X-ray Observations of SNRs and hot ISM in the Large Magellanic Cloud:. the chemical enrichment of the galaxy

Details X-ray Observations of SNRs and hot ISM in the Large Magellanic Cloud:. the chemical enrichment of the galaxy X-ray Observations of SNRs and hot ISM in the Large Magellanic Cloud:. the chemical enrichment of the galaxy

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003omeg.conf..370n&link_type=abstract

ORIGIN OF MATTER AND EVOLUTION OF GALAXIES 2000. Proceedings of the International Symposium. Held 19-21 January 2000 in Universi

Astronomy and Astrophysics

Astrophysics

Scientific paper

The great portion of the elements are thought to be produced in the supernova (SN) explosions and gradually mixed into the interstellar matter (ISM) of the galaxies. We can trace the course of the chemical-pollution of the galaxies by observing the supernova remnants (SNRs) and ISM. We present the X-ray measurements of metal abundances of the Large Magellanic Cloud (LMC). All the archive data in the vicinity of the LMC taken with the Advanced Satellite for Cosmology and Astrophysics (ASCA) were used. The X-ray spectroscopy of the diffuse X-ray emission spreading over a large portion of the LMC was carried out in order to measure the metal abundance of the ISM directly. With the good spectral resolution of ASCA the nature of this diffuse X-ray emission was first confirmed to be thermal in origin, likely to be emitted from hot ionized ISM in the galaxy, because ASCA detected line emissions from various elements, which was beyond the capability of previous X-ray satellites. The X-ray spectrum of diffuse X-ray emission was reproduced by the Non-Equilibrium Ionization (NEI) model with temperature of ~ 1.2 keV. The overall elemental abundances determined from X-ray spectroscopy of ISM is found to be also consistent with previous results determined through X-ray SNR spectroscopy derived by Hughes, Hayashi and Koyama (1998) and previous optical and UV analysis, except overabundance of sulfer.

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