The Galactic Abundances of Fe, Ne, and Mg

Details The Galactic Abundances of Fe, Ne, and Mg The Galactic Abundances of Fe, Ne, and Mg

Oct 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006xmm..prop..143b&link_type=abstract

XMM-Newton Proposal ID #05036901

Astronomy and Astrophysics

Astronomy

Supernovae, Supernova Remnants, Diffuse (Galactic) Emission And Isolated Neutron Stars, 4U0241+61, Xmm-Newton Proposal 05036901

Scientific paper

The history of Galactic star formation is coded in the ISM through elemental abundances and the ratio of the Fe-group to lighter species. This important area has been the domain of optical and UV astronomers, whose abundances of Galactic interstellar gas are subject to significant uncertainties due to (the unknown) depletion onto dust grains and the need to adopt a photoionization model. A new method, using X-ray observations can measure elemental abundances without such biases, and oxygen abundances are already measured with this technique. We extend this method to measure the abundances of Fe, Ne, and Mg by the magnitude of their absorption edges. This requires a high N(HI), so our target is a bright blazar projected close to the Galactic midplane.

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