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SWAG Water Masers in the Galactic Center

Published online by Cambridge University Press:  16 July 2018

Jürgen Ott ,
Nico Krieger ,
Matthew Rickert ,
David Meier ,
Adam Ginsburg ,
Farhad Yusef-Zadeh  and
the SWAG team
Jürgen Ott
Affiliation:
National Radio Astronomy Observatory, 1003 Lopezville Road, Socorro, NM 87801, USA email: [email protected]
Nico Krieger
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, 69120 Heidelberg, Germany email: [email protected]
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 [email protected];
Adam Ginsburg
Affiliation:
National Radio Astronomy Observatory, 1003 Lopezville Road, Socorro, NM 87801, USA email: [email protected]
Farhad Yusef-Zadeh
Affiliation:
Department of Physics and Astronomy and CIERA, Northwestern University, Evanston, IL 60208, USA email: [email protected]
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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.

Keywords

masersGalaxy: centerradio lines: stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S336: Astrophysical Masers: Unlocking the Mysteries of the Universe , September 2017 , pp. 172 - 175
Copyright
Copyright © International Astronomical Union 2018 

References

Ginsburg, A., Walsh, A., Henkel, C., et al. 2015, A&A, 584, L7Google Scholar
Ginsburg, A., Henkel, C., Ao, Y., et al. 2016, A&A, 586, A50Google Scholar
Henshaw, J. D., Longmore, S. N., & Kruijssen, J. M. D., 2016, MNRAS, 463, L122Google Scholar
Krieger, N., et al., 2017, ApJ, 850, 77Google Scholar
Kruijssen, J. M. D., Dale, J. E., & Longmore, S. N., 2015, MNRAS, 447, 1059Google Scholar
Liljestrom, T., Mattila, K., Toriseva, M., & Anttila, R., 1989, A&AA, 79, 19Google Scholar
Lo, K. Y., 2005, ARA&A, 43, 625Google Scholar
Longmore, S. N., Kruijssen, J. M. D., Bally, J., et al. 2013, MNRAS, 433, L15Google Scholar
Molinari, S., Bally, J., Noriega-Crespo, A., et al. 2011, ApJL, 735, L33Google Scholar
Palagi, F., Cesaroni, R., Comoretto, G., Felli, M., & Natale, V., 1993, A&AS, 101, 153Google Scholar
Rickert, M. 2017, Ph.D. Thesis, Northwestern UniversityGoogle Scholar
Ridley, M. G. L., Sormani, M. C., Treß, R. G., Magorrian, J., & Klessen, R. S., 2017, MNRAS, 469, 2251Google Scholar
Yusef-Zadeh, F., Hewitt, J. W., Arendt, R. G., et al. 2009, ApJ, 702, 178Google Scholar