The Abundance Pattern In The Hot ISM Of NGC 4472: Insights And Anomalies

Details The Abundance Pattern In The Hot ISM Of NGC 4472: Insights And Anomalies The Abundance Pattern In The Hot ISM Of NGC 4472: Insights And Anomalies

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21545806l&link_type=abstract

American Astronomical Society, AAS Meeting #215, #458.06; Bulletin of the American Astronomical Society, Vol. 42, p.483

Astronomy and Astrophysics

Astronomy

Scientific paper

Important clues to the chemical and dynamical history of elliptical galaxies are encoded in the abundances of heavy elements in the X-ray emitting plasma. We derive the hot ISM abundance pattern in inner and outer regions of NGC 4472 from analysis of Suzaku spectra, supported by analysis of co-spatial XMM-Newton spectra. The low background and relatively sharp spectral resolution of the Suzaku XIS detectors, combined with the high luminosity and temperature in NGC 4472, enable us to derive a particularly extensive abundance pattern that encompasses O, Ne, Mg, Al, Si, S, Ar, Ca, Fe, and Ni in both regions. We apply simple chemical evolution models to these data, and conclude that the
abundances are best explained by a combination of alpha-element enhanced stellar mass loss and direct injection of Type Ia supernova ejecta. We thus confirm the inference, based on optical data, that the stars in elliptical galaxies have supersolar alpha/Fe ratios, but find that that the present-day SNIa rate is 4-6 times lower than the standard value. We find SNIa yield sets that reproduce Ca and Ar, or Ni, but not all three simultaneously. The low abundance of O relative to Ne and Mg implies that standard core collapse nucleosynthesis models overproduce O by a factor of 2.
This work is supported by NASA ADP and
Suzaku Guest Observer Programs.

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