日本語
 
Help Privacy Policy ポリシー/免責事項
  詳細検索ブラウズ

アイテム詳細


公開

会議論文集

SWAG Water Masers in the Galactic Center

MPS-Authors

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;

External Resource
Fulltext (restricted access)
There are currently no full texts shared for your IP range.
フルテキスト (公開)
公開されているフルテキストはありません
付随資料 (公開)
There is no public supplementary material available
引用

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


引用: https://hdl.handle.net/21.11116/0000-0005-CBDE-D
要旨
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.