Bulletin of the American Physical Society
APS April Meeting 2020
Volume 65, Number 2
Saturday–Tuesday, April 18–21, 2020; Washington D.C.
Session X11: Neutrino DetectionLive
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Sponsoring Units: DAP Chair: Justin Vandenbroucke, University of Wisconsin Room: Maryland A |
Tuesday, April 21, 2020 10:45AM - 10:57AM Live |
X11.00001: Applying Recurrent Neural Networks to IceCube event reconstructions Johannes Wagner The IceCube Neutrino Observatory is a neutrino detector located in the deep glacial ice near the south pole. It is made up of a three-dimensional array of photodetectors contained within a cubic kilometer of ice. These measure the Cherenkov light from secondary particles caused by neutrino interactions. IceCube is primarily concerned with searching for neutrinos from astrophysical and atmospheric sources, making it a powerful tool to study the properties of these elusive particles. As a neutrino experiment, it relies on accurate predictions of particle energies and trajectories. Traditionally, reconstructions are done using likelihood maximization techniques. Recurrent Neural Networks (RNN's) present an interesting opportunity to improve both the speed and resolution of these reconstructions. These networks try to predict desired parameters from given time-series data by minimizing the error between known true values and predicted values. This is a natural fit for IceCube particle data, which consists of a time-series of detector hits. Using an RNN implementation combined with gaussian variance estimation, we can predict both the desired quantities as well as their uncertainties. The most recent results show promise for this new method of IceCube reconstructions. [Preview Abstract] |
Tuesday, April 21, 2020 10:57AM - 11:09AM Live |
X11.00002: A neural network based neutrino vertex reconstruction method for the Askaryan Radio Array (ARA) Yue Pan The Askaryan Radio Array (ARA) is an ultra-high energy (UHE) neutrino (E\textunderscore nu \textgreater 10\textasciicircum 17 eV) detector at South Pole. ARA aims to utilize radio signals detected from UHE neutrino interactions in glacial ice and infer information about the incident neutrinos. To retrieve this information from experiment data, the first step is to reconstruct the neutrino vertex location. By extracting timing from different antennas, the radiation direction and distance to the vertex can be determined. Together with measured polarization and power at the antennas, these can be used to reconstruct the neutrino direction and energy. I will discuss a solution based on neural networks which can achieve an error within 10 percent. [Preview Abstract] |
Tuesday, April 21, 2020 11:09AM - 11:21AM Live |
X11.00003: \emph{Trinity}: An air-shower imaging instrument to detect ultrahigh-energy neutrinos Nepomuk Otte The detection of TeV-PeV neutrinos with IceCube has cracked open a new window in astrophysics. The revelation of a relatively hard spectrum and the unknown origin of the neutrino flux are two motivations to extend neutrino measurements to even higher energies, namely the ultrahigh-energy (UHE) regime above $10^7$\,GeV. The seemingly preferred way to search for UHE neutrinos nowadays is with radio detectors employed in ice (e.g.~ARA and ARIANNA), on balloons (ANITA), or by pointing antennas at mountainous terrain (GRAND). In this talk, I show that a system of imaging detectors can also be a viable UHE neutrino detector if designed right. Based on these design considerations I present \emph{Trinity}, a system of six Cherenkov telescopes. I discuss the sensitivity of the system, how it can be built, address operational constraints, and plans to test the concept. [Preview Abstract] |
Tuesday, April 21, 2020 11:21AM - 11:33AM |
X11.00004: Measuring the High Energy Astrophysical Neutrino Flux with IceCube Austin Schneider The IceCube neutrino observatory has established the existence of an astrophysical diffuse neutrino component above 100 TeV. This discovery was made using the high-energy starting event sample, which uses the outer layer of instrumented volume as a veto to significantly reduce atmospheric background. We present the latest astrophysical neutrino flux measurement using high-energy starting events, extending the sample by 1.5 years for a total of 7.5 years. This new analysis updates the event properties with newer models of light transport in the glacial ice, and has an improved systematic treatment. We also report on the compatibility of our observations with detailed isotropic flux models proposed in the literature as well as the standard generic models such as single, double power-law scenarios. [Preview Abstract] |
Tuesday, April 21, 2020 11:33AM - 11:45AM Not Participating |
X11.00005: A Transient Search with IceCube-DeepCore Michael Larson A time-dependent flux of TeV neutrinos was recently discovered originating from the direction of the blazar TXS 0506+056 using the IceCube Neutrino Observatory. Additional events may be observable by IceCube at lower energies, although the existing analysis rapidly loses sensitivity below about 1 TeV. The densely instrumented DeepCore sub-array provides the ability to reduce the threshold for observation from 1 TeV down to approximately 10 GeV. This energy range, often ignored due to large backgrounds from conventional atmospheric neutrinos, can provide a unique window to probing low energy transient astrophysical fluxes. Using a newly developed sample, an analysis to search for astrophysical sources using these low energy transient sources will be presented. [Preview Abstract] |
Tuesday, April 21, 2020 11:45AM - 11:57AM Not Participating |
X11.00006: Searching for an Excess of Sub-Threshold Neutrino Flares in IceCube Data William Luszczak, Jim Braun, Albrecht Karle Recent results from IceCube regarding TXS 0506+056 suggest the presence of neutrino flares with no detectable gamma ray counterpart ("untriggered" neutrino flares). In this talk, we present a new method for fitting for all such flares simultaneously. In addition to being able to detect the presence of untriggered neutrino flares, this method also has the benefit of producing a neutrino flare curve, describing the temporal structure of the neutrino data associated with a particular location on sky. In this talk, we show results of applying this method across the full sky for 8 years of IceCube data, as well as results corresponding to using this method to stack sources in a catalog of Fermi3LAC blazars. [Preview Abstract] |
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