Population study of Galactic supernova remnants at very high gamma-ray energies with HESS

Abdalla H, Abramowski A, Aharonian F, Benkhali FA, Anguener EO, Arakawa M, Arrieta M, Aubert P, Backes M, Balzer A, Barnard M, Becherini Y, Tjus JB, Berge D, Bernhard S, Bernloehr K, Blackwell R, Boettcher M, Boisson C, Bolmont J, Bonnefoy S, Bordas P, Bregeon J, Brun F, Brun P, Bryan M, Büchele M, Bulik T, Capasso M, Caroff S, Carosi A, Casanova S, Cerruti M, Chakraborty N, Chaves RCG, Chen A, Chevalier J, Colafrancesco S, Condon B, Conrad J, Davids ID, Decock J, Deil C, Devin J, Dewilt P, Dirson L, Djannati-Atai A, Donath A, Drury LO, Dutson K, Dyks J, Edwards T, Egberts K, Emery G, Ernenwein JP, Eschbach S, Farnier C, Fegan S, Fernandes MV, Fernandez D, Fiasson A, Fontaine G, Funk S, Fuessling M, Gabici S, Gallant YA, Garrigoux T, Gate F, Giavitto G, Giebels B, Glawion D, Glicenstein JF, Gottschall D, Grondin MH, Hahn J, Haupt M, Hawkes J, Heinzelmann G, Henri G, Hermann G, Hinton JA, Hofmann W, Hoischen C, Holch TL, Holler M, Horns D, Ivascenko A, Iwasaki H, Jacholkowska A, Jamrozy M, Jankowsky D, Jankowsky F, Jingo M, Jouvin L, Jung-Richardt I, Kastendieck MA, Katarzynski K, Katsuragawa M, Katz U, Kerszberg D, Khangulyan D, Khelifi B, King J, Klepser S, Klochkov D, Kluzniak W, Komin N, Kosack K, Krakau S, Kraus M, Krueger PP, Laffon H, Lamanna G, Lau J, Lees JP, Lefaucheur J, Lemiere A, Lemoine-Goumard M, Lenain JP, Leser E, Lohse T, Lorentz M, Liu R, Lopez-Coto R, Lypova I, Malyshev D, Marandon V, Marcowith A, Mariaud C, Marx R, Maurin G, Maxted N, Mayer M, Meintjes PJ, Meyer M, Mitchell AMW, Moderski R, Mohamed M, Mohrmann L, Mora K, Moulin E, Murach T, Nakashima S, De Naurois M, Ndiyavala H, Niederwanger F, Niemiec J, Oakes L, O'Brien P, Odaka H, Ohm S, Ostrowski M, Oya I, Padovani M, Panter M, Parsons RD, Pekeur NW, Pelletier G, Perennes C, Petrucci PO, Peyaud B, Piel Q, Pita S, Poireau V, Poon H, Prokhorov D, Prokoph H, Puehlhofer G, Punch M, Quirrenbach A, Raab S, Rauth R, Reimer A, Reimer O, Renaud M, De Los Reyes R, Rieger F, Rinchiuso L, Romoli C, Rowell G, Rudak B, Rulten CB, Safi-Harb S, Sahakian V, Saito S, Sanchez DA, Santangelo A, Sasaki M, Schlickeiser R, Schuessler F, Schulz A, Schwanke U, Schwemmer S, Seglar-Arroyo M, Settimo M, Seyffert AS, Shafi N, Shilon I, Shiningayamwe K, Simoni R, Sol H, Spanier F, Spir-Jacob M, Stawarz L, Steenkamp R, Stegmann C, Steppa C, Sushch I, Takahashi T, Tavernet JP, Tavernier T, Taylor AM, Terrier R, Tibaldo L, Tiziani D, Tluczykont M, Trichard C, Tsirou M, Tsuji N, Tuffs R, Uchiyama Y, Van Der Walt DJ, van Eldik C, Van Rensburg C, Van Soelen B, Vasileiadis G, Veh J, Venter C, Viana A, Vincent P, Vink J, Voisin F, Voelk HJ, Vuillaume T, Wadiasingh Z, Wagner SJ, Wagner P, Wagner RM, White R, Wierzcholska A, Willmann P, Wörnlein A, Wouters D, Yang R, Zaborov D, Zacharias M, Zanin R, Zdziarski AA, Zech A, Zefi F, Ziegler A, Zorn J, Zywucka N (2018)


Publication Status: Published

Publication Type: Journal article, Original article

Publication year: 2018

Journal

Publisher: EDP SCIENCES S A

Book Volume: 612

Article Number: A3

DOI: 10.1051/0004-6361/201732125

Abstract

Shell-type supernova remnants (SNRs) are considered prime candidates for the acceleration of Galactic cosmic rays (CRs) up to the knee of the CR spectrum at E approximate to 3 x 10(15) eV. Our MilkyWay galaxy hosts more than 350 SNRs discovered at radio wavelengths and at high energies, of which 220 fall into the H.E.S.S. Galactic Plane Survey (HGPS) region. Of those, only 50 SNRs are coincident with a H.E.S.S source and in 8 cases the very high-energy (VHE) emission is firmly identified as an SNR. The H.E.S.S. GPS provides us with a legacy for SNR population study in VHE gamma-rays and we use this rich data set to extract VHE flux upper limits from all undetected SNRs. Overall, the derived flux upper limits are not in contradiction with the canonical CR paradigm. Assuming this paradigm holds true, we can constrain typical ambient density values around shell-type SNRs to n <= 7 cm(-3) and electron-to-proton energy fractions above 10 TeV to epsilon(ep) <= 5 x 10(-3). Furthermore, comparisons of VHE with radio luminosities in non-interacting SNRs reveal a behaviour that is in agreement with the theory of magnetic field amplification at shell-type SNRs.

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How to cite

APA:

Abdalla, H., Abramowski, A., Aharonian, F., Benkhali, F.A., Anguener, E.O., Arakawa, M.,... Zywucka, N. (2018). Population study of Galactic supernova remnants at very high gamma-ray energies with HESS. Astronomy & Astrophysics, 612. https://dx.doi.org/10.1051/0004-6361/201732125

MLA:

Abdalla, H., et al. "Population study of Galactic supernova remnants at very high gamma-ray energies with HESS." Astronomy & Astrophysics 612 (2018).

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