Publications

Dark Matter signals become brighter righter when inverse-Compton is modeled more accurately

Searches for cosmic-ray positrons are one of the most sensitive probes of dark matter annihilation. This is particularly true for leptophilic dark matter models that can be difficult to detect via other channels. The principle impediment to detecting the sharply peaked positron spectrum from leptophilic dark matter is the cooling of the positrons via synchrotron and inverse-Compton scattering, which has normally been treated via a simplified model that assumes these losses are continuous. We show that when the stochasticity of inverse-Compton losses is taken into account, the expected signal becomes twice as bright, making it easier to detect heavy dark matter.

Strongly Coupled Dark Matter Models Can Produce Antihelium 4

AMS-02 has tentatively detected a flux of antihelium nuclei (around 10 events in total). This observation, if confirmed, would be very exciting because antihelium is not supposed to be produced by standard astrophysics -- and would point towards new physics. More confusingly, a handful of these events may be consistent with antihelium 4 -- which is difficult to produce even in dark matter models. We propose the first realistic dark matter model capable of producing an observable antihelium 4 flux. If the WIMP is very heavy (near unitarity scale), and annihilates through a strongly coupled dark sector, then each annihilation will produce a shower of dark pions with very high multiplicity. If these particles quickly decay to standard model quarks through a portal interaction -- the result is a high multiplicity of baryons produced promptly at the same vertex. This significantly enhances the formation of heavy antinuclei, and makes observations of antihelium-4 possible.

Cosmic-Ray Positrons Strongly Constrain Leptophilic Dark Matter

Observations of antimatter cosmic-rays are powerful probes of dark matter annihilation -- as they are produced copiously by dark matter annihilation but were thought to only be produced through secondary astrophysical processes. Observations by PAMELA and AMS-02 found a significant excess in cosmic-ray positrons, which attracted significant interest from the dark matter community, but has been more successfully explained through the emission of e+e- pairs by high-energy pulsars. Here, we note that -- in scenarios where pulsars dominate the high-energy positron flux -- the smoothness of the positron spectrum can constrain sub-dominant dark matter contributions. This is particularly true for leptophilic dark matter models that produce significant bumps in the cosmic-ray positron spectrum. Using recently released AMS-02 data, we set strong cosntraints on dark matter annihilation to e+e-, mu+mu- and tau+tau- final states - producing limits which fall below the thermal annihilation cross-section in many models.

Antiheliums from Dark Matter

AMS-02 has tentatively detected approximately 10 anti-Helium 3 nuclei. Such an observation would constitute smoking gun evidence of new physics, because the astrophysical production of antihelium is expected to be negligible. However, most studies of dark matter annihilation have concluded that the dark matter induced antihelium flux should also be small. Here, we carefully analyze previous studies, and discover a antihelium production pathway which had been neglected by previous literature -- the displaced vertex decays of Lambda-bottom antibaryons. The optimal mass (roughly 6 proton masses) and anti-baryon number of Lambda_baryons make them optimal candidates to efficiently produce antihelium nuclei. Intriguingly, standard particle physics codes (e.g, Pythia) predict that this pathway should dominate the production of detectable antihelium, increasing the standard antihelium production rate of dark matter annihilation by nearly a factor of 100 compared to previous computations.

Antihelium from Dark Matter

AMS-02 has reported the tentative detection of approximately a dozen anti-Helium 3 and anti-Helium 4 nuclei. Astrophysical interactions capable of making high-energy anti-nuclei are kinematically suppressed, making such a signal a potential smoking gun for dark matter annihilation. Unfortunately, it is also extremely difficult to explain such a signal with dark matter models either, due to the very small range of coalescence momenta that is capable of producing such particles. We present a new astrophysical method for enhancing the dark matter induced anti-Helium flux, by using Alfven waves to reaccelerate very low-energy anti-Helium particles to higher energies, where they may be more readily detected by AMS-02.

A Robust Detection of an Antiproton Excess

Previous studies by Cuoco et al (1610.03071) and Cui et al. (1610.03840) have uncovered evidence for an excess in cosmic-ray antiprotons in the AMS-02 data, centered at a rigidity of around 5 GeV. The resilience of this excess has been called into question by other analyses (e.g., Reinert & Winkler 1712.00002), which argued that uncertainties in the background modeling could decrease the significance of the signal. We utilize an improved method to constrain solar modulation and antiproton production uncertainties, and test number of diffuse emission models, finding that the statistical significance of the excess remains robust, providing an intriguing signal that remains consistent with dark matter annihilation.

Dark Matter Searches with Cosmic Rays

Dark Matter signals become brighter righter when inverse-Compton is modeled more accurately

Research Topics

Strongly Coupled Dark Matter Models Can Produce Antihelium 4

Cosmic-Ray Positrons Strongly Constrain Leptophilic Dark Matter

Antiheliums from Dark Matter

Antihelium from Dark Matter

A Robust Detection of an Antiproton Excess

Full Publication List:

White Papers

Snowmass2021 Cosmic Frontier White Paper: Puzzling Excesses in Dark Matter Searches and How to Resolve Them

Positron Annihilation in the Galaxy

Tim Linden