1993 Fiscal Year Final Research Report Summary
Study of extended X-ray sources
| Project/Area Number |
02402001
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| Research Category |
Grant-in-Aid for General Scientific Research (A)
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| Allocation Type | Single-year Grants |
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| Research Field |
Astronomy
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| Research Institution | Kyoto University (1991-1993)
Nagoya University (1990) |
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Principal Investigator |
KOYAMA Katsuji Kyoto Univ. Physics prof, 理学部, 教授 (10092206)
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| Co-Investigator(Kenkyū-buntansha) |
TSURU T. Kyoto Univ. Physics Instructor, 理学部, 助手 (10243007)
KUNIEDA H. Nagoya Univ. Physics ass. Prof, 理学部, 助教授 (00126856)
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| Project Period (FY) |
1990 – 1993
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| Keywords | X-Ray / Stav Forming Rogin / Super nova Remnant / The Galactic Contor / The Galaxy / Plasma / Active Galactic Nuclei / chonical Abuvdance |
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| Research Abstract |
We have determined point spread function of X-ray telescope (XRT) on board ASCA.Calibrations has been done using the 30-m beam line at ISAS.WE also determined response matrix of the GIS instruments, which are currently used for the ASCA Guest Observers in all of the world
We have installed standard software for the study of X-ray imaging and spectra in our work station. Also point spread function and response matrix were installed in the standard soft were plpackages
X-ray spectral analysis we extensively carried out using the Ginga satellite. We have for the first times detected hard X-ray emission from the star forming region Rho-Oph and SNR IC443, HB9, IC443, RCW86 and Others. Iron K-shell emission from Star forming region of Rho-Oph, Eta-Car and Orion Nebula are discovered
We have carried out systematic study for many young supernova remnants and found that most of them are in non-equilibrium ionization states
We discovered largely extended thin hot plasma from the region of our galactic center. We also performed two-dimensional mapping of the thin hot plasma along the galactic plane
Largely extended X-ray emission is also discovered from the near-by cluster of galaxies The Virgo Cluster. Iron abundance is found to exhibits central peak in the cluster. We have set new upper-limit of X-ray surface brightness of inter-cluster space
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