Constraining the Outburst Properties of the SMBH in Fornax A through X-ray, Infrared, and Radio Observations

Details Constraining the Outburst Properties of the SMBH in Fornax A through X-ray, Infrared, and Radio Observations Constraining the Outburst Properties of the SMBH in Fornax A through X-ray, Infrared, and Radio Observations

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009cfdd.confe.141l&link_type=abstract

Chandra's First Decade of Discovery, Proceedings of the conference held 22-25 September, 2009 in Boston, MA. Edited by Scott Wo

Physics

Agn Jets

Scientific paper

Combined Chandra, Spitzer, XMM-Newton, and VLA observations of the giant radio galaxy NGC 1316 (Fornax A) show features indicative of an AGN outburst likely triggered by a merger with a galaxy with a stellar mass of 0.9-7.8×10^{10} solar masses about 0.4 Gyr ago. X-ray cavities in the Chandra and XMM-Newton images likely result from the radio jet and the expansion of the radio lobes. The dust emission seen at wavelengths longer than 4.5 microns is strongest in the regions with little or no radio emission, suggesting that the expanding radio plasma removes or destroys the dust as well as the hot gas. These results constrain properties of the outburst and the merger galaxy. The size of the X-ray cavities implies a minimum outburst energy of 1.2×10^{58} ergs. The present size of the radio lobes implies that the outburst is at least 0.4 Gyr old. The inferred dust mass implies that the merger galaxy was a late-type spiral with a stellar mass of 0.9-7.8×10^{10} solar masses and a gas mass of 0.4-4.4×10^{10} solar masses.

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