By James E. Hesser (auth.), B. Barbuy, A. Renzini (eds.)
One method of studying approximately stellar populations is to review them at 3 assorted degrees of solution. First in our personal Galaxy; secondly from within reach galaxies the place stars can nonetheless be resolved; and thirdly in distant galaxies within which the stellar inhabitants can merely be studied in built-in mild.
This IAU Symposium lined the total variety of galaxies in its learn in their stellar populations. Interspersed with theoretical papers, the wealth of observational effects presents a major state of the art presentation of the development that has been made during this box.
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Extra resources for The Stellar Populations of Galaxies: Proceedings of the 149th Symposium of the International Astronomical Union, Held in Angra Dos Reis, Brazil, August 5–9, 1991
The wide abundance range in the galactic bulge causes an unusual mix of evolved stars. and IRAS stars are metal rich. On the other hand, the RR Lyraes and H8 stars are evolved from the metal poor population (certain to be very old). The red "clump" giants are evolved from the metal rich population. he bulge. By and large, these clusters are of solar abundance and lower (Armandroff, 1989); direct. he clusters. 1. he abundance distribution of long-lived stars, but this is not possible because the bulge turnoff is too faint.
Canley, B. , & Jones, R. V. 1992, ApJ, in press. (CSJ) Carney, B. , Trammel, S. , and Jones, R. , 1991, PASP, in press. Fernley, J. , Jameson, R. , and Longmore, A. J. 1990, MNRAS, 247, 287. Hesser, J. , Harris, W. , VandenBerg, D. , Allwright, J. W. , and Stetson, P. B. 1987. PASP, 99,739. Jones, R. V. 1988, ApJ, 326,305. Jones, R. , Canley, B. , and Latham, D. W. 1988, ApJ, 332, 206. Jones, R. , Canley, B. , and Latham, D. W. 1992, ApJ, in press. King, C. , and Green, E. M. 1988, in Calibration of Stellar Ages, ed.
A. 1986, MNRAS, 220,413. Suntzeff, N. , Kinman, T. , and Kraft, R. P. 1991, ApJ, 367, 528. van Albada, T. , and Baker, N. 1971, ApJ, 169,311. VandenBerg, D. , and Stetson, P. B. 1990, AJ, 100, 445. 20 HESSER: I would like to make two comments on your excellent review of this very active area. First, the development of the relative age-dating technique via the color difference technique (which has been one of the most exciting ideas in many years for those of us who struggle to understand the age profile of the Galactic halo) is limited to certain metallicity ranges, as you stressed.
The Stellar Populations of Galaxies: Proceedings of the 149th Symposium of the International Astronomical Union, Held in Angra Dos Reis, Brazil, August 5–9, 1991 by James E. Hesser (auth.), B. Barbuy, A. Renzini (eds.)