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Constraints on the Non-thermal X-ray and Gamma-ray Emission Model of Supernova Remnant W44

Presentation #104.11 in the session ISM/Galaxies - Poster Session.

Published onMay 03, 2024
Constraints on the Non-thermal X-ray and Gamma-ray Emission Model of Supernova Remnant W44

Detections of GeV gamma-ray emission from supernova remnant W44 by the Fermi-LAT and AGILE suggest that it may be a source of highly accelerated cosmic rays. W44 is a classic mixed-morphology supernova remnant and is known to be interacting with molecular clouds which increases the frequency of potential interactions between cosmic-ray nuclei and nearby gas particles. Spectral energy distributions (SEDs) constructed from the GeV data indicate that a plausible origin for the gamma-ray emission is the decay of neutral pions produced from these cosmic-ray interactions. However, measurements of the SED of W44 at X-ray and very high energy (VHE) gamma-ray bands are crucial to confirm the hadronic nature of the emission and to estimate contributions from leptonic emission. Here, we present an upper-limit estimate of the nonthermal X-ray flux from W44 based on ~ 300 ks of XMM-Newton observations, as well as measurements of the VHE gamma-ray flux from W44 by the Very Energetic Radiation Imaging Telescope Array System (VERITAS). We construct a non-thermal radiative model of the SED of W44 at radio, X-ray, and gamma-ray wavelengths to probe the population of accelerated particles producing these emissions.

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