Astronomy and Astrophysics – Astrophysics
Scientific paper
Jan 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001iaus..205...36m&link_type=abstract
Galaxies and their Constituents at the Highest Angular Resolutions, Proceedings of IAU Symposium #205, held 15-18 August 2000 at
Astronomy and Astrophysics
Astrophysics
Scientific paper
Molecular gas can be exposed to X-rays in a wide range of astrophysical environments like active nuclei, near supernova remnants, in fast socks, or in molecular clouds with embedded X-ray sources. X-rays will heat and influence the chemisty of the molecular clouds. The Galactic center (GC) is a strong source of diffuse X-ray emission in the 2-10 keV energy range and in lines from several elements and contains warm molecular clouds with an usual chemistry. The origin of the morphology and intensity of the 6.4 keV Fe line and the heating and chemistry in the GC have been a puzzle. We present a map of the GC in the J=1-0 line of SiO covering the region mapped with the ASCA satellite in the 6.4 keV Fe line. We find a correlation between the spatial distribution of the Fe 6.4 keV line and the SiO emission, both on the large scale and within the Sgr A and Sgr B complexes. The SiO abundance increases by a factor of >~20 in the regions with strong Fe 6.4 keV line. This indicates that the Fe 6.4 keV line mainly arises from molecular clouds with large gas phase abundance of refractory elements. We discuss the implications of the correlation on the origin of the hard X-rays, and the heating and the chemistry of the molecular clouds in the GC.
de Vicente P.
Fuente Asuncion
Martín-Pintado Jesús
Planesas Pere
Rodriguez-Fernandez Nemesio J.
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