Fermi Large Area Telescope Observations of Pulsar Wind Nebulae

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LAT detection of PSR B1509-58(Abdo et al., 2010, ApJ, accepted, arXiv:1003.3833)• Detection of PSR B1509-58 at 4.5 σ level above 30 MeV• No pulsed signal detected above 1 GeV• Second peak at 0.34±0.02 almost aligned with COMPTEL• First peak at 0.96 ± 0.02 (not detected by COMPTEL) : harder component ?• Spectral energy distribution : consistent with the break at a few tens ofMeV as described by Kuiper et al. (1999, A&A, 351, 119)LAT profile above30 MeV1.4 GHz radioprofileLight curve (left) and spectral energy distribution (right) of PSR B1509-58See also M. Pilia's talk on tuesdayM.-H. Grondin, High-Energy Emission from Pulsars and their Systems, April 2010 18
LAT Observations of the PWN in MSH 15-52• Gamma-ray emission dominated by the nearby pulsar PSR J1509-5850below 3-4 GeV• Source spatially coincident with the PWN in MSH 15-52 (as seen in X-raysand at TeV energies) detected at a ~8 σ level above 1 GeV• Source significantly extended : R disk= (0.25 ± 0.05)°(Abdo et al., 2010, ApJ, accepted, arXiv:1003.3833)HESS contoursHESS contoursCounts maps above 1 GeV (left) and 10 GeV (right)M.-H. Grondin, High-Energy Emission from Pulsars and their Systems, April 2010 19
Page 1 and 2: Fermi-Large Area TelescopeObservati
Page 3 and 4: CGRO-EGRET (1991-2000)Compton Gamma
Page 5 and 6: Fermi-LAT 1-year catalog(Abdo et al
Page 7 and 8: Earlier γ-ray observations of the
Page 9 and 10: LAT Observations of the Crab Pulsar
Page 11 and 12: LAT Observations of the Crab Pulsar
Page 13 and 14: The Vela Pulsar: Results from the F
Page 15 and 16: LAT Observations of Vela X (spectru
Page 17: The PWN in MSH 15-52young composite
Page 21 and 22: The region of Westerlund 2• An ex
Page 23 and 24: A new PWN associated to PSR J1023-5
Page 25: Conclusions (II)• Population stud

Fermi Large Area Telescope Observations of Pulsar Wind Nebulae

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