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The UV Upturn in Elliptical Galaxies

Published online by Cambridge University Press:  07 August 2017

H.C. Ferguson
H.C. Ferguson*
Affiliation:
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore MD 21218, USA ([email protected])

Abstract

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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.), 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.

Type
Session 6: Stellar Populations in Elliptical Galaxies
Information
Symposium - International Astronomical Union , Volume 164: Stellar Populations , 1995 , pp. 239 - 248
Copyright
Copyright © Kluwer 1995 

References

Baade, W., 1958, Stellar Populations, ed. O'Connell, D.J.K., North Holland, Amsterdam, p.1 Google Scholar
Bohlin, R. C., Cornett, R. H., Hill, J. K., Hill, R. S., O'Connell, R. W. and Stecher, T. P., 1985, Ap. J. 298, L37 CrossRefGoogle Scholar
Bressan, A., Chiosi, C. and Fagotto, F., 1994, Padova preprint Google Scholar
Brocato, E., Matteucci, F., Mazzitelli, I. and Tornambè, A., 1990, Ap. J. 349, 458 CrossRefGoogle Scholar
Burstein, D., Bertola, F., Buson, L. M., Faber, S. M., and Lauer, T. R., 1988, Ap. J. 328, 440 Google Scholar
Castellani, M. and Tornambè, A., 1991, Ap. J. 381, 393 CrossRefGoogle Scholar
Castellani, M., Limongi, M. and Tornambè, A., 1992, Ap. J. 389, 227 CrossRefGoogle Scholar
Davidsen, A. F. and Ferguson, H. C., 1992, The Physics of Nearby Galaxies: Nature or Nurture?, eds. Thuan, T. X., Balkowski, C. and Van, J. T. T., Editions Frontieres, Gif-sur-Yvette, p. 125 Google Scholar
Deharveng, J. M., Joubert, M., Monnet, G. and Donas, J., 1982, A. & A. 106, 16 Google Scholar
Dorman, B., Rood, R. T. and O'Connell, R. W., 1993, Ap. J. 419, 596 Google Scholar
Dorman, B., O'Connell, R. W. and Rood, R. T., 1994, preprint Google Scholar
Ferguson, H. C., et al., 1991, Ap. J. 382, L69 Google Scholar
Friel, E. D. and Janes, K. A., 1993, A. & A. 267, 75 Google Scholar
Garnavich, P. M., Vandenberg, D. A., Zurek, D. and Hesser, J. E., 1994, A. J. 107, 1097 CrossRefGoogle Scholar
Greggio, L. and Renzini, A., 1990, ApJ 364, 35 Google Scholar
Hubeny, I., 1988, Comput. Phys. Commun. 52, 103 Google Scholar
Kurucz, R. L., 1992, priv. comm.Google Scholar
Lee, Y.-W., 1994, Ap. J. 430, L113 Google Scholar
Liebert, J., Saffer, R. A. and Green, E. M., 1994, A. J. 107, 1408 Google Scholar
Newell, E. B., 1973, Ap. J. Suppl. 26, 37 Google Scholar
Reimers, D., 1975, Mem. Soc. R. Liège, ser. 6, 8, 369 Google Scholar
Renzini, A., 1994, A. & A. 285, L5 Google Scholar
Saffer, R. A., 1991, , Univerity of Arizona Google Scholar
Worthey, G., 1992, , UC Santa Cruz Google Scholar