The determination of the stellar O abundance of an elliptical galaxy, NGC 720f

Details The determination of the stellar O abundance of an elliptical galaxy, NGC 720f The determination of the stellar O abundance of an elliptical galaxy, NGC 720f

Oct 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006xmm..prop..168m&link_type=abstract

XMM-Newton Proposal ID #05044901

Physics

Galaxies, Galactic Surveys, Ngc 720, Xmm-Newton Proposal 05044901

Scientific paper

We propose to observe an elliptical galaxy, NGC 720, for 130 ks in order to determine the O abundance of stars in the galaxy. The O abundance is the most important, since it is the most abundant element except H and He, and synthesized only by type II supernovae (SNe). In elliptical galaxies, accumulations of stellar mass loss emit X-rays and therefore, the O abundance of the X-ray emitting gas reflects the stellar metallicity. NGC 720 is relatively isolated and do not show large-scale halos and suitable to look at the pure galactic properties.

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