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

• Published in: The Astrophysical journal Vol. 721; no. 2; pp. 1702 - 1713
• Main Authors: Lanz, Lauranne, Jones, Christine, Forman, William R, Ashby, Matthew L. N, Kraft, Ralph, Hickox, Ryan C
• Format: Journal Article
• Language: English
• Published: Bristol IOP Publishing 01.10.2010; IOP
• Subjects: Astronomy; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; BOLOMETERS; COSMIC RADIO SOURCES; COSMIC RAY SOURCES; COSMIC X-RAY SOURCES; Earth, ocean, space; ENERGY SPECTRA; Exact sciences and technology; GALAXIES; LUMINOSITY; MEASURING INSTRUMENTS; MORPHOLOGY; OPTICAL PROPERTIES; PHYSICAL PROPERTIES; PLASMA; RADIO GALAXIES; RELATIVISTIC PLASMA; SPECTRA; X-RAY GALAXIES; infrared: galaxies; X-ray galaxies; VLA observation; X-rays: galaxies; Spectral energy distribution; Cosmic x-ray sources; Luminosity; Radio observation; Continuum; Late type galaxies; Giant galaxies; galaxies: active; Active galaxy nuclei; Galaxy nuclei; Cosmic radio sources; Radio lobe; Age; Radio galaxies; Infrared observation; Active galaxies; Radio emission; galaxies: structure; Relativistic plasma; Stellar mass; Galaxy structure; Morphology; galaxies: individual (NGC 1316); Jets; Infrared galaxies; Spiral galaxies; X ray emission; radio continuum: galaxies
• ISSN: 0004-637X; 1538-4357
• DOI: 10.1088/0004-637X/721/2/1702

Combined Spitzer, Chandra, XMM-Newton, and VLA observations of the giant radio galaxy NGC 1316 (Fornax A) show a radio jet and X-ray cavities from active galactic nucleus (AGN) outbursts most likely triggered by a merger with a late-type galaxy at least 0.4 Gyr ago. We detect a weak nucleus with a spectral energy distribution typical of a low-luminosity AGN with a bolometric luminosity of 2.4 x 10{sup 42} erg s{sup -1}. We examine the Spitzer IRAC and MIPS images of NGC 1316. We find that the dust emission is strongest in regions with little or no radio emission and that the particularly large infrared luminosity relative to the galaxy's K-band luminosity implies an external origin for the dust. The inferred dust mass implies that the merger spiral galaxy had a stellar mass of (1-6) x10{sup 10} M{sub sun} and a gas mass of (2-4) x10{sup 9} M{sub sun}. X-ray cavities in the Chandra and XMM-Newton images likely result from the expansion of relativistic plasma ejected by the AGN. The soft (0.5-2.0 keV) Chandra images show a small {approx}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. Current radio observations do not show emission within these cavities. The radio lobes lie at radii of 14.'3 (93.3 kpc) and 15.'6 (101 kpc), more distant from the nucleus than the detected X-ray cavities. The relative morphology of the large scale 1.4 GHz and X-ray emission suggests they were products of two distinct outbursts, an earlier one creating the radio lobes and a later one producing the X-ray cavities. Alternatively, if a single outburst created both the X-ray cavities and the radio lobes, this would require that the radio morphology is not fully defined by the 1.4 GHz emission. For the more likely two outbursts scenarios, we use the buoyancy rise times to estimate an age for the more recent outburst that created the X-ray cavities of 0.1 Gyr and the PV work done by the expanding plasma that created the X-ray cavities to estimate the outburst's energy to be 10{sup 58} erg. The present size and location of the radio lobes imply that the outburst that created them happened {approx}0.4 Gyr ago and released {approx}5 x 10{sup 58} erg.