Search for EeV protons of galactic origin

R. U. Abbasi; M. Abe; T. Abu-Zayyad; M. Allen; R. Azuma; E. Barcikowski; J. W. Belz; D. R. Bergman; S. A. Blake; R. Cady; B. G. Cheon; J. Chiba; M. Chikawa; T. Fujii; M. Fukushima; T. Goto; W. Hanlon; Y. Hayashi; M. Hayashi; N. Hayashida; K. Hibino; K. Honda; D. Ikeda; N. Inoue; T. Ishii; R. Ishimori; H. Ito; D. Ivanov; C. C.H. Jui; K. Kadota; F. Kakimoto; O. Kalashev; K. Kasahara; H. Kawai; S. Kawakami; S. Kawana; K. Kawata; E. Kido; H. B. Kim; J. H. Kim; J. H. Kim; S. Kishigami; S. Kitamura; Y. Kitamura; V. Kuzmin; Y. J. Kwon; J. Lan; B. Lubsandorzhiev; J. P. Lundquist; K. Machida; K. Martens; T. Matsuda; T. Matsuyama; J. N. Matthews; M. Minamino; K. Mukai; I. Myers; K. Nagasawa; S. Nagataki; T. Nakamura; T. Nonaka; A. Nozato; S. Ogio; J. Ogura; M. Ohnishi; H. Ohoka; K. Oki; T. Okuda; M. Ono; R. Onogi; A. Oshima; S. Ozawa; I. H. Park; M. S. Pshirkov; D. C. Rodriguez; G. Rubtsov; D. Ryu; H. Sagawa; K. Saito; Y. Saito; N. Sakaki; N. Sakurai; L. M. Scott; K. Sekino; P. D. Shah; T. Shibata; F. Shibata; H. Shimodaira; B. K. Shin; H. S. Shin; J. D. Smith; P. Sokolsky; B. T. Stokes; S. R. Stratton; T. A. Stroman; T. Suzawa; Y. Takahashi; M. Takamura; M. Takeda; R. Takeishi; A. Taketa; M. Takita; Y. Tameda; M. Tanaka; K. Tanaka; H. Tanaka; S. B. Thomas; G. B. Thomson; P. Tinyakov; A. H. Tirone; I. Tkachev; H. Tokuno; T. Tomida; S. Troitsky; Y. Tsunesada; K. Tsutsumi; Y. Uchihori; S. Udo; F. Urban; T. Wong; R. Yamane; H. Yamaoka; K. Yamazaki; J. Yang; K. Yashiro; Y. Yoneda; S. Yoshida; H. Yoshii; R. Zollinger; Z. Zundel

doi:10.1016/j.astropartphys.2016.11.001

Search for EeV protons of galactic origin

R. U. Abbasi, M. Abe, T. Abu-Zayyad, M. Allen, R. Azuma, E. Barcikowski, J. W. Belz, D. R. Bergman, S. A. Blake, R. Cady, B. G. Cheon, J. Chiba, M. Chikawa, T. Fujii, M. Fukushima, T. Goto, W. Hanlon, Y. Hayashi, M. Hayashi, N. HayashidaK. Hibino, K. Honda, D. Ikeda, N. Inoue, T. Ishii, R. Ishimori, H. Ito, D. Ivanov, C. C.H. Jui, K. Kadota, F. Kakimoto, O. Kalashev, K. Kasahara, H. Kawai, S. Kawakami, S. Kawana, K. Kawata, E. Kido, H. B. Kim, J. H. Kim, J. H. Kim, S. Kishigami, S. Kitamura, Y. Kitamura, V. Kuzmin, Y. J. Kwon, J. Lan, B. Lubsandorzhiev, J. P. Lundquist, K. Machida, K. Martens, T. Matsuda, T. Matsuyama, J. N. Matthews, M. Minamino, K. Mukai, I. Myers, K. Nagasawa, S. Nagataki, T. Nakamura, T. Nonaka, A. Nozato, S. Ogio, J. Ogura, M. Ohnishi, H. Ohoka, K. Oki, T. Okuda, M. Ono, R. Onogi, A. Oshima, S. Ozawa, I. H. Park, M. S. Pshirkov, D. C. Rodriguez, G. Rubtsov, D. Ryu, H. Sagawa, K. Saito, Y. Saito, N. Sakaki, N. Sakurai, L. M. Scott, K. Sekino, P. D. Shah, T. Shibata, F. Shibata, H. Shimodaira, B. K. Shin, H. S. Shin, J. D. Smith, P. Sokolsky, B. T. Stokes, S. R. Stratton, T. A. Stroman, T. Suzawa, Y. Takahashi, M. Takamura, M. Takeda, R. Takeishi, A. Taketa, M. Takita, Y. Tameda, M. Tanaka, K. Tanaka, H. Tanaka, S. B. Thomas, G. B. Thomson, P. Tinyakov, A. H. Tirone, I. Tkachev, H. Tokuno, T. Tomida, S. Troitsky, Y. Tsunesada, K. Tsutsumi, Y. Uchihori, S. Udo, F. Urban, T. Wong, R. Yamane, H. Yamaoka, K. Yamazaki, J. Yang, K. Yashiro, Y. Yoneda, S. Yoshida, H. Yoshii, R. Zollinger, Z. Zundel

Department of Physics

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23 Citations (Scopus)

Abstract

Cosmic rays in the energy range 10^18.0–10^18.5 eV are thought to have a light, probably protonic, composition. To study their origin one can search for anisotropy in their arrival directions. Extragalactic cosmic rays should be isotropic, but galactic cosmic rays of this type should be seen mostly along the galactic plane, and there should be a shortage of events coming from directions near the galactic anticenter. This is due to the fact that, under the influence of the galactic magnetic field, the transition from ballistic to diffusive behavior is well advanced, and this qualitative picture persists over the whole energy range. Guided by models of the galactic magnetic field that indicate that the enhancement along the galactic plane should have a standard deviation of about 20° in galactic latitude, and the deficit in the galactic anticenter direction should have a standard deviation of about 50° in galactic longitude, we use the data of the Telescope Array surface detector in 10^18.0 to 10^18.5 eV energy range to search for these effects. The data are isotropic. Neither an enhancement along the galactic plane nor a deficit in the galactic anticenter direction is found. Using these data we place an upper limit on the fraction of EeV cosmic rays of galactic origin at 1.3% at 95% confidence level.

Original language	English
Pages (from-to)	21-26
Number of pages	6
Journal	Astroparticle Physics
Volume	86
DOIs	https://doi.org/10.1016/j.astropartphys.2016.11.001
Publication status	Published - 2017 Jan 1

Bibliographical note

Funding Information:
The Telescope Array experiment is supported by the Japan Society for the Promotion of Science through Grants-in-Aid for Scientific Research on Specially Promoted Research ( 21000002 ) “Extreme Phenomena in the Universe Explored by Highest Energy Cosmic Rays” and for Scientific Research ( 19104006 ), and the Inter-University Research Program of the Institute for Cosmic Ray Research; by the U.S. National Science Foundation awards PHY-0307098 , PHY-0601915 , PHY-0649681 , PHY-0703893 , PHY-0758342 , PHY-0848320 , PHY-1069280 , PHY-1069286 , PHY-1404495 and PHY-1404502 ; by the National Research Foundation of Korea ( 2015R1A2A1A01006870 , 2015R1A2A1A15055344 , 2016R1A5A1013277 , 2007-0093860, 2016R1A2B4014967 ); by the Russian Academy of Sciences, RFBR grant 16-02-00962a (INR), IISN project No. 4.4502.13 , and Belgian Science Policy under IUAP VII/37 (ULB) . The foundations of Dr. Ezekiel R. and Edna Wattis Dumke, Willard L. Eccles, and George S. and Dolores Doré Eccles all helped with generous donations. The State of Utah supported the project through its Economic Development Board , and the University of Utah through the Office of the Vice President for Research. The experimental site became available through the cooperation of the Utah School and Institutional Trust Lands Administration (SITLA), U.S. Bureau of Land Management (BLM), and the U.S. Air Force. We appreciate the assistance of the State of Utah and Fillmore offices of the BLM in crafting the Plan of Development for the site. We also wish to thank the people and the officials of Millard County, Utah for their steadfast and warm support. We gratefully acknowledge the contributions from the technical staffs of our home institutions. An allocation of computer time from the Center for High Performance Computing at the University of Utah is gratefully acknowledged.

Publisher Copyright:
© 2016

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics

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10.1016/j.astropartphys.2016.11.001

Cite this

Abbasi, R. U., Abe, M., Abu-Zayyad, T., Allen, M., Azuma, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Cady, R., Cheon, B. G., Chiba, J., Chikawa, M., Fujii, T., Fukushima, M., Goto, T., Hanlon, W., Hayashi, Y., Hayashi, M., ... Zundel, Z. (2017). Search for EeV protons of galactic origin. Astroparticle Physics, 86, 21-26. https://doi.org/10.1016/j.astropartphys.2016.11.001

@article{46913525d64046718401cc41a8f9252f,

title = "Search for EeV protons of galactic origin",

abstract = "Cosmic rays in the energy range 1018.0–1018.5 eV are thought to have a light, probably protonic, composition. To study their origin one can search for anisotropy in their arrival directions. Extragalactic cosmic rays should be isotropic, but galactic cosmic rays of this type should be seen mostly along the galactic plane, and there should be a shortage of events coming from directions near the galactic anticenter. This is due to the fact that, under the influence of the galactic magnetic field, the transition from ballistic to diffusive behavior is well advanced, and this qualitative picture persists over the whole energy range. Guided by models of the galactic magnetic field that indicate that the enhancement along the galactic plane should have a standard deviation of about 20° in galactic latitude, and the deficit in the galactic anticenter direction should have a standard deviation of about 50° in galactic longitude, we use the data of the Telescope Array surface detector in 1018.0 to 1018.5 eV energy range to search for these effects. The data are isotropic. Neither an enhancement along the galactic plane nor a deficit in the galactic anticenter direction is found. Using these data we place an upper limit on the fraction of EeV cosmic rays of galactic origin at 1.3% at 95% confidence level.",

author = "Abbasi, {R. U.} and M. Abe and T. Abu-Zayyad and M. Allen and R. Azuma and E. Barcikowski and Belz, {J. W.} and Bergman, {D. R.} and Blake, {S. A.} and R. Cady and Cheon, {B. G.} and J. Chiba and M. Chikawa and T. Fujii and M. Fukushima and T. Goto and W. Hanlon and Y. Hayashi and M. Hayashi and N. Hayashida and K. Hibino and K. Honda and D. Ikeda and N. Inoue and T. Ishii and R. Ishimori and H. Ito and D. Ivanov and Jui, {C. C.H.} and K. Kadota and F. Kakimoto and O. Kalashev and K. Kasahara and H. Kawai and S. Kawakami and S. Kawana and K. Kawata and E. Kido and Kim, {H. B.} and Kim, {J. H.} and Kim, {J. H.} and S. Kishigami and S. Kitamura and Y. Kitamura and V. Kuzmin and Kwon, {Y. J.} and J. Lan and B. Lubsandorzhiev and Lundquist, {J. P.} and K. Machida and K. Martens and T. Matsuda and T. Matsuyama and Matthews, {J. N.} and M. Minamino and K. Mukai and I. Myers and K. Nagasawa and S. Nagataki and T. Nakamura and T. Nonaka and A. Nozato and S. Ogio and J. Ogura and M. Ohnishi and H. Ohoka and K. Oki and T. Okuda and M. Ono and R. Onogi and A. Oshima and S. Ozawa and Park, {I. H.} and Pshirkov, {M. S.} and Rodriguez, {D. C.} and G. Rubtsov and D. Ryu and H. Sagawa and K. Saito and Y. Saito and N. Sakaki and N. Sakurai and Scott, {L. M.} and K. Sekino and Shah, {P. D.} and T. Shibata and F. Shibata and H. Shimodaira and Shin, {B. K.} and Shin, {H. S.} and Smith, {J. D.} and P. Sokolsky and Stokes, {B. T.} and Stratton, {S. R.} and Stroman, {T. A.} and T. Suzawa and Y. Takahashi and M. Takamura and M. Takeda and R. Takeishi and A. Taketa and M. Takita and Y. Tameda and M. Tanaka and K. Tanaka and H. Tanaka and Thomas, {S. B.} and Thomson, {G. B.} and P. Tinyakov and Tirone, {A. H.} and I. Tkachev and H. Tokuno and T. Tomida and S. Troitsky and Y. Tsunesada and K. Tsutsumi and Y. Uchihori and S. Udo and F. Urban and T. Wong and R. Yamane and H. Yamaoka and K. Yamazaki and J. Yang and K. Yashiro and Y. Yoneda and S. Yoshida and H. Yoshii and R. Zollinger and Z. Zundel",

note = "Funding Information: The Telescope Array experiment is supported by the Japan Society for the Promotion of Science through Grants-in-Aid for Scientific Research on Specially Promoted Research ( 21000002 ) “Extreme Phenomena in the Universe Explored by Highest Energy Cosmic Rays” and for Scientific Research ( 19104006 ), and the Inter-University Research Program of the Institute for Cosmic Ray Research; by the U.S. National Science Foundation awards PHY-0307098 , PHY-0601915 , PHY-0649681 , PHY-0703893 , PHY-0758342 , PHY-0848320 , PHY-1069280 , PHY-1069286 , PHY-1404495 and PHY-1404502 ; by the National Research Foundation of Korea ( 2015R1A2A1A01006870 , 2015R1A2A1A15055344 , 2016R1A5A1013277 , 2007-0093860, 2016R1A2B4014967 ); by the Russian Academy of Sciences, RFBR grant 16-02-00962a (INR), IISN project No. 4.4502.13 , and Belgian Science Policy under IUAP VII/37 (ULB) . The foundations of Dr. Ezekiel R. and Edna Wattis Dumke, Willard L. Eccles, and George S. and Dolores Dor{\'e} Eccles all helped with generous donations. The State of Utah supported the project through its Economic Development Board , and the University of Utah through the Office of the Vice President for Research. The experimental site became available through the cooperation of the Utah School and Institutional Trust Lands Administration (SITLA), U.S. Bureau of Land Management (BLM), and the U.S. Air Force. We appreciate the assistance of the State of Utah and Fillmore offices of the BLM in crafting the Plan of Development for the site. We also wish to thank the people and the officials of Millard County, Utah for their steadfast and warm support. We gratefully acknowledge the contributions from the technical staffs of our home institutions. An allocation of computer time from the Center for High Performance Computing at the University of Utah is gratefully acknowledged. Publisher Copyright: {\textcopyright} 2016",

year = "2017",

month = jan,

day = "1",

doi = "10.1016/j.astropartphys.2016.11.001",

language = "English",

volume = "86",

pages = "21--26",

journal = "Astroparticle Physics",

issn = "0927-6505",

publisher = "Elsevier",

}

Abbasi, RU, Abe, M, Abu-Zayyad, T, Allen, M, Azuma, R, Barcikowski, E, Belz, JW, Bergman, DR, Blake, SA, Cady, R, Cheon, BG, Chiba, J, Chikawa, M, Fujii, T, Fukushima, M, Goto, T, Hanlon, W, Hayashi, Y, Hayashi, M, Hayashida, N, Hibino, K, Honda, K, Ikeda, D, Inoue, N, Ishii, T, Ishimori, R, Ito, H, Ivanov, D, Jui, CCH, Kadota, K, Kakimoto, F, Kalashev, O, Kasahara, K, Kawai, H, Kawakami, S, Kawana, S, Kawata, K, Kido, E, Kim, HB, Kim, JH, Kim, JH, Kishigami, S, Kitamura, S, Kitamura, Y, Kuzmin, V, Kwon, YJ, Lan, J, Lubsandorzhiev, B, Lundquist, JP, Machida, K, Martens, K, Matsuda, T, Matsuyama, T, Matthews, JN, Minamino, M, Mukai, K, Myers, I, Nagasawa, K, Nagataki, S, Nakamura, T, Nonaka, T, Nozato, A, Ogio, S, Ogura, J, Ohnishi, M, Ohoka, H, Oki, K, Okuda, T, Ono, M, Onogi, R, Oshima, A, Ozawa, S, Park, IH, Pshirkov, MS, Rodriguez, DC, Rubtsov, G, Ryu, D, Sagawa, H, Saito, K, Saito, Y, Sakaki, N, Sakurai, N, Scott, LM, Sekino, K, Shah, PD, Shibata, T, Shibata, F, Shimodaira, H, Shin, BK, Shin, HS, Smith, JD, Sokolsky, P, Stokes, BT, Stratton, SR, Stroman, TA, Suzawa, T, Takahashi, Y, Takamura, M, Takeda, M, Takeishi, R, Taketa, A, Takita, M, Tameda, Y, Tanaka, M, Tanaka, K, Tanaka, H, Thomas, SB, Thomson, GB, Tinyakov, P, Tirone, AH, Tkachev, I, Tokuno, H, Tomida, T, Troitsky, S, Tsunesada, Y, Tsutsumi, K, Uchihori, Y, Udo, S, Urban, F, Wong, T, Yamane, R, Yamaoka, H, Yamazaki, K, Yang, J, Yashiro, K, Yoneda, Y, Yoshida, S, Yoshii, H, Zollinger, R & Zundel, Z 2017, 'Search for EeV protons of galactic origin', Astroparticle Physics, vol. 86, pp. 21-26. https://doi.org/10.1016/j.astropartphys.2016.11.001

TY - JOUR

T1 - Search for EeV protons of galactic origin

AU - Abbasi, R. U.

AU - Abe, M.

AU - Abu-Zayyad, T.

AU - Allen, M.

AU - Azuma, R.

AU - Barcikowski, E.

AU - Belz, J. W.

AU - Bergman, D. R.

AU - Blake, S. A.

AU - Cady, R.

AU - Cheon, B. G.

AU - Chiba, J.

AU - Chikawa, M.

AU - Fujii, T.

AU - Fukushima, M.

AU - Goto, T.

AU - Hanlon, W.

AU - Hayashi, Y.

AU - Hayashi, M.

AU - Hayashida, N.

AU - Hibino, K.

AU - Honda, K.

AU - Ikeda, D.

AU - Inoue, N.

AU - Ishii, T.

AU - Ishimori, R.

AU - Ito, H.

AU - Ivanov, D.

AU - Jui, C. C.H.

AU - Kadota, K.

AU - Kakimoto, F.

AU - Kalashev, O.

AU - Kasahara, K.

AU - Kawai, H.

AU - Kawakami, S.

AU - Kawana, S.

AU - Kawata, K.

AU - Kido, E.

AU - Kim, H. B.

AU - Kim, J. H.

AU - Kishigami, S.

AU - Kitamura, S.

AU - Kitamura, Y.

AU - Kuzmin, V.

AU - Kwon, Y. J.

AU - Lan, J.

AU - Lubsandorzhiev, B.

AU - Lundquist, J. P.

AU - Machida, K.

AU - Martens, K.

AU - Matsuda, T.

AU - Matsuyama, T.

AU - Matthews, J. N.

AU - Minamino, M.

AU - Mukai, K.

AU - Myers, I.

AU - Nagasawa, K.

AU - Nagataki, S.

AU - Nakamura, T.

AU - Nonaka, T.

AU - Nozato, A.

AU - Ogio, S.

AU - Ogura, J.

AU - Ohnishi, M.

AU - Ohoka, H.

AU - Oki, K.

AU - Okuda, T.

AU - Ono, M.

AU - Onogi, R.

AU - Oshima, A.

AU - Ozawa, S.

AU - Park, I. H.

AU - Pshirkov, M. S.

AU - Rodriguez, D. C.

AU - Rubtsov, G.

AU - Ryu, D.

AU - Sagawa, H.

AU - Saito, K.

AU - Saito, Y.

AU - Sakaki, N.

AU - Sakurai, N.

AU - Scott, L. M.

AU - Sekino, K.

AU - Shah, P. D.

AU - Shibata, T.

AU - Shibata, F.

AU - Shimodaira, H.

AU - Shin, B. K.

AU - Shin, H. S.

AU - Smith, J. D.

AU - Sokolsky, P.

AU - Stokes, B. T.

AU - Stratton, S. R.

AU - Stroman, T. A.

AU - Suzawa, T.

AU - Takahashi, Y.

AU - Takamura, M.

AU - Takeda, M.

AU - Takeishi, R.

AU - Taketa, A.

AU - Takita, M.

AU - Tameda, Y.

AU - Tanaka, M.

AU - Tanaka, K.

AU - Tanaka, H.

AU - Thomas, S. B.

AU - Thomson, G. B.

AU - Tinyakov, P.

AU - Tirone, A. H.

AU - Tkachev, I.

AU - Tokuno, H.

AU - Tomida, T.

AU - Troitsky, S.

AU - Tsunesada, Y.

AU - Tsutsumi, K.

AU - Uchihori, Y.

AU - Udo, S.

AU - Urban, F.

AU - Wong, T.

AU - Yamane, R.

AU - Yamaoka, H.

AU - Yamazaki, K.

AU - Yang, J.

AU - Yashiro, K.

AU - Yoneda, Y.

AU - Yoshida, S.

AU - Yoshii, H.

AU - Zollinger, R.

AU - Zundel, Z.

N1 - Funding Information: The Telescope Array experiment is supported by the Japan Society for the Promotion of Science through Grants-in-Aid for Scientific Research on Specially Promoted Research ( 21000002 ) “Extreme Phenomena in the Universe Explored by Highest Energy Cosmic Rays” and for Scientific Research ( 19104006 ), and the Inter-University Research Program of the Institute for Cosmic Ray Research; by the U.S. National Science Foundation awards PHY-0307098 , PHY-0601915 , PHY-0649681 , PHY-0703893 , PHY-0758342 , PHY-0848320 , PHY-1069280 , PHY-1069286 , PHY-1404495 and PHY-1404502 ; by the National Research Foundation of Korea ( 2015R1A2A1A01006870 , 2015R1A2A1A15055344 , 2016R1A5A1013277 , 2007-0093860, 2016R1A2B4014967 ); by the Russian Academy of Sciences, RFBR grant 16-02-00962a (INR), IISN project No. 4.4502.13 , and Belgian Science Policy under IUAP VII/37 (ULB) . The foundations of Dr. Ezekiel R. and Edna Wattis Dumke, Willard L. Eccles, and George S. and Dolores Doré Eccles all helped with generous donations. The State of Utah supported the project through its Economic Development Board , and the University of Utah through the Office of the Vice President for Research. The experimental site became available through the cooperation of the Utah School and Institutional Trust Lands Administration (SITLA), U.S. Bureau of Land Management (BLM), and the U.S. Air Force. We appreciate the assistance of the State of Utah and Fillmore offices of the BLM in crafting the Plan of Development for the site. We also wish to thank the people and the officials of Millard County, Utah for their steadfast and warm support. We gratefully acknowledge the contributions from the technical staffs of our home institutions. An allocation of computer time from the Center for High Performance Computing at the University of Utah is gratefully acknowledged. Publisher Copyright: © 2016

PY - 2017/1/1

Y1 - 2017/1/1

N2 - Cosmic rays in the energy range 1018.0–1018.5 eV are thought to have a light, probably protonic, composition. To study their origin one can search for anisotropy in their arrival directions. Extragalactic cosmic rays should be isotropic, but galactic cosmic rays of this type should be seen mostly along the galactic plane, and there should be a shortage of events coming from directions near the galactic anticenter. This is due to the fact that, under the influence of the galactic magnetic field, the transition from ballistic to diffusive behavior is well advanced, and this qualitative picture persists over the whole energy range. Guided by models of the galactic magnetic field that indicate that the enhancement along the galactic plane should have a standard deviation of about 20° in galactic latitude, and the deficit in the galactic anticenter direction should have a standard deviation of about 50° in galactic longitude, we use the data of the Telescope Array surface detector in 1018.0 to 1018.5 eV energy range to search for these effects. The data are isotropic. Neither an enhancement along the galactic plane nor a deficit in the galactic anticenter direction is found. Using these data we place an upper limit on the fraction of EeV cosmic rays of galactic origin at 1.3% at 95% confidence level.

AB - Cosmic rays in the energy range 1018.0–1018.5 eV are thought to have a light, probably protonic, composition. To study their origin one can search for anisotropy in their arrival directions. Extragalactic cosmic rays should be isotropic, but galactic cosmic rays of this type should be seen mostly along the galactic plane, and there should be a shortage of events coming from directions near the galactic anticenter. This is due to the fact that, under the influence of the galactic magnetic field, the transition from ballistic to diffusive behavior is well advanced, and this qualitative picture persists over the whole energy range. Guided by models of the galactic magnetic field that indicate that the enhancement along the galactic plane should have a standard deviation of about 20° in galactic latitude, and the deficit in the galactic anticenter direction should have a standard deviation of about 50° in galactic longitude, we use the data of the Telescope Array surface detector in 1018.0 to 1018.5 eV energy range to search for these effects. The data are isotropic. Neither an enhancement along the galactic plane nor a deficit in the galactic anticenter direction is found. Using these data we place an upper limit on the fraction of EeV cosmic rays of galactic origin at 1.3% at 95% confidence level.

UR - http://www.scopus.com/inward/record.url?scp=84994627603&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84994627603&partnerID=8YFLogxK

U2 - 10.1016/j.astropartphys.2016.11.001

DO - 10.1016/j.astropartphys.2016.11.001

M3 - Article

AN - SCOPUS:84994627603

SN - 0927-6505

VL - 86

SP - 21

EP - 26

JO - Astroparticle Physics

JF - Astroparticle Physics

ER -

Search for EeV protons of galactic origin

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