Energy dependent morphology of the pulsar wind nebula HESS J1825-137 with Fermi-LAT

Abstract

Taking advantage of more than 11 years of Fermi-LAT data, we perform a new and deep analysis of the pulsar wind nebula (PWN) HESS J1825-137. Combining this analysis with recent H.E.S.S. results we investigate and constrain the particle transport mechanisms at work inside the source as well as the system evolution. The PWN is studied using 11.6 years of Fermi-LAT data between 1 GeV and 1 TeV. In particular, we present the results of the spectral analysis and the first energy-resolved morphological study of the PWN HESS J1825-137 at GeV energies, which provide new insights into the gamma-ray characteristics of the nebula. An optimised analysis of the source returns an extended emission region larger than 2${}^{\circ }$, corresponding to an intrinsic size of about 150 pc, making HESS J1825-137 the most extended gamma-ray PWN currently known. The nebula presents a strong energy dependent morphology within the GeV range, moving from a radius of $\sim 1.4^{\circ }$ below 10 GeV to a radius of $\sim$0.8${}^{\circ }$ above 100 GeV, with a shift in the centroid location. Thanks to the large extension and peculiar energy-dependent morphology, it is possible to constrain the particle transport mechanisms inside the PWN HESS J1825-137. Using the variation of the source extension and position, as well as the constraints on the particle transport mechanisms, we present a scheme for the possible evolution of the system. Finally, we provide an estimate of the electron energy density and we discuss its nature in the PWN and TeV halo-like scenario.

arXiv commentAccepted for publication in Astronomy & Astrophysics, 15 pages, 12 figures

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Cited by in corpus (26)

• Incremental Fermi Large Area Telescope Fourth Source Catalog
• Gamma-ray halos around pulsars as the key to understanding cosmic ray transport in the Galaxy
• Evidence of TeV Halos Around Millisecond Pulsars
• Are pulsar halos rare ?
• Population synthesis of pulsar wind nebulae and pulsar halos in the Milky Way -- Predicted contributions to the very-high-energy sky
• TeV halos and the role of pulsar wind nebulae as sources of cosmic ray positrons
• Investigating $\gamma$-ray halos around three HAWC bright sources in Fermi-LAT data
• A detailed look at the thermal and non-thermal X-ray emission from the Vela supernova remnant with SRG/eROSITA
• Multiple emission components in the Cygnus cocoon detected from Fermi-LAT observations
• Probing the hadronic nature of the gamma-ray emission associated with Westerlund 2
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• A 3D Diffusive and Advective Model of Electron Transport Applied to the Pulsar Wind Nebula HESS J1825-137
• Discovery of an Extended $\gamma$-ray Emission around the Supernova Remnant Candidate associated with PSR J0837$-$2454
• Detecting and characterizing pulsar haloes with the Cherenkov Telescope Array
• Exploring the possible gluon condensation signature in gamma-ray emission from pulsars
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• The Eel Pulsar Wind Nebula: a PeVatron-Candidate Origin for HAWC J1826-128 and HESS J1826-130
• New estimate for the contribution of the Geminga pulsar to the positron excess
• Morphology of supernova remnants and their halos
• GeV emission in the region of the supernova remnant G51.26+0.11
• Unveiling extended gamma-ray emission around HESS J1813-178
• Energy-dependent gamma-ray morphology estimation tool in Gammapy
• The primary proton spectrum of the hadronic PeVatron candidate HAWC J1825-134