Spatially resolved XMM-Newton analysis and a model of the nonthermal emission of MSH 15-52

TL;DR

This paper combines spatially resolved X-ray analysis of PWN MSH 15-52 with a magnetohydrodynamic model to explain its nonthermal emission, successfully matching X-ray spectra and TeV flux levels but not the spectral shape.

Contribution

It introduces a magnetohydrodynamic model for PWN nonthermal emission that aligns with observed X-ray spectra and TeV flux levels, providing new insights into PWN physics.

Findings

Model reproduces spatial variation of X-ray spectra.

Parameter estimates agree with previous studies.

Reproduces H.E.S.S. flux levels but not spectral shape.

Abstract

We present an X-ray analysis and a model of the nonthermal emission of the pulsar wind nebula (PWN) MSH15-52. We analyzed XMM-Newton data to obtain the spatially resolved spectral parameters around the pulsar PSRB1509-58. A steepening of the fitted power-law spectra and decrease in the surface brightness is observed with increasing distance from the pulsar. In the second part of this paper, we introduce a model for the nonthermal emission, based on assuming the ideal magnetohydrodynamic limit. This model is used to constrain the parameters of the termination shock and the bulk velocity of the leptons in the PWN. Our model is able to reproduce the spatial variation of the X-ray spectra. The parameter ranges that we found agree well with the parameter estimates found by other authors with different approaches. In the last part of this paper, we calculate the inverse Compton emission from our model and compare it to the emission detected with the H.E.S.S. telescope system. Our model is able to reproduce the flux level observed with H.E.S.S., but not the spectral shape of the observed TeV {\gamma}-ray emission.