J/ApJ/892/102 XMM X-ray data of Planck ESZ galaxy clusters (Lovisari+, 2020)
X-ray scaling relations for a representative sample of Planck-selected clusters
observed with XMM-Newton.
Lovisari L., Schellenberger G., Sereno M., Ettori S., Pratt G.W.,
Forman W.R., Jones C., Andrade-Santos F., Randall S., Kraft R.
<Astrophys. J., 892, 102 (2020)>
=2020ApJ...892..102L 2020ApJ...892..102L
ADC_Keywords: Clusters, galaxy; X-ray sources; Redshifts
Keywords: Galaxy clusters ; Intracluster medium ; Observational cosmology ;
X-ray astronomy
Abstract:
We report the scaling relations derived by fitting the X-ray
parameters determined from analyzing the XMM-Newton observations of
120 galaxy clusters in the Planck Early Sunyaev-Zel'dovich (SZ) sample
spanning the redshift range of 0.059<z<0.546. We find that the slopes
of all the investigated scaling relations significantly deviate from
the self-similar predictions, if self-similar redshift evolution is
assumed. When the redshift evolution is left free to vary, the derived
slopes are more in agreement with the self-similar predictions.
Relaxed clusters have on average ∼30% higher X-ray luminosity than
disturbed clusters at a given mass, a difference that, depending on
the relative fraction of relaxed and disturbed clusters in the samples
(e.g., SZ vs. X-ray selected), has a strong impact on the
normalization obtained in different studies. Using the core-excised
cluster luminosities reduces the scatter and brings into better
agreement the L-Mtot and L-T relations determined for different
samples. Mtot-T, Mtot-YX, and Mtot-Mgas relations show little
dependence on the dynamical state of the clusters, but the
normalizations of these relations may depend on the mass range
investigated. Although most of the clusters investigated in this work
reside at relatively low redshift, the fits prefer values of γ,
the parameter accounting for the redshift evolution, different from
the self-similar predictions. This suggests an evolution (<2σ
level, with the exception of the Mtot-T relation) of the scaling
relations. For the first time, we find significant evolution
(>3σ) of the Mtot-T relation, pointing to an increase of the
kinetic-to-thermal energy ratio with redshift. This is consistent with
a scenario in which higher-redshift clusters are on average more
disturbed than their lower-redshift counterparts.
Description:
Our sample contains 120 galaxy clusters observed with XMM-Newton and
originally selected from the Planck Early Sunyaev-Zel'dovich (ESZ;
Planck Col.+ 2011, J/A+A/536/A8).
As described in Lovisari+ (2017ApJ...846...51L 2017ApJ...846...51L), these are the ESZ
clusters for which R500 was completely covered by XMM-Newton observations.
Observation data files were downloaded from the XMM-Newton archive.
Throughout this paper, we assume a flat ΛCDM cosmology with
Ωm=0.3 and H0=70km/s/Mpc.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 166 120 Cluster properties
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See also:
B/xmm : XMM-Newton Obs. Log (XMM-Newton Science Operation Center, 2012)
VIII/88 : Planck Early Release Compact Source Catalogue (Planck, 2011)
VIII/91 : Planck Catalog of Compact Sources Release 1 (Planck, 2013)
J/A+A/536/A8 : Planck early results. VIII. ESZ sample. (Planck+, 2011)
J/A+A/535/A4 : X-ray galaxy clusters study (Reichert+, 2011)
J/A+A/575/A30 : HIFLUGCS XMM/Chandra cross-calibration (Schellenberger+, 2015)
J/MNRAS/450/3675 : CoMaLit. IV. Sigma Catalogue (Sereno+, 2015)
J/MNRAS/457/4515 : X-ray_peak-BCG offset for PSZ1 clusters (Rossetti+, 2016)
J/ApJ/843/76 : Cool-core clusters with Chandra obs. (Andrade-Santos+, 2017)
J/MNRAS/468/1917 : Concentration parameter of galaxy clusters (Rossetti+, 2017)
J/MNRAS/469/3738 : Complete sample of galaxy clusters (Schellenberger+, 2017)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- PLCKESZ Planck identifier GLLL.ll+BB.bb (1)
15 A1 --- f_PLCKESZ [*] * = not explained in the paper
17- 21 F5.3 --- z [0.059/0.6] Cluster spectroscopic redshift
23- 27 F5.2 10+14Msun M500 [2.4/17.6] Total mass with R500
29- 32 F4.2 10+14Msun E_M500 [0.04/6] Upper uncertainty in M500
34- 37 F4.2 10+14Msun e_M500 [0.03/5] Lower uncertainty in M500
39- 43 F5.2 10+13Msun Mg500 [2.87/32] Gas mass with R500
45- 48 F4.2 10+13Msun E_Mg500 [0.03/3] Upper uncertainty in Mg500
50- 53 F4.2 10+13Msun e_Mg500 [0.03/6] Upper uncertainty in Mg500
55- 59 F5.2 keV kT [1.67/14.4] Core-included cluster
temperature
61- 64 F4.2 keV E_kT [0.03/1.4] Upper uncertainty in kT
66- 69 F4.2 keV e_kT [0.03/1.4] Lower uncertainty in kT
71- 75 F5.2 keV kTexc [1.4/15.1] Core-excluded cluster
temperature
77- 80 F4.2 keV E_kTexc [0.04/1.6] Upper uncertainty in kTexc
82- 85 F4.2 keV e_kTexc [0.04/1.6] Lower uncertainty in kTexc
87- 91 F5.2 10-7W LX [1.28/27.1] Core-included cluster
0.1-2.4keV luminosity; erg/s
93- 96 F4.2 10-7W E_LX [0.04/1.7] Upper uncertainty in LX
98- 101 F4.2 10-7W e_LX [0.04/1.7] Lower uncertainty in LX
103- 107 F5.2 10-7W LXexc [0.86/18] Core-excluded cluster
0.1-2.4keV luminosity; erg/s
109- 112 F4.2 10-7W E_LXexc [0.01/1.3] Upper uncertainty in LXexc
114- 117 F4.2 10-7W e_LXexc [0.01/1.3] Lower uncertainty in LXexc
119- 123 F5.2 10-7W Lbol [2.6/87] Core-included cluster bolometric
(0.01-100keV) luminosity; erg/s
125- 128 F4.2 10-7W E_Lbol [0.1/8] Upper uncertainty in Lbol
130- 133 F4.2 10-7W e_Lbol [0.1/8] Lower uncertainty in Lbol
135- 139 F5.2 10-7W Lbolexc [1.87/61] Core-excluded cluster
bolometric (0.01-100keV) luminosity;
in erg/s units
141- 144 F4.2 10-7W E_Lbolexc [0.01/4] Upper uncertainty in Lbolexc
146- 149 F4.2 10-7W e_Lbolexc [0.01/4] Lower uncertainty in Lbolexc
151- 152 I2 --- NT [1/33] Number of temperature profile bins
154- 157 F4.2 --- fT [0.3/1.3] Fraction of R500 covered by
temperature profile
159- 161 I3 --- Nsb [4/372] Number of surface brightness
profile bins
163- 166 F4.2 --- fsb [0.5/1.7] Fraction of R500 covered by
surface brightness profile
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Note (1): As in the Planck Early Sunyaev-Zeldovich catalog
(Planck Collaboration et al. 2011A&A...536A...8P 2011A&A...536A...8P ; see VIII/88).
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 16-Aug-2021