Kuzmin, L.A.
Astrophysics
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First measurement of the absorption of $^{3}\overline{\rm He}$ nuclei in matter and impact on their propagation in the galaxy

The ALICE collaboration Acharya, Shreyasi ; Adamova, Dagmar ; Adler, Alexander ; et al.
Nature Phys. 19 (2023) 61-71, 2023.
Inspire Record 2026264 DOI 10.17182/hepdata.133480

In our Galaxy, light antinuclei composed of antiprotons and antineutrons can be produced through high-energy cosmic-ray collisions with the interstellar medium or could also originate from the annihilation of dark-matter particles that have not yet been discovered. On Earth, the only way to produce and study antinuclei with high precision is to create them at high-energy particle accelerators. Although the properties of elementary antiparticles have been studied in detail, the knowledge of the interaction of light antinuclei with matter is limited. We determine the disappearance probability of $^{3}\overline{\rm He}$ when it encounters matter particles and annihilates or disintegrates within the ALICE detector at the Large Hadron Collider. We extract the inelastic interaction cross section, which is then used as input to calculations of the transparency of our Galaxy to the propagation of $^{3}\overline{\rm He}$ stemming from dark-matter annihilation and cosmic-ray interactions within the interstellar medium. For a specific dark-matter profile, we estimate a transparency of about 50%, whereas it varies with increasing $^{3}\overline{\rm He}$ momentum from 25% to 90% for cosmic-ray sources. The results indicate that $^{3}\overline{\rm He}$ nuclei can travel long distances in the Galaxy, and can be used to study cosmic-ray interactions and dark-matter annihilation.

21 data tables
Table 1

Raw primary antihelium3-to-helium3 ratio as a function of the momentum p_primary.

Table 2

Raw primary antihelium3-to-helium3 ratio from Geant4-based MC simulations as a function of the momentum p_primary with default sigma_inel(3Hebar).

Table 3

Raw primary antihelium3-to-helium3 ratio from Geant4-based MC simulations as a function of the momentum p_primary with sigma_inel(3Hebar)x0.5.

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Limits on Dark Matter Annihilation in the Sun using the ANTARES Neutrino Telescope

The ANTARES collaboration Adrian-Martinez, S. ; Albert, A. ; Andre, M. ; et al.
Phys.Lett.B 759 (2016) 69-74, 2016.
Inspire Record 1426493 DOI 10.17182/hepdata.77062

A search for muon neutrinos originating from dark matter annihilations in the Sun is performed using the data recorded by the ANTARES neutrino telescope from 2007 to 2012. In order to obtain the best possible sensitivities to dark matter signals, an optimisation of the event selection criteria is performed taking into account the background of atmospheric muons, atmospheric neutrinos and the energy spectra of the expected neutrino signals. No significant excess over the background is observed and $90\%$ C.L. upper limits on the neutrino flux, the spin--dependent and spin--independent WIMP-nucleon cross--sections are derived for WIMP masses ranging from $ \rm 50$ GeV to $\rm 5$ TeV for the annihilation channels $\rm WIMP + WIMP \to b \bar b, W^+ W^-$ and $\rm \tau^+ \tau^-$.

3 data tables
Table 1

Upper limit on neutrino flux coming from the Sun for different annihiliation channels and WIMP masses. Limits for the $W^+W^-$ channel cannot be produced for WIMP masses below the mass of the $W$ boson.

Table 2

Upper limit on spin-dependent cross-section for different annihiliation channels and WIMP masses. Limits for the $W^+W^-$ channel cannot be produced for WIMP masses below the mass of the $W$ boson.

Table 3

Upper limit on spin-independent cross-section for different annihiliation channels and WIMP masses. Limits for the $W^+W^-$ channel cannot be produced for WIMP masses below the mass of the $W$ boson.