GeV gamma-ray emission from pulsar wind nebula HESS J1356-645 with Fermi-LAT

Abstract

HESS J1356-645 is considered to be a pulsar wind nebula (PWN) associated with the pulsar PSR J1357-6429. We reanalyze the GeV gamma-ray emission in the direction of HESS J1356-645 with more than 13 years of Fermi Large Area Telescope (LAT) data. The extended gamma-ray emission above 5 GeV is found to be spatially coincident with HESS J1356-645. The spectrum in the energy range of 1 GeV-1 TeV can be described by a power law with an index of $\Gamma =1.51\pm 0.10$. The broadband spectrum of HESS J1356-645 can be reproduced by a leptonic model with a broken power-law electronic spectrum. In addition, we found evidence that the morphology of the GeV emission from HESS J1356-645 varies with energy, a behavior which is similar to that of the PWN Vela-X. More broadband observations will be helpful to study the energy-dependent characteristics of HESS J1356-645.

9 pages, 5 figures

References in corpus (7)

• Incremental Fermi Large Area Telescope Fourth Source Catalog
• Energy dependent gamma-ray morphology in the Pulsar wind nebula HESSJ1825-137
• Identification of HESS J1303-631 as a Pulsar Wind Nebula through gamma-ray, X-ray and radio observations
• First X-ray observations of the young pulsar J1357-6429
• Estimating the birth period of pulsars through GLAST/LAT observations of their wind nebulae
• Discovery of X-ray emission from the young radio pulsar PSR J1357-6429
• Suzaku Observations of the old pulsar wind nebula candidate HESS J1356-645