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First Upper Limits on the Radar Cross Section of Cosmic-Ray Induced Extensive Air Showers

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First Upper Limits on the Radar Cross Section of Cosmic-Ray Induced Extensive Air Showers BNL-114194-2017-JA First Upper Limits on the Radar Cross Section of Cosmic-Ray Induced Extensive Air Showers H. Takai Submitted to the Journal of Astroparticle Physics August 2017 Physics Department Brookhaven National Laboratory U.S. Department of Energy USDOE Office of Science (SC), High Energy Physics (HEP) (SC-25) Notice: This manuscript has been authored by employees of Brookhaven Science Associates, LLC under Contract No. DE- SC0012704 with the U.S. Department of Energy. The publisher by accepting the manuscript for publication acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. DISCLAIMER This report was prepared as an account of work sponsored by an agency of the United States Government. Neither the United States Government nor any agency thereof, nor any of their employees, nor any of their contractors, subcontractors, or their employees, makes any warranty, express or implied, or assumes any legal liability or responsibility for the accuracy, completeness, or any third party’s use or the results of such use of any information, apparatus, product, or process disclosed, or represents that its use would not infringe privately owned rights. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not necessarily constitute or imply its endorsement, recommendation, or favoring by the United States Government or any agency thereof or its contractors or subcontractors. The views and opinions of authors expressed herein do not necessarily state or reflect those of the United States Government or any agency thereof. BNL-114194-2017-JA First Upper Limits on the Radar Cross Section of Cosmic-Ray Induced Extensive Air Showers R.U. Abbasia, M. Abeb, M. Abou Bakr Othmanc, T.Abu-Zayyada, M. Allena, R. Andersona, R. Azumad, E. Barcikowskia, J.W. Belza,∗, D.R. Bergmana, D. Bessone,f, S.A. Blakea, M. Byrnea, R. Cadya, M.J. Chaeg, B.G. Cheonh, J. Chibai, M. Chikawaj, W.R. Chok, B. Farhang-Boroujenyc, T. Fujiil, M. Fukushimal,m, W.H. Gillmann, T. Gotoo, W. Hanlona, J.C. Hansone, Y. Hayashio, N. Hayashidap, K. Hibinop, K. Hondaq, D. Ikedal, N. Inoueb, T. Ishiiq, R. Ishimorid, H. Itor, D. Ivanova, C. Jayanthmurthyc, C.C.H. Juia, K. Kadotas, F. Kakimotod, O. Kalashevt, K. Kasaharau, H. Kawaiv, S. Kawakamio, S. Kawanab, K. Kawatal, E. Kidol, H.B. Kimh, J.H. Kima, J.H. Kimw, S. Kitamurad, Y. Kitamurad, S. Kunware, V. Kuzmint, Y.J. Kwonk, J. Lana, S.I. Limg, J.P. Lundquista, K. Machidaq, K. Martensm, T. Matsudax, T. Matsuyamao, J.N. Matthewsa, M. Minaminoo, K. Mukaiq, I. Myersa, K. Nagasawab, S. Nagatakir, T. Nakamuray, T. Nonakal, A. Nozatoj, S. Ogioo, J. Ogurad, M. Ohnishil, H. Ohokal, K. Okil, T. Okudaz, M. Onoaa, A. Oshimaab, S. Ozawau, I.H. Parkac, S. Prohirae, M.S. Pshirkovad,t, A. Rezazadeh-Reyhanic, D.C. Rodrigueza, G. Rubtsovt, D. Ryuw, H. Sagawal, N. Sakuraio, A.L. Sampsona, L.M. Scottae, D. Schurigc, P.D. Shaha, F. Shibataq, T. Shibatal, H. Shimodairal, B.K. Shinh, J.D. Smitha, P. Sokolskya, R.W. Springera, B.T. Stokesa, S.R. Strattona,ae, T.A. Stromana, T. Suzawab, H. Takaiaf, M. Takamurai, M. Takedal, R. Takeishil, A. Taketaag, M. Takital, Y. Tamedap, H. Tanakao, K. Tanakaah, M. Tanakax, S.B. Thomasa, G.B. Thomsona, P. Tinyakovt,ai, I. Tkachevt, H. Tokunod, T. Tomidaaj, S. Troitskyt, Y. Tsunesadao, K. Tsutsumid, Y. Uchihoriak, S. Udop, F. Urbanai, G. Vasiloffa, S. Venkateshc, T. Wonga, R. Yamaneo, H. Yamaokax, K. Yamazakio, J. Yangg, K. Yashiroi, Y. Yonedao, S. Yoshidav, H. Yoshiial, R. Zollingera, Z. Zundela aHigh Energy Astrophysics Institute and Department of Physics and Astronomy, University of Utah, Salt Lake City, Utah, USA bThe Graduate School of Science and Engineering, Saitama University, Saitama, Saitama, Japan cDepartment of Electrical and Computer Engineering, University of Utah, Salt Lake City, Utah, USA dGraduate School of Science and Engineering, Tokyo Institute of Technology, Meguro, Tokyo, Japan eUniversity of Kansas, Lawrence, Kansas, USA fMoscow Engineering and Physics Institute, Moscow, Russia gDepartment of Physics and Institute for the Early Universe, Ewha Womans University, Seodaaemun-gu, Seoul, Korea hDepartment of Physics and The Research Institute of Natural Science, Hanyang University, Seongdong-gu, Seoul, Korea iDepartment of Physics, Tokyo University of Science, Noda, Chiba, Japan jDepartment of Physics, Kinki University, Higashi Osaka, Osaka, Japan kDepartment of Physics, Yonsei University, Seodaemun-gu, Seoul, Korea lInstitute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba, Japan mKavli Institute for the Physics and Mathematics of the Universe (WPI), Todai Institutes for Advanced Study, the University of Tokyo, Kashiwa, Chiba, Japan nGillman & Associates, Salt Lake City, Utah, USA oGraduate School of Science, Osaka City University, Osaka, Osaka, Japan pFaculty of Engineering, Kanagawa University, Yokohama, Kanagawa, Japan qInterdisciplinary Graduate School of Medicine and Engineering, University of Yamanashi, Kofu, Yamanashi, Japan rAstrophysical Big Bang Laboratory, RIKEN, Wako, Saitama, Japan sDepartment of Physics, Tokyo City University, Setagaya-ku, Tokyo, Japan tNational Nuclear Research University, Moscow Engineering Physics Institute, Moscow, Russia uAdvanced Research Institute for Science and Engineering, Waseda University, Shinjuku-ku, Tokyo, Japan vDepartment of Physics, Chiba University, Chiba, Chiba, Japan wDepartment of Physics, School of Natural Sciences, Ulsan National Institute of Science and Technology, UNIST-gil, Ulsan, Korea xInstitute of Particle and Nuclear Studies, KEK, Tsukuba, Ibaraki, Japan yFaculty of Science, Kochi University, Kochi, Kochi, Japan zDepartment of Physical Sciences, Ritsumeikan University, Kusatsu, Shiga, Japa arXiv:1603.05217v1 [astro-ph.IM] 16 Mar 2016 aaDepartment of Physics, Kyushu University, Fukuoka, Fukuoka, Japan abEngineering Science Laboratory, Chubu University, Kasugai, Aichi, Japan acDepartment of Physics, Sungkyunkwan University, Jang-an-gu, Suwon, Korea adSternberg Astronomical Institute Moscow M.V.Lomonosov State University, Moscow, Russia aeDepartment of Physics and Astronomy, Rutgers University - The State University of New Jersey, Piscataway, New Jersey, USA ∗Corresponding Author. Tel.: +01 801 585-9620. Addr.: 115 S 1400 E #201 JFB Email address: [email protected] (J.W. Belz) afBrookhaven National Laboratory, Upton, New York, USA agEarthquake Research Institute, University of Tokyo, Bunkyo-ku, Tokyo, Japan ahGraduate School of Information Sciences, Hiroshima City University, Hiroshima, Hiroshima, Japan aiService de Physique The´orique, Universite´ Libre de Bruxelles, Brussels, Belgium ajDepartment of Computer Science and Engineering, Shinshu University, Nagano, Nagano, Japan akNational Institute of Radiological Science, Chiba, Chiba, Japan alDepartment of Physics, Ehime University, Matsuyama, Ehime, Japan Abstract TARA (Telescope Array Radar) is a cosmic ray radar detection experiment colocated with Telescope Array, the conventional surface scintillation detector (SD) and fluorescence telescope detector (FD) near Delta, Utah, U.S.A. The TARA detector combines a 40 kW, 54.1 MHz VHF transmitter and high-gain transmitting antenna which broadcasts the radar carrier over the SD array and within the FD field of view, towards a 250 MS/s DAQ receiver. TARA has been collecting data since 2013 with the primary goal of observing the radar signatures of extensive air showers (EAS). Simulations indicate that echoes are expected to be short in duration (∼ 10 µs) and exhibit rapidly changing frequency, with rates on the order 1 MHz/µs. The EAS radar cross-section (RCS) is currently unknown although it is the subject of over 70 years of speculation. A novel signal search technique is described in which the expected radar echo of a particular air shower is used as a matched filter template and compared to waveforms obtained by triggering the radar DAQ using the Telescope Array fluorescence detector. No evidence for the scattering of radio frequency radiation by EAS is obtained to date. We report the first quantitative RCS upper limits using EAS that triggered the Telescope Array Fluorescence Detector. Keywords: cosmic ray, radar, digital signal processing, radar cross-section 1. Introduction for UHECR detection. TARA is the most advanced CR radar detection experiment to date, improving upon Ultra-high energy cosmic ray (UHECR, primary en- 18 other experiments with several key attributes: ergy E0 > 10 eV) research is limited primarily by low flux. There are currently two dominant detection tech- • The transmitter is under the direct control of ex- niques, surface detectors (SD) comprised of plastic scin- perimenters, and in a radio-quiet area isolated from tillator or water Cherenkov detectors, and fluorescence other radio frequency (RF) sources. The power and telescope detectors (FD). Conventional detection meth- radiation pattern are known at all times. ods have been successful in mapping out the UHECR spectrum, observing the GZK cutoff [1, 2, 3] and locat- • Forward power up to 40 kW and gain exceeding ing a potential “hotspot” in CR arrival directions [4]. 20 dB maximize energy density in the radar field. However, large SD arrays are expensive to build and maintain, and FD telescopes have limited statistics due • Continuous wave (CW) transmission gives 100% to their low duty cycle
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