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Stellar populations in the BAaDE survey

Published online by Cambridge University Press:  14 May 2020

Megan O. Lewis Open the ORCID record for Megan O. Lewis [Opens in a new window] ,
Ylva M. Pihlström ,
Loránt O. Sjouwerman ,
Michael C. Stroh  and
the BAaDE team
Megan O. Lewis
Affiliation:
Department of Physics and Astronomy, University of New Mexico, 1919 Lomas Blvd., Albuquerque, NM, USA email: [email protected] National Radio Astronomy Observatory, P. O. Box O, Socorro, NM, USA
Ylva M. Pihlström
Affiliation:
Department of Physics and Astronomy, University of New Mexico, 1919 Lomas Blvd., Albuquerque, NM, USA email: [email protected]
Loránt O. Sjouwerman
Affiliation:
National Radio Astronomy Observatory, P. O. Box O, Socorro, NM, USA
Michael C. Stroh
Affiliation:
Department of Physics and Astronomy, University of New Mexico, 1919 Lomas Blvd., Albuquerque, NM, USA email: [email protected]
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Abstract

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The BAaDE (Bulge Asymmetries and Dynamical Evolution) project is an SiO maser survey of the Galactic Plane. About 19,000 sources have been observed at 43 GHz with the VLA, and the production of spectra for each of these sources is well underway. The primary goal of the project is to collect line-of-sight velocities for all the detected masers in the sample to probe Galactic dynamics. With an expected detection rate of over 60% we should collect over 11,000 velocities to probe the Galactic potential. The survey is also a large sample of infrared sources to explore the different evolved stellar populations within the Milky Way. So far we discern three distinct groups in the BAaDE sample: the main group containing oxygen-rich, evolved stars with a high SiO maser detection rate, a much smaller population of carbon-rich evolved stars, and finally a group of likely young stellar objects with no maser emission. These populations are separated using 2MASS and MSX color-color diagrams, and we find a particularly useful cut between the young and evolved objects using the MSX [D] –[E] color. Identification of these populations will isolate BAaDE’s evolved star sample, and will more tightly define the region in IR color-color diagrams where SiO masers occur yielding a better understanding of these kinematical probes. Using our color-divisions we can also study the distribution of each of the populations within the Galactic Plane.

Keywords

Galaxy: stellar contentstars: AGB and post-AGBmasers
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S353: Galactic Dynamics in the Era of Large Surveys , June 2019 , pp. 43 - 44
Copyright
© International Astronomical Union 2020

References

Egan, M. P., Price, S. D., Kraemer, K. E., et al. 2003, The Midcourse Space Experiment Point Source Catalog, Version 2.3 (October 2003), Air Force Research Laboratory Technical Report AFRL-VS-TR-2003-1589 (Springfield, VA: NTIS)CrossRefGoogle Scholar
Lumsden, S. L., Hoare, M. G., Oudmaijer, R. D., & Richards, D. 2002, MNRAS, 336, 621CrossRefGoogle Scholar
Sjouwerman, L.O., Capen, S., & Claussen, M.J. 2009, ApJ, 705, 155410.1088/0004-637X/705/2/1554CrossRefGoogle Scholar
van der Veen, W. E. C. J. & Habing, H. J. 1988, A&A, 194, 125Google Scholar