J/ApJ/774/23 Chandra observations of SPT-SZ clusters (McDonald+, 2013)
The growth of cool cores and evolution of cooling properties in a sample
of 83 galaxy clusters at 0.3 < z < 1.2 selected from the SPT-SZ survey.
McDonald M., Benson B.A., Vikhlinin A., Stalder B., Bleem L.E., de Haan T.,
Lin H.W., Aird K.A., Ashby M.L.N., Bautz M.W., Bayliss M., Bocquet S.,
Brodwin M., Carlstrom J.E., Chang C.L., Cho H.M., Clocchiatti A.,
Crawford T.M., Crites A.T., Desai S., Dobbs M.A., Dudley J.P., Foley R.J.,
Forman W.R., George E.M., Gettings D., Gladders M.D., Gonzalez A.H.,
Halverson N.W., High F.W., Holder G.P., Holzapfel W.L., Hoover S.,
Hrubes J.D., Jones C., Joy M., Keisler R., Knox L., Lee A.T., Leitch E.M.,
Liu J., Lueker M., Luong-Van D., Mantz A., Marrone D.P., McMahon J.J.,
Mehl J., Meyer S.S., Miller E.D., Mocanu L., Mohr J.J., Montroy T.E.,
Murray S.S., Nurgaliev D., Padin S., Plagge T., Pryke C., Reichardt C.L.,
Rest A., Ruel J., Ruhl J.E., Saliwanchik B.R., Saro A., Sayre J.T.,
Schaffer K.K., Shirokoff E., Song J., Suhada R., Spieler H.G.,
Stanford S.A., Staniszewski Z., Stark A.A., Story K., van Engelen A.,
Vanderlinde K., Vieira J.D., Williamson R., Zahn O., Zenteno A.
<Astrophys. J., 774, 23 (2013)>
=2013ApJ...774...23M 2013ApJ...774...23M
ADC_Keywords: Clusters, galaxy ; X-ray sources ; Accretion ; Surveys
Keywords: early universe; galaxies: clusters: general;
galaxies: clusters: intracluster medium; X-rays: galaxies: clusters
Abstract:
We present first results on the cooling properties derived from
Chandra X-ray observations of 83 high-redshift (0.3<z<1.2) massive
galaxy clusters selected by their Sunyaev-Zel'dovich signature in the
South Pole Telescope data. We measure each cluster's central cooling
time, central entropy, and mass deposition rate, and compare these
properties to those for local cluster samples. We find no significant
evolution from z∼0 to z∼1 in the distribution of these properties,
suggesting that cooling in cluster cores is stable over long periods
of time. We also find that the average cool core entropy profile in
the inner ∼100kpc has not changed dramatically since z∼1, implying
that feedback must be providing nearly constant energy injection to
maintain the observed "entropy floor" at ∼10keV cm2.
Description:
The clusters used in this work were selected based on their
Sunyaev-Zel'dovich effect (SZ) signature in the 2500deg2 SPT-SZ
survey (South Pole Telescope). The SPT-SZ survey was completed in
2011 November, producing maps in three frequency bands (95, 150, and
220GHz), with a key science goal of discovering clusters via the SZ
effect (Staniszewski et al. 2009ApJ...701...32S 2009ApJ...701...32S; Vanderlinde et al.
2010ApJ...722.1180V 2010ApJ...722.1180V; Williamson et al. 2011ApJ...738..139W 2011ApJ...738..139W; Benson et
al. 2013ApJ...763..147B 2013ApJ...763..147B; Reichardt et al. 2013, J/ApJ/763/127).
The clusters considered in this work have additionally been observed
with the Chandra X-Ray Observatory, with exposures typically
sufficient to obtain ∼2000 X-ray source counts. The majority of the
clusters have been observed through a Chandra X-Ray Visionary Project
to obtain X-ray imaging of the 80 clusters detected with the highest
SZ significance (ξ) in the first 2000deg2 of the 2500deg2
SPT-SZ survey at z>0.4 (B. A. Benson et al., in preparation). The
final sample used in this work, referred to as SPT-XVP, is summarized
in Table 1.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 61 83 Summary of Chandra X-ray observations
table2.dat 140 83 *Cooling properties of 83 clusters in the SPT-XVP
(South Pole Telescope Sunyaev-Zel'dovich) sample
--------------------------------------------------------------------------------
Note on table2.dat: This table provides cool core and cooling flow properties
for the full sample of 83 galaxy clusters at 0.3<z<1.2. A complete description
of how these values were measured is presented in Section 2. We use the
subscript "0" to represent the measured quantity in our smallest annulus:
r<0.012R500. All of these data are deprojected, using our mass-modeling
technique described in Section 3.
--------------------------------------------------------------------------------
See also:
B/chandra : The Chandra Archive Log (CXC, 1999-2014)
VIII/88 : Planck Early Release Compact Source Catalogue (Planck, 2011)
VIII/76 : Leiden/Argentine/Bonn (LAB) Survey of Galactic HI (Kalberla+ 2005)
J/ApJS/216/27 : New galaxy clusters in the SPT-SZ survey (Bleem+, 2015)
J/ApJ/772/25 : Massive SZE clusters observations with ACT (Sifon+, 2013)
J/ApJ/763/127 : GCls discovered in the SPT survey (Reichardt+, 2013)
J/ApJ/761/22 : NIR galaxy cluster cand. in the SPT survey (Song+, 2012)
J/ApJS/191/340 : Southern Cosmology Survey. II. (Menanteau+, 2010)
J/ApJ/704/1586 : BCGs with radio AGN (Sun, 2009)
J/ApJS/182/12 : ICM entropy profiles (ACCEPT) (Cavagnolo+, 2009)
J/ApJ/694/992 : SED of cluster radio galaxies (Lin+, 2009)
J/ApJ/660/239 : MaxBCG cat. of galaxy clusters from SDSS (Koester+, 2007)
J/MNRAS/376/1073 : Sunyaev-Zel'dovich effect in galaxy clusters (Zemcov+, 2007)
J/A+A/412/657 : CO in cooling flow of clusters of galaxies (Salome+, 2003)
J/MNRAS/306/857 : ROSAT Brightest Cluster Sample. III. (Crawford+, 1999)
J/MNRAS/292/419 : Cooling flows in 207 clusters of galaxies (White+, 1997)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- --- [SPT-CL]
7- 16 A10 --- SPT-CL Cluster identifier (JHHMM+DDMM)
18 A1 --- r_SPT-CL Flag on SPT-CL (1)
20- 26 F7.3 deg RAdeg Right ascension (J2000) (2)
28- 34 F7.3 deg DEdeg Declination (J2000) (2)
36- 61 A26 --- ObsID Chandra observation identifier(s)
--------------------------------------------------------------------------------
Note (1): Flag as follows:
a = Brodwin et al. (2010ApJ...721...90B 2010ApJ...721...90B).
b = Foley et al. (2011ApJ...731...86F 2011ApJ...731...86F).
c = McDonald et al. (2012Natur.488..349M 2012Natur.488..349M).
Note (2): Positions listed here are of the X-ray centroid (Section 2.2).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- --- [SPT-CL]
7- 16 A10 --- SPT-CL Cluster identifier (JHHMM+DDMM)
18- 22 F5.3 cm-3 ne0 [0.002/0.3] Central (r<0.012R500) electron
density
24- 28 F5.3 cm-3 e_ne0 [0/0.004] ne0 uncertainty
30- 33 F4.1 keV kT0 [0.9/19] Central (r<0.012R500) temperature
35- 38 F4.1 keV e_kT0 [0.2/22.5] kT0 uncertainty
40- 43 F4.2 --- CSB [0.01/0.4] Surface brightness concentration
(Santos et al. 2008A&A...483...35S 2008A&A...483...35S) (3)
45- 48 F4.2 --- E_CSB [0/0.03] Positive error on CSB
50- 53 F4.2 --- e_CSB [0.01/0.05] Negative error on CSB
55- 58 F4.2 --- alpha [0.02/1.3] Electron density slope
dlogρ/dlog(r) at 0.04R500
60- 63 F4.2 --- e_alpha [0/0.2] alpha uncertainty
65- 69 F5.1 keV.cm2 K0 [10/681] Central (r<0.012R500) entropy (4)
71- 76 F6.1 keV.cm2 E_K0 [1/1386] Positive error on K0
78- 83 F6.1 keV.cm2 e_K0 [1/1346] Negative error on K0
85- 89 F5.2 Gyr tcool0 [0.1/25.1] Central (r<0.012R500) cooling
time
91- 95 F5.2 Gyr E_tcool0 [0.01/51.6] Positive error on tcool0
97-101 F5.2 Gyr e_tcool0 [0.01/49.4] Negative error on tcool0
103-108 F6.1 Msun/yr dM/dt7.7 [0/1882]? Mass deposition rate within
r(tcool<7.7Gyr)
110-115 F6.1 Msun/yr E_dM/dt7.7 [0/1324]? Positive error on dM/dt7.7
117-121 F5.1 Msun/yr e_dM/dt7.7 [0/102]? Negative error on dM/dt7.7
123-128 F6.1 Msun/yr dM/dtU [0/1882]? Mass deposition rate within
r(tcool<tUniv)
130-134 F5.1 Msun/yr E_dM/dtU [-0/659]? Positive error on dM/dtU
136-140 F5.1 Msun/yr e_dM/dtU [0/101.3]? Negative error on dM/dtU
--------------------------------------------------------------------------------
Note (3): In Santos et al. 2008A&A...483...35S 2008A&A...483...35S, the optimal CSB is defined in
equation (5) as: CSB=SB(r<40kpc)/SB(r<400kpc) i.e. a peak radius of
40kpc and a cluster bulk radius of 400kpc.
Note (4): specific entropy K=kT/ne2/3
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 26-Feb-2015