Cosmic-ray electron spectrum above 100GeV from PPB-BETS experiment in Antarctica

Yoshida, Kenji; Torii, Shoji; Yamagami, T.; Tamura, T.; Kitamura, Hisashi; Chang, Jin; Iijima, Issei; Kadokura, Akira; Kasahara, K.; Katayose, Y.; Kobayashi, Tadashi; Komori, Y.; Matsuzaka, Y.; Mizutani, K.; Murakami, Hiroyuki; Namiki, M.; Nishimura, Jun; Ohta, Shigeo; Saito, Yoshitaka; Shibata, M.; Tateyama, N.; Yamagishi, Hisakazu; Yuda, T.

doi:10.1016/j.asr.2007.04.043

Cited by 54 publications

(43 citation statements)

References 14 publications

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“…The CR electron and positron data used are as follows: AMS01 (AMS Collaboration et al 2002), CAPRICE94 (Boezio et al 2000), HEAT (DuVernois et al 2001), SANRIKU (Kobayashi 1999), BETS (Torii et al 2001), PPT-BETS (Yoshida et al 2008), ATIC-1-2 (Chang et al 2008), H.E.S.S. (Aharonian et al 2008(Aharonian et al , 2009, Fermi-LAT (Abdo et al 2009b;Ackermann et al 2010), PAMELA (Adriani et al 2011).…”

Section: Electron and Positron Datamentioning

confidence: 99%

The interstellar cosmic-ray electron spectrum from synchrotron radiation and direct measurements

Strong

Orlando

Jaffe

2011

A&A

194

249

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Aims. We exploit synchrotron radiation to constrain the low-energy interstellar electron spectrum, using various radio surveys and connecting with electron data from Fermi-LAT and other experiments. Methods. The GALPROP programme for cosmic-ray propagation, gamma-ray and synchrotron radiation is used. Secondary electrons and positrons are included. Propagation models based on cosmic-ray and gamma-ray data are tested against synchrotron data from 22 MHz to 94 GHz. Results. The synchrotron data confirm the need for a low-energy break in the cosmic-ray electron injection spectrum. The interstellar spectrum below a few GeV has to be lower than standard models predict, and this suggests less solar modulation than usually assumed. Reacceleration models are more difficult to reconcile with the synchrotron constraints. We show that secondary leptons are important for the interpretation of synchrotron emission. We also consider a cosmic-ray propagation origin for the low-energy break. Conclusions. Exploiting the complementary information on cosmic rays and synchrotron gives unique and essential constraints on electrons, and has implications for gamma rays. This connection is especially relevant now in view of the ongoing Planck and Fermi missions.

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Section: Electron and Positron Datamentioning

confidence: 99%

The interstellar cosmic-ray electron spectrum from synchrotron radiation and direct measurements

Strong

Orlando

Jaffe

2011

A&A

194

249

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“…2 as a function of the energy at the top of the instrument together with previous measurements [6][7][8][9][10][11][12].…”

Section: Resultsmentioning

confidence: 99%

“…AMS total errors are the quadratic sum of the statistical and systematic errors [3]. Also shown are the results from earlier experiments [6][7][8][9][10][11][12].…”

Section: Discussionmentioning

confidence: 99%

AMS-02: Cosmic electron and positron (e⁻+ e⁺) spectrum up to 1 TeV

Bazo

2016

EPJ Web of Conferences

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Abstract. The AMS-02 spectrometer, on the ISS since 2011, performs highly accurate measurements of cosmic rays up to the TeV region. We review the analysis of the cosmic (e + + e − ) flux in the energy range between 0.5 GeV and 1 TeV, based on 10.6 million (e + + e − ) events. The high statistics and detector energy resolution allow for a study of the spectral shape of unprecedented quality, thus improving our understanding of the production, acceleration and propagation of cosmic rays. The resulting energy spectrum does not show prominent features.

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Section: Dramatis Personaementioning

confidence: 99%

“…The Fermi Gamma-ray Space Telescope (Fermi LAT) can map the entire gamma-ray sky between 300 MeV and 500 GeV over all spatial scales, with an angular resolution that ranges from 0. HEAT [7], CAPRICE [8], BETS [9], and H.E.S.S.[10] of a model considering contributions to the e ± flux from the following categories: e − from distant (> 3 kpc) SNRs (dot-dashed yellow) and local SNRs (dotted green), secondary e ± (long dashed red) and e ± from PWNe (short dashed blue). The model is derived from a simultaneous fit to all AMS-02 data.…”

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confidence: 99%

Pulsar Wind Nebulae and Cosmic Rays: A Bedtime Story

Weinstein¹

2014

Nuclear Physics B - Proceedings Supplements

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The role pulsar wind nebulae play in producing our locally observed cosmic ray spectrum remains murky, yet intriguing. Pulsar wind nebulae are born and evolve in conjunction with SNRs, which are favored sites of Galactic cosmic ray acceleration. As a result they frequently complicate interpretation of the gamma-ray emission seen from SNRs. However, pulsar wind nebulae may also contribute directly to the local cosmic ray spectrum, particularly the leptonic component. This paper reviews the current thinking on pulsar wind nebulae and their connection to cosmic ray production from an observational perspective. It also considers how both future technologies and new ways of analyzing existing data can help us to better address the relevant theoretical questions. A number of key points will be illustrated with recent results from the VHE (E > 100 GeV) gamma-ray observatory VERITAS. Keywords: IntroductionThe discovery of cosmic rays in the early twentieth century [1, 2] inaugurated a decades-long, serialized mystery story that has yet to be completed. At the heart of the mystery lies a set of of simple questions. What particles appear in the cosmic ray spectrum that we see from Earth? Where do these particles originate? How are they accelerated? In recent decades direct cosmic ray observations have brought us a wealth of information on the cosmic ray spectrum and its composition, clues to the types of environments in which cosmic rays are born. The interaction of these particles with interstellar magnetic fields, however, prevents them from being traced back to their point of origin.In order to pursue the other half of this mystery-the nature of cosmic ray accelerators-we must use the secondary photon radiation produced in these cosmic ray nurseries. These high-energy (300 MeV -100 GeV) and very high-energy (VHE; E > 100 GeV) gamma rays are not deflected by interstellar magnetic fields and can be used to map cosmic ray populations in and near their parent accelerators. The different processes by which relativistic cosmic ray electrons, protons, and heavier nuclei produce high-energy gamma rays leave characteristic imprints on the gamma-ray energy spectrum of particular astrophysical accelerators. These features may be used to constrain the composition and energy spectrum of accelerated particle populations.The local cosmic ray spectrum is known to be a mix of protons and heavier nuclei, with a smaller admixture of leptons. A mix of astrophysical accelerators within and outside our Galaxy is believed to contribute, including shocks arising in supernova remnants (SNRs), shocks formed by interacting high-velocity winds from massive stars [3], pulsars, and active galactic nuclei (AGN). We focus here on a single subplot of a much larger story-the role played by pulsar wind nebulae (PWNe) in our quest to understand the Galactic cosmic ray spectrum. Dramatis PersonaeNo single gamma-ray observatory provides a complete picture of the gamma-ray sky at all energies and spatial scales. The Fermi Gamma-ray Space Telescope (...

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Cosmic-ray electron spectrum above 100GeV from PPB-BETS experiment in Antarctica

Cited by 54 publications

References 14 publications

The interstellar cosmic-ray electron spectrum from synchrotron radiation and direct measurements

The interstellar cosmic-ray electron spectrum from synchrotron radiation and direct measurements

AMS-02: Cosmic electron and positron (e⁻+ e⁺) spectrum up to 1 TeV

Pulsar Wind Nebulae and Cosmic Rays: A Bedtime Story

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Cosmic-ray electron spectrum above 100GeV from PPB-BETS experiment in Antarctica

Cited by 54 publications

References 14 publications

The interstellar cosmic-ray electron spectrum from synchrotron radiation and direct measurements

The interstellar cosmic-ray electron spectrum from synchrotron radiation and direct measurements

AMS-02: Cosmic electron and positron (e−+ e+) spectrum up to 1 TeV

Pulsar Wind Nebulae and Cosmic Rays: A Bedtime Story

Contact Info

Product

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AMS-02: Cosmic electron and positron (e⁻+ e⁺) spectrum up to 1 TeV