J/ApJ/907/L30ivo://CDS.VizieR/J/ApJ/907/L30doi:10.26093/cds/vizier.19079030CDSAlbert A.Alfaro R.Alvarez C.Camacho J.R.A.Arteaga-Velazquez J.C.,Arunbabu K.P.Rojas D.A.Ayala Solares H.A.Baghmanyan V.,Belmont-Moreno E.BenZvi S.Y.Brisbois C.Capistran T.Carraminana A.,Casanova S.Cotti U.Cotzomi J.De la Fuente E.Hernandez R.D.,Dingus B.L.DuVernois M.A.Durocher M.Diaz-Velez J.C.Engel K.,Espinoza C.Fang K.Fleischhack H.Fraija N.Galvan-Gamez A.Garcia D.,Garcia-Gonzalez J.A.Garfias F.Giacinti G.Gonzalez M.M.Goodman J.A.,Harding J.P.Hona B.Huang D.Hueyotl-Zahuantitla F.Huntemeyer P.,Iriarte A.Jardin-Blicq A.Joshi V.Kunde G.J.Lara A.Lee W.H.,Vargas H.L.Linnemann J.T.Longinotti A.L.Luis-Raya G.Lundeen J.,Malone K.Marandon V.Martinez O.Martinez-Castro J.Matthews J.A.,Miranda-Romagnoli P.Moreno E.Mostafa M.Nayerhoda A.Nellen L.,Newbold M.Nisa M.U.Noriega-Papaqui R.Omodei N.Peisker A.,Araujo Y.P.Perez-Perez E.G.Rho C.D.Rosa-Gonzalez D.Salazar H.,Greus F.S.Sandoval A.Schneider M.Serna F.Springer R.W.,Tollefson K.Torres I.Torres-Escobedo R.Urena-Mena F.Villasenor L.,Willox E.Zhou H.de Leon C.2022-08-26T06:41:06Z2022-06-24T07:24:16ZCDS support team

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

cds-question@unistra.frgamma-ray-astronomyspectral-energy-distributionThe Earth is bombarded by ultrarelativistic particles, known as cosmic rays (CRs). CRs with energies up to a few PeV (=1015eV), the knee in the particle spectrum, are believed to have a Galactic origin. One or more factories of PeV CRs, or PeVatrons, must thus be active within our Galaxy. The direct detection of PeV protons from their sources is not possible since they are deflected in the Galactic magnetic fields. Hundred TeV {gamma}-rays from decaying {pi}0, produced when PeV CRs collide with the ambient gas, can provide the decisive evidence of proton acceleration up to the knee. Here we report the discovery by the High Altitude Water Cerenkov (HAWC) observatory of the {gamma}-ray source, HAWCJ1825-134, whose energy spectrum extends well beyond 200TeV without a break or cutoff. The source is found to be coincident with a giant molecular cloud. The ambient gas density is as high as 700protons/cm^3^. While the nature of this extreme accelerator remains unclear, CRs accelerated to energies of several PeV colliding with the ambient gas likely produce the observed radiation.2021ApJ...907L..30Ahttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/907/L30CatalogResearchIsServedByTAP VizieR generic servicerelated-toB/psr : ATNF Pulsar Catalogue (Manchester+, 2005)J/A+A/275/67 : Velocity Field of the outer Galaxy (Brand+ 1993)J/A+A/404/223 : 2MASS IR star clusters in the Galaxy (Bica+, 2003)J/ApJ/649/759 : Bubbles in the galactic disk (Churchwell+, 2006)J/ApJS/212/1 : The WISE catalog of Galactic HII regions (Anderson+, 2014)J/A+A/594/A116 : HI4PI spectra and column density maps (HI4PI team+, 2016)J/A+A/585/A101 : Milky Way global survey star clusters. V. (Kharchenko+, 2016)J/ApJ/834/57 : Milky Way molecular cloud from 12CO (Miville-Deschenes+, 2017)J/A+A/612/A1 : H.E.S.S. Galactic Plane Survey (HESS+, 2018)J/A+A/621/A116 : HESSJ1825-137 particle transport (H.E.S.S.Collaboration, 2019)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/907/L30https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/907/L30http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/907/L30https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/907/L30https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/907/L30http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/907/L30GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapGamma-raydefaultJ/ApJ/907/L30/fig2{gamma}-ray spectral energy distributionsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDIdentifiermeta.id;meta.maincharEmed[1.22/225] Median energyTeVphys.energy;stat.medianfloatFlux[4.9e-13/1.6e-11]? FluxTeV.cm**-2.s**-1phot.flux.density;em.gamma.harddoublenullableE_Flux[2e-13/5e-12]? Upper limit on FluxTeV.cm**-2.s**-1stat.error;stat.maxdoublenullablee_Flux[2e-13/6e-12]? Lower limit on FluxTeV.cm**-2.s**-1stat.error;phot.fluxdoublenullableLimitUpper limit flag; True or Falsemeta.codechar