Discriminating different scenarios to account for the cosmic<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:msup><mml:mi>e</mml:mi><mml:mo>±</mml:mo></mml:msup></mml:math>excess by synchrotron and inverse Compton radiation

Zhang, Juan; Bi, Xiao-Jun; Liu, Jia; Liu, Siming; Yin, Peng-Fei; Yuan, Qiang; Zhu, Shou-hua

doi:10.1103/physrevd.80.023007

Cited by 76 publications

(35 citation statements)

References 83 publications

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“…That is to say both the astrophysical scenario and DM scenario can give comparable fit to the e þ e À data. We may not be able to discriminate these two scenarios from the e þ e À spectra [36,[64][65][66][67], but need to resort to other probes such as the e þ e À anisotropy [68] and -rays [69].…”

Section: Dark Matter Annihilation Scenariomentioning

confidence: 97%

Cosmic ray Monte Carlo: A global fitting method in studying the properties of the new sources of cosmice±excesses

Liu

Yuan

et al. 2012

Phys. Rev. D

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Recently, the PAMELA collaboration published the cosmic nuclei and electron spectra with high precision, together with the cosmic antiproton data updated, and the Fermi-LAT collaboration also updated the measurement of the total e þ e À spectrum to lower energies. In this paper we develop a Markov Chain Monte Carlo (MCMC) package CosRayMC, based on the Galactic Propagation (GALPROP) cosmic ray propagation model to study the implications of these new data. It is found that if only the background electrons and secondary positrons are considered, the fit is very bad with 2 red % 3:39. Taking into account the extra e þ e À sources of pulsars or dark matter annihilation we can give much better fit to these data, with the minimum 2 red % 1:04. This means the extra sources are necessary with a very high significance in order to fit the data. However, the data show little difference between pulsar and dark matter scenarios. Both the background and extra source parameters are well constrained with this MCMC method. The antiproton data can further constrain the branching ratio of dark matter annihilation into quarks to be B q < 0:5% at 2 confidence level. The possible systematical uncertainties of the present study are discussed.

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Section: Dark Matter Annihilation Scenariomentioning

confidence: 97%

Cosmic ray Monte Carlo: A global fitting method in studying the properties of the new sources of cosmice±excesses

Liu

Yuan

et al. 2012

Phys. Rev. D

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“…The extragalactic component is analyzed elsewhere (Abdo et al 2010a). Here we focus on searching for a potential signal from DM annihilation/decay in the halo of the Milky Way (for previous work related to this topic, see Zhang et al 2009;Cirelli et al 2010;Malyshev et al 2011;Baxter & Dodelson 2011;Lin et al 2010;Abbasi et al 2011).…”

Section: Introductionmentioning

confidence: 99%

CONSTRAINTS ON THE GALACTIC HALO DARK MATTER FROMFERMI-LAT DIFFUSE MEASUREMENTS

Ackermann¹,

Ajello²,

Atwood³

et al. 2012

ApJ

217

211

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We have performed an analysis of the diffuse gamma-ray emission with the Fermi Large Area Telescope (LAT) in the Milky Way halo region, searching for a signal from dark matter annihilation or decay. In the absence of a robust dark matter signal, constraints are presented. We consider both gamma rays produced directly in the dark matter annihilation/decay and produced by inverse Compton scattering of the e + /e − produced in the annihilation/decay. Conservative limits are derived requiring that the dark matter signal does not exceed the observed diffuse gamma-ray emission. A second set of more stringent limits is derived based on modeling the foreground astrophysical diffuse emission using the GALPROP code. Uncertainties in the height of the diffusive cosmic-ray halo, the distribution of the cosmic-ray sources in the Galaxy, the index of the injection cosmic-ray electron spectrum, and the column density of the interstellar gas are taken into account using a profile likelihood formalism, while the parameters governing the cosmic-ray propagation have been derived from fits to local cosmic-ray data. The resulting limits impact the range of particle masses over which dark matter thermal production in the early universe is possible, and challenge the interpretation of the PAMELA/Fermi-LAT cosmic ray anomalies as the annihilation of dark matter.

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“…The diffusion coefficient in momentum space D pp is related to the spatial diffusion coefficient D by [14,[57][58][59] …”

Section: Propagation Parameters and E ± Backgroundmentioning

confidence: 99%

Pulsar interpretation of lepton spectra measured by AMS-02

Feng

Zhang

2016

Eur. Phys. J. C

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Alpha Magnetic Spectrometer (AMS-02) recently published its lepton spectra measurement. The results show that the positron fraction no longer increases above ∼200 GeV. The aim of this work is to investigate the possibility that the excess of positron fraction is due to pulsars. Nearby known pulsars from the ATNF catalog are considered to be a possible primary positron source of the high energy positrons. We find that the pulsars with age T (0.45−4.5) × 10 5 year and distance d < 0.5 kpc can explain the behavior of positron fraction of AMS-02 in the range of high energy. We show that each of the four pulsars-Geminga, J1741-2054, Monogem, and J0942-5552-is able to be a single source satisfying all considered physical requirements. We also discuss the possibility that these high energy e ± are from multiple pulsars. The multiple pulsar contribution predicts a positron fraction with some structures at higher energies.

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Discriminating different scenarios to account for the cosmice±excess by synchrotron and inverse Compton radiation

Cited by 76 publications

References 83 publications

Cosmic ray Monte Carlo: A global fitting method in studying the properties of the new sources of cosmice±excesses

Cosmic ray Monte Carlo: A global fitting method in studying the properties of the new sources of cosmice±excesses

CONSTRAINTS ON THE GALACTIC HALO DARK MATTER FROMFERMI-LAT DIFFUSE MEASUREMENTS

Pulsar interpretation of lepton spectra measured by AMS-02

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