Inference of the Mass Composition of Cosmic Rays with Energies from <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:msup><mml:mn>10</mml:mn><mml:mn>18.5</mml:mn></mml:msup></mml:math> to <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mrow><mml:mn>10</mml:mn></mml:mrow><mml:mrow><mml:mn>20</mml:mn></mml:mrow></mml:msup><mml:mtext> </mml:mtext><mml:mtext> </mml:mtext><mml:mi>eV</mml:mi></mml:mrow></mml:math> Using the Pierre Auger Observatory and Deep Learning
Adila Abdul HalimUniversity of AdelaideP. AbreuUniversidade de Lisboa—ULM. AgliettaINFNI. AllekotteBariloche Atomic CentreKévin Almeida CheminantInstitute of Nuclear Physics PANA. AlmelaInstituto de Tecnologías en Detección y AstropartículasRoberto AloisioINFN Laboratori Nazionali del Gran SassoJaime Álvarez-MuñizUniversidade de Santiago de CompostelaJuan Ammerman YebraUniversidade de Santiago de CompostelaGioacchino Alex AnastasiINFNL. AnchordoquiCity University of New YorkB. AndradaInstituto de Tecnologías en Detección y AstropartículasLuciana Andrade DouradoINFN Laboratori Nazionali del Gran SassoS. AndringaUniversidade de Lisboa—ULL. ApollonioINFNC. AramoP. R. Araújo FerreiraRWTH Aachen UniversityE. ArnoneINFNJuan Carlos Arteaga VelázquezUniversidad Michoacana de San Nicolás de HidalgoP. AssisUniversidade de Lisboa—ULGael Flores AvilaObservatorio Pierre Auger and Comisión Nacional de Energía AtómicaEmanuele AvoconeINFN Laboratori Nazionali del Gran SassoAlena BakalováInstitute of Physics of the Czech Academy of SciencesFelicia BarbatoINFN Laboratori Nazionali del Gran SassoAdriel Bartz MocellinColorado School of MinesCorinne BératUniversité Grenoble AlpesM. E. BertainaINFNGopal BhattaInstitute of Nuclear Physics PANMarta BianciottoINFNPeter L. BiermannUniversität Siegen, Department Physik-Experimentelle Teilchenphysik, Siegen, GermanyV. BinetInstituto de Física de Rosario (IFIR)Kathrin BismarkInstituto de Tecnologías en Detección y Astropartículas (CNEA, CONICET, UNSAM)Teresa BisterRadboud University NijmegenJonathan BiteauUniversité Paris-SaclayJiří BlažekInstitute of Physics of the Czech Academy of SciencesC. BleveUniversité Grenoble AlpesJ. BlümerKarlsruhe Institute of Technology (KIT)M. BoháčováInstitute of Physics of the Czech Academy of SciencesDenise BoncioliUniversità dell’AquilaC. BonifaziECyT-UNSAM and CONICETL. Bonneau ArbeletcheUniversidade Estadual de Campinas (UNICAMP)Nataliia BorodaiInstitute of Nuclear Physics PANJ. BrackCharles University, Faculty of Mathematics and Physics, Institute of Particle and Nuclear Physics, Prague, Czech RepublicP. G. Brichetto OrcheraInstituto de Tecnologías en Detección y AstropartículasF. L. BriechleRWTH Aachen UniversityA. BuenoUniversidad de Granada and C.A.F.P.ES. BuitinkVrije Universiteit BrusselsMario BuscemiINFNM. BüskenInstituto de Tecnologías en Detección y Astropartículas (CNEA, CONICET, UNSAM)Anthony BwembyaRadboud University NijmegenK. S. Caballero‐MoraUniversidad Autónoma de ChiapasS. Cabana-FreireUniversidade de Santiago de CompostelaLorenzo CaccianigaINFNF. CampuzanoConsejo Nacional de Investigaciones Científicas y TécnicasR. CarusoINFNA. CastellinaINFNF. CatalaniUniversidade de São PauloG. CataldiLorenzo CazonUniversidade de Santiago de CompostelaM. CerdaObservatorio Pierre AugerBerenika ČermákováKarlsruhe Institute of Technology (KIT)A. CermenatiINFN Laboratori Nazionali del Gran SassoC. DobrigkeitUniversidade Estadual de Campinas (UNICAMP)J. ChudobaInstitute of Physics of the Czech Academy of SciencesL. ChytkaPalacky UniversityR. W. ClayUniversity of AdelaideAgustín Cobos CeruttiInstituto de Tecnologías en Detección y AstropartículasRoberta ColalilloINFNM. R. ColucciaR. ConceiçãoUniversidade de Lisboa—ULAntonio CondorelliUniversité Paris-SaclayGiovanni ConsolatiINFNM. ConteINFNFabio ConvengaUniversità dell’AquilaD. Correia dos SantosUniversidade Federal do Rio de JaneiroP. J. CostaUniversidade de Lisboa—ULC. E. CovaultCase Western Reserve UniversityM. CristinzianiUniversität SiegenCarlo Salvattore Cruz SanchezUniversidad Nacional de La PlataS. DassoInstituto de Astronomía y Física del Espacio (IAFE, CONICET-UBA)K. DaumillerKarlsruhe Institute of Technology (KIT)B. R. DawsonUniversity of AdelaideR. M. de AlmeidaUniversidade Federal do Rio de JaneiroBeatriz de ErricoUniversidade Federal do Rio de JaneiroJoaquín de JesúsInstituto de Tecnologías en Detección y AstropartículasS. J. de JongRadboud University NijmegenJ. R. T. de Mello NetoUniversidade Federal do Rio de JaneiroI. De MitriINFN Laboratori Nazionali del Gran SassoJ. de OliveiraCiência e Tecnologia do Rio de Janeiro (IFRJ)Danelise de Oliveira FrancoF. de PalmaINFNV. de SouzaUniversidade de São PauloEmanuele De VitoINFNA. Del PopoloINFNO. DelignyUniversité Paris-SaclayN. DennerInstitute of Physics of the Czech Academy of SciencesL. DevalKarlsruhe Institute of Technology (KIT)A. di MatteoA John JoelUniversidad Nacional de San Agustin de ArequipaM. Dobre“Horia Hulubei” National Institute for Physics and Nuclear Engineering
ABI
Annotatsiya
We present measurements of the atmospheric depth of the shower maximum X_{max}, inferred for the first time on an event-by-event level using the surface detector of the Pierre Auger Observatory. Using deep learning, we were able to extend measurements of the X_{max} distributions up to energies of 100 EeV (10^{20} eV), not yet revealed by current measurements, providing new insights into the mass composition of cosmic rays at extreme energies. Gaining a 10-fold increase in statistics compared to the fluorescence detector data, we find evidence that the rate of change of the average X_{max} with the logarithm of energy features three breaks at 6.5±0.6(stat)±1(syst) EeV, 11±2(stat)±1(syst) EeV, and 31±5(stat)±3(syst) EeV, in the vicinity to the three prominent features (ankle, instep, suppression) of the cosmic-ray flux. The energy evolution of the mean and standard deviation of the measured X_{max} distributions indicates that the mass composition becomes increasingly heavier and purer, thus being incompatible with a large fraction of light nuclei between 50 and 100 EeV.
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