Seminars

IIHE Invited seminar: The Neutrino Cross Section at High Energies - New Results from IceCube

by Dr Colton Hill (Technische Universität München)

→ Europe/Brussels
G/1-G.1.03 - J. Sacton (Building G)

G/1-G.1.03 - J. Sacton

Building G

45
Description
Abstract: IceCube is a cubic-kilometer neutrino telescope at the geographic South Pole, which detects neutrinos from a few GeV to a few PeV -- energies largely inaccessible to terrestrial accelerators. The multi-purpose detector serves both as a central instrument in multi-messenger astrophysics, as well as a unique laboratory to study fundamental physics.

Starting from TeV energies, the Earth is no longer transparent to neutrinos, the flux becomes measurably attenuated while traversing the Earth. The attenuation depends directly on the cross section, largely decoupling measurements of the cross section from uncertainties associated with predictions of the atmospheric and astrophysical neutrino fluxes. 

This new IceCube result exploits this, combining multiple event selections into an all-sky, all-flavour sample, achieving leading sensitivity to the total cross section between 750 GeV and 10 PeV. This seminar will present the analysis strategy and key results, then discuss implications for future high energy neutrino experiments, such as IceCube-Gen2, where interactions explore unmeasured kinematic environments.

 
Short Bio: I graduated with my PhD from University of Manchester working on the (at that time) very new liquid Argon neutrino programme at FermiLab, including MicroBooNE and SBND, publishing the first electron neutrino cross section measurement on Argon. I then moved to Chiba University in Japan to work on IceCube, primarily developing hardware for the IceCube Upgrade, travelling twice to the South Pole to deploy the new detector between 2024 and 2026. Recently I moved to TU Munich, where I now lead calibration efforts of the Upgrade, and have returned to studying neutrino cross sections, including how current modelling impacts measurements from GeV to PeV energies.