Hostname: page-component-848d4c4894-5nwft Total loading time: 0 Render date: 2024-05-16T18:10:11.937Z Has data issue: false hasContentIssue false
  • English
  • Français

The Tip of the Red Giant Branch as a Population II Distance Indicator

Published online by Cambridge University Press:  25 May 2016

Shoko Sakai
Shoko Sakai*
Affiliation:
Jet Propulsion Laboratory IPAC Caltech 100-22 Pasadena CA 91125 USA

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The period–luminosity (PL) relation of the Cepheid variable stars is the most reliable primary distance indicator for nearby galaxies, and serves as the foundation of the extragalactic distance scale, providing the firm calibration for various secondary distance indicators. However, a major disadvantage of the Cepheid distance scale is that it can only be applied to late–type systems with recent or current star formation. An alternative distance indicator is a Pop II, tip of the red giant branch (TRGB) method, which is extremely attractive because of its applicability to all morphological types of galaxies. As long as a metal–poor RGB stars are present in abundant numbers, the distance can be estimated with an accuracy that is as good as that of the Cepheid PL relation.

Type
I. Cosmological Parameters, H0, q0, Ω0 and Λ
Information
Symposium - International Astronomical Union , Volume 183: Cosmological Parameters and the Evolution of the Universe , 1999 , pp. 48 - 53
Copyright
Copyright © Kluwer 1999 

References

Baade, W., 1944, ApJ, 100, 137 Google Scholar
Beaulieu, J.P. 1997, A&A, 318, L47 Google Scholar
Caldwell, N., Armandroff, T.E., Da Costa, G.S. & Seitzer, P., 1997, AJ, in press Google Scholar
Carney, B.W., Storm, J., & Jones, R.V., 1992, ApJ, 386, 663 Google Scholar
Da Costa, G. S. & Armandroff, T. E., 1990, AJ, 100, 162 Google Scholar
Elson, R.A.W., 1997, MNRAS, 286, 771 CrossRefGoogle Scholar
Ferguson, H., von Hippel, T. & Tanvir, N.I., 1997, in press Google Scholar
Frogel, J.A., Cohen, J.G. & Persson, S.E., 1983, ApJ, 275, 773 Google Scholar
Gould, A., 1994, ApJ, 426, 542 Google Scholar
Harris, W.E., Durrell, P.R., Pierce, M.J. & Secker, J., 1997, in preparation Google Scholar
Iben, I. & Renzini, A. 1983, ARAA, 21, 271 Google Scholar
Kennicutt, et al. 1998, ApJ, in press Google Scholar
Kochanek, C.S., 1997, ApJ, in press Google Scholar
Lee, M. G., Freedman, W. L. & Madore, B. F., 1993, ApJ, 417, 553 Google Scholar
Lee, Y.-W., Demarque, P. & Zinn, R., 1990, ApJ, 350, 155 Google Scholar
Madore, B. F. & Freedman, W. L., 1995, AJ, 109, 1645 CrossRefGoogle Scholar
Sakai, S., Madore, B. F., & Freedman, W. L., 1996, ApJ, 461, 713 Google Scholar
Sakai, S., Madore, B. F., Freedman, W. L., Lauer, T. R., Ajhar, E. A. & Baum, W. A., 1997, ApJ, 478, 49 CrossRefGoogle Scholar
Sakai, S., Madore, B.F., & Freedman, W.L., 1997, ApJ, 480, 589 Google Scholar
Salaris, M. & Cassisi, S., 1996, AA, 305, 858 Google Scholar
Salaris, M. & Cassisi, S., 1997, MNRAS, 289, 406 Google Scholar
Sandage, A.R., 1971, in Nuclei of Galaxies, ed. O'Connell, D.J.K. Google Scholar
Soria, R. et al., 1996, ApJ, 465, 79 CrossRefGoogle Scholar