The UV Upturn in Elliptical Galaxies |
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| Authors: | HC Ferguson |
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| Institution: | (1) Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA |
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| Abstract: | The hot stellar component in elliptical galaxies offers clues to both stellar evolution and galaxy evolution. Current observations
suggest that extreme horizontal branch (EHB) stars dominate the far-UV emission from galaxies with the strongest "UV upturns,"
while post asymptotic giant branch (PAGB) stars are probably significant contributors for weaker galaxies. Spectra near the
Lyman limit indicate that a rather narrow range of temperature (and hence EHB star mass) is required. However, other arguments
suggest that most of the helium-burning stars in elliptical galaxies are in the red clump. The HB star mass distribution therefore appears
to be strongly bimodal. Such bimodality is qualitatively reproduced by two radically different stellar population models,
(those of Lee and Bressan et al., 1994), both of which require that the galaxies be very old. However, the Galactic open cluster NGC 6791 also contains EHB
stars and exhibits strong bimodality, indicating that old age may not necessarily be a requirement for the UV upturn phenomenon.
This revised version was published online in July 2006 with corrections to the Cover Date. |
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