EVN Observations of HESS J1943+213: Evidence for an Extreme TeV BL Lac Object

TL;DR

This study uses high-resolution VLBI observations to identify HESS J1943+213 as an extreme high-frequency-peaked BL Lac object, revealing its core-jet structure and emphasizing the importance of radio imaging in classifying elusive TeV sources.

Contribution

It provides the deepest VLBI imaging of HESS J1943+213, confirming its classification as an extreme HBL and highlighting the role of radio observations in identifying similar hidden sources.

Findings

HESS J1943+213 has a core-jet structure consistent with an extreme HBL.

Radio properties match those of low-luminosity blazars.

High-resolution radio imaging is crucial for identifying such sources.

Abstract

We report on the 1.6 GHz (18 cm) VLBI observations of the unresolved, steady TeV source HESS J1943+213 located in the Galactic plane, performed with the European VLBI Network (EVN) in 2014. Our new observations with a nearly full EVN array provide the deepest image of HESS J1943+213 at the highest resolution ever achieved, enabling us to resolve the long-standing issues of the source identification. The milliarcsecond-scale structure of HESS J1943+213 has a clear asymmetric morphology, consisting of a compact core and a diffuse jet-like tail. This is broadly consistent with the previous e-EVN observations of the source performed in 2011, and re-analyzed in this work. The core component is characterized by the brightness temperature of $\gtrsim1.8 \times 10^9$ K, which is typical for low-luminosity blazars in general. Overall, radio properties of HESS J1943+213 are consistent with the source classification as an "extreme high-frequency-peaked BL Lac object". Remarkably, we note that since HESS J1943+213 does not reveal any optical or infrared signatures of the AGN activity, it would never be recognized and identified as a BL Lac object, if not its location close to the Galactic plane where the High Energy Stereoscopic System has surveyed, and the follow-up dedicated X-ray and radio studies triggered by the source detection in the TeV range. Our results suggest therefore a presence of an unrecognized, possibly very numerous population of particularly extreme HBLs, and simultaneously demonstrate that the low-frequency VLBI observations with high-angular resolution are indispensable for a proper identification of such objects.