Measurement of the flux of primary cosmic ray antiprotons with energies of 60 MeV to 350 GeV in the PAMELA experiment

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

doi:10.1134/s002136401222002x

Cited by 123 publications

(122 citation statements)

References 23 publications

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“…For a WIMP mass m χ of 1 TeV, the positron production rate needs to be enhanced by a factor of a thousand to match the measurements. The second difficulty lies in the absence, up to 100 GeV, of a similar excess in the antiprotons, since the PAMELA measurements of the antiprotonto-proton ratio (Adriani et al 2009a) and of the absolute flux (Adriani et al 2010(Adriani et al , 2013b are consistent with the expected astrophysical background of secondary species. DM particles cannot couple with quarks under the penalty of overproducing antiprotons as shown by Cirelli et al (2009b) and confirmed by Donato et al (2009).…”

Section: Introductionmentioning

confidence: 89%

A new look at the cosmic ray positron fraction

Boudaud

Aupetit

Caroff

et al. 2015

A&A

130

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Context. The positron fraction in cosmic rays has recently been measured with improved accuracy up to 500 GeV, and it was found to be a steadily increasing function of energy above ∼10 GeV. This behaviour contrasts with standard astrophysical mechanisms, in which positrons are secondary particles, produced in the interactions of primary cosmic rays during their propagation in the interstellar medium. The observed anomaly in the positron fraction triggered a lot of excitement, as it could be interpreted as an indirect signature of the presence of dark matter species in the Galaxy, the so-called weakly interacting massive particles (WIMPs). Alternatively, it could be produced by nearby sources, such as pulsars. Aims. These hypotheses are probed in light of the latest AMS-02 positron fraction measurements. As regards dark matter candidates, regions in the annihilation cross section to mass plane, which best fit the most recent data, are delineated and compared to previous measurements. The explanation of the anomaly in terms of a single nearby pulsar is also explored. Methods. The cosmic ray positron transport in the Galaxy is described using a semi-analytic two-zone model. Propagation is described with Green functions as well as with Bessel expansions. For consistency, the secondary and primary components of the positron flux are calculated together with the same propagation model. The above mentioned explanations of the positron anomaly are tested using χ 2 fits. The numerical package MicrOMEGAs is used to model the positron flux generated by dark matter species. The description of the positron fraction from conventional astrophysical sources is based on the pulsar observations included in the Australia Telescope National Facility (ATNF) catalogue. Results. The masses of the favoured dark matter candidates are always larger than 500 GeV, even though the results are very sensitive to the lepton flux. The Fermi measurements point systematically to much heavier candidates than the recently released AMS-02 observations. Since the latter are more precise, they are much more constraining. A scan through the various individual annihilation channels disfavours leptons as the final state. On the contrary, the agreement is excellent for quark, gauge boson, or Higgs boson pairs, with best-fit masses in the 10 to 40 TeV range. The combination of annihilation channels that best matches the positron fraction is then determined at fixed WIMP mass. A mixture of electron and tau lepton pairs is only acceptable around 500 GeV. Adding b-quark pairs significantly improves the fit up to a mass of 40 TeV. Alternatively, a combination of the four-lepton channels provides a good fit between 0.5 and 1 TeV, with no muons in the final state. Concerning the pulsar hypothesis, the region of the distance-to-age plane that best fits the positron fraction for a single source is determined. Conclusions. The only dark matter species that fulfils the stringent gamma ray and cosmic microwave background bounds is a particle annihilating into...

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Section: Introductionmentioning

confidence: 89%

A new look at the cosmic ray positron fraction

Boudaud

Aupetit

Caroff

et al. 2015

A&A

130

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“…More recently, measurements of the cosmic ray antiproton spectrum by PAMELA [10][11][12] (and in the near future, by AMS-02) have reached the level of precision required to probe thermal dark matter particle candidates with masses in the range of ∼10-100 GeV [13][14][15][16][17][18][19][20][21][22], yielding constraints that can be comparably stringent to those derived from gamma-ray telescopes [23,24]. Such constraints are, however, subject to large astrophysical uncertainties associated with the propagation of cosmic rays through the Milky Way.…”

Section: Introductionmentioning

confidence: 99%

“…In this study, we revisit the cosmic ray antiproton spectrum, as measured by the PAMELA experiment [10][11][12], and consider the implications for annihilating dark matter. To this end, we make use of a large set of propagation models, with parameters fit to the observed spectra of boron, carbon, beryllium, and other cosmic ray nuclei (as identified and evaluated in Ref.…”

Section: Introductionmentioning

confidence: 99%

What does the PAMELA antiproton spectrum tell us about dark matter?

Linden

Mertsch

2015

J. Cosmol. Astropart. Phys.

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Measurements of the cosmic ray antiproton spectrum can be used to search for contributions from annihilating dark matter and to constrain the dark matter annihilation cross section. Depending on the assumptions made regarding cosmic ray propagation in the Galaxy, such constraints can be quite stringent. We revisit this topic, utilizing a set of propagation models fit to the cosmic ray boron, carbon, oxygen and beryllium data. We derive upper limits on the dark matter annihilation cross section and find that when the cosmic ray propagation parameters are treated as nuisance parameters (as we argue is appropriate), the resulting limits are significantly less stringent than have been previously reported. We also note (as have several previous groups) that simple GALPROPlike diffusion-reacceleration models predict a spectrum of cosmic ray antiprotons that is in good agreement with PAMELA's observations above ∼5 GeV, but that significantly underpredict the flux at lower energies. Although the complexity of modeling cosmic ray propagation at GeV-scale energies makes it difficult to determine the origin of this discrepancy, we consider the possibility that the excess antiprotons are the result of annihilating dark matter. Suggestively, we find that this excess is best fit for mDM ∼ 35 GeV and σv ∼ 10 −26 cm 3 /s (to bb), in good agreement with the mass and cross section previously shown to be required to generate the gamma-ray excess observed from the Galactic Center.

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“…For a dark matter mass larger than a few GeV, the flux of antiprotons features a cut off at the dark matter mass. The most accurate measurements of thep flux at the Earth was reported by the space-borne detectors PAMELA [44] and AMS-02 [45]. The discovery of an excess around 100 GeV was recently claimed [46,47].…”

Section: Jhep11(2017)132mentioning

confidence: 99%

“…We derived constraints on the dark matter annihilation cross section σv from the cosmic ray antiproton flux measured by PAMELA [44] as well as AMS-02 [45], following the procedure described in [75]. Secondary antiprotons constitute the astrophysical background.…”

Section: Indirect Detectionmentioning

confidence: 99%

Robustness of dark matter constraints and interplay with collider searches for New Physics

Arbey

Robbins

Mahmoudi

et al. 2017

J. High Energ. Phys.

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Abstract:We study the implications of dark matter searches, together with collider constraints, on the phenomenological MSSM with neutralino dark matter and focus on the consequences of the related uncertainties in some detail. We consider, inter alia, the latest results from AMS-02, Fermi-LAT and XENON1T. In particular, we examine the impact of the choice of the dark matter halo profile, as well as the propagation model for cosmic rays, for dark matter indirect detection and show that the constraints on the MSSM differ by one to two orders of magnitude depending on the astrophysical hypotheses. On the other hand, our limited knowledge of the local relic density in the vicinity of the Earth and the velocity of Earth in the dark matter halo leads to a factor 3 in the exclusion limits obtained by direct detection experiments. We identified the astrophysical models leading to the most conservative and the most stringent constraints and for each case studied the complementarities with the latest LHC measurements and limits from Higgs, SUSY and monojet searches. We show that combining all data from dark matter searches and colliders, a large fraction of our supersymmetric sample could be probed. Whereas the direct detection constraints are rather robust under the astrophysical assumptions, the uncertainties related to indirect detection can have an important impact on the number of the excluded points.

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Measurement of the flux of primary cosmic ray antiprotons with energies of 60 MeV to 350 GeV in the PAMELA experiment

Cited by 123 publications

References 23 publications

A new look at the cosmic ray positron fraction

A new look at the cosmic ray positron fraction

What does the PAMELA antiproton spectrum tell us about dark matter?

Robustness of dark matter constraints and interplay with collider searches for New Physics

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