Published February 9, 2017
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Probing Sagittarius A* accretion with ALMA
- Creators
- Murchikova, Elena M.
Chicago
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Abstract
The submm Hydrogen recombination line technique can be used as a probe of the Galactic Center. We present the results of our H30α observations of ionized gas from within 0.015 pc around SgrA*. The observations were obtained on ALMA in cycle 3. The line was not detected, but we were able to set a limit on the mass of the cool gas (T~ 10^4 K) at 2 × 10^(-3)M⊙. This is the unique probe of gas cooler than T ~10^6 K traced by X-ray emission. The total amount of gas near SgrA* gives us clues to understanding the accretion rate of SgrA*.
Additional Information
© 2017 International Astronomical Union. Published online: 09 February 2017. I am grateful to Nick Scoville, Jin Koda, Yuri Levin and Sterl Phinney for discussion and to Dr. David and Barbara Groce for their kindness and support. This paper makes use of the following ALMA data: ADS/JAO.ALMA# 2015.1.00311.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ.Attached Files
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Additional details
- Eprint ID
- 74541
- Resolver ID
- CaltechAUTHORS:20170227-092825764
- Created
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2017-02-27Created from EPrint's datestamp field
- Updated
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2021-11-11Created from EPrint's last_modified field
- Caltech groups
- TAPIR
- Series Name
- Proceedings of the International Astronomical Union
- Series Volume or Issue Number
- 322