Upper limits on very-high-energy gamma-ray emission from core-collapse supernovae observed with H.E.S.S.

H.E.S.S. Collaboration, H.E.S.S. and Abdalla, H. and Aharonian, F. and Drury, L. O'C. and Mackey, J. and ca 200 co-authors, A.N. (2019) Upper limits on very-high-energy gamma-ray emission from core-collapse supernovae observed with H.E.S.S. Astronomy & Astrophysics, 626. A57. ISSN 0004-6361

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Official URL: https://doi.org/10.1051/0004-6361/201935242

Abstract

Young core-collapse supernovae with dense-wind progenitors may be able to accelerate cosmic-ray hadrons beyond the knee of the cosmic-ray spectrum, and this may result in measurable gamma-ray emission. We searched for gamma-ray emission from ten supernovae observed with the High Energy Stereoscopic System (H.E.S.S.) within a year of the supernova event. Nine supernovae were observed serendipitously in the H.E.S.S. data collected between December 2003 and December 2014, with exposure times ranging from 1.4 to 53 h. In addition we observed SN 2016adj as a target of opportunity in February 2016 for 13 h. No significant gamma-ray emission has been detected for any of the objects, and upper limits on the >1 TeV gamma-ray flux of the order of 10^-13 cm-2s-1 are established, corresponding to upper limits on the luminosities in the range 2 x 10^39 to 1 x 10^42 erg s-1. These values are used to place model-dependent constraints on the mass-loss rates of the progenitor stars, implying upper limits between 2 x 10^-5 and 2 x 10^-3 Msun yr-1 under reasonable assumptions on the particle acceleration parameters.

Item Type: Article
Uncontrolled Keywords: Reproduced with permission from Astronomy & Astrophysics, © ESO.
Divisions: School of Cosmics Physics > Astronomy and Astrophysics
Date Deposited: 17 Jan 2020 15:12
Last Modified: 17 Jan 2020 15:12
URI: http://dair.dias.ie/id/eprint/1078

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