Bulletin of the American Physical Society
APS April Meeting 2023
Volume 68, Number 6
Minneapolis, Minnesota (Apr 15-18)
Virtual (Apr 24-26); Time Zone: Central Time
Session GG01: V: Neutrino Physics and Astrophysics I |
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Sponsoring Units: DPF Chair: Heidi Schellman, Oregon State University Room: Virtual Room 1 |
Monday, April 24, 2023 3:30PM - 3:42PM Withdrawn |
GG01.00001: Probing BSM Physics with Neutrinos from Astrophysical Sources at IceCube Kiara Carloni The recent observation of NGC 1068 by the IceCube Neutrino Observatory has opened a new window to neutrino physics at astrophysical scales. In this Letter, we propose a new method to probe the nature of neutrino masses using these observations. In particular, our method enables searching for signatures of pseudo-Dirac neutrinos with mass-squared differences that reach down to δm2 ≥ 10−21 eV2, improving the reach of terrestrial experiments by more than a billion. Finally, we discuss how the discovery of a constellation of neutrino sources can further increase the sensitivity and cover a wider range of δm2 values. |
Monday, April 24, 2023 3:42PM - 3:54PM |
GG01.00002: IceCube Angular Resolution Improvement via Muon Pre-pulse Effect Miaochen Jin, William G Thompson, Carlos A Arguelles Delgado The IceCube neutrino observatory utilizes Digital Optical Modules (DOMs) to detect Cherenkov photons emitted by charged leptons and hadrons in ice. Each DOM consists of a photomultiplier tube (PMT) enclosed in a spherical transparent glass shell. This study aims at improving IceCube angular resolution for subset of muon tracks by observing and successfully identifying pre-pulses created when muons pass directly through the DOMs. Such a capability will provide us with accurate pivot points in the muon track, significantly benefitting reconstruction algorithms. We study the scenario when a muon either hits the glass shell and emits Cherenkov light, or hits the PMT dynodes directly and creates photoelectrons, thereby creating a pre-pulse that arises before the main pulse caused by Cherenkov emission by the primary lepton in ice. |
Monday, April 24, 2023 3:54PM - 4:06PM |
GG01.00003: Status of the Measurement of Neutrinos Elastically Scattering Off Electrons in the NOvA Near Detector Yiwen Xiao Neutrinos elastically scattering off atomic electrons is a purely leptonic process whose cross section can be precisely calculated in the standard model. A measurement of this process can provide an in-situ constraint to the absolute neutrino flux in an accelerator-based νμ beam. NOvA is a long-baseline neutrino experiment optimized to observe the oscillation of muon neutrinos to electron neutrinos. It consists of a near detector located 1 km downstream of the neutrino production target at Fermilab and a far detector located 810 km away in Ash River, Minnesota. This talk presents the status of the neutrino-electron elastic scattering measurement, including strategies of selecting signals, as well as the prospect of reducing the flux uncertainty. |
Monday, April 24, 2023 4:06PM - 4:18PM |
GG01.00004: Calorimetric Detector Response in NOvA Maria Manrique Plata NOvA, the NuMI Off-Axis νe Appearance experiment, is a long baseline neutrino oscillation experiment which uses a predominantly muon neutrino, or antineutrino, beam. It is composed of two functionally equivalent liquid scintillator detectors separated by 809 km; a 300 ton near detector located at Fermilab and a 14kt far detector located at Ash River, Minnesota. NOvA’s physics analyses require accurate energy reconstruction. The following studies were performed, using near detector events, to better understand NOvA’s calorimetric detector response. First, we use the π0 → γγ decay, where the invariant π0 mass is directly correlated to the energy scale, to peek at the electromagnetic energy scale calibration. Secondly, we explore NOvA’s calorimetric response to events fully composed of electromagnetic particles, events fully composed of hadronic particles, and events with a mix of both. The lessons learned from quantifying the detector response will be incorporated into future energy reconstruction software. |
Monday, April 24, 2023 4:18PM - 4:30PM |
GG01.00005: TAMBO: Searching for Tau Neutrinos in the Peruvian Andes William G Thompson The detection of high-energy astrophysical neutrinos by IceCube has opened a new window on our Universe. While IceCube has measured the flux of these neutrinos at energies up to several PeV, much remains to be discovered regarding their origin and nature. Currently, measurements are limited by the small sample size of astrophysical neutrinos and by the difficulty of discriminating between electron and tau neutrinos. |
Monday, April 24, 2023 4:30PM - 4:42PM |
GG01.00006: Observation of the central engine of GRB170817A: the spin-down of a Kerr black hole based on multimessenger calorimetry and event timing Maurice Van Putten The central engine of GRB170817A is probed by a contemporaneous descending chirp in gravitational radiation in model-agnostic spectrograms with equal sensitivity to ascending and descending chirps using time-symmetric butterfly matched filtering, calibrated by software injection experiments. Statistical significance is expressed by probabilities of false alarm (PFA; type I errors) derived from event-timing analysis on the start-time $t_s$. PDF($t_s$)s are identified by high-resolution image analyses of the available spectrograms. For merged (H1,L1)-spectrograms, a PFA $p_1$ derives from causality given GW170817-GRB17081A. A statistically independent confirmation is presented in individual H1 and L1 analyses, in a second PFA $p_2$ of consistency in their respective observations of $t_s$ . A combined PFA derives from their product since mean and (respectively) difference in timing are statistically independent. PFAs in event timing thus produce $p_1 = 8.3 imes 10^{-4}$ and $p_2 = 4.9 imes 10^{-5}$ for the output ${cal E}_GW simeq 3.5\%M_odot c^2$ ($p_1p_2 = 4.1 imes 10^{-8}$ , equivalent Z-score 5.48). ${cal E}_GW$ exceeds $E_J$ of the hyper-massive neutron star in the immediate aftermath of GW170817, yet it is consistent with $E_J$ rejuvenated in delayed gravitational collapse to a Kerr black hole. Similar results may apply to energetic core-collapse supernovae. (van Putten, M.H.P.M., & Della Valle, M., 2022, A&A, in press, https://doi.org/10.1051/0004-6361/202142974.) |
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