Hostname: page-component-586b7cd67f-gb8f7 Total loading time: 0 Render date: 2024-11-29T21:44:18.090Z Has data issue: false hasContentIssue false
  • English
  • Français

AGB maser stars as tracers of stellar populations

Published online by Cambridge University Press:  12 April 2016

H.J. Habing
H.J. Habing*
Affiliation:
Sterrewacht Leiden, Postbus 9513, 2300 RA Leiden, The Netherlands

Abstract

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.

Masers are known to occur in circumstellar envelopes of AGB stars that are long-period variables and have entered the TP-AGB phase. The maser radiation is intrinsically weak and detection limits prevent us from seeing maser stars much beyond the Galactic Center. Very deep searches have led to the detection of a handful of maser stars in the Large Magellanic Cloud. Some 1000 stellar masers are known. They trace a population of stars with main sequence masses between 1 and 6 M⊙ and ages between 2 and 8 Gyr, the same population that is traced by Cepheids. Their distribution in our Galaxy is the same as that of the red giants, and therefore the stars trace the galactic bar. An outstanding feature is a small disk of radius 150 pc around the galactic center. The disk is in rapid, solid body rotation and leads to a good measurement of the mass density within that distance for Sgr A.

Type
Part 3. Variable stars as tracers of different stellar populations – galactic and globular clusters, LMC/SMC and Local Group galaxies
Information
International Astronomical Union Colloquium , Volume 193: Variable Stars in the Local Group , 2004 , pp. 138 - 143
Copyright
Copyright © Astronomical Society of the Pacific 2004

References

Honma, M., et al. 2003 PAS J, 55, L57 Google Scholar
Lindqvist, M., Habing, H.J., Winnberg, A., 1992, A&A, 259, 118 Google Scholar
Messineo, M., Habing, H.J., Sjouwerman, L.O., Omont, A., Menten, K.M., 2002, aap, 393, 115 Google Scholar
Miyazaki, A., Deguchi, S., Tsuboi, M., Kasuga, T., Takano, S., 2001 PASJ, 53, 501 Google Scholar
Ortiz, R., Blommaert, J.A.D.L., Copet, E., Ganesh, S., Habing, H.J., Messineo, M., Omont, A., Schultheis, M., Schuller, F., 2002, A&A, 388, 279 Google Scholar
Robin, A.C., Reylé, C., Derrière, S., Picaud, S., 2003, A&A, 409, 523 Google Scholar
Sevenster, M.N., Chapman, J.M., Habing, H.J., Killeen, N.E.B., Lindqvist, M., 1997a, A&AS, 122, 79 Google Scholar
Sevenster, M.N., Chapman, J.M., Habing, H.J., Killeen, N.E.B., Lindqvist, M., 1997b, A&AS, 124, 509 Google Scholar
Sevenster, M.N., Dejonghe, H., Habing, H.J. 1995 A&A, 299, 689 Google Scholar
Sevenster, M.N., van Langevelde, H.J., Moody, R.A., Chapman, J.M., Habing, H.J., Killeen, N.E.B. 2001 A&A, 366, 481 Google Scholar
Vlemmings, W., 2002, Ph.D.Thesis, University of Leiden Google Scholar
Wood, P.R., et al. 1999 IAU Symp. 191: Asymptotic Giant Branch Stars, 191, 151 Google Scholar