TY - JOUR
T1 - X-ray spectroscopy of the core of the perseus cluster with suzaku
T2 - Elemental abundances in the intracluster medium
AU - Tamura, T.
AU - Maeda, Y.
AU - Mitsuda, K.
AU - Fabian, A. C.
AU - Sanders, J. S.
AU - Furuzawa, A.
AU - Hughes, J. P.
AU - Iizuka, R.
AU - Matsushita, K.
AU - Tamagawa, T.
N1 - Copyright:
Copyright 2015 Elsevier B.V., All rights reserved.
PY - 2009
Y1 - 2009
N2 - The results from Suzaku observations of the central region of the Perseus cluster are presented. Deep exposures with the X-ray Imaging Spectrometer provide high-quality X-ray spectra from the intracluster medium. X-ray lines from helium-like Cr and Mn have been detected significantly for the first time in clusters. In addition, elemental abundances of Ne, Mg, Si, S, Ar, Ca, Fe, and Ni are accurately measured within 10′ (or 220kpc) from the cluster center. The relative abundance ratios are found to be within a range of 0.8-1.5 times the solar value. These abundance ratios are compared with previous measurements, those in extremely metal-poor stars in the Galaxy, and theoretical models.
AB - The results from Suzaku observations of the central region of the Perseus cluster are presented. Deep exposures with the X-ray Imaging Spectrometer provide high-quality X-ray spectra from the intracluster medium. X-ray lines from helium-like Cr and Mn have been detected significantly for the first time in clusters. In addition, elemental abundances of Ne, Mg, Si, S, Ar, Ca, Fe, and Ni are accurately measured within 10′ (or 220kpc) from the cluster center. The relative abundance ratios are found to be within a range of 0.8-1.5 times the solar value. These abundance ratios are compared with previous measurements, those in extremely metal-poor stars in the Galaxy, and theoretical models.
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U2 - 10.1088/0004-637X/705/1/L62
DO - 10.1088/0004-637X/705/1/L62
M3 - Article
AN - SCOPUS:77949507825
VL - 705
SP - L62-L66
JO - Nippon rinsho. Japanese journal of clinical medicine
JF - Nippon rinsho. Japanese journal of clinical medicine
SN - 0047-1852
IS - 1 PART 2
ER -