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Combined Spitzer, Chandra, XMM-Newton, and VLA observations of the giantradio galaxy NGC 1316 (Fornax A) show a radio jet and X-ray cavities from AGNoutbursts likely triggered by a merger with a late-type galaxy at least 0.4 Gyrago. We detect a weak nucleus with an SED typical of a low-luminosity AGN witha bolometric luminosity of 2.4x10^42 erg/s. The Spitzer IRAC and MIPS imagesshow dust emission strongest in regions with little or no radio emission. Thelarge infrared luminosity relative to the galaxy's K-band luminosity implies anexternal origin for the dust. The dust mass implies that the merger spiralgalaxy had a stellar mass of 1-6x10^10 M_sun and a gas mass of 2-4x10^9 M_sun.Chandra images show a small ~15"(1.6 kpc) cavity coincident with the radio jet,while the XMM-Newton image shows two large X-ray cavities lying 320"(34.8 kpc)east and west of the nucleus, each approximately 230"(25 kpc) in radius. Theradio lobes lie at radii of 14.3'(93 kpc) and 15.6'(101 kcp), more distant fromthe nucleus than the detected X-ray cavities. The relative morphology of thelarge scale 1.4 GHz and X-ray emission suggests they were products of twodistinct outbursts, an earlier one creating the radio lobes and a later oneproducing the X-ray cavities. Alternatively, if a single outburst created boththe X-ray cavities and the radio lobes, this would require that the morphologyis not fully defined by the 1.4 GHz emission. For the more likely two outburstscenario, we use the buoyancy rise times to estimate an age for the more recentoutburst of 0.1 Gyr and use the associated PV work done by the expanding plasmato create the X-ray cavities to estimate the outburst's energy of 10^58 ergs.The present size and location of the large radio lobes implies that the AGNoutburst that created them happened ~0.4 Gyr ago and released ~5x10^58 ergs.(abridged)

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