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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
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:
FileName Lrecl Records Explanations
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
See also: B/xmm : XMM-Newton Observation Log (XMM-Newton Science Operation Center, 2009) Byte-by-byte Description of file: clusters.dat
Bytes Format Units Label Explanations
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) 30- 35 A6 --- Type Type of cluster: cD or non-cD (G1)
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
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) 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)
Note (2): Exposure times after screening out the background flares.
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
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
Note (1): 1σ statistical error, considering a 10% systematic uncertainty in the ICM temperature derived from the 1T model
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
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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