Fermi LAT Discovery of Gamma-rays from the Giant Radio Lobes of Centaurus A C.C. Teddy Cheung (NRC/NRL) Lukasz Stawarz (ISAS/JAXA) Yasushi Fukazawa (Hiroshima)

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Fermi LAT Discovery of Gamma-rays from the Giant Radio Lobes of Centaurus A C.C. Teddy Cheung (NRC/NRL) Lukasz Stawarz (ISAS/JAXA) Yasushi Fukazawa (Hiroshima) Jürgen Knödlseder (CESR) on behalf of the Fermi-LAT Collaboration

Gamma-ray Imaging of a Radio Galaxy Pre-launch expectation that lobes can produce γ-rays via inverse Compton process Cen A is (uniquely) large enough to directly image with LAT -- derive physical conditions What does this mean for LAT radio galaxies (& blazars) in general? Over ½ of the total >100 MeV observed LAT flux in the lobes Feain et al. (2010) Cen A ATCA 1.4 GHz

Cen A the Radio Galaxy ☐ Nearest Radio-loud AGN Radio source extent: L~10 o At D=3.7 Mpc, L=600 kpc

Cen A the Radio Galaxy All-sky 408 MHz (Haslam et al. 1982) ☐ Nearest Radio-loud AGN Radio source extent: L~10 o At D=3.7 Mpc, L=600 kpc

Not a Complete Surprise ? ? How far does high-energy spectrum extend ?  IC/CMB γ-ray lobes? Expect L γ /L S ~ U CMB /U B ~ 1-10 Cheung 2007 (1 st GLAST symp)  LAT resolution = 0.8 O at 1GeV so can image the radio structure

Lobes detected by WMAP at GHz Page et al LAT predictions for Cen A: Hardcastle, et al WMAP LAT IC/CMB IC/EBL Expectations for Fermi LAT

Here’s what LAT sees in γ-rays Background (isotropic and diffuse) and field point sources subtracted WMAP images provided by Nils Odegard (GSFC) LAT >200 MeV WMAP 22 GHz PSF

Gamma-ray and Radio Counts Profiles South LobeNorth Lobe Regions 1 & 2 (north) and 4 & 5 (south) as defined in Hardcastle et al. 2009

Relevant Photon Fields Dominant photon fields are CMB and IR+optical extragalactic background light (EBL) CMB starlight dust EBL (various)

Inverse Compton Emission First inverse Compton (IC) lobe measurements in γ-rays! Good fits of LAT spectra with B ~ 1 μG in both lobes Approximate energy equipartition, i.e., U e /U B ~ 1 to 4 IC/CMB X-rays in radio lobes: U e /U B ~1-10 SAS-3 LAT

Inverse Compton Emission: Close-up Detected LAT emission dominated by IC/CMB component for the modeled electron energy spectra EBL component dominating at highest-energies (>GeV)

Gamma-ray probe of the EBL? Different EBL models/compilations give (only) slight differences in predicted inverse Compton gamma-ray spectrum

Inferred Physical Parameters LAT detected γ-ray emission requires TeV electrons in 100’s kpc-scale lobes that are probably accelerated in-situ Non-thermal plasma / ambient gas in approximate pressure balance Jet Calorimetry: E tot = erg radiated in both lobes over 30 Myrs Jet power ~7 x erg s -1 (~10 -5 L edd ) sub-Eddington, typical for low power radio galaxies LAT γ-ray image requires a very extended source (L~10 o in this case) – other examples?