Sunyaev-Zel'dovich sample of 164 clusters with z≤0.35
and in a flux- limited X-ray sample of 100 clusters with z≤0.30,
using Chandra observations. We use four metrics to identify cool-core
clusters: (1) the concentration parameter, which is the ratio of the
integrated emissivity profile within 0.15 r500 to that within
r500; (2) the ratio of the integrated emissivity profile within
40kpc to that within 400kpc; (3) the cuspiness of the gas density
profile, which is the negative of the logarithmic derivative of the
gas density with respect to the radius, measured at 0.04 r500; and
(4) the central gas density, measured at 0.01 r500. We find that the
sample of X-ray-selected clusters, as characterized by each of these
metrics, contains a significantly larger fraction of cool-core
clusters compared to the sample of SZ-selected clusters (44%±7%
versus 28%±4% using the concentration parameter in the 0.15-1.0
r500 range, 61%±8% versus 36%±5% using the concentration
parameter in the 40-400 kpc range, 64%±8% versus 38%±5% using the
cuspiness, and 53%±7% versus 39±5% using the central gas density).
Qualitatively, cool-core clusters are more X-ray luminous at fixed
mass. Hence, our X-ray, flux-limited sample, compared to the
approximately mass-limited SZ sample, is overrepresented with
cool-core clusters. We describe a simple quantitative model that uses
the excess luminosity of cool-core clusters compared to non-cool-core
clusters at fixed mass to successfully predict the observed fraction
of cool-core clusters in X-ray-selected samples.
Description:
The main goal of this work is to compare the fraction of cool-core
(CC) clusters in X-ray-selected and SZ-selected samples.
The first catalog of 189 SZ clusters detected by the Planck mission
was released in early 2011 (Planck Collaboration 2011, VIII/88/esz). A
Chandra XVP (X-ray Visionary Program--PI: Jones) and HRC Guaranteed
Time Observations (PI: Murray) combined to form the Chandra-Planck
Legacy Program for Massive Clusters of Galaxies. For each of the 164
ESZ Planck clusters at z≤0.35, we obtained Chandra exposures
sufficient to collect at least 10000 source counts.
The X-ray sample used here is an extension of the Voevodkin &
Vikhlinin (2004ApJ...601..610V 2004ApJ...601..610V) sample. This sample contains 100
clusters and has an effective redshift depth of z<0.3. All have
Chandra observations. Of the 100 X-ray-selected clusters, 49 are also
in the ESZ sample, and 47 are in the HIFLUGCS (Reiprich & Boehringer
2002ApJ...567..716R 2002ApJ...567..716R) catalog.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table4.dat 107 199 *Planck Early Sunyaev-Zel'dovich (ESZ) sample
table5.dat 123 112 *X-ray sample
--------------------------------------------------------------------------------
Note on table4.dat and table5.dat: See the "Description" section above for
an explanation on the samples.
--------------------------------------------------------------------------------
See also:
B/chandra : The Chandra Archive Log (CXC, 1999-2014)
VIII/88 : Planck Early Release Compact Source Catalogue (Planck, 2011)
J/AJ/98/64 : VLA survey of Abell clusters of galaxies I. (Zhao+ 1989)
J/ApJ/511/65 : Einstein images of galaxy clusters (Jones & Forman, 1999)
J/ApJS/182/12 : ICM entropy profiles (ACCEPT) (Cavagnolo+, 2009)
J/A+A/536/A8 : Planck early results. VIII. ESZ sample. (Planck+, 2011)
J/ApJ/771/137 : WMAP observations of Planck ESZ clusters (Ma+, 2013)
J/ApJ/774/23 : Chandra observations of SPT-SZ clusters (McDonald+, 2013)
J/MNRAS/436/275 : Relaxation param. of 2092 rich galaxy clusters (Wen+, 2013)
J/A+A/580/A95 : Planck/AMI Sunyaev-Zel'dovich measurements (Perrott+, 2015)
J/A+A/592/A48 : Annotations to the 2nd Planck cluster catalog (Khatri, 2016)
J/MNRAS/457/4515 : X-ray_peak-BCG offset for PSZ1 clusters (Rossetti+, 2016)
J/PAZh/43/559 : Planck galaxy cluster catalogue extension (Burenin, 2017)
http://hea-www.cfa.harvard.edu/CHANDRA_PLANCK_CLUSTERS/ : Chandra-Planck
Legacy Program for Massive Clusters of Galaxies home page
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 13 A13 --- PLCKESZ Cluster Name (Glll.ll+bb.bb)
15- 15 A1 --- Sub [PS ] Secondary subcluster flag (G1)
17- 18 I2 h RAh Hour of Right Ascension (J2000)
20- 21 I2 min RAm Minute of Right Ascension (J2000)
23- 28 F6.3 s RAs Second of Right Ascension (J2000)
30- 30 A1 --- DE- Sign of the Declination (J2000)
31- 32 I2 deg DEd Degree of Declination (J2000)
34- 35 I2 arcmin DEm Arcminute of Declination (J2000)
37- 41 F5.2 arcsec DEs Arcsecond of Declination (J2000)
43- 48 F6.4 --- z [0.01/0.5] Redshift
50- 54 F5.3 --- CSB [0.07/0.8] Concentration parameter in
the 0.15-1.0 r500
56- 60 F5.3 --- e_CSB [0.001/0.2] Uncertainty in CSB
62- 67 F6.4 --- CSB4 [0.01/0.5] Concentration parameter in
the 40-400kpc range
69- 74 F6.4 --- e_CSB4 [0.0001/0.3] Uncertainty in CSB4
76- 80 F5.3 --- delta [0.03/1.5] Cuspiness of the gas density profile
82- 86 F5.3 --- e_delta [0.01/0.9] Uncertainty in delta
88- 94 F7.5 cm-3 n-core [0.001/0.2] Central gas density
96-102 F7.5 cm-3 e_n-core [/0.06] Uncertainty in n-core
104-107 F4.2 --- rmax [0.4/3.1] Maximum radius where the emission
integral is computed, in units of r500
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 A14 --- Cluster Cluster Name
16- 16 A1 --- Sub [PS ] Secondary subcluster flag (G1)
18- 30 A13 --- PLCKESZ Planck name (Glll.ll+bb.bb)
32- 32 I1 --- f_PLCKESZ [1]? Planck cosmology SZ sample, PSZ1
34- 35 I2 h RAh Hour of Right Ascension (J2000)
37- 38 I2 min RAm Minute of Right Ascension (J2000)
40- 45 F6.3 s RAs Second of Right Ascension (J2000)
47- 47 A1 --- DE- Sign of the Declination (J2000)
48- 49 I2 deg DEd Degree of Declination (J2000)
51- 52 I2 arcmin DEm Arcminute of Declination (J2000)
54- 58 F5.2 arcsec DEs Arcsecond of Declination (J2000)
60- 64 F5.3 --- z [0.01/0.3] Redshift
66- 70 F5.3 --- CSB [0.1/0.8] Concentration parameter in
the 0.15-1.0 r500
72- 76 F5.3 --- e_CSB [0.002/0.2] Uncertainty in CSB
78- 83 F6.4 --- CSB4 [0.01/0.8] Concentration parameter in
the 40-400kpc range
85- 90 F6.4 --- e_CSB4 [0/0.3] Uncertainty in CSB4
92- 96 F5.3 --- delta [0.03/2.3] Cuspiness of the gas density profile
98-102 F5.3 --- e_delta [0.002/0.9] Uncertainty in delta
104-110 F7.5 cm-3 n-core [0.001/0.2] Central gas density
112-118 F7.5 cm-3 e_n-core [0.0001/0.06] Uncertainty in n-core
120-123 F4.2 --- rmax [0.4/3.5] Maximum radius where the emission
integral is computed, in units of r500
--------------------------------------------------------------------------------
Global notes:
Note (G1): The secondary subcluster flag segregates principal cluster
components (P) used in the comparisons in this paper and secondary
subclusters (S).
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 28-Feb-2018