Observations of the $\gamma$-ray pulsar J1932+1916 in X-rays

TL;DR

This paper reports the detection of X-ray emission from the gamma-ray pulsar J1932+1916 using Suzaku and Swift data, identifying its X-ray counterpart and exploring its possible association with a nearby supernova remnant.

Contribution

First detection of X-ray emission from PSR J1932+1916, providing spectral analysis and potential association with a supernova remnant, constraining its distance and properties.

Findings

Detected X-ray counterpart consistent with pulsar and nebula

Estimated pulsar distance between 2-6 kpc

Suggested association with supernova remnant G54.4-0.3

Abstract

We present the analysis of the archival Suzaku and Swift X-ray observations of the young $\gamma$-ray pulsar J1932+1916 field. The data revealed a point-like object at the $\gamma$-ray position of the pulsar and diffuse X-ray emission around it. Spectra of the point-like source and diffuse emission are well-described by absorbed power-law models with spectral parameters typical for pulsar plus pulsar wind nebula systems. Therefore we suggest that Suzaku and Swift detected the X-ray counterpart of PSR J1932+1916. Assuming this interpretation, we constrain the distance to the pulsar in the range of 2-6 kpc. We also suggest possible association of the pulsar with the nearby supernova remnant G54.4-0.3 and discuss its implications for the pulsar proper motion, age and distance.