Hostname: page-component-78c5997874-s2hrs Total loading time: 0 Render date: 2024-11-10T05:35:14.139Z Has data issue: false hasContentIssue false
  • English
  • Français

Estimating distances to AGB stars using IR data

Published online by Cambridge University Press:  07 February 2024

Rajorshi Bhattacharya Open the ORCID record for Rajorshi Bhattacharya [Opens in a new window] ,
Ylva M. Pihlström  and
Loránt O. Sjouwerman Open the ORCID record for Loránt O. Sjouwerman [Opens in a new window]
Rajorshi Bhattacharya*
Affiliation:
University of New Mexico, Albuquerque, NM, USA.
Ylva M. Pihlström
Affiliation:
University of New Mexico, Albuquerque, NM, USA.
Loránt O. Sjouwerman
Affiliation:
National Radio Astronomy Observatory, Socorro, NM, USA
*
email: rbhattacharya1995@unm.edu
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.

We present a method to estimate distances to AGB stars, utilizing the rich infrared data sets available for these infrared-bright targets. The method is based on the assumption that stars with intrinsically similar properties (metallicity, initial mass, etc.) produce similar spectral energy distributions (SEDs) and similar luminosities. We here discuss the results for AGB stars belonging to the BAaDE survey sample whose distances were calibrated using the template SEDs of stars with their VLBI parallaxes. As VLBI parallaxes are only known for a handful of sources, the resulting templates only cover a small subset of the BAaDE sample. Additional methods to derive suitable templates will therefore also be required. The work on expanding the template set is promising, although more fine tuning is still needed.

Keywords

Asymptotic giant branch starsMilky Wayinfraredspectral energy distributions
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S380: Cosmic Masers: Proper Motion toward the Next-Generation Large Projects , December 2022 , pp. 116 - 118
Check for updates
Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution and reproduction, provided the original article is properly cited.
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

Abuter, R., Amorim, A., Bauböck, M., Berger, J., Bonnet, H., Brandner, W., Clénet, Y., Du Foresto, V. C., De Zeeuw, P., Dexter, J., et al. 2019, A&A, 625, L10.Google Scholar
Andriantsaralaza, M., Ramstedt, S., Vlemmings, W. T., & De Beck, E. 2022, arXiv preprint arXiv:2209.03906,.Google Scholar
Xu, S., Zhang, B., Reid, M. J., Zheng, X., & Wang, G. 2019, ApJ, 875, 114.10.3847/1538-4357/ab0e83CrossRefGoogle Scholar
Supplementary material: PDF

Bhattacharya et al. supplementary material

Bhattacharya et al. supplementary material

Download Bhattacharya et al. supplementary material(PDF)
PDF 401.8 KB