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SWAG: Distribution and Kinematics of an Obscured AGB Population toward the Galactic Center

Published online by Cambridge University Press:  30 December 2019

Jürgen Ott Open the ORCID record for Jürgen Ott [Opens in a new window] ,
David S. Meier ,
Adam Ginsburg ,
Farhad Yusef-Zadeh ,
Nico Krieger  and
Cornelia Jäschke
Jürgen Ott
Affiliation:
National Radio Astronomy Observatory, 1003 Lopezville Road, Socorro, NM 87801, USA emails: [email protected], [email protected] New Mexico Institute of Mining and Technology, 801 Leroy Place, Socorro, NM 87801, USA email: [email protected]
David S. Meier
Affiliation:
National Radio Astronomy Observatory, 1003 Lopezville Road, Socorro, NM 87801, USA emails: [email protected], [email protected] New Mexico Institute of Mining and Technology, 801 Leroy Place, Socorro, NM 87801, USA email: [email protected]
Adam Ginsburg
Affiliation:
National Radio Astronomy Observatory, 1003 Lopezville Road, Socorro, NM 87801, USA emails: [email protected], [email protected]
Farhad Yusef-Zadeh
Affiliation:
Department of Physics and Astronomy and CIERA, Northwestern University, Evanston, IL 60208, USA email: [email protected]
Nico Krieger
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, 69120 Heidelberg, Germany emails: [email protected], [email protected]
Cornelia Jäschke
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, 69120 Heidelberg, Germany emails: [email protected], [email protected]
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Abstract

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Outflows from AGB stars enrich the Galactic environment with metals and inject mechanical energy into the ISM. Radio spectroscopy can recover both properties through observations of molecular lines. We present results from SWAG: “Survey of Water and Ammonia in the Galactic Center”. The survey covers the entire Central Molecular Zone (CMZ), the inner 3.35° × 0.9° (∼480 × 130 pc) of the Milky Way that contains 5 × 107 M⊙ of molecular gas. Although our survey primarily targets the CMZ, we observe across the entire sightline through the Milky Way. AGB stars are revealed by their signature of double peaked 22 GHz water maser lines. They are distinguished by their spectral signatures and their luminosities, which reach up to 10−7 L⊙. Higher luminosities are usually associated with Young Stellar Objects located in CMZ star forming regions. We detect a population of ∼600 new water masers that can likely be associated with AGB outflows.

Keywords

stars: AGB and post-AGBISM: moleculesGalaxy: centerradio lines: stars
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. 485 - 486
Copyright
© International Astronomical Union 2019 

References

Jäschke, C. 2018, BS Thesis, University of Heidelberg, Germany Google Scholar
Krieger, N. et al. ApJ, 2017, 850, 77 CrossRefGoogle Scholar
Rickert, M. 2017, PhD Thesis, University of Illinois, USAGoogle Scholar