PoS(ICRC2021)234 International th 12–23 July 2021 July 12–23 37 SICS CONFERENCE SICS CONFERENCE Berlin | Germany Berlin Berlin | Germany Cosmic Ray Conference Ray Cosmic ICRC 2021 THE ASTROPARTICLE PHY ICRC 2021 THEASTROPARTICLE PHY https://pos.sissa.it/ ONLINE and Douglas Bergman on behalf of the Telescope Array ∗ † [email protected], [email protected] International Cosmic Ray Conference (ICRC 2021) A complete list of collaborators see Pos(ICRC2021) Presenter ∗ † th Reconstruction of an EAS seenCherenkov using non-imaging yield Cherenkov of detectors requires many simulatingparameterizes EAS’s the both with the angular given distribution shower andshower, one can energy parameters. calculate distribution the Cherenkov photon of yield charged (at Since a particles fixedelectrons. point) within Shower from the In a Universality Cherenkov this cones of work, we compare botharrival time the distributions CWLD from (Cherenkov Cherenkov universality Width calculations Lateral with those Distribution) from(imaging and CORSIKA atmospheric iact Cherenkov telescope) simulations. Since universality calculationsless are computationally much expensive than shower simulation programscould like be CORSIKA, accomplished reconstruction more efficiently using Cherenkov data. Dept. of Physics & Astronomy andUniversity of High Utah, Energy Utah, Astrophysics Inst., USA E-mail: Copyright owned by the author(s) under the terms of the Creative Commons 0 © Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). 37 July 12th – 23rd, 2021 Online – Berlin, Germany Collaboration Isaac Buckland CHASM (CHerenkov Air Shower Model): SimulatingCherenkov the Profiles of Cosmic Ray Air Showers PoS(ICRC2021)234 of max # Isaac Buckland at 863 g/cm2, max - refer to the atmospheric depth max # and max - 2 The simulation of cosmic ray air showers is a computationally expensive process. This work Shower universality is the principle that properties of secondary particles in an air shower such An efficient Cherenkov signal simulation will enable a hybrid analysis of the low-energy To demonstrate the veracity of the Cherenkov universality model, we generated a Cherenkov illustrates how shower universality can beray air used showers. to The CHASM simulate python the moduleand was Cherenkov is developed light for intended all profile shower to geometries of be and cosmic packages profiles, a like computationally efficient CORSIKA. alternative CHASM to iscurrent Monte progress still Carlo and air functionality. in shower We development. present simulation simulationsshower of This Cherenkov types, distributions work from as various is well meantTelescope) extension. as to comparisons showcase its to CORSIKA’s IACT (Imaging Atmospheric Cherenkov 2. What is Shower Universality? as propagation direction, energy, and lateraldistributions spread [1][ can be2]. represented bysecondary These universal particle parameterized parameterizations properties such vary as as energyenergy (i.e. a interval the shower will directional develops be distribution and narrower ofCherenkov for particles take light higher in into in a energies). given account a Charged cone particlesin determined in which by a they particle shower propagate. energy will andtable produce Published of the fits Cherenkov atmospheric angular to index distributions secondary of atshower particle various refraction development. atmospheric distributions CHASM indices generates were of a used refraction showerthe to profile and Cherenkov in create stages table the of a to Earth’s calculate atmosphere, the then photon accesses yield at user defined locations. 3. NICHE (Non Imaging CHErenkov) and TALE (Telescope Array Low Energy) cosmic ray spectrum using dataImaging from CHErenkov) detectors both near the the Middle TALE Drum fluorescence telescopearray site. detector relative to In and1 Figure the thewe position see NICHE the ofof (Non NICHE the view. Middle Drum The observatory, lying NICHETube) directly sensitive detectors beneath to TALE’s are Cherenkov field light simple between lightperformed 300 looking buckets and for coincidence 450 consisting events nm. between of NICHENICHE a There and TALE. event is PMT In with currently2, Figure the (Photo-Multiplier we an Cherenkov see signal analysis a being sweeping sample diagonally through the array. 4. Universality vs. CORSIKA light profile using universality, and comparedsion. it to This a downward profile proton generated shower by has CORSIKA’s IACT a exten- primary energy of 108 GeV, Universality of Cherenkov Light in EAS 1. Introduction 67 million particles, and a polar angle of 10 degrees. at shower maximum and the maximumcounters number were of defined secondary at shower the particles, altitude respectively. of IACT the lowest Telescope Array NICHE counter (1564 m above PoS(ICRC2021)234 Isaac Buckland 3 Left: the orientation of the NICHE array with respect to the Middle Drum observatory. Right: Event display for NICHE event. The circle size of each triggered detector is scaled by the signal Figure 2: pulse area. The time of each trigger is represented by its color. Figure 1: One of the NICHE counters with Middle Drum in the background Universality of Cherenkov Light in EAS PoS(ICRC2021)234 Isaac Buckland . 4 max - of 80 million particles, and a first-interaction height of 10 Km. max # of 785 g/cm2, an max Left: Comparison of Cherenkov lateral distribution from both CORSIKA and universality. Right: - As photons propagate in the atmosphere to the counting location, they are delayed compared 4 Figure is a plot of the Cherenkov signal at the counter plane. Each pixel represents one The first iteration of CHASM is being tested for implementation in nuSpaceSim, a compre- to the speed ofvertically light traveling in photon a would vacuum. experienceorbital by observations For the (nuSpaceSim), downward cosine showers, photons of itatmosphere propagate its is before for polar sufficient they thousands angle. to enter ofpropagation divide the kilometers with In the vacuum in respect the delay of the to context a the space. upper of atmosphere becomes As steeper the compared photons to their get polar higher, angle their with angle of 6. Atmospheric Curvature and Photon Timing photon counter location. The ringCherenkov cone where at the development stages maximum near signal is found forms due to the shower’s The resulting Cherenkov light was calculatedan at altitude an of array 525 of locations km.coordinate normal system used4 to Figure by theshows CHASM. shower the The axis origin showersurface. at is orientation, Standard where as physics the spherical shower well axis coordinate as intersects conventions the with apply the for x Earth’s the and shower polar z angle. axes of the Figure 3: Comparison of arrival time distribution from both CORSIKA and universality. sea level). The total numbershown of in photons collected3, Figure at and increasing theshower distances core from arrival in the3. time Figure shower core distributions are are compared for a counter5. 70 m from Hypothetical the Tau Primary Upward Air Shower hensive neutrino simulation package for space-based andskimming suborbital the experiments Earth [3]. may interact Tau neutrinos via theing charged-current interaction tau in particle the leaves Earth’s the crust. Earth Theshower. and result- For decays, serving this as demo, the an primarywith upward an particle shower in profile an was upward generated going using air the Gaisser-Hillas function Universality of Cherenkov Light in EAS PoS(ICRC2021)234 Isaac Buckland 5 Top: Diagram of an upward air shower axis showing the orientation of an orbital counter array. Figure 4: Bottom: Cherenkov light signal atkm. an orbital counter array normal to the shower axis at an altitude of 525 Universality of Cherenkov Light in EAS PoS(ICRC2021)234 (1) Isaac Buckland ) 'ℎ ℎ 2 , there is about a seven nanosecond delay if + + 2 ?? ' A ( A + 2 6 2 ℎ = 0 \ cos Left: Diagram of the geometry used to account for the curvature of the atmosphere in upward While comparisons between our model and CORSIKA are consistent for most regimes, we For the upward shower shown in4 Figures and [1] S. Lafebre, et al., Astropart. Phys. 31 (2009)[2] 243. M. Giller, et al., J. Phys. G 30[3] (2004) 97. J. Krizmanic, et al., PoS(ICRC2019)936. see disagreements in total Cherenkov production closecenter (within of the 50 shower’s footprint, m as forshower downward well showers) stages. as to Perturbations inconsistent the to arrival the times model formainly are photons result necessary produced from to in our compensate early approximation for these ofIn differences, Cherenkov production reality, which secondary being charged localized particles to spread theand out shower a in axis. counter space, will and generate those a travellingof light in CHASM signal between will the slightly contain axis sooner methods than for our smoothing model out predicts. these inconsistencies. Future iterations References 7. Discussion Figure 5: shower timing calculations. Right:neglected Comparison and of accounted arrival for. time distribution when atmospheric curvature is respect to the original z-axis.via the This law difference of cosines was on calculated the as inscribed a triangle function in5 of Figure and atmospheric1. equation height the curvature of the atmospherearrival is time neglected. distribution at5 Figure one ofshows the the counters both in the the original ring and peak. corrected Universality of Cherenkov Light in EAS PoS(ICRC2021)234 , , , , , , , , , , , , , , , , 3 7 3 4 3 3 3 4 11 19 13 13 13 21 11 13 , 17 , T. Seki , S. Udo , J.H. Kim 4 5 , Y. Omura , M. Takeda , D. Shinto 34 , I. Buckland 6 , T. Inadomi 7 3 26 , Y. Yoshioka 11 , R. Fukushima , F. Kakimoto , G.B. Thomson , J.N. Matthews , T. Nakamura 19 9 3 4 , 16 , D.C. Rodriguez 24 7 Isaac Buckland 3 , M. Kuznetsov , K. Sato 17 13 , H.B. Kim , H.S. Shin , D. Ikeda 14 , T. Okuda , S.A. Blake , Y. Uchihori 29 12 3 19 , M. Takamura 25 , F. Yoshida 4 , 6 4 , K. Kadota , S.B. Thomas 3 4 , K. Sano , T. Matsuyama 4 , T. Nakamura 4 , E. Kido , M. Fukushima , J. Remington , V. Kuzmin 7 13 4 , Y. Oku 28 13 , B.K. Shin 7 , K. Honda , 7 7 17 , K. Yashiro , D.R. Bergman , Y. Takahashi , Y. Tanoue 3 36 4 , C.C.H. Jui , Y. Tsunesada 32 , N. Sakurai 4 15 7 , K. Kawata 2 , S. Kurisu , H. Ohoka , R. Fujiwara , H. Matsumiya 7 4 , R. Higuchi 13 , R. Nakamura 12 4 , J. Yang 11 , J.W. Belz , H. Shimodaira , Y. Takagi 11 3 7 2 , T. Sako , M.S. Pshirkov , S. Jeong , M. Tanaka , R. Tsuda 7 3 15 31 17 , S. Kawana , K. Fujita 4 7 , Y. Kubota , M. Ohnishi , K. Nakai , K. Hibino 4 , K. Machida 25 14 11 , 7 , T. Shibata , T. Suzawa 4 23 3 , , M. Potts , K. Yamazaki 19 , N. Sakaki 3 , K. Tanaka 15 13 , E. Barcikowski 13 4 4 , S. Troitsky , H.M. Jeong , K. Fujisue 13 8 13 , S. Kawakami , S. Ogio 4 20 , S. Nagataki , S. Kishigami , N. Hayashida , Y. Arai 3 , N. Shibata , Y. Saito 4 3 , I.H. Park Libre de Bruxelles, Brussels, Belgium 4 10 , H. Tanaka , T.A. Stroman 12 , T. Fujii 3 27 © 7 19 , J.P. Lundquist , M. Yamamoto , T. Tomida 17 , H. Oda 7 7 , H. Iwakura 33 , H. Kawai 3 , I. Myers 19 , M. Allen 3 12 , , R. Sahara , Y. Kimura , F. Shibata 1 7 , M. Hayashi 15 , S. Ozawa 3 13 , B.T. Stokes , Y. Tameda 4 , K. Yada 7 3 , M. Chikawa 13 6 Department of Physics, Loyola University Chicago, Chicago, Illinois, USA , T. Nonaka , D. Ivanov , H. Tokuno 13 , S. Kasami 3 1 orique, Università 14 17 18 © , K. Mukai 4 , H. Sagawa , W. Hanlon , B. Lubsandorzhiev , N. Sone , S.W. Kim , T. Wong , M. Takita 3 3 29 , J. Chiba 15 , Y. Shibasaki 15 , A. Oshima 35 , T. Abu-Zayyad 30 5 3 4 2 , H. Ito 12 , I. Tkachev , A. Nakazawa , D. Ryu , and Z. Zundel 21 , K. Kasahara , 13 , M. Abe , F. Urban 17 , K.H. Lee 17 17 , A. Taketa 1 , 17 , P. Sokolsky 7 , R. Gonzalez , P.D. Shah 7 13 , M. Minamino , M.H. Kim 22 3 , R. Onogi , T. Ishii 3 7 4 3 , B.G. Cheon 2 3 14 Department of Research Planning and Promotion, Quantum Medical Science Directorate, National Institutes for Quantum and Information Engineering Graduate School of ScienceFaculty and of Technology, Engineering, Shinshu Kanagawa University, Nagano, University, Yokohama, Nagano, Kanagawa, Japan Interdisciplinary Japan Graduate School of Medicine andAcademic Engineering, Assembly School University of of Yamanashi, Science Kofu, and Yamanashi,Astrophysical Japan Technology Big Institute Bang of Laboratory, Engineering, RIKEN, Shinshu Wako, Saitama, University,Department Nagano, Japan of Nagano, Japan Physics, Sungkyunkwan University, Jang-an-gu,Department Suwon, Korea of Physics, Tokyo City University, Setagaya-ku,Institute Tokyo, Japan for Nuclear Research of theFaculty Russian of Academy Systems of Engineering Sciences, and Moscow, Russia Science, Shibaura Institute of Technology, Minato-ku, Tokyo,Department Japan of Physics, Chiba University, Chiba,Service Chiba, de Japan Physique Thà Department of Physics, Yonsei University, Seodaemun-gu, Seoul,Center Korea for Astrophysics and Cosmology, University ofFaculty Nova of Gorica, Science, Nova Kochi Gorica, University, Kochi, Slovenia Kochi,Nambu Japan Yoichiro Institute of Theoretical andDepartment Experimental of Physics, Osaka Physical Sciences, City Ritsumeikan University, Osaka, University, Kusatsu, Osaka, Shiga, Japan Japan Sternberg Astronomical Institute, Moscow M.V. Lomonosov StateDepartment University, of Moscow, Russia Physics, School of NaturalEarthquake Sciences, Research Ulsan Institute, National University Institute of of Tokyo, Bunkyo-ku,Graduate Science Tokyo, School and Japan of Technology, UNIST-gil, Information Ulsan, Sciences, Korea HiroshimaInstitute City of University, Particle Hiroshima, and Hiroshima, Nuclear Japan Studies,Graduate KEK, School Tsukuba, of Ibaraki, Science Japan and Engineering, Tokyo Institute of Technology, Meguro, Tokyo, Japan CEICO, Institute of Physics, Czech AcademyDepartment of of Sciences, Physics Prague, and Czech Institute Republic for the Early Universe, Ewha Womans University, Seodaaemun-gu, Seoul, Korea Quantum ICT Advanced Development Center, National Institute for Information and Communications Technology, Koganei, Tokyo, Department of Engineering Science, Faculty of Engineering, Osaka Electro-Communication University, Neyagawa-shi, Osaka, Japan Kavli Institute for the Physics and Mathematics of the Universe (WPI), Todai Institutes for Advanced Study, University of Tokyo, The Hakubi Center for Advanced Research and Graduate School of Science, Kyoto University, Kitashirakawa-Oiwakecho, Sakyo-ku, The Graduate School of Science andHigh Engineering, Energy Saitama Astrophysics Institute University, Saitama, and Saitama, DepartmentGraduate Japan of School Physics of and Science, Astronomy, University Osaka of CityDepartment Utah, University, of Osaka, Salt Physics Osaka, Lake and Japan City, The Utah, Research USA Department Institute of of Physics, Natural Tokyo Science, University of Hanyang University, Science,Institute Seongdong-gu, Noda, for Seoul, Cosmic Chiba, Korea Ray Japan Research, University of Tokyo, Kashiwa, Chiba, Japan P. Tinyakov T. Uehama 3 4 5 6 7 8 Kyoto, Japan 9 Kashiwa, Chiba, Japan 10 11 12 13 14 15 16 17 18 19 20 21 J.D. Smith R. Takeishi Y. Zhezher 2 22 23 24 25 26 27 Japan 28 29 30 31 32 33 34 Radiological Science and Technology, Chiba,35 Chiba, Japan 36 R. Mayta Y. Nakamura M. Ono K. Sekino Y.J. Kwon G.I. Rubtsov J.H. Kim Universality of Cherenkov Light in EAS Full Authors List: Telescope Array Collaboration R.U. Abbasi O. Kalashev R. Cady N. Inoue G. Furlich