Fermi Large Area Telescope Observations of Pulsar Wind Nebulae
Fermi Large Area Telescope Observations of Pulsar Wind Nebulae
Fermi Large Area Telescope Observations of Pulsar Wind Nebulae
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LAT <strong>Observations</strong> <strong>of</strong> Vela X (spectrum)• As noted by de Jager et al. (2008, ApJ, 689, L125), the SED strongly favors a twocomponentleptonic model• Hadronic model is disfavoured• SEDs were computed from evolving power-law electron populations, one eachfor the X-ray/VHE-peak cocoon and radio/MeV-peak halo:– Halo : This region requires a 130 GeV exponential cut-<strong>of</strong>f controlledby the cut-<strong>of</strong>f <strong>of</strong> the injected spectrum– Cocoon :• Synchrotron/Comptonpeak ratio <strong>of</strong> the cocoonimplies a B=4µG with smalluncertainty• This region requires a 600TeV exponential cut-<strong>of</strong>fcontrolled by the coolingbreakMultiwavelength spectrum <strong>of</strong> Vela XSee also A. Pellizzoni & F. Mattana's talks today(Abdo et al., 2010, ApJ, 713, 146)M.-H. Grondin, High-Energy Emission from <strong>Pulsar</strong>s and their Systems, April 2010 16
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