Direct Measurement of the Cosmic-Ray Proton Spectrum from 50 GeV to 10 TeV with the Calorimetric Electron Telescope on the International Space Station

Adriani, O.; Akaike, Yosui; Asano, Kentaro; Asaoka, Y.; Bagliesi, M. G.; Berti, Eugenio; Bigongiari, G.; Binns, W. R.; Bonechi, Simone; Bongi, M.; Brogi, P.; Bruno, A.; Buckley, J. H.; Cannady, N.; Castellini, G.; Checchia, C.; Cherry, M. L.; Collazuol, G.; Felice, V. Di; Ebisawa, Ken; Fuke, H.; Guzik, T. G.; Hams, T.; Hasebe, Nobuyuki; Hibino, K.; Ichimura, M.; Ioka, Kunihito; Ishizaki, W.; Israel, M. H.; Kasahara, K.; Kataoka, J.; Kataoka, Ryuho; Katayose, Y.; Kato, C.; Kawanaka, Norita; Kawakubo, Y.; Kohri, Kazunori; Krawczynski, H.; Krizmanic, John F.; Lomtadze, T.; Maestro, P.; Marrocchesi, P. S.; Messineo, A.; Mitchell, J. W.; Miyake, Shoko; Моисеев, А. А.; Mori, Kunishiro; Mori, M.; Mori, N.; Motz, H.; Munakata, K.; Murakami, Hiroyuki; Nakahira, S.; Nishimura, Jun; Nolfo, G. A. de; Okuno, S.; Ormes, J. F.; Ozawa, S.; Pacini, Lorenzo; Palma, F.; Papini, P.; Penacchioni, A. V.; Rauch, B. F.; Ricciarini, S.; Sakai, Kazuhiro; Sakamoto, T.; Sasaki, Misao; Shimizu, Yuki; Shiomi, A.; Sparvoli, R.; Спиллантини, П.; Stolzi, Francesco; Suh, J. E.; Sulaj, A.; Takahashi, Ichiro; Takayanagi, M.; Takita, M.; Tamura, T.; Terasawa, T.; Tomida, H.; Torii, Shoji; Tsunesada, Y.; Uchihori, Y.; Ueno, S.; Vannuccini, E.; Wefel, J. P.; Yamaoka, K.; Yanagita, S.; Yoshida, A.; Yoshida, Kenji

doi:10.1103/physrevlett.122.181102

Cited by 155 publications

(127 citation statements)

References 81 publications

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“…Note added: During the final stage for the publication of this paper, the CALET collaboration reported new measurements of the proton spectrum from 50 GeV to 10 TeV and confirmed the spectral hardening feature found by other measurements ( 42 ). The lack of measurements above 10 TeV of CALET, however, hampers a cross-check of our main finding.…”

Section: Methodssupporting

confidence: 70%

Measurement of the cosmic ray proton spectrum from 40 GeV to 100 TeV with the DAMPE satellite

An¹,

Asfandiyarov²,

Azzarello³

et al. 2019

Sci. Adv.

186

123

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The precise measurement of the spectrum of protons, the most abundant component of the cosmic radiation, is necessary to understand the source and acceleration of cosmic rays in the Milky Way. This work reports the measurement of the cosmic ray proton fluxes with kinetic energies from 40 GeV to 100 TeV, with 2 1 / 2 years of data recorded by the DArk Matter Particle Explorer (DAMPE). This is the first time that an experiment directly measures the cosmic ray protons up to~100 TeV with high statistics. The measured spectrum confirms the spectral hardening at~300 GeV found by previous experiments and reveals a softening at~13.6 TeV, with the spectral index changing from~2.60 to~2.85. Our result suggests the existence of a new spectral feature of cosmic rays at energies lower than the so-called knee and sheds new light on the origin of Galactic cosmic rays.

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Section: Methodssupporting

confidence: 70%

Measurement of the cosmic ray proton spectrum from 40 GeV to 100 TeV with the DAMPE satellite

An¹,

Asfandiyarov²,

Azzarello³

et al. 2019

Sci. Adv.

186

123

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“…Setting the diffusion zone half-height L ¼ 3 kpc and the width of the spiral arm thickness to 0.65 kpc, this model reproduces the AMS-02 B/C ratio[64] and proton spectrum[65] measurements if assuming a common injection index γ i ¼ −2.32 for all nuclei. This model predicts the hardening in the proton spectrum matching the index change as recently measured by CALET[66] as a pure propagation effect, without any break in the injection index.Model B is designed as an alternative with high diffusion coefficient already at low energy, choosing D 0 ¼ 3.7 × 10 28 cm 2 =s which implies a much larger diffusion zone half-height of L ¼ 15. With a constant diffusion coefficient index δ h ¼ 0.5, the slope changes in B/C ratio FIG.…”

supporting

confidence: 67%

Cosmic-ray signatures of dark matter from a flavor dependent gauge symmetry model with neutrino mass mechanism

et al. 2020

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We propose an extension to the Standard Model accommodating two families of Dirac neutral fermions and Majorana fermions under additional Uð1Þ e−μ × Z 3 × Z 2 symmetries where Uð1Þ e−μ is a flavor dependent gauge symmetry related to the first and second family of the lepton sector, which features a twoloop induced neutrino mass model. The two families are favored by minimally reproducing the current neutrino oscillation data and two mass difference squares and canceling the gauge anomalies at the same time. As a result, we have a prediction for neutrino masses. The lightest Dirac neutral fermion is a dark matter candidate with tree-level interaction restricted to electron, muon and neutrinos, which makes it difficult to detect in direct dark matter search as well as indirect search focusing on the τ-channel, such as through γ-rays. It may however be probed by search for dark matter signatures in electron and positron cosmic rays, and allows interpretation of a structure appearing in the CALET electron þ positron spectrum around 350-400 GeV as its signature, with a boost factor ∼40 Breit-Wigner enhancement of the annihilation cross section.

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“…The spectral hardening for protons measured by AMS02 is centered at higher rigidity (ρ p 336 +95 −52 GV) in comparison to the PAMELA results, and has a smaller step in spectral index ∆α 0.133 +0.056 −0.037 (with α 1 2.849 +0.006 −0.005 , and α 2 2.716 +0.037 −0.056 ). Measurements of the proton spectrum above 1 TeV have been now obtained by several CR calorimeters: ATIC [5], CREAM [6], CALET [7], NUCLEON [8,9] and DAMPE [10]. The ATIC, CREAM and NUCLEON detectors cover only the energy range E 1 TeV, and therefore do not observe directly the hardening, but only the spectral shape above it.…”

Section: Measurements Of the Cr Proton Spectrummentioning

confidence: 99%

The shape of the cosmic ray proton spectrum

Lipari

Vernetto

2020

Astroparticle Physics

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Recent observations of cosmic ray protons in the energy range 10 2 -10 5 GeV have revealed that the spectrum cannot be described by a simple power law. A hardening of the spectrum around an energy of order few hundred GeV, first observed by the magnetic spectrometers PAMELA and AMS02, has now been confirmed by several calorimeter detectors (ATIC, CREAM, CALET, NUCLEON and DAMPE). These new measurements reach higher energy and indicate that the hardening corresponds to a larger step in spectral index than what estimated by the magnetic spectrometers. Data at still higher energy (by CREAM, NUCLEON and DAMPE) show that the proton spectrum undergoes a marked softening at E ≈ 10 4 GeV. Understanding the origin of these unexpected spectral features is a significant challenge for models of the Galactic cosmic rays. An important open question is whether additional features are present in the proton spectrum between the softening and the "Knee". Extensive Air Shower detectors, using unfolding procedures that require the modeling of cosmic ray showers in the atmosphere, estimated the proton flux below and around the Knee (at E 3 PeV). These results however have large systematic uncertainties and are in poor agreement with each other. The measurement in the PeV energy range, recently presented by IceTop/IceCube, indicates a proton flux higher than extrapolations of the direct measurements calculated assuming a constant slope, and therefore requires the existence of an additional spectral hardening below the Knee. A clarification of this point is very important for an understanding of the origin of the Galactic cosmic rays, and is also essential for a precise calculation of the spectra of atmospheric neutrinos in the energy range (E 10 TeV) where they constitute the foreground for the emerging astrophysical ν signal.

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Direct Measurement of the Cosmic-Ray Proton Spectrum from 50 GeV to 10 TeV with the Calorimetric Electron Telescope on the International Space Station

Cited by 155 publications

References 81 publications

Measurement of the cosmic ray proton spectrum from 40 GeV to 100 TeV with the DAMPE satellite

Measurement of the cosmic ray proton spectrum from 40 GeV to 100 TeV with the DAMPE satellite

Cosmic-ray signatures of dark matter from a flavor dependent gauge symmetry model with neutrino mass mechanism

The shape of the cosmic ray proton spectrum

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