Study of a pulsar wind nebula candidate around the intermediate-age pulsar PSR J1413-6205 with H.E.S.S
Abstract
Very-high-energy γ-ray emission provides constraints on the morphology and the physics mechanisms involved in the evolution of pulsar wind nebulae (PWNe). In the Galactic plane, around 312 of Galactic longitude, a promising region two-degree wide containing five powerful pulsars may offer a new insight on the transition between TeV-emitting PWNe and pulsar halos. Their rotational energies range from 1035 to 1037 erg s-1 for ages between 13.6 and 62.8 kyr. Extended emission is detected with H.E.S.S. (High Energy Stereoscopic System) in their vicinity, notably around the pulsar PSR J1413-6205. We processed 124 hours of H.E.S.S observations with an algorithm improving background fitting for the study of extended sources. We applied a three-dimensional likelihood analysis technique to model the different sources in the region using a configuration that optimizes the collection area at the highest energies. This contribution focuses on the detection of a new extended source around PSR J1413-6205 over 5σ with a hard spectrum. Preliminary results on this source show a radius of 0.12 0.01 stat, an index of 2.06 0.20 stat and a lower limit on a cut-off energy of 17 TeV, at a 90% confidence level. The detected emission is consistent with previous PWN models.