VHE gamma-ray study of the composite SNR MSH 15-52 with H.E.S.S
Michelle Tsirou, Yves Gallant, Roberta Zanin, Regis Terrier (for the, H.E.S.S. Collaboration)
TL;DR
This paper presents an in-depth analysis of VHE gamma-ray emission from the composite SNR MSH 15-52 using H.E.S.S., comparing it with X-ray data to explore magnetic fields and cosmic ray origins.
Contribution
It provides detailed VHE gamma-ray observations of MSH 15-52, enhancing understanding of PWN morphology and implications for cosmic ray acceleration.
Findings
Extended gamma-ray emission observed beyond the X-ray PWN
Comparison reveals insights into magnetic field strength in the nebula
Results support PWN as potential sources of cosmic ray electrons and positrons
Abstract
The composite supernova remnant (SNR) MSH 15-52 comprises the bright X-ray pulsar wind nebula (PWN) of PSR B1509-58, surrounded by a shell which is a prominent object in the radio domain. H.E.S.S. had discovered extended very-high-energy (VHE) gamma-ray emission coincident with the PWN. With additional H.E.S.S. observations performed since the 2005 discovery paper, we study the properties of the emission in greater detail. We compare the VHE gamma-ray morphology of the PWN with that in synchrotron emission, obtained from archival X-ray observations, and discuss the implications on the magnetic field in the nebula. In particular, we discuss potential extended gamma-ray emission beyond the X-ray PWN, which may allow for conclusions on scenarios of PWNe as sources of cosmic ray electrons and positrons.
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