We present γ-ray observations with the Large Area Telescope (LAT) on board the Fermi Gamma-Ray Space Telescope of the nearby radio galaxy Centaurus A (Cen A). The previous EGRET detection is confirmed, and the localization is improved using data from the first 10 months of Fermi science operation. In previous work, we presented the detection of the lobes by the LAT; in this work, we concentrate on the γ-ray core of Cen A. Flux levels as seen by the LAT are not significantly different from that found by EGRET, nor is the extremely soft LAT spectrum (Γ = 2.67 ± 0.10stat ± 0.08sys where the photon flux is Φ vprop E –Γ). The LAT core spectrum, extrapolated to higher energies, is marginally consistent with the non-simultaneous HESS spectrum of the source. The LAT observations are complemented by simultaneous observations from Suzaku, the Swift Burst Alert Telescope and X-ray Telescope, and radio observations with the Tracking Active Galactic Nuclei with Austral Milliarcsecond Interferometry program, along with a variety of non-simultaneous archival data from a variety of instruments and wavelengths to produce a spectral energy distribution (SED). We fit this broadband data set with a single-zone synchrotron/synchrotron self-Compton model, which describes the radio through GeV emission well, but fails to account for the non-simultaneous higher energy TeV emission observed by HESS from 2004 to 2008. The fit requires a low Doppler factor, in contrast to BL Lac objects which generally require larger values to fit their broadband SEDs. This indicates that the γ-ray emission originates from a slower region than that from BL Lac objects, consistent with previous modeling results from Cen A. This slower region could be a slower moving layer around a fast spine, or a slower region farther out from the black hole in a decelerating flow. The fit parameters are also consistent with Cen A being able to accelerate ultra-high energy cosmic-rays, as hinted at by results from the Auger observatory.

FERMI LARGE AREA TELESCOPE VIEW OF THE CORE OF THE RADIO GALAXY CENTAURUS A

BALDINI, LUCA;RAZZANO, MASSIMILIANO;
2010-01-01

Abstract

We present γ-ray observations with the Large Area Telescope (LAT) on board the Fermi Gamma-Ray Space Telescope of the nearby radio galaxy Centaurus A (Cen A). The previous EGRET detection is confirmed, and the localization is improved using data from the first 10 months of Fermi science operation. In previous work, we presented the detection of the lobes by the LAT; in this work, we concentrate on the γ-ray core of Cen A. Flux levels as seen by the LAT are not significantly different from that found by EGRET, nor is the extremely soft LAT spectrum (Γ = 2.67 ± 0.10stat ± 0.08sys where the photon flux is Φ vprop E –Γ). The LAT core spectrum, extrapolated to higher energies, is marginally consistent with the non-simultaneous HESS spectrum of the source. The LAT observations are complemented by simultaneous observations from Suzaku, the Swift Burst Alert Telescope and X-ray Telescope, and radio observations with the Tracking Active Galactic Nuclei with Austral Milliarcsecond Interferometry program, along with a variety of non-simultaneous archival data from a variety of instruments and wavelengths to produce a spectral energy distribution (SED). We fit this broadband data set with a single-zone synchrotron/synchrotron self-Compton model, which describes the radio through GeV emission well, but fails to account for the non-simultaneous higher energy TeV emission observed by HESS from 2004 to 2008. The fit requires a low Doppler factor, in contrast to BL Lac objects which generally require larger values to fit their broadband SEDs. This indicates that the γ-ray emission originates from a slower region than that from BL Lac objects, consistent with previous modeling results from Cen A. This slower region could be a slower moving layer around a fast spine, or a slower region farther out from the black hole in a decelerating flow. The fit parameters are also consistent with Cen A being able to accelerate ultra-high energy cosmic-rays, as hinted at by results from the Auger observatory.
2010
Abdo, Aa; Ackermann, M; Ajello, M; Atwood, Wb; Baldini, Luca; Ballet, J; Barbiellini, G; Bastieri, D; Baughman, Bm; Bechtol, K; Bellazzini, R; Berenji, B; Blandford, Rd; Bloom, Ed; Bonamente, E; Borgland, Aw; Bouvier, A; Brandt, Tj; Bregeon, J; Brez, A; Brigida, M; Bruel, P; Buehler, R; Buson, S; Caliandro, Ga; Cameron, Ra; Cannon, A; Caraveo, Pa; Carrigan, S; Casandjian, Jm; Cavazzuti, E; Cecchi, C; Celik, O; Charles, E; Chekhtman, A; Cheung, Cc; Chiang, J; Ciprini, S; Claus, R; Cohen Tanugi, J; Colafrancesco, S; Cominsky, Lr; Conrad, J; Costamante, L; Davis, Ds; Dermer, Cd; de Angelis, A; de Palma, F; do Couto e., Silva E; Drell, Ps; Dubois, R; Dumora, D; Falcone, A; Farnier, C; Favuzzi, C; Fegan, Sj; Finke, J; Focke, Wb; Fortin, P; Frailis, M; Fukazawa, Y; Funk, S; Fusco, P; Gargano, F; Gasparrini, D; Gehrels, N; Georganopoulos, M; Germani, S; Giebels, B; Giglietto, N; Giommi, P; Giordano, F; Giroletti, M; Glanzman, T; Godfrey, G; Grandi, P; Grenier, Ia; Grondin, Mh; Grove, Je; Guillemot, L; Guiriec, S; Hadasch, D; Harding, Ak; Hase, H; Hayashida, M; Hays, E; Horan, D; Hughes, Re; Itoh, R; Jackson, Ms; Johannesson, G; Johnson, As; Johnson, Tj; Johnson, Wn; Kadler, M; Kamae, T; Katagiri, H; Kataoka, J; Kawai, N; Kishishita, T; Knodlseder, J; Kuss, M; Lande, J; Latronico, L; Lee, Sh; Lemoine Goumard, M; Garde, Ml; Longo, F; Loparco, F; Lott, B; Lovellette, Mn; Lubrano, P; Makeev, A; Mazziotta, Mn; Mcconville, W; Mcenery, Je; Michelson, Pf; Mitthumsiri, W; Mizuno, T; Moiseev, Aa; Monte, C; Monzani, Me; Morselli, A; Moskalenko, Iv; Murgia, S; Muller, C; Nakamori, T; Naumann Godo, M; Nolan, Pl; Norris, Jp; Nuss, E; Ohno, M; Ohsugi, T; Ojha, R; Okumura, A; Omodei, N; Orlando, E; Ormes, Jf; Ozaki, M; Pagani, C; Paneque, D; Panetta, Jh; Parent, D; Pelassa, V; Pepe, M; Pesce Rollins, M; Piron, F; Plotz, C; Porter, Ta; Raino, S; Rando, R; Razzano, Massimiliano; Razzaque, S; Reimer, A; Reimer, O; Reposeur, T; Ripken, J; Ritz, S; Rodriguez, Ay; Roth, M; Ryde, F; Sadrozinski, Hfw; Sanchez, D; Sander, A; Scargle, Jd; Sgro, C; Siskind, Ej; Smith, Pd; Spandre, G; Spinelli, P; Starck, Jl; Stawarz, L; Strickman, Ms; Suson, Dj; Tajima, H; Takahashi, H; Takahashi, T; Tanaka, T; Thayer, Jb; Thayer, Jg; Thompson, Dj; Tibaldo, L; Torres, Df; Tosti, G; Tramacere, A; Uchiyama, Y; Usher, Tl; Vandenbroucke, J; Vasileiou, V; Vilchez, N; Vitale, V; Waite, Ap; Wang, P; Winer, Bl; Wood, Ks; Yang, Z; Ylinen, T; Ziegler, M.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11568/194936
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