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An anomalous positron abundance in cosmic rays with energies 1.5–100 GeV

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Listed:
  • O. Adriani

    (University of Florence, Via Sansone 1, I-50019 Sesto Fiorentino, Florence, Italy
    INFN, Sezione di Florence, Via Sansone 1, I-50019 Sesto Fiorentino, Florence, Italy)

  • G. C. Barbarino

    (University of Naples “Federico II”, Via Cintia, I-80126 Naples, Italy
    INFN, Sezione di Naples, Via Cintia, I-80126 Naples, Italy)

  • G. A. Bazilevskaya

    (Lebedev Physical Institute, Leninsky Prospekt 53, RU-119991 Moscow, Russia)

  • R. Bellotti

    (University of Bari, Via Amendola 173, I-70126 Bari, Italy
    INFN, Sezione di Bari, Via Amendola 173, I-70126 Bari, Italy)

  • M. Boezio

    (INFN, Sezione di Trieste, Padriciano 99, I-34012 Trieste, Italy)

  • E. A. Bogomolov

    (Ioffe Physical Technical Institute, Polytekhnicheskaya 26, RU-194021 St Petersburg, Russia)

  • L. Bonechi

    (University of Florence, Via Sansone 1, I-50019 Sesto Fiorentino, Florence, Italy
    INFN, Sezione di Florence, Via Sansone 1, I-50019 Sesto Fiorentino, Florence, Italy)

  • M. Bongi

    (INFN, Sezione di Florence, Via Sansone 1, I-50019 Sesto Fiorentino, Florence, Italy)

  • V. Bonvicini

    (INFN, Sezione di Trieste, Padriciano 99, I-34012 Trieste, Italy)

  • S. Bottai

    (INFN, Sezione di Florence, Via Sansone 1, I-50019 Sesto Fiorentino, Florence, Italy)

  • A. Bruno

    (University of Bari, Via Amendola 173, I-70126 Bari, Italy
    INFN, Sezione di Bari, Via Amendola 173, I-70126 Bari, Italy)

  • F. Cafagna

    (INFN, Sezione di Bari, Via Amendola 173, I-70126 Bari, Italy)

  • D. Campana

    (INFN, Sezione di Naples, Via Cintia, I-80126 Naples, Italy)

  • P. Carlson

    (KTH, AlbaNova University Centre)

  • M. Casolino

    (INFN, Sezione di Roma “Tor Vergata”, Via della Ricerca Scientifica 1, I-00133 Rome, Italy)

  • G. Castellini

    (IFAC, Via Madonna del Piano 10, I-50019 Sesto Fiorentino, Florence, Italy)

  • M. P. De Pascale

    (INFN, Sezione di Roma “Tor Vergata”, Via della Ricerca Scientifica 1, I-00133 Rome, Italy
    University of Rome “Tor Vergata”, Via della Ricerca Scientifica 1, I-00133 Rome, Italy)

  • G. De Rosa

    (INFN, Sezione di Naples, Via Cintia, I-80126 Naples, Italy)

  • N. De Simone

    (INFN, Sezione di Roma “Tor Vergata”, Via della Ricerca Scientifica 1, I-00133 Rome, Italy
    University of Rome “Tor Vergata”, Via della Ricerca Scientifica 1, I-00133 Rome, Italy)

  • V. Di Felice

    (INFN, Sezione di Roma “Tor Vergata”, Via della Ricerca Scientifica 1, I-00133 Rome, Italy
    University of Rome “Tor Vergata”, Via della Ricerca Scientifica 1, I-00133 Rome, Italy)

  • A. M. Galper

    (Moscow Engineering and Physics Institute, Kashirskoe Shosse 31, RU-11540 Moscow, Russia)

  • L. Grishantseva

    (Moscow Engineering and Physics Institute, Kashirskoe Shosse 31, RU-11540 Moscow, Russia)

  • P. Hofverberg

    (KTH, AlbaNova University Centre)

  • S. V. Koldashov

    (Moscow Engineering and Physics Institute, Kashirskoe Shosse 31, RU-11540 Moscow, Russia)

  • S. Y. Krutkov

    (Ioffe Physical Technical Institute, Polytekhnicheskaya 26, RU-194021 St Petersburg, Russia)

  • A. N. Kvashnin

    (Lebedev Physical Institute, Leninsky Prospekt 53, RU-119991 Moscow, Russia)

  • A. Leonov

    (Moscow Engineering and Physics Institute, Kashirskoe Shosse 31, RU-11540 Moscow, Russia)

  • V. Malvezzi

    (INFN, Sezione di Roma “Tor Vergata”, Via della Ricerca Scientifica 1, I-00133 Rome, Italy)

  • L. Marcelli

    (INFN, Sezione di Roma “Tor Vergata”, Via della Ricerca Scientifica 1, I-00133 Rome, Italy)

  • W. Menn

    (Universität Siegen)

  • V. V. Mikhailov

    (Moscow Engineering and Physics Institute, Kashirskoe Shosse 31, RU-11540 Moscow, Russia)

  • E. Mocchiutti

    (INFN, Sezione di Trieste, Padriciano 99, I-34012 Trieste, Italy)

  • S. Orsi

    (KTH, AlbaNova University Centre
    INFN, Sezione di Roma “Tor Vergata”, Via della Ricerca Scientifica 1, I-00133 Rome, Italy)

  • G. Osteria

    (INFN, Sezione di Naples, Via Cintia, I-80126 Naples, Italy)

  • P. Papini

    (INFN, Sezione di Florence, Via Sansone 1, I-50019 Sesto Fiorentino, Florence, Italy)

  • M. Pearce

    (KTH, AlbaNova University Centre)

  • P. Picozza

    (INFN, Sezione di Roma “Tor Vergata”, Via della Ricerca Scientifica 1, I-00133 Rome, Italy
    University of Rome “Tor Vergata”, Via della Ricerca Scientifica 1, I-00133 Rome, Italy)

  • M. Ricci

    (INFN, Laboratori Nazionali di Frascati, Via Enrico Fermi 40, I-00044 Frascati, Italy)

  • S. B. Ricciarini

    (INFN, Sezione di Florence, Via Sansone 1, I-50019 Sesto Fiorentino, Florence, Italy)

  • M. Simon

    (Universität Siegen)

  • R. Sparvoli

    (INFN, Sezione di Roma “Tor Vergata”, Via della Ricerca Scientifica 1, I-00133 Rome, Italy
    University of Rome “Tor Vergata”, Via della Ricerca Scientifica 1, I-00133 Rome, Italy)

  • P. Spillantini

    (University of Florence, Via Sansone 1, I-50019 Sesto Fiorentino, Florence, Italy
    INFN, Sezione di Florence, Via Sansone 1, I-50019 Sesto Fiorentino, Florence, Italy)

  • Y. I. Stozhkov

    (Lebedev Physical Institute, Leninsky Prospekt 53, RU-119991 Moscow, Russia)

  • A. Vacchi

    (INFN, Sezione di Trieste, Padriciano 99, I-34012 Trieste, Italy)

  • E. Vannuccini

    (INFN, Sezione di Florence, Via Sansone 1, I-50019 Sesto Fiorentino, Florence, Italy)

  • G. Vasilyev

    (Ioffe Physical Technical Institute, Polytekhnicheskaya 26, RU-194021 St Petersburg, Russia)

  • S. A. Voronov

    (Moscow Engineering and Physics Institute, Kashirskoe Shosse 31, RU-11540 Moscow, Russia)

  • Y. T. Yurkin

    (Moscow Engineering and Physics Institute, Kashirskoe Shosse 31, RU-11540 Moscow, Russia)

  • G. Zampa

    (INFN, Sezione di Trieste, Padriciano 99, I-34012 Trieste, Italy)

  • N. Zampa

    (INFN, Sezione di Trieste, Padriciano 99, I-34012 Trieste, Italy)

  • V. G. Zverev

    (Moscow Engineering and Physics Institute, Kashirskoe Shosse 31, RU-11540 Moscow, Russia)

Abstract

A hint of dark matter? Cosmic ray positrons are known to be produced in interactions in the interstellar medium. As well as originating from this 'secondary source', positrons might also be generated in primary sources such as pulsars and microquasars — or by dark matter annihilation. A new measurement of the positron fraction in the cosmic radiation for the energy range 1.5–100 GeV has been made using data from the PAMELA satellite experiment. Previous measurements, made predominantly by balloon-borne instruments, yield a positron fraction compatible with 'secondary source' production from interactions between cosmic ray nuclei and interstellar matter. Above 10 GeV the new measurements deviate significantly from this expectation, pointing to the presence of a primary source, either a nearby astrophysical object or dark matter particle annihilations.

Suggested Citation

  • O. Adriani & G. C. Barbarino & G. A. Bazilevskaya & R. Bellotti & M. Boezio & E. A. Bogomolov & L. Bonechi & M. Bongi & V. Bonvicini & S. Bottai & A. Bruno & F. Cafagna & D. Campana & P. Carlson & M. , 2009. "An anomalous positron abundance in cosmic rays with energies 1.5–100 GeV," Nature, Nature, vol. 458(7238), pages 607-609, April.
    • Handle: RePEc:nat:nature:v:458:y:2009:i:7238:d:10.1038_nature07942
    DOI: 10.1038/nature07942
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    Cited by:

    1. Omar Tibolla & Sarah Kaufmann & Paula Chadwick, 2022. "Pulsar Wind Nebulae and Unidentified Galactic Very High Energy Sources," J, MDPI, vol. 5(3), pages 1-16, July.

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