# Velocity independent constraints on spin-dependent DM-nucleon interactions from IceCube and PICO

## TL;DR

This paper derives velocity-independent constraints on spin-dependent dark matter-nucleon interactions by combining IceCube and PICO data, accounting for deviations from the Standard Halo Model and local substructures.

## Contribution

It introduces a method to set conservative, velocity-independent limits on DM interactions using complementary neutrino and recoil data, considering non-standard halo models.

## Key findings

- Constraints on spin-dependent cross-section: σ_SD ≲ 3×10^−39 cm^2 at 1 TeV.
- Results are independent of DM velocity distribution assumptions.
- Constraints scale inversely with local DM density.

## Abstract

Adopting the Standard Halo Model (SHM) of an isotropic Maxwellian velocity distribution for dark matter (DM) particles in the Galaxy, the most stringent current constraints on their spin-dependent scattering cross-section with nucleons come from the IceCube neutrino observatory and the PICO-60 C$_3$F$_8$ superheated bubble chamber experiments. The former is sensitive to high energy neutrinos from the self-annihilation of DM particles captured in the Sun, while the latter looks for nuclear recoil events from DM scattering off nucleons. Although slower DM particles are more likely to be captured by the Sun, the faster ones are more likely to be detected by PICO. Recent N-body simulations suggest significant deviations from the SHM for the smooth halo component of the DM, while observations hint at a dominant fraction of the local DM being in substructures. We use the method of Ferrer et al. (2015) to exploit the complementarity between the two approaches and derive conservative constraints on DM-nucleon scattering. Our results constrain $\sigma_{\mathrm{SD}} \lesssim 3 \times 10^{-39} \mathrm{cm}^2$ (6 $ \times 10^{-38} \mathrm{cm}^2$) at $\gtrsim 90\%$ C.L. for a DM particle of mass 1~TeV annihilating into $\tau^+ \tau^-$ ($b\bar{b}$) with a local density of $\rho_{\mathrm{DM}} = 0.3~\mathrm{ GeV/cm}^3$. The constraints scale inversely with $\rho_{\mathrm{DM}}$ and are independent of the DM velocity distribution.