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Title:
Deep X-Ray Observations of Supernova Remnants G359.1-0.5 and G359.0-0.9 with ASCA
Authors:
Bamba, Aya; Yokogawa, Jun; Sakano, Masaaki; Koyama, Katsuji
Affiliation:
AA(Department of Physics, Graduate School of Science, Kyoto University, Sakyo-ku, Kyoto 606-8502; (AB):), AB(Department of Physics, Graduate School of Science, Kyoto University, Sakyo-ku, Kyoto 606-8502; (AB):), AC(Department of Physics, Graduate School of Science, Kyoto University, Sakyo-ku, Kyoto 606-8502; (AB):), AD(Department of Physics, Graduate School of Science, Kyoto University, Sakyo-ku, Kyoto 606-8502)
Publication:
Publ. of the Astronomical Society of Japan, v.52, p.259. (PASJ Homepage)
Publication Date:
04/2000
Origin:
PASJ
PASJ Keywords:
GALAXY: CENTER, GALAXY: DIFFUSE PLASMA, ISM: ABUNDANCES, ISM: INDIVIDUAL (G3591-05, G3590-09), SUPERNOVA REMNANTS, X-RAYS: ISM
Bibliographic Code:
2000PASJ...52..259B

Abstract

We present the results of deep ASCA observations of two shell-like radio supernova remnants (SNRs) located in the direction to the galactic center (GC) region. Unlike the radio morphology, G359.1-0.5 shows center-filled X-rays with prominent Kalpha lines of He-like silicon and H-like sulfur. The plasma requires at least two temperature components: a silicon-dominated cool plasma of 0.6 keV temperature and a sulfur-dominated higher temperature plasma of 4.4 keV. Because the absorption column is ~ 6times 1022 H cm-2, this SNR would be near to the GC. The spherical plasma is attributable to supernova ejecta with the total mass of Si and S being about 0.1 MO and 0.3 MO , respectively. X-rays from G359.0-0.9 trace the partial shell structure of the radio emission. The spectrum is well fitted to a single-temperature plasma of 0.4 keV with a non-solar abundance of magnesium or iron. Because the absorption column is not very large, ~ 1.8times 1022 H cm-2, G359.0-0.9 would be in front of the GC region. The total supernova energy, interstellar density near to the X-ray emitting shell, and age of the SNR are estimated to be 1.2*E51 erg, 0.5 cm-3, and 1.8*E4 yr, respectively. We also discuss possible implications on the origin of the large-scale hot plasma surrounding the GC.

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