Hostname: page-component-78c5997874-lj6df Total loading time: 0 Render date: 2024-11-10T16:39:13.866Z Has data issue: false hasContentIssue false
  • English
  • Français

Probing Sagittarius A* accretion with ALMA

Published online by Cambridge University Press:  09 February 2017

Elena Murchikova
Elena Murchikova*
Affiliation:
TAPIR, California Institute of Technology, MC 350-17, Pasadena, CA 91125, USA email: lena@caltech.edu
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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~ 104 K) at 2 × 10−3M⊙. This is the unique probe of gas cooler than T ~106 K traced by X-ray emission. The total amount of gas near SgrA* gives us clues to understanding the accretion rate of SgrA*.

Keywords

Galaxy: centerISM: lines and bandsblack hole physics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S322: The Multi-Messenger Astrophysics of the Galactic Centre , July 2016 , pp. 21 - 24
Copyright
Copyright © International Astronomical Union 2017 

References

Scoville, N. & Murchikova, E. 2013, ApJ, 779, 75 CrossRefGoogle Scholar
Ghez, A. et al. 2000, Nature, 407, 349 CrossRefGoogle Scholar
Schödel, R., Merritt, D., & Eckart, A. 2009, A&A, 502, 91 Google Scholar
Genzel, R. et al. 2010, Rev Mod Phys, 82, 3121 CrossRefGoogle Scholar
Melia, F. & Falcke, H. 2001, ARAA, 39, 309 CrossRefGoogle Scholar
Russell, C. M. P., Wang, Q. D., & Cuadra, J. 2016, arXiv:1607.01562Google Scholar