Multi-wavelength study of HESS J1741-302

TL;DR

This multi-wavelength study investigates potential counterparts to the TeV gamma-ray source HESS J1741-302, analyzing X-ray, GeV gamma-ray, and radio data to explore its nature and possible origins.

Contribution

The paper provides the first detailed multi-wavelength analysis of HESS J1741-302, assessing candidate sources and their likelihood of producing TeV gamma-rays.

Findings

CXOU J174112.1-302908 likely a low-mass star, not a TeV source

WR 98a is a colliding wind binary with no associated TeV emission

Suzaku J1740.5-3014 is a magnetized CV, unlikely linked to TeV emission

Abstract

We present the results of two Chandra X-ray Observatory ( CXO) observations of TeV gamma-ray source HESS J1741-302A/B. Our analysis also includes GeV gamma-ray and radio data. We investigate whether there is any connection between HESS J1741-302A/B and the sources seen at lower energies. One of the brightest X-ray sources in the HESS J1741-302B field, CXOU J174112.1-302908, appears to be associated with a low-mass star (possibly representing a quiescent LMXB or CV), hence, it is unlikely to be a source of TeV gamma-rays. In the same field we detected X-rays from WR 98a, which is likely to be a colliding wind binary with massive stars, however, no TeV emission has been reported so far from such systems although a predictions have been made. Finally, Suzaku source J1740.5-3014 (which is not covered by the CXO observations) appears to be a hard X-ray source detected by INTERGAL ISGRI which supports the magnetized CV classification and also makes its association with the TeV emission unlikely. The young pulsar, undetected in X-rays and located near the CV, may be the contributor of relativistic particles responsible for the TeV emission. Alternatively, HESS J1741-302 could be a new type of accelerator, which is dark at lower energies.