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The 6.4 keV Fe Line and the SiO Emission in the GC

Published online by Cambridge University Press:  13 May 2016

J. Martín-Pintado ,
P. de Vicente ,
N. Rodríguez-Fernández ,
A. Fuente  and
P. Planesas
J. Martín-Pintado
Affiliation:
Observatorio Astronómico Nacional, Apartado 1143, E-28800, Alcalá de Henares, Spain
P. de Vicente
Affiliation:
Observatorio Astronómico Nacional, Apartado 1143, E-28800, Alcalá de Henares, Spain
N. Rodríguez-Fernández
Affiliation:
Observatorio Astronómico Nacional, Apartado 1143, E-28800, Alcalá de Henares, Spain
A. Fuente
Affiliation:
Observatorio Astronómico Nacional, Apartado 1143, E-28800, Alcalá de Henares, Spain
P. Planesas
Affiliation:
Observatorio Astronómico Nacional, Apartado 1143, E-28800, Alcalá de Henares, Spain

Abstract

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We present a map of the Galactic center in the J=l-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. The SiO abundance increases by more than 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.

Type
The Inner Regions of Galaxies
Information
Symposium - International Astronomical Union , Volume 205: Galaxies and their Constituents at the Highest Angular Resolutions , 2001 , pp. 36 - 37
Copyright
Copyright © Astronomical Society of the Pacific 2001 

References

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Martín-Pintado, J., de Vicente, N.J. Rodriguez-Fernandez, P., Fuente, A., Planesas, P. 1997, A&A 365, L5.Google Scholar