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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
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) 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) 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 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 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 A1 --- Sub [PS ] Secondary subcluster flag (G1) 18- 30 A13 --- PLCKESZ Planck name (Glll.ll+bb.bb) 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 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
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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