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SWAG Water Masers in the Galactic Center

MPG-Autoren

Ott,  Jürgen
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Krieger,  Nico
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Rickert,  Matthew
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Meier,  David
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Ginsburg,  Adam
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Yusef-Zadeh,  Farhad
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Team,  SWAG
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Externe Ressourcen

https://ui.adsabs.harvard.edu/abs/2018IAUS..336..172O
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Zitation

Ott, J., Krieger, N., Rickert, M., Meier, D., Ginsburg, A., Yusef-Zadeh, F., et al. (2018). SWAG Water Masers in the Galactic Center.


Zitierlink: https://hdl.handle.net/21.11116/0000-0005-CBDE-D
Zusammenfassung
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.