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Probing Sagittarius A* accretion with ALMA

Murchikova, Elena M. (2017) Probing Sagittarius A* accretion with ALMA. In: The Multi-Messenger Astrophysics of the Galactic Centre. Proceedings of the International Astronomical Union. No.322. Cambridge University Press , Cambridge, pp. 21-24. ISBN 9781107169890. http://resolver.caltech.edu/CaltechAUTHORS:20170227-092825764

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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*.


Item Type:Book Section
Related URLs:
URLURL TypeDescription
https://doi.org/10.1017/S174392131601214XDOIArticle
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.
Group:TAPIR
Subject Keywords:Galaxy: center, ISM: lines and bands, black hole physics
Record Number:CaltechAUTHORS:20170227-092825764
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20170227-092825764
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:74541
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:27 Feb 2017 18:03
Last Modified:08 Jun 2018 16:54

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