L K Eppens, J A Combi, E M Reynoso, F Garcí a, E Mestre, L Abaroa, G E Romero, P L Luque-Escamilla, J Martí

A high-energy study of the supernova remnant G296.5+10.0

  • Space and Planetary Science
  • Astronomy and Astrophysics
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Abstract We report a detailed multi-wavelength study of the supernova remnant G296.5+10.0 using archival data from XMM-Newton and Fermi-LAT complemented with ATCA observations. In the X-ray band, we performed an adaptive smoothing on the double background subtracted images to construct an X-ray mosaic map with six individual observations. Below 2.0 keV, G296.5+10.0 is asymmetrical, with the south-east side of the radio shell brighter than the south-west one. The spatially resolved X-ray spectral study confirms the thermal origin of the plasma, with enhanced metal abundances, probably arising from ejecta material according to the H i and infrared ($140~{\mu \rm m}$) distributions. In the γ-ray band, we analyzed 14 years of accumulated Fermi observations below 500 GeV via different fitting processes. To discuss the origin of the γ-ray emission, we compare the GeV results with H i structures probably associated with the SNR and with the radio spectral indices found at various positions towards the radio shell. Moreover, we identified diverse sources candidates to contribute γ-ray emissions observed. Also, we calculated the lepto-hadronic spectral energy distribution of the remnant for synchrotron, inverse Compton, Bremsstrahlung and proton-proton processes. The emission at low energies can be explained by electron-synchrotron radiation, with a weak magnetic field of B = 25 μG, while the γ-ray data can be explained by hadronic interactions. Employing the reddening-distance method, we computed a distance of 1.4 kpc for the SNR, implying an age of 14, 000 yr.

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