Population study of Galactic supernova remnants at very high γ-ray energies with H.E.S.S

H. E. S. S. CollaborationAbdalla, H.H.AbdallaAbramowski, A.A.AbramowskiAharonian, F.F.AharonianAit Benkhali, F.F.Ait BenkhaliAngüner, E. O.E. O.AngünerArakawa, M.M.ArakawaArrieta, M.M.ArrietaAubert, P.P.AubertBackes, M.M.BackesBalzer, A.A.BalzerBarnard, M.M.BarnardBecherini, Y.Y.BecheriniBecker Tjus, J.J.Becker TjusBerge, D.D.BergeBernhard, S.S.BernhardBernlöhr, K.K.BernlöhrBlackwell, R.R.BlackwellBöttcher, M.M.BöttcherBoisson, C.C.BoissonBolmont, J.J.BolmontBonnefoy, S.S.BonnefoyBordas, P.P.BordasBregeon, J.J.BregeonBrun, F.F.BrunBrun, P.P.BrunBryan, M.M.BryanBüchele, M.M.BücheleBulik, T.T.BulikCapasso, M.M.CapassoCaroff, S.S.CaroffCarosi, A.A.CarosiCasanova, S.S.CasanovaCerruti, M.M.CerrutiChakraborty, N.N.ChakrabortyChaves, R. C. G.R. C. G.ChavesChen, A.A.ChenChevalier, J.J.ChevalierColafrancesco, S.S.ColafrancescoCondon, B.B.CondonConrad, J.J.ConradDavids, I. D.I. D.DavidsDecock, J.J.DecockDeil, C.C.DeilDevin, J.J.DevindeWilt, P.P.deWiltDirson, L.L.DirsonDjannati-Ataï, A.A.Djannati-AtaïDonath, A.A.DonathDrury, L. O. 'C.L. O. 'C.DruryDutson, K.K.DutsonDyks, J.J.DyksEdwards, T.T.EdwardsEgberts, K.K.EgbertsEmery, G.G.EmeryErnenwein, J. -P.J. -P.ErnenweinEschbach, S.S.EschbachFarnier, C.C.FarnierFegan, S.S.FeganFernandes, M. V.M. V.FernandesFernandez, D.D.FernandezFiasson, A.A.FiassonFontaine, G.G.FontaineFunk, S.S.FunkFüßling, M.M.FüßlingGabici, S.S.GabiciGallant, Y. A.Y. A.GallantGarrigoux, T.T.GarrigouxGaté, F.F.GatéGiavitto, G.G.GiavittoGiebels, B.B.GiebelsGlawion, D.D.GlawionGlicenstein, J. F.J. F.GlicensteinGottschall, D.D.GottschallGrondin, M. -H.M. -H.GrondinHahn, J.J.HahnHaupt, M.M.HauptHawkes, J.J.HawkesHeinzelmann, G.G.HeinzelmannHenri, G.G.HenriHermann, G.G.HermannHinton, J. A.J. A.HintonHofmann, W.W.HofmannHoischen, C.C.HoischenHolch, T. L.T. L.HolchHoller, M.M.HollerHorns, D.D.HornsIvascenko, A.A.IvascenkoIwasaki, H.H.IwasakiJacholkowska, A.A.JacholkowskaJamrozy, M.M.JamrozyJankowsky, D.D.JankowskyJankowsky, F.F.JankowskyJingo, M.M.JingoJouvin, L.L.JouvinJung-Richardt, I.I.Jung-RichardtKastendieck, M. A.M. A.KastendieckKatarzyński, K.K.KatarzyńskiKatsuragawa, M.M.KatsuragawaKatz, U.U.KatzKerszberg, D.D.KerszbergKhangulyan, D.D.KhangulyanKhélifi, B.B.KhélifiKing, J.J.KingKlepser, S.S.KlepserKlochkov, D.D.KlochkovKluźniak, W.W.KluźniakKomin, Nu.Nu.KominKosack, K.K.KosackKrakau, S.S.KrakauKraus, M.M.KrausKrüger, P. P.P. P.KrügerLaffon, H.H.LaffonLamanna, G.G.LamannaLau, J.J.LauLees, J. -P.J. -P.LeesLefaucheur, J.J.LefaucheurLemière, A.A.LemièreLemoine-Goumard, M.M.Lemoine-GoumardLenain, J. -P.J. -P.LenainLeser, E.E.LeserLohse, T.T.LohseLorentz, M.M.LorentzLiu, R.R.LiuLópez-Coto, R.R.López-CotoLypova, I.I.LypovaMalyshev, D.D.MalyshevMarandon, V.V.MarandonMarcowith, A.A.MarcowithMariaud, C.C.MariaudMarx, R.R.MarxMaurin, G.G.MaurinMaxted, N.N.MaxtedMayer, M.M.MayerMeintjes, P. J.P. J.MeintjesMeyer, M.M.MeyerMitchell, A. M. W.A. M. W.MitchellModerski, R.R.ModerskiMohamed, M.M.MohamedMohrmann, L.L.MohrmannMorå, K.K.MoråMoulin, E.E.MoulinMurach, T.T.MurachNakashima, S.S.Nakashimade Naurois, M.M.de NauroisNdiyavala, H.H.NdiyavalaNiederwanger, F.F.NiederwangerNiemiec, J.J.NiemiecOakes, L.L.OakesO'Brien, P.P.O'BrienOdaka, H.H.OdakaOhm, S.S.OhmOstrowski, M.M.OstrowskiOya, I.I.OyaPadovani, MarcoMarcoPadovaniPanter, M.M.PanterParsons, R. D.R. D.ParsonsPekeur, N. W.N. W.PekeurPelletier, G.G.PelletierPerennes, C.C.PerennesPetrucci, P. -O.P. -O.PetrucciPeyaud, B.B.PeyaudPiel, Q.Q.PielPita, S.S.PitaPoireau, V.V.PoireauPoon, H.H.PoonProkhorov, D.D.ProkhorovProkoph, H.H.ProkophPühlhofer, G.G.PühlhoferPunch, M.M.PunchQuirrenbach, A.A.QuirrenbachRaab, S.S.RaabRauth, R.R.RauthReimer, A.A.ReimerReimer, O.O.ReimerRenaud, M.M.Renaudde los Reyes, R.R.de los ReyesRieger, F.F.RiegerRinchiuso, L.L.RinchiusoRomoli, C.C.RomoliRowell, G.G.RowellRudak, B.B.RudakRulten, C. B.C. B.RultenSafi-Harb, S.S.Safi-HarbSahakian, V.V.SahakianSaito, S.S.SaitoSanchez, D. A.D. A.SanchezSantangelo, A.A.SantangeloSasaki, M.M.SasakiSchlickeiser, R.R.SchlickeiserSchüssler, F.F.SchüsslerSchulz, A.A.SchulzSchwanke, U.U.SchwankeSchwemmer, S.S.SchwemmerSeglar-Arroyo, M.M.Seglar-ArroyoSettimo, M.M.SettimoSeyffert, A. S.A. S.SeyffertShafi, N.N.ShafiShilon, I.I.ShilonShiningayamwe, K.K.ShiningayamweSimoni, R.R.SimoniSol, H.H.SolSpanier, F.F.SpanierSpir-Jacob, M.M.Spir-JacobStawarz, Ł.Ł.StawarzSteenkamp, R.R.SteenkampStegmann, C.C.StegmannSteppa, C.C.SteppaSushch, I.I.SushchTakahashi, T.T.TakahashiTavernet, J. -P.J. -P.TavernetTavernier, T.T.TavernierTaylor, A. M.A. M.TaylorTerrier, R.R.TerrierTibaldo, L.L.TibaldoTiziani, D.D.TizianiTluczykont, M.M.TluczykontTrichard, C.C.TrichardTsirou, M.M.TsirouTsuji, N.N.TsujiTuffs, R.R.TuffsUchiyama, Y.Y.Uchiyamavan der Walt, D. J.D. J.van der Waltvan Eldik, C.C.van Eldikvan Rensburg, C.C.van Rensburgvan Soelen, B.B.van SoelenVasileiadis, G.G.VasileiadisVeh, J.J.VehVenter, C.C.VenterViana, A.A.VianaVincent, P.P.VincentVink, J.J.VinkVoisin, F.F.VoisinVölk, H. J.H. J.VölkVuillaume, T.T.VuillaumeWadiasingh, Z.Z.WadiasinghWagner, S. J.S. J.WagnerWagner, P.P.WagnerWagner, R. M.R. M.WagnerWhite, R.R.WhiteWierzcholska, A.A.WierzcholskaWillmann, P.P.WillmannWörnlein, A.A.WörnleinWouters, D.D.WoutersYang, R.R.YangZaborov, D.D.ZaborovZacharias, M.M.ZachariasZanin, R.R.ZaninZdziarski, A. A.A. A.ZdziarskiZech, A.A.ZechZefi, F.F.ZefiZiegler, A.A.ZieglerZorn, J.J.ZornŻywucka, N.N.Żywucka2020-10-122020-10-1220180004-6361http://hdl.handle.net/20.500.12386/27713Shell-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 ≈ 3 × 1015 eV. Our Milky Way 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 γ-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 ∊ep ≤ 5 × 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.STAMPAenPopulation study of Galactic supernova remnants at very high γ-ray energies with H.E.S.SArticle10.1051/0004-6361/2017321252-s2.0-85045517455000429404700003https://www.aanda.org/articles/aa/abs/2018/04/aa32125-17/aa32125-17.html2018A&A...612A...3HFIS/05 - ASTRONOMIA E ASTROFISICAERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation::PE9_8 Formation and evolution of galaxies