The 6.7 keV-line emission in the Galactic Centre

Details The 6.7 keV-line emission in the Galactic Centre The 6.7 keV-line emission in the Galactic Centre

Oct 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006xmm..prop..210s&link_type=abstract

XMM-Newton Proposal ID #05058703

Computer Science

Supernovae, Supernova Remnants, Diffuse (Galactic) Emission And Isolated Neutron Stars, Gcps_3, Xmm-Newton Proposal 05058703

Scientific paper

The Galactic Centre Region emits a strong 6.7-keV line attributable to Ka emission of He-like iron, of which the origin has remained a puzzle since its discovery. Arguably, recent Chandra results imply that the line is produced in a hot extended plasma. However, we have shown that the line has a relatively smooth, circularly symmetric distribution centred on Sgr A* and a surface brightness which falls off with radius as 1/r over the range r=3 -12 . This mirrors the distribution of the stellar population and adds strong support to the hypothesis that the 6.7-keV line originates in the summed emission of faint point sources. Here we propose to measure the surface brightness distribution of the 6.7-keV line out to a radius of ~35 as a test of the competing scenarios for its origin.

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