Radio study of the extended TeV source VER J1907+062

TL;DR

This study uses new radio observations and interstellar medium data to investigate the origin of the TeV source VER J1907+062, proposing a dual-source scenario involving leptonic and hadronic processes at different distances.

Contribution

It provides the first high-quality radio imaging of VER J1907+062 and suggests a novel dual-origin scenario for its gamma-ray emission, combining leptonic and hadronic sources.

Findings

No radio PWN detected at the source location.

Molecular clouds are associated with the supernova remnant G40.5-0.5.

The TeV emission likely originates from two separate sources at different distances.

Abstract

This paper aims to provide new insights on the origin of the TeV source VER J1907+062 through new high-quality radio observations. We used the Karl G. Jansky Very Large Array (VLA) to observe the whole extension of VER J1907+062 at 1.5 GHz with a mosaicking technique and the PSR J1907+0602 in a single pointing at 6 GHz. These data were used together with $^{12}$CO and atomic hydrogen observations obtained from public surveys to investigate the interstellar medium in the direction of VER J1907+062. The new radio observations do not show any evidence of a pulsar wind nebula (PWN) driven by the pulsars present in the field and no radio counterpart to the proposed X-ray PWN powered by PSR J1907+0602 is seen in the new VLA image at 6 GHz down to a noise level of 10 $\mu$Jy/beam. Molecular clouds were discovered over the eastern, southern, and western borders of the radio shell of G40.5$-$0.5, suggesting an association with this supernova remnant. We explored several scenarios for the origin of VER J1907+062. We propose as the most probable scenario one in which the TeV emission is produced by two separated gamma-ray sources located at different distances: one of leptonic origin and associated with a PWN powered by PSR J1907+0602 at $\sim 3.2$ kpc and another of hadronic origin and produced by the interaction between G40.5$-$0.5 and the surrounding molecular gas at $\sim 8.7$ kpc.