J/A+A/527/A134 Fe abundances for 28 XMM galaxy clusters (Matsushita, 2011)
Radial profiles of Fe abundance in the intracluster medium of nearby clusters
observed with XMM-Newton.
Matsushita K.
<Astron. Astrophys., 527, A134 (2011)>
=2011A&A...527A.134M 2011A&A...527A.134M
ADC_Keywords: Clusters, galaxy ; X-ray sources ; Abundances, [Fe/H]
Keywords: galaxies: clusters: general - X-rays: galaxies: clusters -
intergalactic medium
Abstract:
The abundances of Fe in the intracluster medium of nearby (z<0.08)
clusters were measured up to 0.3∼0.5r180.
We analyzed 28 clusters of galaxies observed with XMM-Newton. We
derived Fe abundances from the flux ratios of Fe lines to the
continuum within an energy range of 3.5-6keV to minimize and
evaluate systematic uncertainties.
Description:
In the XMM-Newton archival data, we selected the 28 brightest clusters
of galaxies with z<0.08 and total exposures above 7ks after
filtering out background flares.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
clusters.dat 35 28 Clusters studied (from table 1 of paper)
table1.dat 63 118 Cluster samples in the XMM-Newton archival data
table2.dat 59 130 Results of spectral fitting of annular spectra
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See also:
B/xmm : XMM-Newton Observation Log (XMM-Newton Science Operation Center, 2009)
Byte-by-byte Description of file: clusters.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- Cluster Cluster name
7- 13 A7 --- OName Other name of cluster
15- 19 F5.3 --- z Redshift
21- 23 F3.1 keV <kT> Adopted average temperature of ICM used to
calculate the virial radius r180
25- 28 F4.1 10+20cm-2 NH Galactic value of the hydrogen column density
(Dickey & Lockman, 1990ARA&A..28..215D 1990ARA&A..28..215D)
30- 35 A6 --- Type Type of cluster: cD or non-cD (G1)
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- Cluster Cluster name
7- 13 A7 --- OName Other name of cluster
15- 19 F5.3 --- z Redshift
21- 23 F3.1 keV <kT> Adopted average temperature of ICM used to
calculate the virial radius r180
25- 28 F4.1 10+20cm-2 NH Galactic value of the hydrogen column density
(Dickey & Lockman, 1990ARA&A..28..215D 1990ARA&A..28..215D)
30- 35 A6 --- Type Type of cluster: cD or non-cD (G1)
37- 46 I10 --- ObsID XMM Obs ID
48- 51 F4.1 ks ExpPN Exposure time of PN camera (2)
53- 57 F5.1 ks ExpMOS1 Exposure time of MOS1 camera (2)
59- 63 F5.1 ks ExpMOS2 Exposure time of MOS2 camera (2)
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Note (2): Exposure times after screening out the background flares.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- Cluster Cluster name
8- 11 F4.2 --- rl Lower value of radius interval, in units of r180
12 A1 --- --- [-]
13- 16 F4.2 --- ru Upper value of radius interval, in units of r180
18- 22 F5.2 keV kT Best-fit ICM temperature derived from
the 1T model fits
24- 27 F4.2 keV e_kT 1σ statistical error on kT
29- 32 F4.2 [Sun] FeA Best-fit Fe abundance using the ICM temperature
derived from the 1T model fits
(from FFeHeK/F3.5-6)
34- 37 F4.2 [Sun] e_FeA 1σ statistical error on FeA (1)
39- 43 F5.2 [Sun] DFeA Difference in the derived FeA abundances using
the best-fit multi-T model and the 1T model
45- 48 F4.2 [Sun] FeB ? Best-fit Fe abundance using the ICM
temperature derived from the 1T model fits
(for FFeHK/F3.5-6)
50- 53 F4.2 [Sun] e_FeB ? 1σ statistical error on FeB (1)
55- 59 F5.2 [Sun] DFeB ? Difference in the derived FeB abundances using
the best-fit multi-T model and the 1T model
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Note (1): 1σ statistical error, considering a 10% systematic
uncertainty in the ICM temperature derived from the 1T model
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Global Notes:
Note (G1): Types as follows:
cD = cD clusters, which are relaxed clusters with a cD galaxy at
their center.
non-cD = Other clusters
History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 29-Jun-2011