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SWAG Water Masers in the Galactic Center

Published online by Cambridge University Press:  16 July 2018

Jürgen Ott
Affiliation:
National Radio Astronomy Observatory, 1003 Lopezville Road, Socorro, NM 87801, USA email: jott@nrao.edu
Nico Krieger
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, 69120 Heidelberg, Germany email: krieger@mpia.de
Matthew Rickert
Affiliation:
Department of Physics and Astronomy and CIERA, Northwestern University, Evanston, IL 60208, USA;
David Meier
Affiliation:
New Mexico Institute of Mining and Technology, 801 Leroy Place, Socorro, NM 87801, USA email David.Meier@nmt.edu;
Adam Ginsburg
Affiliation:
National Radio Astronomy Observatory, 1003 Lopezville Road, Socorro, NM 87801, USA email: aginsbur@nrao.edu
Farhad Yusef-Zadeh
Affiliation:
Department of Physics and Astronomy and CIERA, Northwestern University, Evanston, IL 60208, USA email: zadeh@northwestern.edu
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Abstract

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The Galactic Center contains large amounts of molecular and ionized gas as well as a plethora of energetic objects. Water masers are an extinction-insensitive probe for star formation and thus ideal for studies of star formation stages in this highly obscured region. With the Australia Telescope Compact Array, we observed 22 GHz water masers in the entire Central Molecular Zone with sub-parsec resolution as part of the large SWAG survey: “Survey of Water and Ammonia in the Galactic Center”. We detect of order 600 22 GHz masers with isotropic luminosities down to ~10−7 L. Masers with luminosities of ≳10−6 L are likely associated with young stellar objects. They appear to be close to molecular gas streamers and may be due to star formation events that are triggered at pericenter passages near Sgr A*. Weaker masers are more widely distributed and frequently show double line features, a tell-tale sign for an origin in evolved star envelopes.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2018 

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