Speaker
Description
We investigate the origin of unidentified, extended TeV source 1LHAASO J0500+4454, considering three possible origins: cosmic rays interacting with a molecular cloud (MC), particles accelerated in a currently undetected supernova remnant (SNR), and an energetic outflow powered by a pulsar.
Upper limits on the CO and X-ray emission from the $\gamma$-ray emitting region disfavor the MC and SNR scenarios, respectively.
If a nebula of inverse Compton scattering $e^{\pm}$ powers 1LHAASO J0500+4454,
then SED modeling indicates that the current particle energy in the nebula is $\sim 10^{48}$~erg.
If the coincident magnetar \psr's rotational energy powered 1LHAASO J0500+4454, then a conservative energy budget calculation requires an initial magnetar spin period $P_{0} \lesssim 10$~ms and a spin-down timescale $\tau_{\rm sd} \lesssim 30$~yr, which has implications for the origins of magnetars.
Furthermore, if 1LHAASO J0500+4454's age is similar to the magnetar's characteristic age, then it was likely a PeVatron at birth.
