J/MNRAS/513/3013 Galaxy clusters with Chandra/XMM-Newton images (Yuan+, 2022)
Dynamical state of galaxy clusters evaluated from X-ray images.
Yuan Z.S., Han J.L., Wen Z.L.
<Mon. Not. R. Astron. Soc. 513, 3013-3021 (2022)>
=2022MNRAS.513.3013Y 2022MNRAS.513.3013Y (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; X-ray sources ; Positional data ; Redshifts ;
Morphology
Keywords: galaxies: clusters: general -
galaxies: clusters: intracluster medium - galaxies: groups: general -
X-rays: galaxies: clusters
Abstract:
X-ray images of galaxy clusters often show disturbed structures that
are indications of cluster mergers. To complement our previous work on
the dynamical state of 964 clusters observed by Chandra, we process
the X-ray images for 1308 clusters from XMM-Newton archival data,
together with the images of 22 clusters newly released by Chandra, and
we evaluate their dynamical state from these X-ray images. The
concentration index c, the centroid shift ω and the power ratio
P3/P0 are calculated in circular regions with a certain radius of 500
kpc, and the morphology index δ is estimated within elliptical
regions that can be adapted to the cluster size and shape. In
addition, the dynamical parameters for 42 clusters previously
estimated from Chandra images are upgraded based on the newly
available redshifts. Good consistence is found between dynamical
parameters derived from XMM-Newton and Chandra images for the
overlapped sample of clusters in the two data sets. The dependence of
mass scaling relations on the dynamical state is shown by using the
data of 388 clusters. All data and related software are available at
http://zmtt.bao.ac.cn/galaxy_clusters/dyXimages/.
Description:
In this work we use the XMM-Newton X-ray telescope which has observed
more than 1000 clusters of galaxies with a larger field of view than
Chandra. As a continuation of Yuan & Han (2020MNRAS.497.5485Y 2020MNRAS.497.5485Y, Cat.
J/MNRAS/497/5485), we calculate the dynamical parameters for 1308
clusters in the archived XMM-Newton data and also for clusters newly
released by Chandra, (i.e see section Introduction).
Firstly as combination of X-ray data archives in XMM-Newton with found
892 clusters with good data quality with which we combine several
large cluster catalogues. We obtained a sample of 416 clusters
serendipitously detected in any XMM-Newton observations to reach 1308
observed clusters. The table1.dat contains their dynamical parameters
computed in the section 3 Parameters for dynamical states, for data
images extraction please see the section 2.2 X-ray image processing.
In a second time as explicited in the appendix A, we proceeded in a
same way as for table1.dat results to make an unified list for 1844
clusters being observed by Chandra and XMM-Newton telescopes, results
are presented in the tablea1.dat.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 120 1308 *Dynamical parameters for 1308 clusters observed
by XMM-Newton
tablea1.dat 121 1844 *Dynamical parameters for 1844 clusters of
galaxies derived from the Chandra and
XMM-Newton images
--------------------------------------------------------------------------------
Note on table1.dat and tablea1.dat: Where the dynamical parameter for the
cluster can not be calculated since the redshift is not avaliable or if the
circular region with radius of 500 kpc for parameter calculation significantly
exceed the CCD camera coverage.
--------------------------------------------------------------------------------
See also:
J/MNRAS/497/5485 : Dynamical state for 964 galaxy clusters (Yuan+, 2020)
VII/110A : Rich Clusters of Galaxies (Abell+ 1989)
J/A+A/534/A109 : MCXC Meta-Catalogue X-ray galaxy Clusters (Piffaretti+,2011)
J/ApJ/785/104 : redMaPPer. I. Algorithm applied to SDSS DR8 (Rykoff+, 2014)
J/ApJS/199/34 : Clusters of galaxies in SDSS-III (Wen+, 2012)
J/MNRAS/475/343 : 2MASS, WISE, and SuperCOSMOS clusters of galaxies
(Wen+, 2018)
J/A+A/652/A12 : The new X-Class catalogue (Koulouridis+, 2021)
J/ApJS/253/56 : Galaxy clusters from the DESI surveys. I. (Zou+, 2021)
http://zmtt.bao.ac.cn/galaxy_clusters/dyXimages/ : catalgues and images home
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 A19 --- Cluster Cluster's name from the XMM-Newton data
archives (Name)
21- 29 F9.5 deg RAdeg Right ascension (J2000) (RA)
31- 39 F9.5 deg DEdeg Declination (J2000) (DEC)
41- 46 F6.4 --- z ?=9.9999 Redshift (z) (1)
48- 57 I010 --- ObsID Observation identifier number from
XMM-Newton data archives (OBS_id)
59- 63 F5.2 [-] log(c) ? Concentration index (logc) (2)
65- 68 F4.2 [-] e_log(c) ? Mean error of log (c) (elogc)
70- 74 F5.2 [-] log(w) ? The centroid shift (logw) (3)
76- 79 F4.2 [-] e_log(w) ? Mean error of log (w) (elogw)
81- 86 F6.2 [-] log(P3/P0) ? Logarithm of the power ratio P3/P0
(logP3/P0) (4)
88- 91 F4.2 [-] e_log(P3/P0) ? Mean error of log (P3/P0) (elogP3/P0)
93- 96 F4.2 --- kappa Profile parameter (kappa) (5)
98- 102 F5.2 [-] log(alpha) Logarithm of the asymmetry factor α
(logalpha) (6)
104- 107 F4.2 [-] e_log(alpha) Mean error of log (alpha) (elogalpha)
109- 113 F5.2 --- delta The morphology index δ (delta) (6)
115- 118 F4.2 --- e_delta Mean error of δ (edelta)
120 A1 --- Note [- c] Notes on observations (Note) (7)
--------------------------------------------------------------------------------
Note (1): Redshift with value of "9.9999" means the redshift information is not
yet avaliable for the cluster.
Note (2): The concentration index c is defined by Santos et al.
(2008A&A...483...35S 2008A&A...483...35S) as the equation 1 shows in the section 3
Parameter for dynamical states.
Note (3): Based on the simulations by Poole et al. (2006MNRAS.373..881P 2006MNRAS.373..881P),
Cassano et al. (2010ApJ...721L..82C 2010ApJ...721L..82C) clearly wrote the formula for
the centroid shift ω as in the equation 2 of the section 3
Parameter for dynamical states.
Note (4): Buote & Tsai (1995ApJ...452..522B 1995ApJ...452..522B) characterized substructures of
clusters in various scales and defined the ratio between P3 and
P0 as a good dynamical proxy. P0 and P3 are defined in the
equation 3 of the section 3 Parameter for dynamical states.
Note (5): Further in the section 3, we define the profile parameter κ
as in the equation 8.
Note (6): Also, the asymmetry factor α can be calculated as the equation 9
shows. Then, the morphology index δ is defined as combination of
the profile parameter κ and the asymmetry factor α as
exposed in the eqaution 10 of the section 3 Parameter for dynamical
states.
Note (7): Observations are done as follows:
- = Observed only by XMM-Newton, 902 clusters in our sample
c = Observed by XMM-Newton, and by Chandra, 406 clusters in our sample
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 20 A20 --- Cluster Cluster's name from the XMM-Newton data
archives (Name)
22- 30 F9.5 deg RAdeg Right ascension (J2000) (RA)
32- 40 F9.5 deg DEdeg Declination (J2000) (DEC)
42- 47 F6.4 --- z ?=9.9999 Redshift (z) (1)
49- 58 I010 --- ObsID Observation identifier number from
XMM-Newton data archives (OBS_id)
60- 64 F5.2 [-] log(c) ?=0 Concentration index (logc) (2)
66- 69 F4.2 [-] e_log(c) ?=0 Mean error of log (c) (elogc)
71- 75 F5.2 [-] log(w) ?=0 The centroid shift (logw) (3)
77- 80 F4.2 [-] e_log(w) ?=0 Mean error of log (w) (elogw)
82- 87 F6.2 [-] log(P3/P0) ?=0 Logarithm of the power ratio
P3/P0 (logP3/P0) (4)
89- 92 F4.2 [-] e_log(P3/P0) ?=0 Mean error of log (P3/P0)
(elogP3/P0)
94- 97 F4.2 --- kappa Profile parameter (kappa) (5)
99- 103 F5.2 [-] log(alpha) Logarithm of the asymmetry factor α
(logalpha) (6)
105- 108 F4.2 [-] e_log(alpha) Mean error of log (alpha) (elogalpha)
110- 114 F5.2 --- delta The morphology index δ (delta) (6)
116- 119 F4.2 --- e_delta Mean error of δ (edelta)
121 I1 --- Note [1/6] Notes on observations (Note) (7)
--------------------------------------------------------------------------------
Note (1): Redshift with value of "9.9999" means the redshift information is not
yet avaliable for the cluster.
Note (2): The concentration index c is defined by Santos et al.
(2008A&A...483...35S 2008A&A...483...35S) as the equation 1 shows in the section 3
Parameter for dynamical states.
Note (3): Based on the simulations by Poole et al. (2006MNRAS.373..881P 2006MNRAS.373..881P),
Cassano et al. (2010ApJ...721L..82C 2010ApJ...721L..82C) clearly wrote the formula for
the centroid shift ω as in the equation 2 of the section 3
Parameter for dynamical states.
Note (4): Buote & Tsai (1995ApJ...452..522B 1995ApJ...452..522B) characterized substructures of
clusters in various scales and defined the ratio between P3 and
P0 as a good dynamical proxy. P0 and P3 are defined in the
equation 3 of the section 3 Parameter for dynamical states.
Note (5): Further in the section 3, we define the profile parameter κ
as in the equation 8.
Note (6): Also, the asymmetry factor α can be calculated as the equation 9
shows. Then, the morphology index δ is defined as combination of
the profile parameter κ and the asymmetry factor α as
exposed in the eqaution 10 of the section 3 Parameter for dynamical
states.
Note (7): Observations are done as follows:
1 = Observed only by Chandra, 476 clusters in our sample
2 = Observed only by XMM-Newton, 900 clusters in our sample
3 = With both XMM-Newton and Chandra images and parameter devired from
Chandra images, 82 clusters in our sample
4 = With both Chandra and XMM-Newton images but parameters from
XMM-Newton, 326 clusters in our sample
5 = Newly released archive of Chandra, 22 clusters in our sample
6 = From Chandra with newly available redshift, 38 clusters in
our sample
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Luc Trabelsi [CDS] 06-Jan-2025