Bulletin of the American Physical Society
APS April Meeting 2018
Volume 63, Number 4
Saturday–Tuesday, April 14–17, 2018; Columbus, Ohio
Session R17: Detection and Origin of Astrophysical Neutrinos |
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Sponsoring Units: DAP DPF Chair: John Beacom, The Ohio State University Room: B234-235 |
Monday, April 16, 2018 10:45AM - 10:57AM |
R17.00001: The IceCube Neutrino Observatory: Future Plans Tyce DeYoung The IceCube Neutrino Observatory, located at the US South Pole Station, is the world’s largest neutrino detector. Recent observations have revealed the existence of a substantial flux of high energy neutrinos emitted by astrophysical sources. Proposed upgrades of the IceCube Observatory would further illuminate the identity and dynamics of these sources, as well as providing better probes of fundamental neutrino physics. [Preview Abstract] |
Monday, April 16, 2018 10:57AM - 11:09AM |
R17.00002: Improvements in IceCube event reconstructions Tianlu Yuan At the highest energies, the angular resolution of IceCube is limited primarily by ice property uncertainties. Charged-current interactions with an outgoing muon have a smaller dependence on ice modeling when reconstructing the incoming direction. Interaction channels without a high-energy muon are more affected by the ice properties. This talk will highlight the impact of using a new ice-model for both cascades and tracks. I will frame this discussion by means of the recent track event coincident with a blazar flare and latest high-energy starting neutrino event (HESE) sample. [Preview Abstract] |
Monday, April 16, 2018 11:09AM - 11:21AM |
R17.00003: An update on the IceCube enhanced starting track event selection and realtime stream Sarah Mancina, Kyle Jero IceCube is a detector built in the South Pole ice that observes astrophysical neutrinos as an unambiguous signature of the origin of cosmic rays. IceCube analyses which look in the southern sky face a large background of atmospheric neutrinos and muons. In this talk we will present an event sample which selects for muon tracks from neutrinos which begin inside the detector and rejects incoming backgrounds. The selection determines if an event starts inside the detector or not based on the event’s reconstructed direction and hit pattern. This starting track selection has a high astrophysical neutrino purity above 10 TeV in the southern sky. We will present our most recent results from our neutrino point source and diffuse flux searches and provide a look at the realtime events stream derived from the selection. [Preview Abstract] |
Monday, April 16, 2018 11:21AM - 11:33AM |
R17.00004: Abstract Withdrawn
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Monday, April 16, 2018 11:33AM - 11:45AM |
R17.00005: Relic Supernova Neutrinos and the Nuclear Equation of State Grant Mathews, Jun Hidaka, Toshitaka Kajino Understanding the mechanism of core-collapse supernova explosions requires knowledge of the nuclear equation of state (EoS). Recent multidimensional numerical simulations indicate that explosions are possible. Nevertheless, it is not yet fully understood which equation of state is realized in the proto-neutron star formed during the SNe explosion. We examine the EoS dependence of the neutrino emission from failed supernovae (fSNe) as a probe of the properties of the nuclear EoS due to its influence on the relic supernova neutrino spectrum. We consider a variety of astrophysical scenarios, which include different progenitor masses for a successful explosion, the cosmological star formation rate, starbursts, quiescent star formation, and the metallicity dependence of the initial mass function. We find a robust EoS dependence, and we highlight the usefulness of future neutrino detectors to distinguish the nuclear EoS. [Preview Abstract] |
Monday, April 16, 2018 11:45AM - 11:57AM |
R17.00006: Supernova Neutrino Detection at the NOvA Experiment Justin Vasel, Andrey Sheshukov, Alec Habig The next galactic core-collapse supernova will deliver a wealth of neutrinos which for the first time humanity is well-situated to measure. These explosions produce neutrinos with energies between a few and 100 MeV over a period of tens of seconds. Galactic supernovae are relatively rare events, occurring with a frequency of just a few per century. It is therefore essential that all neutrino detectors capable of detecting these neutrinos are ready to trigger on this signal when it occurs. This talk summarizes the ongoing efforts to detect these neutrinos in the NOvA detectors, including the development of a supernova trigger, background rejection, and event reconstruction. [Preview Abstract] |
Monday, April 16, 2018 11:57AM - 12:09PM |
R17.00007: Distinguishing DSNB signal from atmospheric neutrino backgrounds in Super-Kamiokande and future SK-Gd Bei Zhou, John Beacom Detection of the diffuse supernova neutrino background (DSNB) is of great importance, which will greatly help the understanding of both core-collapse physics and neutrino physics. However, after tens of years' effort of Super-Kamiokande (SK), DSNB is still hidden in the remaining backgrounds, dominated by decay electrons from invisible muons induced by atmospheric $\nu_\mu$ and prompt electrons from atmospheric $\nu_e$ interactions. In this work we explore the underlying physics of the dominant backgrounds and propose new detection methods for DSNB observation, for both current SK and future SK-Gd, which has the neutron-tagging ability. These methods, if adopted by SK, will greatly improve the detectability of DSNB. [Preview Abstract] |
Monday, April 16, 2018 12:09PM - 12:21PM |
R17.00008: Supernova Neutrino Studies for the Deep Underground Neutrino Experiment Erin Conley Currently, the mechanism behind supernova core collapse is not fully understood. Neutrinos carry a majority of the core collapse energy and their detection will provide crucial information about the supernova. Comprehending the physics of how massive stars die will lead to a better understanding of the creation of elements, properties of neutrinos, and constraints on beyond-the-Standard-Model physics. This talk will report on simulation studies of supernova neutrinos in the Deep Underground Neutrino Experiment (DUNE) and development of algorithms to distinguish interaction channels of neutrinos with liquid argon. [Preview Abstract] |
Monday, April 16, 2018 12:21PM - 12:33PM |
R17.00009: Detecting Neutrinos with DarkSide-20k Ziping Ye The core detector of DarkSide-20k experiment is a two-phase liquid argon time projection chamber (LAr TPC) with 20 tons fiducial mass. It is designed to register possible nuclear recoil events due to rare scattering of dark matter particles off atomic nuclei, and is located deep underground at Gran Sasso National Lab (LNGS) in Italy. DarkSide-20k can achieve background free rare event searches thanks to the following features: a cosmic ray muon veto, a neutron veto, low-radioactivity argon in the TPC, pulse shape discrimination between nuclear recoil and electron recoil, and 3D coordinate reconstruction. It is thus ideal for weakly interacting massive particle (WIMP) searches. As a bonus, it is also very promising for studying neutrinos. Coherent neutrino-nucleus scattering (CNNS) would produce nuclear recoils with energies similar to collisions from dark matter particles. Our studies show that DarkSide-20k could uniquely contribute to the detection of supernova burst neutrinos, diffuse supernova and stellar neutrinos, and other sources of neutrinos. Detecting neutrinos in DarkSide-20k would also defines the neutrino floor for WIMP searches. [Preview Abstract] |
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