Multi-wavelength observations of 2HWC J1928+177: dark accelerator or new TeV gamma-ray binary?

TL;DR

This study investigates the nature of the unidentified TeV gamma-ray source 2HWC J1928+177, exploring whether it is a dark accelerator or a new gamma-ray binary, through multi-wavelength observations and modeling.

Contribution

The paper presents multi-wavelength observational analysis and modeling to identify the nature of 2HWC J1928+177, proposing possible scenarios including a pulsar wind nebula, hadronic interactions, or a gamma-ray binary.

Findings

Detection of a variable X-ray point source within the HAWC error circle.

X-ray spectra consistent with an absorbed power-law, indicating potential binary nature.

Possible association with an IR source suggests a new TeV gamma-ray binary.

Abstract

2HWC J1928+177 is a Galactic TeV gamma-ray source detected by the High Altitude Water Cherenkov (HAWC) Observatory up to ~ 56 TeV. The HAWC source, later confirmed by H.E.S.S., still remains unidentified as a dark accelerator since there is no apparent supernova remnant or pulsar wind nebula detected in the lower energy bands. The radio pulsar PSR J1928+1746, coinciding with the HAWC source position, has no X-ray counterpart. Our SED modeling shows that inverse Compton scattering in the putative pulsar wind nebula can account for the TeV emission only if the unseen nebula is extended beyond r ~ 4 [arcmin]. Alternatively, TeV gamma rays may be produced by hadronic interactions between relativistic protons from an undetected supernova remnant associated with the radio pulsar and a nearby molecular cloud G52.9+0.1. NuSTAR and Chandra observations detected a variable X-ray point source within the HAWC error circle, potentially associated with a bright IR source. The X-ray spectra can be fitted with an absorbed power-law model with $N_{\rm H} = (9\pm3)\times10^{22}$ cm$^{-2}$ and $\Gamma_X = 1.6\pm0.3$ and exhibit long-term X-ray flux variability over the last decade. If the X-ray source, possibly associated with the IR source (likely an O star), is the counterpart of the HAWC source, it may be a new TeV gamma-ray binary powered by collisions between the pulsar wind and stellar wind. Follow-up X-ray observations are warranted to search for diffuse X-ray emission and determine the nature of the HAWC source.