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The Pulsar Wind Nebula (PWN) 3C 58 is energized by one of the highestspin-down power pulsars known (5% of Crab pulsar) and it has been compared tothe Crab Nebula due to their morphological similarities. This object wasdetected by Fermi-LAT with a spectrum extending beyond 100 GeV. We analyzed 81hours of 3C 58 data taken with the MAGIC telescopes and we detected VHEgamma-ray emission for the first time at TeV energies with a significance of5.7 sigma and an integral flux of 0.65% C.U. above 1 TeV. The differentialenergy spectrum between 400 GeV and 10 TeV is well described by a power-lawfunction $d\Phi/dE=f_{o}(E/1TeV)^{-\Gamma}$ with$f_{o}=(2.0\pm0.4stat\pm0.6sys) 10^{-13}cm^{-2}s^{-1}TeV^{-1}$ and$\Gamma=2.4\pm0.2sta\pm0.2sys$. This leads 3C 58 to be the least luminous PWNever detected at VHE and the one with the lowest flux at VHE to date. Accordingto time-dependent models in which electrons up-scatter photon fields, the bestrepresentation favors a distance to the PWN of 2 kpc and FIR comparable to CMBphoton fields. If we consider an unexpectedly high FIR density, the data canalso be reproduced by models assuming a 3.2 kpc distance. A low magnetic field,far from equipartition, is required to explain the VHE data. Hadroniccontribution from the hosting supernova remnant (SNR) requires unrealisticenergy budget given the density of the medium, disfavoring cosmic rayacceleration in the SNR as origin of the VHE gamma-ray emission.

Discovery of TeV gamma-ray emission from the Pulsar Wind Nebula 3C 58 by MAGIC