J/MNRAS/471/4990 Nearby galaxy clusters X-ray point sources (Caglar+, 2017)
XMM-Newton view of X-ray overdensities from nearby galaxy clusters:
the environmental dependencies.
Caglar T., Hudaverdi M.
<Mon. Not. R. Astron. Soc., 471, 4990-5007 (2017)>
=2017MNRAS.471.4990C 2017MNRAS.471.4990C (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Galaxies, nearby ; X-ray sources
Keywords: galaxies: active - galaxies: clusters: general - X-rays: galaxies -
X-rays: galaxies: clusters - galaxies: clusters: individual -
galaxies: clusters: intracluster medium
Abstract:
In this work, we studied 10 nearby (z≤0.038) galaxy clusters to
understand possible interactions between hot plasma and member
galaxies. A multi-band source detection was applied to detect
point-like structures within the intra-cluster medium. We examined the
spectral properties of a total of 391 X-ray point sources within each
cluster's potential well. log N versus log S was studied in the energy
range 2-10 keV to measure X-ray overdensities. Optical overdensities
were also calculated to solve suppression/triggering phenomena for
nearby galaxy clusters. X-ray and optical flux/luminosity properties
(X/O, LX/LB and LX/LK) were investigated for optically
identified member galaxies. The X-ray luminosities of our point
sources were found to be faint [40.08≤log(LX)≤42.39erg/s]. The
luminosity range of point sources reveals possible contributions to
X-ray emission from low-luminosity active galactic nuclei, X-ray
binaries and star formation. We estimated ∼2 times higher X-ray
overdensities from galaxies within galaxy clusters compared to fields.
Our results demonstrate that optical overdensities are much higher
than X-ray overdensities at a cluster's centre, whereas X-ray
overdensities increase through the outskirts of clusters. We conclude
that high pressure from a cluster's centre affects the balance of
galaxies and they lose a significant amount of their fuel. As a
result, the clustering process quenches the X-ray emission of the
member galaxies. We also find evidence that the existence of X-ray
bright sources within a cluster environment can be explained by two
main phenomena: contributions from off-nuclear sources and/or active
galactic nucleus (AGN) triggering caused by galaxy interactions rather
than AGN fuelling.
Description:
We used archival data from XMM-Newton in our analysis, and all
observational data were gathered from the XMM-Newton Science
Archive. In our survey, we concentrated on selecting the XMM-Newton
observational data that were taken in full frame mode for MOS and
extended full frame mode for pn.
The X-ray and optical properties of identified member galaxies are
given in Table A1.
The galaxy colour survey is given in Table B1 and the properties of
point sources studied in this work are given in Table B2.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 99 40 X-ray to optical properties of individual galaxies
tableb1.dat 86 47 Galaxy colour survey
tableb2.dat 93 391 Properties of point sources studied in this work
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See also:
B/xmm : XMM-Newton Observation Log (XMM-Newton Science Operation Center, 2012-)
IX/55 : XMM-Newton Serendipitous Source Catalogue 3XMM-DR8 (XMM-SSC, 2018)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 28 A28 --- Name Galaxy name
30- 37 F8.6 --- z Redshift from NASA/IPAC Extragalactic Database
Astronomical Database
39- 43 F5.2 mag Rmag ? R-band magnitude from the Vizier database
45- 49 F5.2 --- FX/FO ? X-ray to optical flux ratio
51- 55 F5.2 mag Bmag Apparent blue magnitude from Vizier data base
57- 61 F5.2 mag Kmag ? Apparent K magnitude from
Tully (2015, Cat. J/AJ/149/171) and
Dalya et al. (2016, Cat. VII/275)
63- 67 F5.2 [10-7W] logLX Hard band logarithmic X-ray luminosity from
spectral analysis
69- 73 F5.2 [Lsun] logLK ? K-band luminosity calculated from extinction
corrected K-band magnitude
75- 79 F5.2 [Lsun] logLB Logarithmic blue optical luminosity calculated
from extinction corrected B-band magnitude
81- 83 A3 --- MType Morphological type of galaxy
85- 99 A15 --- Cluster Name of cluster host for identified galaxies
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Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 21 A21 --- Name Source name, XMMU JHHMMSS.s+DDMMSS
23- 27 F5.2 --- HR Hardness ratio (1)
29- 32 F4.2 --- e_HR Hardness ratio error (1)
34- 39 F6.2 [mW/m2] logFX Logarithmic X-ray flux
41- 45 F5.2 [10-7W] logLX Logarithmic X-ray luminosity
47- 51 F5.2 mag rmag r-band magnitude
53- 57 F5.2 mag g-r g-r/b-r colour index
59- 62 F4.2 Mpc Dist Projected distance from the centre of
the related galaxy cluster
64- 65 I2 % P Likelihood of optical association
67- 70 A4 --- Type Galaxy type in colour
72- 86 A15 --- Cluster Cluster name
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Note (1): defined as (H-S)/(H+S), where H is the count rate in 2.0-10.0keV and
S is the count rate in 0.5-2.0keV.
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Byte-by-byte Description of file: tableb2.dat
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Bytes Format Units Label Explanations
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1- 21 A21 --- Name Object name, XMMU JHHMMSS.s+DDMMSS
23- 26 I4 ct NCount Net count
28- 33 F6.2 [mW/m2] LogFX Logarithmic X-ray flux
35- 39 F5.2 [10-7W] logLX Logarithmic X-ray luminosity
41- 55 A15 --- Cluster Cluster name
57- 84 A28 --- OptCTP Optical counterpart
86- 93 F8.6 --- z ? Redshift
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 17-Jun-2020