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Hot Stellar Populations in the M31 Bulge

Published online by Cambridge University Press:  07 August 2017

Henry C. Ferguson  and
Arthur F. Davidsen
Henry C. Ferguson
Affiliation:
University of Cambridge, Institute of Astronomy
Arthur F. Davidsen
Affiliation:
Center for Astrophysical Sciences, The Johns Hopkins University

Abstract

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We investigate the possibility that the Far-UV spectral energy distributions (SED's) of M31 and NGC 1399 differ only in the relative contribution from classical PAGB stars and in the amount of extinction. A good fit to the M31 spectrum is obtained for E(B-V) = 0.11 if about 65% of the flux comes from PAGB stars and the rest from stars of the type producing the far-UV emission in NGC1399. We speculate that the UV continuum in both galaxies is dominated by stars in post-horizontal branch phases of evolution, with a distribution of post-HB masses governed primarily by the metallicity and metallicity spread of the population. This hypothesis can qualitatively explain both the relative fluxes of UV rising branches in NGC1399 and M31 and the shapes of their SED's.

Type
Contributed Papers
Information
Symposium - International Astronomical Union , Volume 153: Galactic Bulges , 1993 , pp. 415 - 416
Copyright
Copyright © Kluwer 1993 

References

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