Cosmic-Ray Electron Flux Measured by the PAMELA Experiment between 1 and 625 GeV

Adriani, O.; Barbarino, G. C.; Bazilevskaya, G. A.; Bellotti, R.; Boezio, M.; Bogomolov, É. A.; Bongi, M.; Bonvicini, V.; Борисов, С. В.; Bottai, S.; Bruno, A.; Cafagna, F.; Campana, D.; Carbone, R.; Carlson, P.; Casolino, M.; Castellini, G.; Consiglio, L.; Pascale, M. P. De; Santis, C. De; Simone, N. De; Felice, V. Di; Galper, A. M.; Gillard, W.; Grishantseva, L.; Jerse, G.; Karelin, A. V.; Koldashov, S. V.; Krutkov, S. Y.; Kvashnin, A. N.; Leonov, A.; Malakhov, V.; Malvezzi, V.; Marcelli, L.; Mayorov, A. G.; Menn, W.; Mikhailov, V. V.; Mocchiutti, E.; Monaco, A.; Mori, N.; Nikonov, N.; Osteria, G.; Palma, F.; Papini, P.; Pearce, Mark; Picozza, P.; Pizzolotto, C.; Ricci, M.; Ricciarini, S.; Rossetto, L.; Sarkar, R.; Simon, M.; Sparvoli, R.; Спиллантини, П.; Stochaj, S. J.; Stockton, J.; Stozhkov, Y. I.; Vacchi, A.; Vannuccini, E.; Vasilyev, G.; Voronov, S. A.; Wu, J.; Yurkin, Y. T.; Zampa, G.; Zampa, N.; Zverev, V. G.

doi:10.1103/physrevlett.106.201101

Cited by 320 publications

(245 citation statements)

References 31 publications

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“…The Fermi Large Area Telescope (LAT) satellite confirmed the excess of the e − + e + flux for energies over 100 GeV [16,17]. The Fermi-LAT results are consistent with those of the PAMELA collaboration, which measured the cosmic ray electron flux up to 625 GeV [18]. To date the Fermi-LAT data are the most precise indication of such an anomaly in the electron-positron spectrum.…”

Section: Introductionsupporting

confidence: 73%

“…The observed tension in our data is dramatically increased when one incorporates the recently released PAMELA e − flux [18] in our electron-positron related data. For consistency we checked the result that we would obtain if we excluded this new electron flux data into our…”

Section: The Presence or Absence Of A Cosmic Ray Anomalymentioning

confidence: 70%

“…We defined our e + + e − spectrum by using data from these three experiments. The PAMELA collaboration recently released their measurement of the e − only spectrum [18] confirming the behaviour of the e + + e − spectrum as measured by Fermi-LAT. The energy ranges that these data points were selected over are listed in Table 1.…”

Section: Experimental Data Used In This Analysismentioning

confidence: 87%

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Uncertainties in Dark Matter Indirect Detection

Auchettl¹,

Balázs²

2012

Open Questions in Cosmology

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Section: Introductionsupporting

confidence: 73%

Section: The Presence or Absence Of A Cosmic Ray Anomalymentioning

confidence: 70%

Section: Experimental Data Used In This Analysismentioning

confidence: 87%

See 1 more Smart Citation

Uncertainties in Dark Matter Indirect Detection

Auchettl¹,

Balázs²

2012

Open Questions in Cosmology

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“…In the local Milky Way, this energy density is just 6 × 10 −4 eV cm −3 (see Adriani et al 2011, and references therein). In the models consistent with constraints, however, the 10 GeV e ± energy density is 0.016-0.10 eV cm −3 , with a value of 0.035 eV cm −3 in our fiducial model.…”

Section: Notesmentioning

confidence: 99%

Diffuse Hard X-Ray Emission in Starburst Galaxies as Synchrotron From Very High Energy Electrons

Lacki

Thompson

2012

ApJ

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The origin of the diffuse hard X-ray (2-10 keV) emission from starburst galaxies is a long-standing problem. We suggest that synchrotron emission of 10-100 TeV electrons and positrons (e ± ) can contribute to this emission, because starbursts have strong magnetic fields. We consider three sources of e ± at these energies: (1) primary electrons directly accelerated by supernova remnants, (2) pionic secondary e ± created by inelastic collisions between cosmic ray (CR) protons and gas nuclei in the dense interstellar medium of starbursts, and (3) pair e ± produced between the interactions between 10 and 100 TeV γ -rays and the intense far-infrared (FIR) radiation fields of starbursts. We create one-zone steady-state models of the CR population in the Galactic center (R 112 pc), NGC 253, M82, and Arp 220's nuclei, assuming a power-law injection spectrum for electrons and protons. We consider different injection spectral slopes, magnetic field strengths, CR acceleration efficiencies, and diffusive escape times, and include advective escape, radiative cooling processes, and secondary and pair e ± . We compare these models to extant radio and GeV and TeV γ -ray data for these starbursts, and calculate the diffuse synchrotron X-ray and inverse Compton (IC) luminosities of these starbursts in the models which satisfy multiwavelength constraints. If the primary electron spectrum extends to ∼PeV energies and has a proton/electron injection ratio similar to the Galactic value, we find that synchrotron emission contributes 2%-20% of their unresolved, diffuse hard X-ray emission. However, there is great uncertainty in this conclusion because of the limited information on the CR electron spectrum at these high energies. IC emission is likewise a minority of the unresolved X-ray emission in these starbursts, from 0.1% in the Galactic center to 10% in Arp 220's nuclei, with the main uncertainty being the starbursts' magnetic field. We also model generic starbursts, including submillimeter galaxies, in the context of the FIR-X-ray relation, finding that anywhere between 0% and 16% of the total hard X-ray emission is synchrotron for different parameters, and up to 2% in the densest starbursts assuming an E −2.2 injection spectrum and a diffusive escape time of 10 Myr (E/3 GeV) −1/2 (h/100 pc). Neutrino observations by IceCube and TeV γ -ray data from HESS, VERITAS, and CTA can further constrain the synchrotron X-ray emission of starbursts. Our models do not constrain the possibility of hard, second components of primary e ± from sources like pulsars in starbursts, which could enhance the synchrotron X-ray emission further.

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“…The associated inflaton particle is expected to have a mass in the range 270-1800 MeV [289]. Another class of models invokes the axial-vector portal in theories of dark matter that seek to address the cosmic ray anomalies [292][293][294][295][296][297], and to explain the suppression of CP violation in strong interactions [298]. To couple the axion portal to a hidden sector containing a TeV-scale dark matter particle, while also explaining the suppression of CP violation in strong interactions, Ref.…”

Section: Search For Light Particles Decaying Into Visible Final Statesmentioning

confidence: 99%

Rare B decays as tests of the Standard Model

Blake

Lanfranchi

Straub

2017

Progress in Particle and Nuclear Physics

120

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One of the most interesting puzzles in particle physics today is that new physics is expected at the TeV energy scale to solve the hierarchy problem, and stabilise the Higgs mass, but so far no unambiguous signal of new physics has been found. Strong constraints on the energy scale of new physics can be derived from precision tests of the electroweak theory and from flavour-changing or CP -violating processes in strange, charm and beauty hadron decays. Decays that proceed via flavour-changing-neutral-current processes are forbidden at the lowest perturbative order in the Standard Model and are, therefore, rare. Rare b hadron decays are playing a central role in the understanding of the underlying patterns of Standard Model physics and in setting up new directions in model building for new physics contributions. In this article the status and prospects of this field are reviewed.

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Cosmic-Ray Electron Flux Measured by the PAMELA Experiment between 1 and 625 GeV

Cited by 320 publications

References 31 publications

Uncertainties in Dark Matter Indirect Detection

Uncertainties in Dark Matter Indirect Detection

Diffuse Hard X-Ray Emission in Starburst Galaxies as Synchrotron From Very High Energy Electrons

Rare B decays as tests of the Standard Model

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