Exploring a SNR/Molecular Cloud Association Within HESS J1745-303

TL;DR

This study investigates the nature of the unidentified gamma-ray source HESS J1745-303 by combining multi-wavelength data, suggesting it may be partly explained by a supernova remnant, molecular cloud, or pulsar association.

Contribution

It introduces a multi-wavelength analysis approach to identify potential counterparts of HESS J1745-303, proposing a possible SNR/molecular cloud association as an explanation.

Findings

No single counterpart fully explains the VHE emission.

A supernova remnant/molecular cloud association may account for part of the emission.

A high-spin-down-flux pulsar could also contribute to the observed gamma rays.

Abstract

HESS J1745-303 is an extended, unidentified VHE (very high energy) gamma-ray source discovered using HESS in the Galactic Plane Survey. Since no obvious counterpart has previously been found in longer-wavelength data, the processes that power the VHE emission are not well understood. Combining the latest VHE data with recent XMM-Newton observations and a variety of source catalogs and lower-energy survey data, we attempt to match (from an energetic and positional standpoint) the various parts of the emission of HESS J1745-303 with possible candidates. Though no single counterpart is found to fully explain the VHE emission, we postulate that at least a fraction of the VHE source may be explained by a supernova-remnant/molecular-cloud association and/or a high-spin-down-flux pulsar.