New cosmic ray MIN-MED-MAX benchmark models for dark matter indirect signatures

Discussion timeslot (ZOOM-Meeting): 15. July 2021 - 18:00
ZOOM-Meeting URL: https://desy.zoom.us/j/91896950007
ZOOM-Meeting ID: 91896950007
ZOOM-Meeting Passcode: ICRC2021
Corresponding Session: https://icrc2021-venue.desy.de/channel/16-Cosmic-Ray-Antiparticles-and-Electrons-CRD-DM-GAD-MM/128
Live-Stream URL: https://icrc2021-venue.desy.de/livestream/Discussion-06/7

Abstract:
Galactic charged cosmic rays, notably positrons, antiprotons and light antinuclei, are powerful probes of dark matter annihilation or decay, in particular for candidates heavier than a few MeV or tiny evaporating primordial black holes. Recent measurements by PAMELA, AMS-02, or Voyager on positrons and antiprotons already translate into constraints on several models over a large mass range. However, these constraints depend on galactic transport models, in particular the diffusive halo size L, subject to theoretical and statistical uncertainties.rnrnI will first discuss the new constraints which we have set on L as reported in AandA 639 (2020) A74. Using Be/B data on top of the secondary-to-primary ratios Li/C and B/C, we derive an average value of $L=5^{+3}_{-2}$ kpc at $1sigma$. These constraints improve by a factor of 2 when low-energy 10Be/9Be data are included.rnrnUsing these results, we have updated, in a comprehensive analysis soon to be released, the so-called MIN-MED-MAX benchmark transport parameters that yield generic minimal, median, and maximal dark matter produced fluxes. I will discuss how we have defined these benchmark configurations from a selection of models based on the diffusive halo height L and on a specific low-energy transport parameter that depends on the cosmic ray transport scheme. I will illustrate our results with a 100 GeV dark matter species annihilating into bb quark or electron-positron pairs, and present the positron and antiproton fluxes that this particle generates at the Earth. With our revised MIN-MED-MAX sets, the uncertainties on primary fluxes improve by a factor of 3-4 (positrons) and 7 (antiprotons) with respect to their former version.'

Authors: PIERRE SALATI
Co-Authors: Mathieu Boudaud | Marco CIRELLI | Laurent Derôme | Yoann GÉNOLINI | Julien Lavalle | David Maurin | Pasquale Dario Serpico
Collaboration: Cosmic Ray Alpine Collaboration (CRAC)

Indico-ID: 668
Proceeding URL: https://pos.sissa.it/395/572