A measurement of the absolute flux of cosmic-ray electrons

Golden, R. L.; Mauger, B. G.; Badhwar, G. D.; Daniel, R. R.; Lacy, Jeffrey L.; Stephens, S. A.; Zipse, J. E.

doi:10.1086/162720

Cited by 67 publications

(31 citation statements)

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“…In Figure 17, we present the BETS results with previous measurements (Webber, Simpson, & Cane 1980 ;Tang 1984 ;Golden et al 1984Golden et al , 1994Barwick et al 1998 ;Kobayashi et al 1999 ;Boezio et al 2000) to compare with the calculation of two cases of di †usion coefficients. The coefficients have the same energy dependence, E0.3, but the factor is di †erent by a factor of 2.…”

Section: Resultsmentioning

confidence: 82%

“…Many novel detectors have been invented to overcome the difficulty by using a combination of an electromagnetic calorimeter and a device for particle identiÐcation, such as a gas Cherenkov counter & Meyer 1973), a transition (Muller radiation detector (Prince 1979 ;Tang 1984 ;& Tang Muller 1987), or a magnet spectrometer (Buffington, Orth, & Smoot 1975 ;Golden et al 1984Golden et al , 1994. Recent advanced detectors for measuring positrons separately from negative electrons have been constructed in combination with a transition radiation detector (Barwick et al 1997) or a Ring Imaging Cherenkov (RICH) detector (Boezio et al 2000) with a system of magnet spectrometer and calorimeter.…”

Section: Introductionmentioning

confidence: 99%

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The Energy Spectrum of Cosmic‐Ray Electrons from 10 to 100 GeV Observed with a Highly Granulated Imaging Calorimeter

Torii

Tamura

Tateyama

et al. 2001

ApJ

117

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Cosmic-ray electrons1 have been observed in the energy range from 12 to D100 GeV with a new balloon-borne payload, the Balloon-borne Electron Telescope with Scintillating Fibers (BETS). This is the Ðrst publication of the absolute energy spectrum of electrons measured with a highly granulated Ðber calorimeter. The calorimeter makes it possible to select electrons against the background protons by detailed observation of both the longitudinal and the lateral shower development. The performance of the detector was calibrated by the CERN-SPS accelerator beams : electrons from 5 to 100 GeV, protons from 60 to 250 GeV. The balloon observations were carried out twice, in 1997 and 1998, at the Sanriku Balloon Center (Institute of Space and Astronautical Science) in Japan. The observation time was D13 hr in all at an altitude above 34 km. A total of 1349 electron candidates were collected, and the 628 events with energies above 12.5 GeV, well above the geomagnetic rigidity cuto † of D10 GV, have been used to compose a di †erential absolute energy spectrum at the top of the atmosphere. The energy spectrum is described by a power-law index of 3.00^0.09, and the absolute di †erential intensity at 10 GeV is 0.199^0.015 m~2 s~1 sr~1 GeV~1. The overall shape of the energy spectrum in 10 D 100 GeV can be explained by a di †usion model, in which we assume an energy-dependent di †usion coefficient (PE0.3) for an injection spectrum, E~2.4.

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Section: Resultsmentioning

confidence: 82%

Section: Introductionmentioning

confidence: 99%

The Energy Spectrum of Cosmic‐Ray Electrons from 10 to 100 GeV Observed with a Highly Granulated Imaging Calorimeter

Torii

Tamura

Tateyama

et al. 2001

ApJ

117

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“…Positron fraction experimental situation before 1990 ( on the right) compared with the foreseen secondary production in the interstellar medium and an exotic model. For the experimental data the references are: Golden et al [16], Müller & Tang [17], Buffington et al [18], Daugherty et al [19], Fanselow et al [20] modulated ratios for a pure secondary origin of the antiprotons. The others are more exotic models.…”

Section: The Second Generation Experimentsmentioning

confidence: 99%

Antimatter research in space

Picozza

Morselli

2003

J. Phys. G: Nucl. Part. Phys.

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Abstract. Two of the most compelling issues facing astrophysics and cosmology today are to understand the nature of the dark matter that pervades the universe and to understand the apparent absence of cosmological antimatter. For both issues, sensitive measurements of cosmic-ray antiprotons and positrons, in a wide energy range, are crucial.Many different mechanisms can contribute to antiprotons and positrons production, ranging from conventional reactions like p + p → p + p+anything up to exotic processes like neutralino annihilation. The open problems are so fundamental (i.e.: is the universe symmetric in matter and antimatter ?) that experiments in this field will probably be of the greatest interest in the next years.Here we will summarize the present situation, showing the different hypothesis and models and the experimental measurements needed to lead to a more established scenario.

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“…From the electron events, with the above selection and energy determination, we derived the cosmic-ray electron spectrum above 100 GeV by using the following formula: Figure 7 presents the electron + positron energy spectrum multiplied by the cube of energy, in comparison with other electron observations [13][14][15][16][17][18][19][20][21] and a calculated spectrum of electrons from SNRs excluding nearby sources at distances less than 1 kpc and times younger than 1×10 5 yr 22) . The combined spectrum of BETS and PPB-BETS can be represented by a single power-law function of …”

Section: Electron Energy Spectrummentioning

confidence: 99%

Dark Matter Search by High-Energy Electron Observations

Yoshida

Torii

Kasahara

et al. 2009

Trans. JSASS Space Tech. Japan

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It has been pointed out in particle physics that mono-energetic electrons and positrons can be produced in the annihilation of WIMP dark matter. Although the propagation through the Galaxy would broaden the line spectrum, the observed spectrum would still have the distinctive feature in the region of sub-TeV, which indicates the existence of WIMP dark matter in the Galactic halo. The recent positron fraction spectrum by the PAMELA experiment shows a significant sharp rise up to ∼100 GeV, and the electron + positron spectrum by the ATIC experiment also shows an excess in the several 100 GeV region. In order to increase greatly the amount of statistics up to higher energies, we need to observe the high-energy electrons and positrons for much longer exposure times by space utilization such as CALET on the ISS. : correction factor of the proton contamination in the RE-cut with energy dependence C eg : correction factor of the gamma-ray contamination in the gamma-ray rejection with energy dependence C enh : correction of enhancement of flux due to the energy resolution C 2nd: flux of secondary (atmospheric) electrons at the observation altitude C atm : correction factor of energy loss of primary electrons in the overlying atmosphere

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A measurement of the absolute flux of cosmic-ray electrons

Cited by 67 publications

References 0 publications

The Energy Spectrum of Cosmic‐Ray Electrons from 10 to 100 GeV Observed with a Highly Granulated Imaging Calorimeter

The Energy Spectrum of Cosmic‐Ray Electrons from 10 to 100 GeV Observed with a Highly Granulated Imaging Calorimeter

Antimatter research in space

Dark Matter Search by High-Energy Electron Observations

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