Hostname: page-component-586b7cd67f-l7hp2 Total loading time: 0 Render date: 2024-11-26T09:06:38.101Z Has data issue: false hasContentIssue false

Possible Detection of Quasi-Periodic Oscillations from Sgr A* at 43 GHz

Published online by Cambridge University Press:  09 February 2017

Yuhei Iwata
Affiliation:
Department of Physics, Faculty of Science and Technology, Keio University, 3-14-1 Hiyoshi, Kohoku-ku, Yokohama, Kanagawa, Japan email: [email protected]
Tomoharu Oka
Affiliation:
Department of Physics, Faculty of Science and Technology, Keio University, 3-14-1 Hiyoshi, Kohoku-ku, Yokohama, Kanagawa, Japan email: [email protected]
Makoto Miyoshi
Affiliation:
National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo, Japan
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.

Quasi-periodic oscillations (QPOs) are believed to be indirect evidence for black holes. Several authors have reported detections of QPOs from Sgr A*, the nucleus of our Galaxy, in infrared and X-ray wavelength during flare-ups. Miyoshi et al. (2011) reported a tentative detection of QPOs in the 43 GHz light curve of Sgr A* obtained with the Very Long Baseline Array (VLBA). To confirm their detection, we reanalysed their VLBA data very conservatively. The 43 GHz flux was calculated for every 15 seconds by assuming a two-dimensional Gaussian-shape spatial structure. The Lomb-Scargle periodogram of the 43 GHz flux just after a millimeter wave flare of Sgr A*, shows three apparent peaks at 10.2, 14.6 and 32.1 min. Two of them are barely consistent with the previously reported QPOs. Using the resonant oscillation model, we estimated the spin parameter of the Sgr A* black hole to be 0.56 assuming the mass of 4.3 × 106M.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2017 

References

Ghez, A. M., Salim, S., Weinberg, N. N., et al. 2008, ApJ, 689, 1044 Google Scholar
Gillessen, S., Eisenhauer, F., Trippe, S., et al. 2009, ApJ, 692, 1075 Google Scholar
Genzel, R., Schödel, R., Ott, T., et al. 2003, Nature, 425, 934 CrossRefGoogle Scholar
Yusef-Zadeh, F., Roberts, D., Wardle, M., Heinke, C. O., & Bower, G. C. 2006, ApJ, 650, 189 Google Scholar
Kato, S. & Fukue, J. 2006, PASJ, 58, 909 CrossRefGoogle Scholar
Miyoshi, M., Shen, Z.-Q., Oyama, T., Takahashi, R., & Kato, Y. 2011, PASJ, 63, 1093 Google Scholar
Miyazaki, A., Shen, Z.-Q., Miyoshi, M., Tsuboi, M., & Tsutsumi, T. 2006, in: Schödel, R., Bower, G. C., Muno, M. P., Nayakshin, S. & Ott, T. (eds.), J. Phys. Conf. Ser., 54, 363 Google Scholar
Bower, G. C., Falcke, H., Herrnstein, R. M., et al. 2004, Science, 304, 704 Google Scholar
Scargle, J. D. 1982, ApJ, 263, 835 CrossRefGoogle Scholar
Kato, Y., Miyoshi, M., Takahashi, R., Negoro, H., & Matsumoto, R. 2010, MNRAS, 403, L74 Google Scholar