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Asymptotic Giant Branch Variables in Nearby Galaxies

Published online by Cambridge University Press:  30 December 2019

Patricia A. Whitelock Open the ORCID record for Patricia A. Whitelock [Opens in a new window]
Patricia A. Whitelock*
Affiliation:
South African Astronomical Observatory, P O Box 9, 7935 Observatory, South Africa Department of Astronomy, University of Cape Town, 7701 Rondebosch, South Africa email: [email protected]
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Abstract

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Certain types of large amplitude AGB variable are proving to be powerful distance indicators that will rival Cepheids in the James Webb Space Telescope era of high precision infrared photometry. These are predominantly found in old populations and have low mass progenitors. At the other end of the AGB mass-scale, large amplitude variables, particularly those undergoing hot bottom burning, are the most luminous representatives of their population. These stars are < 1 Gyr old, are often losing mass copiously and are vital to our understanding of the integrated light of distant galaxies as well as to chemical enrichment. However, the evolution of such very luminous AGB variables is rapid and remains poorly understood. Here I discuss recent infrared observations of both low- and intermediate-mass Mira variables in the Local Group and beyond.

Keywords

stars: AGB and post-AGBstars: carbonstars: late-typestars: mass lossstars: variables: othergalaxies: dwarfgalaxies: individual (NGC3109 Sgr dIG NGC4258 M33)(galaxies:) Magellanic Cloudsinfrared: stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S343: Why Galaxies Care About AGB Stars: A Continuing Challenge through Cosmic Time , August 2018 , pp. 275 - 282
Copyright
© International Astronomical Union 2019 

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