TY - JOUR
T1 - Suzaku observations of tycho's supernova remnant
AU - Tamagawa, Toru
AU - Hayato, Asami
AU - Nakamura, Satoshi
AU - Terada, Yukikatsu
AU - Bamba, Aya
AU - HLraga, Junko S.
AU - Hughes, John P.
AU - Hwang, Una
AU - Kataoka, Jun
AU - Kinugasa, Kenzo
AU - Kunieda, Hideyo
AU - Tanaka, Takaaki
AU - Tsunemi, Hiroshi
AU - Ueno, Masaru
AU - Holt, Stephen S.
AU - Kokubun, Motohide
AU - Mlyata, Emi
AU - Szymkowiak, Andrew
AU - Takahashi, Tadayuki
AU - Tamura, Keisuke
AU - Ueno, Daisuke
AU - Makishima, Kazuo
PY - 2009
Y1 - 2009
N2 - Tycho's supernova remnant was observed by the XIS and HXD instruments onboard the Suzaku satellite on 2006 June 26-29 for 92 ks. The spectrum up to 30 keV was well fitted with a two-component model, consisting of a power-law with a photon index of 2.7 and a thermal bremsstrahlung model with a temperature of 4.7 keV. The former component can alternatively be modeled as synchrotron emission from a population of relativistic electrons with an estimated roll-off energy of around 1 keV. In the XIS spectra, in addition to the prominent Fe Ka line (6.445 keV), we observed for the first time significant Ka line emission from trace species Cr and Mn at energies of 5.48 keV and 5.95 keV, respectively. Faint K/5 lines from Ca (4.56keV) and Fe (7.11 keV) were also seen. The ionization states of Cr and Mn, based on their line centroids, are estimated to be similar to that of Fe Ka (Fexv orxvi).
AB - Tycho's supernova remnant was observed by the XIS and HXD instruments onboard the Suzaku satellite on 2006 June 26-29 for 92 ks. The spectrum up to 30 keV was well fitted with a two-component model, consisting of a power-law with a photon index of 2.7 and a thermal bremsstrahlung model with a temperature of 4.7 keV. The former component can alternatively be modeled as synchrotron emission from a population of relativistic electrons with an estimated roll-off energy of around 1 keV. In the XIS spectra, in addition to the prominent Fe Ka line (6.445 keV), we observed for the first time significant Ka line emission from trace species Cr and Mn at energies of 5.48 keV and 5.95 keV, respectively. Faint K/5 lines from Ca (4.56keV) and Fe (7.11 keV) were also seen. The ionization states of Cr and Mn, based on their line centroids, are estimated to be similar to that of Fe Ka (Fexv orxvi).
KW - Acceleration of particles - ISM
KW - Individual (Tycho)
KW - Supernova remnants - X-rays
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U2 - 10.1093/pasj/61.sp1.s167
DO - 10.1093/pasj/61.sp1.s167
M3 - Article
AN - SCOPUS:64849108663
SN - 0004-6264
VL - 61
SP - S167-S174
JO - Publication of the Astronomical Society of Japan
JF - Publication of the Astronomical Society of Japan
IS - SUPPL. 1
ER -