University of Wisconsin-Madison

A measurement of the atmospheric electron neutrino spectrum with IceCube

One atmospheric neutrino is detected in IceCube about every six minutes. That’s an impressive rate compared to the astrophysical neutrino flux, which is about one contained event per month.

A precise measurement of this atmospheric neutrino flux will impact both neutrino astronomy and neutrino oscillation analyses, and it will also shed light on pion and kaon production in air showers, which still has large uncertainties at high energies.

In a new analysis by the IceCube Collaboration, the atmospheric electron neutrino spectrum is measured at energies between 0.1 TeV and 100 TeV, extending previous measurements to higher energies and yielding improved precision. The results, which have been submitted to Physical Review D, find good agreement with models of the conventional electron neutrino flux.

The atmospheric electron neutrino flux result (shown as red-filled triangles). Markers indicate the IceCube measurements of the atmospheric neutrino flux while lines show the theoretical models. The black circles and the blue band come from previous measurements of the conventional muon neutrino flux by IceCube. The open triangles show a previous measurement of the electron neutrino flux with an smaller IceCube-DeepCore dataset.  Image: IceCube Collaboration.
The atmospheric electron neutrino flux result (shown as red-filled triangles). Markers indicate the IceCube measurements of the atmospheric neutrino flux while lines show the theoretical models. The black circles and the blue band come from previous measurements of the conventional muon neutrino flux by IceCube. The open triangles show a previous measurement of the electron neutrino flux with an smaller IceCube-DeepCore dataset. Image: IceCube Collaboration.

Most atmospheric neutrinos are muon neutrinos produced by two-body decays of charged pions and kaons: the so-called conventional muon neutrino flux. Three-body decays of charged and neutral kaons are thought to be the main contributors to the conventional electron neutrino flux. And decays of mesons containing charm quarks, the so-called prompt component, will produce extra and equal amounts of muon and electron neutrinos. So far, the prompt contribution remains unmeasured, with this (and other) analyses providing weak constraints.

The conventional neutrino flux is thus dominated by muon neutrinos and is well studied in a wide energy range. However, the electron neutrino component is not well known, especially at high energies, where it becomes the main background for searches of astrophysical neutrinos. At those energies, the prompt component is also expected to become an important contributor to the total neutrino flux.

Data, shown with points, is compared to Monte Carlo predictions. A solid green line shows the sum of all Monte Carlos predictions, while the atmospheric neutrino predictions are shown with a cyan dotted line (muon neutrinos) and a blue solid line (electron neutrinos). The cosmic-ray muon background simulation is shown with a red line. Image: IceCube Collaboration.
Data, shown with points, is compared to Monte Carlo predictions. A solid green line shows the sum of all Monte Carlos predictions, while the atmospheric neutrino predictions are shown with a cyan dotted line (muon neutrinos) and a blue solid line (electron neutrinos). The cosmic-ray muon background simulation is shown with a red line. Image: IceCube Collaboration.

In this study, IceCube researchers use the first year of data with the full detector configuration, from May 2011 to May 2012, to measure the atmospheric electron neutrino flux. They select fully contained cascade events, which are mainly induced by electron neutrinos interacting in IceCube but also by neutral current interactions of muon and tau neutrinos. The largest background, though, is due to downward atmospheric muons, which above 500 GeV can easily penetrate the ice to the depth of IceCube.

The final selection includes only events above 300 GeV and with a cascade vertex in the fiducial region, which strongly reduces the cosmic-ray muon background. Other cuts are introduced to separate the atmospheric cascade signal from the remaining CR muon background. The final selection keeps the muon background to low levels, but the muon neutrino background becomes the highest component of the sample.

"We have measured the conventional electron neutrino flux with only one year of IceCube data,” says Chang Hyon Ha, an IceCube researcher at Lawrence Berkeley National Laboratory (LBNL). “One can expect a growing physics potential with multiyear data that will provide us with large samples of both conventional muon and electron neutrinos,” adds Chang Hyon.

The study also measures the conventional electron neutrino flux normalization, which relates to the relative contribution from pions and kaons to the conventional neutrino fluxes. The kaon contribution is found to be slightly above standard calculations, which indicates that current models of cosmic-ray interactions may underestimate the strange quark content in the air shower.

LBNL senior scientist Spencer Klein, who oversaw the analysis, noted that “the hint of a higher kaon contribution may be because the standard references assume proton-proton interactions. Studies at heavy-ion colliders find that the kaon contribution is higher in nuclear collisions involving heavier nuclei.” And also measurements of muon contents for inclined muon showers in several air shower experiments seem to point in the same direction.

+ Info “Measurement of the Atmospheric Spectrum with IceCube,” IceCube Collaboration: M.G. Aartsen et al. Published in Physical Review D91 (2015) 122004, arxiv.org/abs/1504.03753 journals.aps.org