Testing a Reported Correlation between Arrival Directions of Ultra-high-energy Cosmic Rays and a Flux Pattern from nearby Starburst Galaxies using Telescope Array Data

Abbasi, Rasha; 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.; Matteo, Armando di; Fujii, Toshihiro; Fujita, Keitaro; Fukushima, M.; Furlich, Greg; Goto, Toru; Hanlon, W.; Hayashi, Motoki; Hayashi, Y.; Hayashida, N.; Hibino, K.; Honda, K.; Ikeda, D.; Inoue, N.; Ishii, Takaaki; Ishimori, R.; Ito, Hirotaka; Ivanov, D.; Jeong, Hyeonju; Jeong, S.; Jui, C.; Kadota, K.; Kakimoto, F.; Kalashev, O.; Kasahara, K.; Kawai, H.; Kawakami, S.; Kawana, S.; Kawata, K.; Kido, E.; Kim, H. B.; Kim, J. H.; Kim, J. H.; Kishigami, S.; Kitamura, S.; Kitamura, Yoshihisa; Kuzmin, V.; Kuznetsov, M.; Kwon, Y. J.; Lee, K. H.; Лубсандоржиев, Б.; Lundquist, Jon Paul; Machida, K.; Martens, K.; Matsuyama, T.; Matthews, J. N.; Mayta, R.; Minamino, M.; Mukai, K.; Myers, I.; Nagasawa, K.; Nagataki, Shigehiro; Nakamura, R.; Nakamura, Tôru; Nonaka, T.; Oda, Hiroyuki; Ogio, S.; Ogura, J.; Ohnishi, M.; Ohoka, H.; Okuda, Takeshi; Omura, Yugo; Ono, M.; Onogi, R.; Oshima, A.; Ozawa, S.; Park, I. H.; Пширков, М. С.; Remington, Jackson; Rodriguez, D.; Рубцов, Г.; Ryu, Dongsu; Sagawa, H.; Sahara, Ryosuke; Saito, Koji; Saito, Yoshinori; Sakaki, N.; Sakurai, N.; Scott, L. M.; Seki, T.; Sekino, K.; Shah, P. D.; Shibata, F.; Shibata, T.; Shimodaira, Hidetoshi; Shin, B. K.; Shin, Han-Back; Smith, J. D.; Sokolsky, P.; Stokes, B. T.; Stratton, S. R.; Stroman, T. A.; Suzawa, T.; Takagi, Y.; Takahashi, Yoshiyuki; Takamura, M.; Takeda, M.; Takeishi, Ryuji; Taketa, A.; Takita, M.; Tameda, Y.; Tanaka, Hidekazu; Tanaka, K.; Tanaka, M.; Thomas, S. B.; Thomson, G. B.; Tinyakov, P.; Tkachev, I.; Tokuno, H.; Tomida, T.; Troitsky, S.; Tsunesada, Y.; Tsutsumi, K.; Uchihori, Y.; Udo, S.; Urban, Federico R.; Wong, Tony; Yamamoto, M.; Yamane, R.; Yamaoka, H.; Yamazaki, K.; Yang, J.; Yashiro, K.; Yoneda, Y.; Yoshida, Shigeru; Yoshii, H.; Zhezher, Yana; Zundel, Z.

doi:10.3847/2041-8213/aaebf9

Cited by 53 publications

(58 citation statements)

References 14 publications

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“…Moreover the possibility to accelerate protons up to the 100 PeV scale has been discussed in various works, invoking cosmic-ray accelerations due to hypernovae [65,66], strong magnetic fields in Arp220-like galaxies [25], Galaxy mergers [67,68] and AGN winds [12,[69][70][71]. Complementary to these expectations, recent measurements by the two Ultra-High Energy Cosmic Ray (UHECR) observatories see first indications for a directional correlation between the arrival directions of cosmic rays above 39 EeV and nearby SBG [72,73]. Should HAGS be the sources of these UHECR, the local abundance of sources capable of reaching 200 PeV should be rather high.…”

Section: Resultsmentioning

confidence: 87%

IceCube neutrinos from hadronically powered gamma-ray galaxies

Palladino¹,

Fedynitch²,

Rasmussen³

et al. 2019

J. Cosmol. Astropart. Phys.

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In this work we use a multi-messenger approach to determine if the high energy diffuse neutrino flux observed by the IceCube Observatory can originate from γ-ray sources powered by Cosmic Rays interactions with gas. Typical representatives of such sources are Starburst and Ultra-Luminous Infrared Galaxies. Using the three most recent calculations of the non-blazar contribution to the extragalactic γ-ray background measured by the Fermi-LAT collaboration, we find that a hard power-law spectrum with spectral index α ≤ 2.12 is compatible with all the estimations for the allowed contribution from non-blazar sources, within 1σ. Using such a spectrum we are able to interpret the IceCube results, showing that various classes of hadronically powered γ-ray galaxies can provide the dominant contribution to the astrophysical signal above 100 TeV and about half of the contribution to the energy flux between 10-100 TeV. With the addition of neutrinos from the Galactic plane, it is possible to saturate the IceCube signal at high energy. Our result shows that these sources are still well motivated candidates.

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Section: Resultsmentioning

confidence: 87%

IceCube neutrinos from hadronically powered gamma-ray galaxies

Palladino¹,

Fedynitch²,

Rasmussen³

et al. 2019

J. Cosmol. Astropart. Phys.

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“…This is because including directions too close to the edge of the FoV of one of the observatories would result in larger statistical fluctuations due to very large values of 1/ω(n i ) near the edge. tics they cannot make a statistically significant corroboration or refutation of the reported possible correlation between UHECRs and SBGs [36]. It is important to note, however, that E TA < E TA .…”

Section: A Uhecr Anisotropiesmentioning

confidence: 72%

Ultrahigh-energy cosmic ray composition from the distribution of arrival directions

et al. 2018

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The sources of ultrahigh-energy cosmic rays (UHECRs) have been difficult to catch. It was recently pointed out that while sources of UHECR protons exhibit anisotropy patterns that become denser and compressed with rising energy, nucleus-emitting-sources give rise to a cepa stratis (onion-like) structure with layers that become more distant from the source position with rising energy. The peculiar shape of the hot spots from nucleus-accelerators is steered by the competition between energy loss during propagation and deflection on the Galactic magnetic field (GMF). Here, we run a full-blown simulation study to accurately characterize the deflections of UHECR nuclei in the GMF. We show that while the cepa stratis structure provides a global description of anisotropy patterns produced by UHECR nuclei en route to Earth, the hot spots are elongated depending on their location in the sky due to the regular structure of the GMF. We demonstrate that with a high-statistics sample at the high-energy-end of the spectrum, like the one to be collected by NASA's POEMMA mission, the energy dependence of the hot-spot contours could become a useful observable to identify the nuclear composition of UHECRs. This new method to determine the nature of the particle species is complementary to those using observables of extensive air showers, and therefore is unaffected by the large systematic uncertainties of hadronic interaction models. arXiv:1810.04251v3 [astro-ph.HE]

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“…Here, the warm spot is related to Cen A and around 7% of the total flux is attributed to the selected AGNs. These claims were reassessed in a new analysis of the TA data [373], which gave results consistent with both the PAO anisotropy and with isotropy, due to the small number of events.…”

Section: Anisotropiesmentioning

confidence: 93%

Cosmic ray models

Kachelrieß

Semikoz

2019

Progress in Particle and Nuclear Physics

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We review progress in high-energy cosmic ray physics focusing on recent experimental results and models developed for their interpretation. Emphasis is put on the propagation of charged cosmic rays, covering the whole range from ∼ (20 − 50) GV, i.e. the rigidity when solar modulations can be neglected, up to the highest energies observed. We discuss models aiming to explain the anomalies in Galactic cosmic rays, the knee, and the transition from Galactic to extragalactic cosmic rays.

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Testing a Reported Correlation between Arrival Directions of Ultra-high-energy Cosmic Rays and a Flux Pattern from nearby Starburst Galaxies using Telescope Array Data

Cited by 53 publications

References 14 publications

IceCube neutrinos from hadronically powered gamma-ray galaxies

IceCube neutrinos from hadronically powered gamma-ray galaxies

Ultrahigh-energy cosmic ray composition from the distribution of arrival directions

Cosmic ray models

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