Evidence for a Supergalactic Structure of Magnetic Deflection Multiplets of Ultra-High Energy Cosmic Rays. (arXiv:2005.07312v1 [astro-ph.HE])

Evidence for a Supergalactic Structure of Magnetic Deflection Multiplets of Ultra-High Energy Cosmic Rays. (arXiv:2005.07312v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_Telescope_Array/0/1/0/all/0/1">Telescope Array Collaboration</a>: <a href="http://arxiv.org/find/astro-ph/1/au:+Abbasi_R/0/1/0/all/0/1">R.U. Abbasi</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Abe_M/0/1/0/all/0/1">M. Abe</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Abu_Zayyad_T/0/1/0/all/0/1">T. Abu-Zayyad</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Allen_M/0/1/0/all/0/1">M. Allen</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Azuma_R/0/1/0/all/0/1">R. Azuma</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Barcikowski_E/0/1/0/all/0/1">E. Barcikowski</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Belz_J/0/1/0/all/0/1">J.W. Belz</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Bergman_D/0/1/0/all/0/1">D.R. Bergman</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Blake_S/0/1/0/all/0/1">S.A. Blake</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Cady_R/0/1/0/all/0/1">R. Cady</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Cheon_B/0/1/0/all/0/1">B.G. Cheon</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Chiba_J/0/1/0/all/0/1">J. Chiba</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Chikawa_M/0/1/0/all/0/1">M. Chikawa</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Matteo_A/0/1/0/all/0/1">A. di Matteo</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Fujii_T/0/1/0/all/0/1">T. Fujii</a> (8), <a href="http://arxiv.org/find/astro-ph/1/au:+Fujisue_K/0/1/0/all/0/1">K. Fujisue</a> (9), <a href="http://arxiv.org/find/astro-ph/1/au:+Fujita_K/0/1/0/all/0/1">K. Fujita</a> (10), <a href="http://arxiv.org/find/astro-ph/1/au:+Fujiwara_R/0/1/0/all/0/1">R. Fujiwara</a> (10), <a href="http://arxiv.org/find/astro-ph/1/au:+Fukushima_M/0/1/0/all/0/1">M. Fukushima</a> (9,11), <a href="http://arxiv.org/find/astro-ph/1/au:+Furlich_G/0/1/0/all/0/1">G. Furlich</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Hanlon_W/0/1/0/all/0/1">W. Hanlon</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Hayashi_M/0/1/0/all/0/1">M. Hayashi</a> (12), <a href="http://arxiv.org/find/astro-ph/1/au:+Hayashi_Y/0/1/0/all/0/1">Y. Hayashi</a> (10), <a href="http://arxiv.org/find/astro-ph/1/au:+Hayashida_N/0/1/0/all/0/1">N. Hayashida</a> (13), <a href="http://arxiv.org/find/astro-ph/1/au:+Hibino_K/0/1/0/all/0/1">K. Hibino</a> (13), <a href="http://arxiv.org/find/astro-ph/1/au:+Higuchi_R/0/1/0/all/0/1">R. Higuchi</a> (9), <a href="http://arxiv.org/find/astro-ph/1/au:+Honda_K/0/1/0/all/0/1">K. Honda</a> (14), <a href="http://arxiv.org/find/astro-ph/1/au:+Ikeda_D/0/1/0/all/0/1">D. Ikeda</a> (15), <a href="http://arxiv.org/find/astro-ph/1/au:+Inadomi_T/0/1/0/all/0/1">T. Inadomi</a> (16), <a href="http://arxiv.org/find/astro-ph/1/au:+Inoue_N/0/1/0/all/0/1">N. Inoue</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Ishii_T/0/1/0/all/0/1">T. Ishii</a> (14), <a href="http://arxiv.org/find/astro-ph/1/au:+Ishimori_R/0/1/0/all/0/1">R. Ishimori</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Ito_H/0/1/0/all/0/1">H. Ito</a> (17), <a href="http://arxiv.org/find/astro-ph/1/au:+Ivanov_D/0/1/0/all/0/1">D. Ivanov</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Iwakura_H/0/1/0/all/0/1">H. Iwakura</a> (16), <a href="http://arxiv.org/find/astro-ph/1/au:+Jeong_H/0/1/0/all/0/1">H.M. Jeong</a> (18), <a href="http://arxiv.org/find/astro-ph/1/au:+Jeong_S/0/1/0/all/0/1">S. Jeong</a> (18), <a href="http://arxiv.org/find/astro-ph/1/au:+Jui_C/0/1/0/all/0/1">C.C.H. Jui</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Kadota_K/0/1/0/all/0/1">K. Kadota</a> (19), <a href="http://arxiv.org/find/astro-ph/1/au:+Kakimoto_F/0/1/0/all/0/1">F. Kakimoto</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Kalashev_O/0/1/0/all/0/1">O. Kalashev</a> (20), <a href="http://arxiv.org/find/astro-ph/1/au:+Kasahara_K/0/1/0/all/0/1">K. Kasahara</a> (21), <a href="http://arxiv.org/find/astro-ph/1/au:+Kasami_S/0/1/0/all/0/1">S. Kasami</a> (22), <a href="http://arxiv.org/find/astro-ph/1/au:+Kawai_H/0/1/0/all/0/1">H. Kawai</a> (23), <a href="http://arxiv.org/find/astro-ph/1/au:+Kawakami_S/0/1/0/all/0/1">S. Kawakami</a> (10), <a href="http://arxiv.org/find/astro-ph/1/au:+Kawana_S/0/1/0/all/0/1">S. Kawana</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Kawata_K/0/1/0/all/0/1">K. Kawata</a> (9), <a href="http://arxiv.org/find/astro-ph/1/au:+Kido_E/0/1/0/all/0/1">E. Kido</a> (9), et al. (102 additional authors not shown)

Evidence for a large-scale supergalactic cosmic ray multiplet (arrival
directions correlated with energy) structure is reported for ultra-high energy
cosmic ray (UHECR) energies above 10$^{19}$ eV using seven years of data from
the Telescope Array (TA) surface detector and updated to 10 years. Previous
energy-position correlation studies have made assumptions regarding magnetic
field shapes and strength, and UHECR composition. Here the assumption tested is
that, since the supergalactic plane is a fit to the average matter density of
the local Large Scale Structure (LSS), UHECR sources and intervening
extragalactic magnetic fields are correlated with this plane. This
supergalactic deflection hypothesis is tested by the entire field-of-view (FOV)
behavior of the strength of intermediate-scale energy-angle correlations. These
multiplets are measured in spherical cap section bins (wedges) of the FOV to
account for coherent and random magnetic fields. The structure found is
consistent with supergalactic deflection, the previously published energy
spectrum anisotropy results of TA (the hotspot and coldspot), and toy-model
simulations of a supergalactic magnetic sheet. The seven year data post-trial
significance of this supergalactic structure of multiplets appearing by chance,
on an isotropic sky, is found by Monte Carlo simulation to be 4.19$sigma$. The
ten years of data post-trial significance is 4.09$sigma$. Furthermore, the
starburst galaxy M82 is shown to be a possible source of the TA Hotspot, and an
estimate of the supergalactic magnetic field using UHECR measurements is
presented.

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