Detection of X-Ray Emission from the Unidentified TeV Gamma-Ray Source TeV J2032+4130

TL;DR

This study used Suzaku to detect diffuse X-ray emission from the unidentified TeV gamma-ray source TeV J2032+4130, revealing structures coincident with a gamma-ray pulsar and analyzing the emission mechanisms involved.

Contribution

First detection of diffuse X-ray emission associated with TeV J2032+4130, linking X-ray and gamma-ray observations to understand the source's emission processes.

Findings

Detected diffuse X-ray emission with Suzaku.

X-ray spectrum fits a power-law with photon index ~2.

Gamma-ray to X-ray flux ratio is about 10.

Abstract

We observed the first unidentified TeV gamma-ray source TeV J2032+4130 with Suzaku. Owing to Suzaku's high sensitivity for detection of diffuse X-ray emission, we found two small structures in the TeV emitting region. One of them is coincident with a gamma-ray pulsar PSR J2032+4127, which was discovered by the Fermi Gamma-ray Space Telescope. By subtracting contribution of point sources estimated by Chandra data, we obtained diffuse X-ray spectrum. The X-ray spectrum can be reproduced by a power-law model with a photon index of about 2, and an X-ray flux of 2x10^{-13} erg s^-1 cm^-2. The ratio of the gamma-ray flux to the X-ray flux is about 10. If the origin of the TeV gamma-ray is inverse Compton scattering of microwave background by high energy electrons, the ratio corresponds to the magnetic field strength of ~1 microG. However, the smaller size of the X-ray emission than that of the TeV emission suggests that energy loss of the electrons can explain the large ratio of the gamma-ray flux with a reasonable magnetic field strength of a few microG.