Hostname: page-component-cd9895bd7-fscjk Total loading time: 0 Render date: 2024-12-27T07:47:33.620Z Has data issue: false hasContentIssue false
  • English
  • Français

Infrared Studies of the Variability and Mass Loss of Some of the Dustiest Asymptotic Giant Branch Stars in the Magellanic Clouds

Published online by Cambridge University Press:  30 December 2019

B. Sargent Open the ORCID record for B. Sargent [Opens in a new window] ,
S. Srinivasan ,
M. Boyer Open the ORCID record for M. Boyer [Opens in a new window] ,
M. Feast Open the ORCID record for M. Feast [Opens in a new window] ,
P. Whitelock ,
M. Marengo Open the ORCID record for M. Marengo [Opens in a new window] ,
M. A. T. Groenewegen ,
M. Meixner Open the ORCID record for M. Meixner [Opens in a new window] ,
J. L. Hora  and
M. Otsuka
B. Sargent
Affiliation:
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA; email: sargent@stsci.edu
S. Srinivasan
Affiliation:
Academia Sinica, Institute of Astronomy and Astrophysics, 11F of AS/NTU Astronomy-Mathematics Building, No. 1, Sec. 4, Roosevelt Rd., Taipei 10617, Taiwan, R.O.C.
M. Boyer
Affiliation:
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA; email: sargent@stsci.edu
M. Feast
Affiliation:
South African Astronomical Observatory, P.O. Box 9, Observatory, 7935, South Africa University of Cape Town, Private Bag X3, Rondebosch 7701, Republic of South Africa
P. Whitelock
Affiliation:
South African Astronomical Observatory, P.O. Box 9, Observatory, 7935, South Africa University of Cape Town, Private Bag X3, Rondebosch 7701, Republic of South Africa
M. Marengo
Affiliation:
Iowa State University, A313E Zaffarano, Ames, IA 50010, USA
M. A. T. Groenewegen
Affiliation:
Koninklijke Sterrenwacht van België, Ringlaan 3, B-1180 Brussels, Belgium
M. Meixner
Affiliation:
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA; email: sargent@stsci.edu
J. L. Hora
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS-65, Cambridge, MA 02138-1516, USA
M. Otsuka
Affiliation:
Academia Sinica, Institute of Astronomy and Astrophysics, 11F of AS/NTU Astronomy-Mathematics Building, No. 1, Sec. 4, Roosevelt Rd., Taipei 10617, Taiwan, R.O.C. Kyoto University, Okayama Observatory, Honjo, Kamogata, Asakuchi, Okayama, 719-0232, Japan
Rights & Permissions [Opens in a new window]

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.

The asymptotic giant branch (AGB) stars with the reddest colors have the largest amounts of circumstellar dust. AGB stars vary in their brightness, and studies show that the reddest AGB stars tend to have longer periods than other AGB stars and are more likely to be fundamental mode pulsators than other AGB stars. Such stars are difficult to study, as they are often not detected at optical wavelengths. Therefore, they must be observed at infrared wavelengths. Using the Spitzer Space Telescope, we have observed a sample of very dusty AGB stars in the Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) over Cycles 9 through 12 during the Warm Spitzer mission. For each cycle’s program, we typically observed a set of AGB stars at both 3.6 and 4.5 μm wavelength approximately monthly for most of a year. We present results from our analysis of the data from these programs.

Keywords

infrared: starsstars: AGB and post-AGB
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. 498 - 499
Copyright
© International Astronomical Union 2019 

References

Asplund, M., Grevesse, N., and Sauval, A. J., et al. 2004, A&A, 417, 751 Google Scholar
Bonanos, A. Z., Massa, D. L., Sewilo, M., et al. 2009, AJ, 138, 1003 CrossRefGoogle Scholar
Dufour, R. J., Shields, G. A., & Talbot, R. J. Jr. 1982, ApJ, 252, 461 CrossRefGoogle Scholar
Gruendl, R. A., Chu, Y.-H., Seale, J. P., et al. 2008, ApJ, 688, L9 CrossRefGoogle Scholar
Ita, Y. 2005, The Astronomical Herald, 98, 163 Google Scholar
Jones, O., Meixner, M., Sargent, B. A., et al. 2015, ApJ, 811, 145 CrossRefGoogle Scholar
Nishida, S., Tanabé, T., Nakada, Y., et al. 2000, MNRAS, 313, 136 CrossRefGoogle Scholar
Polsdofer, E., Seale, J., Sewiło, M., et al. 2015, AJ, 149, 78 CrossRefGoogle Scholar
Riebel, D., Meixner, M., Fraser, O., et al. 2010, ApJ, 723, 1195 CrossRefGoogle Scholar
Schaefer, B. E., Simon, M., Prato, L., & Barman, T. 2008, AJ, 135, 112 CrossRefGoogle Scholar
Sloan, G. C., Kraemer, K. E., McDonald, I., et al. 2016, ApJ, 826, 44 CrossRefGoogle Scholar
Srinivasan, S., Meixner, M., Leitherer, C., et al. 2009, AJ, 137, 4810 CrossRefGoogle Scholar
Srinivasan, S., Boyer, M. L., Kemper, F., et al. 2016, MNRAS 457, 2814 CrossRefGoogle Scholar
Szewczyk, O., Pietrzyski, G., Gieren, W., et al. 2009, AJ, 138, 1661 CrossRefGoogle Scholar
Tanabé, T., Nishida, S., Matsumoto, S., et al. 1997, Nature, 385, 509 CrossRefGoogle Scholar
Vijh, U., Meixner, M., Babler, B., et al. 2009, AJ, 137, 3139 CrossRefGoogle Scholar