We report the detection of high-energy γ-ray emission from the young and energetic pulsar PSR B1509 – 58 and its pulsar wind nebula (PWN) in the composite supernova remnant G320.4 – 1.2 (aka MSH 15 – 52). Using 1 yr of survey data with the Fermi-Large Area Telescope (LAT), we detected pulsations from PSR B1509 – 58 up to 1 GeV and extended γ-ray emission above 1 GeV spatially coincident with the PWN. The pulsar light curve presents two peaks offset from the radio peak by phases 0.96 ± 0.01 and 0.33 ± 0.02. New constraining upper limits on the pulsar emission are derived below 1 GeV and confirm a severe spectral break at a few tens of MeV. The nebular spectrum in the 1-100 GeV energy range is well described by a power law with a spectral index of (1.57 ± 0.17 ± 0.13) and a flux above 1 GeV of (2.91 ± 0.79 ± 1.35) × 10–9 cm–2 s–1. The first errors represent the statistical errors on the fit parameters, while the second ones are the systematic uncertainties. The LAT spectrum of the nebula connects nicely with Cherenkov observations, and indicates a spectral break between GeV and TeV energies.

DETECTION OF THE ENERGETIC PULSAR PSR B1509-58 AND ITS PULSAR WIND NEBULA IN MSH 15-52 USING THE FERMI-LARGE AREA TELESCOPE

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

Abstract

We report the detection of high-energy γ-ray emission from the young and energetic pulsar PSR B1509 – 58 and its pulsar wind nebula (PWN) in the composite supernova remnant G320.4 – 1.2 (aka MSH 15 – 52). Using 1 yr of survey data with the Fermi-Large Area Telescope (LAT), we detected pulsations from PSR B1509 – 58 up to 1 GeV and extended γ-ray emission above 1 GeV spatially coincident with the PWN. The pulsar light curve presents two peaks offset from the radio peak by phases 0.96 ± 0.01 and 0.33 ± 0.02. New constraining upper limits on the pulsar emission are derived below 1 GeV and confirm a severe spectral break at a few tens of MeV. The nebular spectrum in the 1-100 GeV energy range is well described by a power law with a spectral index of (1.57 ± 0.17 ± 0.13) and a flux above 1 GeV of (2.91 ± 0.79 ± 1.35) × 10–9 cm–2 s–1. The first errors represent the statistical errors on the fit parameters, while the second ones are the systematic uncertainties. The LAT spectrum of the nebula connects nicely with Cherenkov observations, and indicates a spectral break between GeV and TeV energies.
2010
Abdo, Aa; Ackermann, M; Ajello, M; Allafort, A; Asano, K; Baldini, Luca; Ballet, J; Barbiellini, G; Baring, Mg; Bastieri, D; Bechtol, K; Bellazzini, R; Berenji, B; Blandford, Rd; Bloom, Ed; Bonamente, E; Borgland, Aw; Bregeon, J; Brez, A; Brigida, M; Bruel, P; Buson, S; Caliandro, Ga; Cameron, Ra; Camilo, F; Caraveo, Pa; Carrigan, S; Casandjian, Jm; Cecchi, C; Celik, O; Chekhtman, A; Cheung, Cc; Chiang, J; Ciprini, S; Claus, R; Cohen Tanugi, J; Conrad, J; den Hartog, Pr; Dermer, Cd; de Luca, A; de Palma, F; Dormody, M; Silva, Ede; Drell, Ps; Dubois, R; Dumora, D; Farnier, C; Favuzzi, C; Fegan, Sj; Ferrara, Ec; Focke, Wb; Frailis, M; Fukazawa, Y; Funk, S; Fusco, P; Gargano, F; Gehrels, N; Germani, S; Giglietto, N; Giordano, F; Glanzman, T; Godfrey, G; Gotthelf, Ev; Grenier, Ia; Grondin, Mh; Grove, Je; Guillemot, L; Guiriec, S; Hanabata, Y; Harding, Ak; Hays, E; Hobbs, G; Horan, D; Hughes, Re; Johannesson, G; Johnson, As; Johnson, Tj; Johnson, Wn; Johnston, S; Kamae, T; Kanai, Y; Kanbach, G; Katagiri, H; Kataoka, J; Kawai, N; Keith, M; Kerr, M; Knodlseder, J; Kuss, M; Lande, J; Latronico, L; Lemoine Goumard, M; Garde, Ml; Longo, F; Loparco, F; Lott, B; Lovellette, Mn; Lubrano, P; Makeev, A; Manchester, Rn; Marelli, M; Mazziotta, Mn; Mcenery, Je; Michelson, Pf; Mitthumsiri, W; Mizuno, T; Moiseev, Aa; Monte, C; Monzani, Me; Morselli, A; Moskalenko, Iv; Murgia, S; Nakamori, T; Nolan, Pl; Norris, Jp; Nuss, E; Ohno, M; Ohsugi, T; Omodei, N; Orlando, E; Ormes, Jf; Paneque, D; Panetta, Jh; Parent, D; Pelassa, V; Pepe, M; Pesce Rollins, M; Piron, F; Porter, Ta; Raino, S; Rando, R; Razzano, Massimiliano; Rea, N; Reimer, A; Reimer, O; Reposeur, T; Rodriguez, Ay; Romani, Rw; Roth, M; Ryde, F; Sadrozinski, Hfw; Sander, A; Parkinson, Pms; Sgro, C; Siskind, Ej; Smith, Da; Smith, Pd; Spandre, G; Spinelli, P; Starck, Jl; Strickman, Ms; Suson, Dj; Takahashi, H; Takahashi, T; Tanaka, T; Thayer, Jb; Thayer, Jg; Thompson, Dj; Thorsett, Se; Tibaldo, L; Torres, Df; Tosti, G; Tramacere, A; Uchiyama, Y; Usher, Tl; Vasileiou, V; Venter, C; Vilchez, N; Vitale, V; Waite, Ap; Wang, P; Weltevrede, 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/11568/194819
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