J/MNRAS/483/540 Diverse galaxy cluster metallicity profiles (Lovisari+, 2019)
The non-uniformity of galaxy cluster metallicity profiles.
Lovisari L., Reiprich T.H.
<Mon. Not. R. Astron. Soc., 483, 540-557 (2019)>
=2019MNRAS.483..540L 2019MNRAS.483..540L (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; X-ray sources
Keywords: galaxies: clusters: intracluster medium - galaxies: groups: general -
X-rays: galaxies: clusters
Abstract:
We study a sample of 207 nearby galaxy groups and clusters observed
with XMM-Newton. Key aspects of this sample include the large size,
the high data quality, and the large diversity of cluster dynamical
states. We determine the overall metallicity within 0.3R500 and the
radial distribution of the metals. On average, we find a mild
dependence of the core metallicity with the average temperature of the
system in agreement with previous results. However, we identify the
cause of this mild dependence to be due to relaxed systems only;
disturbed systems do not show this trend, on average. The large
scatter observed in this relation is strongly associated with the
dynamical state of the systems: relaxed systems have, on average, a
higher metallicity in the core than disturbed objects. The radial
profiles of relaxed systems are centrally peaked and show a steep
decrease with radius, flattening beyond 0.3-0.4R500. The metallicity
of disturbed systems is also higher in the centre but at much lower
values than what is observed for relaxed objects. This finding is
consistent with the picture that cluster mergers mix the abundance
distribution by inducing large-scale motions. The scatter of the
radial profiles is quite large, but while for relaxed systems it
decreases almost monotonically as function of the radius, for
disturbed systems it shows a significant boost at large radii. Systems
with a central radio source have a flatter profile indicating that
central AGNs are an efficient mechanism to uplift and redistribute the
metals in the ICM.
Description:
The aim of this work is the study of the metal enrichment of the ICM
in groups and clusters of galaxies, and the determination of the
impact of merging and interactions in the distribution of the
metallicity in the ICM. We choose to look at a sample of local galaxy
groups and clusters with available XMM-Newton data. As input
catalogue, we have used the MCXC catalogue (see Piffaretti et al.
2011A&A...534A.109P 2011A&A...534A.109P, Cat. J/A+A/534/A109) and restricted the search to
all the objects in the NORAS, REFLEX, and eBCS sub-catalogues (Ebeling
et al. 1998MNRAS.301..881E 1998MNRAS.301..881E, Cat. J/MNRAS/301/881, 2000MNRAS.318..333E 2000MNRAS.318..333E,
Cat. J/MNRAS/318/333 ; Bohringer et al. 2000ApJS..129..435B 2000ApJS..129..435B, Cat.
J/ApJS/129/435, 2004A&A...425..367B 2004A&A...425..367B, Cat. J/A+A/425/367). By arbitrary
use of an upper redshift cut of 0.1, we found 207 objects with useful
(i.e. not flared) XMM-Newton observations (listed in Table E1).
Clusters with multiple X-ray peaks, and clusters with an estimated
0.3R500 extending beyond the XMM-Newton field-of-view (FOV) were
removed from the sample.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablee1.dat 110 260 Properties of the clusters
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablee1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- Name Cluster name
14- 15 I2 h RAh Right ascension (J2000)
17- 18 I2 min RAm Right ascension (J2000)
20- 23 F4.1 s RAs Right ascension (J2000)
25 A1 --- DE- Declination sign (J2000)
26- 27 I2 deg DEd Declination (J2000)
29- 30 I2 arcmin DEm Declination (J2000)
32- 33 I2 arcsec DEs Declination (J2000)
35- 39 F5.3 --- z Redshift
41- 50 I10 --- ID XMM-Newton observation ID
52- 67 A16 ks texp Clean exposure times for MOS1,MOS2 and pn
69- 74 F6.4 10+14Msun M500 Mass used to estimate R500 taken from
Piffaretti et al. (2011A&A...534A.109P 2011A&A...534A.109P)
76- 80 F5.3 Sun Acore Core abundance (in Sun units)
82- 86 F5.3 Sun e_Acore Error on Acore
88- 92 F5.3 --- w Centroid-shift parameter
94- 98 F5.3 --- e_w Error on w
100-104 F5.3 --- c Surface brightness concentration parameter
106-110 F5.3 --- e_c Error on c
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 06-Jul-2022