Speaker
Description
Pulsar halos are a recent class of extended very high-energy (VHE) sources discovered by the HAWC observatory towards the Geminga and Monogem pulsars. These VHE sources are interpreted as the inverse Compton emission from electrons and positrons diffusing in the interstellar medium at an inhibited rate, having escaped the pulsar wind nebula. Our aim is to search for new pulsar halos using Imaging Atmospheric Cherenkov Telescope data - in particular on sources from the H.E.S.S. Galactic Plane Survey - and to constrain their physical properties.
Using a physically-motivated model of pulsar halos, we created template-based models of the spatial and energetic distributions of the expected gamma-ray emission using the Gammapy library. Promising candidate sources to apply this model are extended VHE sources associated with energetic pulsars, some of which also exhibit spectral continuity and morphological compatibility with ultra-high-energy sources. One such source is HESS J1831-098, which is associated to 1LHAASO J1831-1007u and could be powered by the radio pulsar PSR J1831-0952 with a characteristic age of 128 kyr. We present a spectro-morphological analysis of this source with H.E.S.S. data revealing that the emission can be well described with a pulsar halo model and we discuss the implication of the derived physical parameters of the model.
| Collaboration(s) | On behalf of the H.E.S.S. Collaboration |
|---|
