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The high-energy gamma-ray detection of G73.9+0.9, a supernova remnant interacting with a molecular cloud

Zdziarski, Andrzej A. ; Malyshev, Denys ; deOñaWilhelmi, Emma ; Pedaletti, Giovanna ; Yang, Ruizhi ; Chernyakova, Maria ; López-Caniego, Marcos ; Mikołajewska, Joanna ; Basak, Rupal

In: Monthly Notices of the Royal Astronomical Society, 2015, vol. 455, no. 2, p. 1451-1458

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    Titre
    • The high-energy gamma-ray detection of G73.9+0.9, a supernova remnant interacting with a molecular cloud
    Auteur
    • Zdziarski, Andrzej A.. Centrum Astronomiczne im. M. Kopernika, Bartycka 18, PL-00-716 Warszawa, Poland
    • Malyshev, Denys. ISDC Data Centre for Astrophysics, Astronomy Department, Geneva University, Ch. d'Ecogia 16, Versoix CH-1290, Switzerland
    • deOñaWilhelmi, Emma. Institut de Ciències de l'Espai (IEEC-CSIC), Campus UAB, Torre C5, 2a planta, E-08193 Bellaterra, Spain
    • Pedaletti, Giovanna. Institut de Ciències de l'Espai (IEEC-CSIC), Campus UAB, Torre C5, 2a planta, E-08193 Bellaterra, Spain
    • Yang, Ruizhi. Max-Planck-Institut für Kernphysik, PO Box 103980, D-69029 Heidelberg, Germany
    • Chernyakova, Maria. School of Physical Sciences, Dublin City University, Glasnevin, Dublin 9, Ireland
    • López-Caniego, Marcos. European Space Agency, ESAC, Planck Science Office, Camino bajo del Castillo, s/n, Urbanización Villafranca del Castillo, Villanueva de la Cañada, Madrid, Spain
    • Mikołajewska, Joanna. Centrum Astronomiczne im. M. Kopernika, Bartycka 18, PL-00-716 Warszawa, Poland
    • Basak, Rupal. Centrum Astronomiczne im. M. Kopernika, Bartycka 18, PL-00-716 Warszawa, Poland
    Type de document
    • Postprint
    Langue
    • Anglais
    Publié dans
    • Monthly Notices of the Royal Astronomical Society, 2015, vol. 455, no. 2, p. 1451-1458. Oxford University Press
    Autre version électronique
    Identifiant OAI-PMH
    • oai:doc.rero.ch:295097
    Summary
    We have analysed the Fermi Large Area Telescope (LAT) data on the SNR G73.9+0.9. We have confirmed a previous detection of high-energy γ-rays from this source at a high significance of ≃12σ. The observed spectrum shows a significant curvature, peaking in EFE at ∼1 GeV. We have also calculated the flux upper limits in the mm-wavelength and X-ray ranges from Planck and XMM-Newton, respectively. We have inspected the intensity of the CO (1→0) emission line and found a large peak at a velocity range corresponding to the previously estimated source distance of ∼4kpc, which may indicate an association between a molecular cloud and the supernova remnant (SNR). The γ-ray emission appears due to interaction of accelerated particles within the SNR with the matter of the cloud. The most likely radiative process responsible for the γ-ray emission is decay of neutral pions produced in ion-ion collisions. While a dominant leptonic origin of this emission can be ruled out, the relativistic electron population related to the observed radio flux will necessarily lead to a certain level of bremsstrahlung γ-ray emission. Based on this broad-band modelling, we have developed a method to estimate the magnetic field, yielding B ≳ 80 μG at our best estimate of the molecular cloud density (or less at a lower density). G73.9+0.9 appears similar, though somewhat weaker, to other SNRs interacting with a local dense medium detected by the LAT