Hostname: page-component-7bb8b95d7b-s9k8s Total loading time: 0 Render date: 2024-09-29T18:51:54.702Z Has data issue: false hasContentIssue false
  • English
  • Français

SiO maser line ratios in the BAaDE Survey

Published online by Cambridge University Press:  07 February 2024

Megan O. Lewis Open the ORCID record for Megan O. Lewis [Opens in a new window] ,
Ylva M. Pihlström Open the ORCID record for Ylva M. Pihlström [Opens in a new window]  and
Loránt O. Sjouwerman Open the ORCID record for Loránt O. Sjouwerman [Opens in a new window]
Megan O. Lewis*
Affiliation:
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Warsaw, Poland 00-716.
Ylva M. Pihlström
Affiliation:
University of New Mexico, Albuquerque, NM, USA 87131
Loránt O. Sjouwerman
Affiliation:
National Radio Astronomy Observatory, Socorro, NM, USA 87801
*
email: [email protected]
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.

Multi-transition SiO maser emission has been detected in over 10 thousand evolved stars across the plane of the Milky Way by the Bulge Asymmetries and Dynamical Evolution (BAaDE) survey. In addition to the large source catalog of the survey, the frequency coverage is also unprecedented: the J=1-0 (43 GHz) data cover seven separate transitions of SiO, and the J=2-1 (86 GHz) data cover ten SiO transitions. In contrast, most other SiO maser data only probe the SiO v=1 and v=2 at 43 GHz and/or the v=1 at 86 GHz. Our extended range allows for the derivation of SiO line ratios for a huge population of evolved stars, including those derived from rare transitions associated with 29SiO and 30SiO isotopologues. We examine how these ratios are affected by the specific combinations of transitions that are detected in a single source. Furthermore, we present a class of ‘isotopologue dominated’ sources where the 29SiO transitions are the brightest in the 43 GHz spectrum. Finally, using Optical Gravitational Lensing Experiment (OGLE) light curves of our maser stars, changes in line ratios as a function of stellar phase are discussed.

Keywords

SiO masersasymptotic giant branch starsstellar variabilitycircumstellar envelopes
Type
Contributed 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. 314 - 318
Check for updates
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

Alcolea, J., Bujarrabal, V., & Gomez-Gonzalez, J. 1990, A&A, 231, 431 Google Scholar
Cho, S.-H. & Ukita, N. 1995, PASJ, 47, 1 Google Scholar
Desmurs, J. F., Bujarrabal, V., Lindqvist, M., Alcolea, J., Soria-Ruiz, R., & Bergman, P. 2014, A&A, 565, A127 Google Scholar
Dike, V., Morris, M. R., Rich, R. M., Lewis, M. O., Quiroga-Nuñez, L. H., Stroh, M. C., Trapp, A. C., & Claussen, M. J. 2021, AJ, 161, 111 10.3847/1538-3881/abd479CrossRefGoogle Scholar
Lewis, M. O., Pihlström, Y. M., Sjouwerman, L. O., & Quiroga-Nuñez, L. H. 2020, ApJ, 901, 98 10.3847/1538-4357/abaf46CrossRefGoogle Scholar
Nyman, L. A., Hall, P. J., & Le Bertre, T. 1993, A&A, 280, 551 Google Scholar
Rizzo, J. R., Cernicharo, J., & Garcia-Miro, C. 2021, ApJS, 253, 44 10.3847/1538-4365/abe469CrossRefGoogle Scholar
Sobolev, A. M., Ladeyschikov, D. A., & Nakashima, J 2019, Research in Astronomy and Astrophysics, 19, 34 10.1088/1674-4527/19/3/34CrossRefGoogle Scholar
Stroh, M. C., Pihlström, Y. M., Sjouwerman, L. O., Lewis, M. O., Claussen, M. J., Morris, M. R., & Rich, R. M. 2019, ApJS, 244, 25 10.3847/1538-4365/ab3c35CrossRefGoogle Scholar