Discovery of GeV gamma-ray emission from PWN Kes 75 and PSR J1846-0258

Abstract

We report the detection of gamma-ray emission from PWN Kes 75 and PSR J1846-0258. Through modeling the spectral energy distribution incorporating the new Fermi-LAT data, we find the the observed gamma-ray emission is likely a combination of both the PWN and pulsar magnetosphere. The spectral shape of this magnetospheric emission is similar to the gamma-ray spectrum of rotation powered pulsars detected by Fermi-LAT and the results from our best-fit model suggest the pulsar's magnetospheric emission accounts for 1% of the current spin-down luminosity. Prior works attempted to characterize the properties of this system and found a low supernova explosion energy and low SN ejecta mass. We re-analyze the broadband emission incorporating the new Fermi emission and compare the implications of our results to prior reports. The best-fit gamma-ray emission model suggests a second very hot photon field possibly generated by the stellar wind of a Wolf-Rayet star embedded within the nebula, which supports the low ejecta mass found for the progenitor in prior reports and here in the scenario of binary mass transfer.

arXiv commentAccepted for publication in ApJ. 10 pages, 5 figures, 2 tables

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• Searching for Magnetar Binaries Disrupted by Core-Collapse Supernovae
• Broadband X-ray Spectroscopy of the Pulsar Wind Nebula in HESS J1640-465
• Fermi-LAT Gamma-ray Emission Discovered from the Composite Supernova Remnant B0453-685 in the Large Magellanic Cloud
• Spatio-spectral-temporal Modelling of Two Young Pulsar Wind Nebulae
• NuSTAR and XMM-Newton Observations of PSR J1930+1852 and Its Pulsar Wind Nebula