J/A+A/612/A3ivo://CDS.VizieR/J/A+A/612/A3doi:10.26093/cds/vizier.36120003CDSHess CollaborationAbdalla H.Abramowski A.Aharonian F.,Ait Benkhali F.Anguner E.O.Arakawa M.Arrieta M.Aubert P.,Backes M.Balzer A.Barnard M.Becherini Y.Becker Tjus J.Berge D.,Bernhard S.Bernlohr K.Blackwell R.Bottcher M.Boisson C.,Bolmont J.Bonnefoy S.Bordas P.Bregeon J.Brun F.Brun P.Bryan M.,Buchele M.Bulik T.Capasso M.Caroff S.Carosi A.Casanova S.,Cerruti M.Chakraborty N.Chaves R.C.G.Chen A.Chevalier J.,Colafrancesco S.Condon B.Conrad J.Davids I.D.Decock J.Deil C.,Devin J.Dewilt P.Dirson L.Djannati-Atai A.Donath A.Drury L.O.,Dutson K.Dyks J.Edwards T.Egberts K.Emery G.Ernenwein J.-P.,Eschbach S.Farnier C.Fegan S.Fernandes M.V.Fernandez D.,Fiasson A.Fontaine G.Funk S.Fussling M.Gabici S.Gallant Y.A.,Garrigoux T.Gate F.Giavitto G.Giebels B.Glawion D.,Glicenstein J.F.Gottschall D.Grondin M.-H.Hahn J.Haupt M.,Hawkes J.Heinzelmann G.Henri G.Hermann G.Hinton J.A.Hofmann W.,Hoischen C.Holch T.L.Holler M.Horns D.Ivascenko A.Iwasaki H.,Jacholkowska A.Jamrozy M.Jankowsky D.Jankowsky F.Jingo M.,Jouvin L.Jung-Richardt I.Kastendieck M.A.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.Kruger P.P.Laffon H.Lamanna G.Lau J.Lees J.-P.,Lefaucheur J.Lemiere A.Lemoine-Goumard M.Lenain J.-P.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 P.J.Meyer M.Mitchell A.M.W.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 R.D.Pekeur N.W.Pelletier G.Perennes C.Petrucci P.-O.,Peyaud B.Piel Q.Pita S.Poireau V.Poon H.Prokhorov D.Prokoph H.,Puhlhofer 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 C.B.Safi-Harb S.Sahakian V.Saito S.,Sanchez D.A.Santangelo A.Sasaki M.Schlickeiser R.Schussler F.,Schulz A.Schwanke U.Schwemmer S.Seglar-Arroyo M.Settimo M.,Seyffert A.S.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 J.-P.Tavernier T.,Taylor A.M.Terrier R.Tibaldo L.Tiziani D.Tluczykont M.,Trichard C.Tsirou M.Tsuji N.Tuffs R.Uchiyama Y.Van Der Walt D.J.,Van Eldik C.Van Rensburg C.Van Soelen B.Vasileiadis G.Veh J.,Venter C.Viana A.Vincent P.Vink J.Voisin F.Volk H.J.,Vuillaume T.Wadiasingh Z.Wagner S.J.Wagner P.Wagner R.M.White R.,Wierzcholska A.Willmann P.Wornlein A.Wouters D.Yang R.Zaborov D.,Zacharias M.Zanin R.Zdziarski A.A.Zech A.Zefi F.Ziegler A.,Zorn J.Zywucka N.2018-10-01T11:51:46Z2018-09-07T12:01:57ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frgamma-ray-astronomysupernova-remnantsmilky-way-galaxyShell-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~=3x10^15^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 {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<=7cm^-3^ and electron-to-proton energy fractions above 10TeV to {epsilon}_ep_<=5x10^-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.2018A&A...612A...3Hhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/612/A3CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-tohttp://www.physics.umanitoba.ca/snr/SNRcat : SNRCat Home Pagehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/612/A3https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/612/A3http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/612/A3https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/612/A3https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/612/A3http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/612/A3GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/612/A3/tablea1 (Results overview)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/612/A3/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/612/A3/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/612/A3/tablea1?GETtext/xml+votable180.050000true268.8578-25.83370.0055555555555555566/12968 12970 14342 14353 14413-14414 14449 14453-14454 28718 28800 28803 28806 28809 28811-28813 28815 28837 28842 28846 28848 28878 28882 28887 28890 28894 28900 28914-28915 29094 29096 29103 29106 29115-29116 29119 29166 29253 29460 29507 29510-29511 29522 30211 30268 30319 30331 30335 30423 30426 30607 30642 30645 30709 37335 37828 37893 37901 37904 37912 37926 37929 37937 38400 41587 41594 41643 41647 41670 41673-41674 41676-41677 41681-41682 41767 41769 41772 41779 41800 41802-41803 41806 41809 41814 41821 42362 42381-42382 42401 42404 42445 42454 42456 42459 42497 43019-43020 43024https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/612/A3?format=asciiGamma-raydefaultJ/A+A/612/A3/tablea1Results overviewrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSourceSource designation (GLLL.l+B.b)meta.id;meta.maincharGLONGalactic longitudedegpos.galactic.lonGLATGalactic latitudedegpos.galactic.latRONRadius of the circular analysis regionsdegphys.angSizefloatTypeSNR morphology type (1)stat.snr;src.morph.typecharDist? Distance (2)kpcpos.distancefloatnullableLTimeCorrected observation live timehtime.expofloatAvzenithAveraged zenith angledegposfloatCDetecClosest HESS source detectedmeta.id.crosscharSep? Angular distance of closest HESS sourcedegpos.angDistancefloatnullableFulUpper limit on the integrated flux in the (1,10)TeV interval1e-13cm**-2.s**-1phot.flux.density;em.gamma.hardfloatsigniSignificance (sigma)stat.fit.goodnessfloatWpxnul? Upper limit on the product of proton energy content above 10TeV and ambient density, (Wpxn)^ul^[>10TeV]1e+41Wphys.energy.density;stat.maxfloatnullableWeul? Upper limit on the total energy content in electrons, W^ul^_e_[>10TeV]1e+38Wphys.energy;stat.maxfloatnullableSimbadSimbad column added by the CDSmeta.ref.urlchar_RA.icrsRight ascension (ICRS) (computed by VizieR, not part of the original data. The format may include more digits than the original data because of internal accuracy requirements in VizieR and across other CDS services)degpos.eq.ranullableindexed_DE.icrsDeclination (ICRS) (computed by VizieR, not part of the original data. The format may include more digits than the original data because of internal accuracy requirements in VizieR and across other CDS services)degpos.eq.decnullableindexed