Energy Spectrum of Cosmic-Ray Electron and Positron from 10 GeV to 3 TeV Observed with the Calorimetric Electron Telescope on the International Space Station

Adriani, O.; Akaike, Yosui; Asano, Kentaro; Asaoka, Y.; Bagliesi, M. G.; Bigongiari, G.; Binns, W. R.; Bonechi, Simone; Bongi, M.; Brogi, P.; 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.; Hareyama, M.; Hasebe, Nobuyuki; Hibino, K.; Ichimura, M.; Ioka, Kunihito; Ishizaki, W.; Israel, M. H.; Javaid, A.; Kasahara, K.; Kataoka, J.; Kataoka, Ryuho; Katayose, Y.; Kato, C.; Kawanaka, Norita; Kawakubo, Y.; Krawczynski, H.; Krizmanic, John F.; Kuramata, S.; Lomtadze, T.; Maestro, P.; Marrocchesi, P. S.; Messineo, A.; Mitchell, J. W.; Miyake, Shoko; Mizutani, K.; Моисеев, А. А.; Möri, K.; 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, Yuya; Shiomi, A.; Sparvoli, R.; Спиллантини, П.; Stolzi, Francesco; Takahashi, Ichiro; Takayanagi, M.; Takita, M.; Tamura, T.; Tateyama, N.; 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; Yuda, T.

doi:10.1103/physrevlett.119.181101

Cited by 133 publications

(95 citation statements)

References 39 publications

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“…The indirect searches aimt a detecting the products of WIMP annihilations (e.g., gamma rays, neutrinos, positrons, electrons, and antiprotons). The FERMI-LAT, DAMPE [29], CALET [30], HAWC [31], HESS [32], VERITAS [33], MAGIC [34] or the planned CTA [35] are working in the photons channel, while IceCube [36] in neutrinos and FERMI-LAT [37] in antimatter. Concerning particle accelerators, DM (WIMPs) production together with jets (other particles) should give rise to a large amount of energy.…”

Section: Introductionmentioning

confidence: 99%

Dark compact objects: An extensive overview

et al. 2019

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We study the structure of compact objects that contain non-self annihilating, self-interacting dark matter admixed with ordinary matter made of neutron star and white dwarf materials. We extend the previous work Phys. Rev. D 92 123002 (2015) on these dark compact objects by analyzing the effect of weak and strongly interacting dark matter with particle masses in the range of 1-500 GeV, so as to set some constraints in the strength of the interaction and the mass of the dark matter particle. We find that the total mass of the compact objects increases with decreasing dark matter particle mass. In the strong interacting case and for dark matter particle masses in the range 1-10 GeV, the total mass of the compact objects largely exceeds the 2M constraint for neutron star masses and the nominal 1M for white dwarfs, while for larger dark matter particle masses or in the weakly interacting case the compact objects show masses in agreement or smaller than these constraints, thus hinting at the exclusion of strongly self-interacting dark matter of masses 1-10 GeV in the interior of these compact objects. Moreover, we observe that the smaller the dark matter particle mass, the larger the quantity of dark matter captured is, putting constraints on the dark matter mass trapped in the compact objects so as to fullfill 2M observations. Finally, the inhomogeneity of distribution of dark matter in the Galaxy implies a mass dependence of compact objects from the environment which can be used to put constraints on the characteristics of the Galaxy halo DM profile and on particle mass. In view of the these results, we discuss the formation of the dark compact objects in an homogeneous and non-homogeneous dark matter environment. In the ΛCDM model, a parameterization of the big-bang cosmology with six parameters, the DE is associated with the cosmological constant Λ, and the material components of the Universe are the ones indicated previously. The quoted ΛCDM paradigm, describes correctly many of the observations[2, 6-9], but has some drawbacks. On large scale CMB shows some anomalies, such as that the Planck 2015 data are in tension with the CFHTLenS weak lensing [10], and σ 8 [11]. There is also another tension with the value of the Hubble parameter measured by SNIa 1 . Another big issue of the paradigm is the nature of DM. A "zoo" of candidates have been proposed, with masses in the range of 10 −33 GeV (Fuzzy DM) to 10 15 GeV (Wimpzillas). In that large "zoo", 1 The ΛCDM paradigm has some other drawbacks, as the cosmological constant problem [12,13], the unknown nature of DE [14-16] and the so called "small scale problems" [17].

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Section: Introductionmentioning

confidence: 99%

Dark compact objects: An extensive overview

et al. 2019

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“…Recently the HESS [1], DAMPE [2] and CALET [3] collaborations reported on the presence of a break at ∼ 1 TeV in the cosmic ray (CR) electron spectrum. Moreover, the HESS collaboration measured the electron spectrum up to ∼ 20 TeV [1] and found, remarkably, that it does not exhibit any cut-off up to this very high energy.…”

Section: Introductionmentioning

confidence: 99%

Local fading accelerator and the origin of TeV cosmic ray electrons

et al. 2019

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The total cosmic ray electron spectrum (electrons plus positrons) exhibits a break at a particle energy of ∼ 1 TeV and extends without any attenuation up to ∼ 20 TeV. Synchrotron and inverse Compton energy losses strongly constrain both the age and the distance of the potential sources of TeV and multi-TeV electrons to ≈ 10 5 yr and ≈ 100 − 500 pc, depending on both the absolute value and energy dependence of the cosmic ray diffusion coefficient. This suggests that only a few, or just one nearby discrete source may explain the observed spectrum of high energy electrons. On the other hand the measured positron fraction, after initially increasing with particle energy, saturates at a level well below 0.5 and likely drops above ∼ 400 − 500 GeV. This means that the local source(s) of TeV electrons should not produce positrons in equal amount, ruling out scenarios involving pulsars/pulsar winds as the main sources of high energy leptons. In this paper we show that a single, local, and fading source can naturally account for the entire spectrum of cosmic ray electrons in the TeV domain. Even though the nature of such source remains unclear, we discuss known cosmic ray accelerators, such as supernova remnant and stellar wind shocks, which are believed to accelerate preferentially electrons rather than positrons.

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“…PAMELA [33,34] and more so AMS-02 [35][36][37] have measured the electron and positron spectra in the GeV-TeV range with unprecedented precision. CALET [38] and DAMPE [39] have contributed measurements of the all-electron spectrum, that is the sum of electron and positron spectra, up to and around a TeV. While there are indications that the positron flux is cutting off around a few hundred GeV [40], the electron spectrum is surprisingly featureless up to hundreds of GeV.…”

Section: Introductionmentioning

confidence: 99%

Stochastic cosmic ray sources and the TeV break in the all-electron spectrum

Mertsch

2018

J. Cosmol. Astropart. Phys.

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Despite significant progress over more than 100 years, no accelerator has been unambiguously identified as the source of the locally measured flux of cosmic rays. Highenergy electrons and positrons are of particular importance in the search for nearby sources as radiative energy losses constrain their propagation to distances of about 1 kpc around 1 TeV. At the highest energies, the spectrum is therefore dominated and shaped by only a few sources whose properties can be inferred from the fine structure of the spectrum at energies currently accessed by experiments like AMS-02, CALET, DAMPE, Fermi-LAT, H.E.S.S. and ISS-CREAM. We present a stochastic model of the Galactic all-electron flux and evaluate its compatibility with the measurement recently presented by the H.E.S.S. collaboration. To this end, we have MC generated a large sample of the all-electron flux from an ensemble of random distributions of sources. We confirm the non-Gaussian nature of the probability density of fluxes at individual energies previously reported in analytical computations. For the first time, we also consider the correlations between the fluxes at different energies, treating the binned spectrum as a random vector and parametrising its joint distribution with the help of a pair-copula construction. We show that the spectral break observed in the allelectron spectrum by H.E.S.S. and DAMPE is statistically compatible with a distribution of astrophysical sources like supernova remnants or pulsars, but requires a rate smaller than the canonical supernova rate. This important result provides an astrophysical interpretation of the spectrum at TeV energies and allows differentiating astrophysical source models from exotic explanations, like dark matter annihilation. We also critically assess the reliability of using catalogues of known sources to model the electron-positron flux. arXiv:1809.05104v2 [astro-ph.HE]

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Energy Spectrum of Cosmic-Ray Electron and Positron from 10 GeV to 3 TeV Observed with the Calorimetric Electron Telescope on the International Space Station

Cited by 133 publications

References 39 publications

Dark compact objects: An extensive overview

Dark compact objects: An extensive overview

Local fading accelerator and the origin of TeV cosmic ray electrons

Stochastic cosmic ray sources and the TeV break in the all-electron spectrum

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