Bulletin of the American Physical Society
2023 APS April Meeting
Volume 68, Number 6
Minneapolis, Minnesota (Apr 15-18)
Virtual (Apr 24-26); Time Zone: Central Time
Session Q13: Neutrino Astronomy III |
Hide Abstracts |
Sponsoring Units: DAP Chair: Luke Kelley Room: Marquette IV - 2nd Floor |
Monday, April 17, 2023 3:45PM - 3:57PM |
Q13.00001: The Cherenkov Telescope onboard EUSO-SPB2 Mission, Science and Status Mahdi Bagheri We present the status of the Cherenkov Telescope to be flown on a NASA ultra-long-duration balloon flight. The Extreme Universe Space Observatory on a Super Pressure Balloon 2 (EUSO-SPB2) carries a Fluorescence Telescope (FT) and a Cherenkov Telescope (CT) and is scheduled to launch in April or May 2023 from Wanaka, New Zealand as a precursor for future space-based missions to measure cosmic rays and astrophysical neutrinos via air shower's Fluorescence and Cherenkov signals. The science objectives involving the CT are to classify known and unknown sources of background, make the first observation of cosmic rays via the Cherenkov technique from suborbital altitude and perform target-of-opportunity searches in response to international multi-messenger alerts. CT will be able to slew and tilt towards neutrino transient targets and use the Earth-skimming technique to search for Very-High-Energy (VHE) tau neutrinos below the Earth's limb (E > 10 PeV). The Cherenkov telescope is equipped with a 512-pixel SiPM camera, covering a 12.8° x 6.4° (Horizontal x Vertical) field of view provided by Schmidt optics focused in stereo mode. Camera signals are digitized with a 100 MS/s readout system. We discuss the science goals, report the telescope development and integration status, and present recent field test results. |
Monday, April 17, 2023 3:57PM - 4:09PM |
Q13.00002: Progress on Trinity an IACT searching for UHE Neutrinos Mathew Potts Trinity is an Imaging Air Cherenkov Telescope (IACT) that is designed to search for Ultra-High-Energy (UHE) earth-skimming neutrinos. It has a novel optical structure design, pointing at the horizon, that will observe Cherenkov radiation from upward-going neutrino-induced air showers. Trinity is expected to be sensitive to neutrinos with energies between 1-10,000 PeV. The expected sensitivity of Trinity will play a role in filling the gap between the observed astrophysical neutrinos observed by IceCube and the predicted sensitivity of radio UHE neutrinos detectors. As a proof of concept, we are in the process of building a smaller demonstrator in Milford, Utah. This work will show the latest sensitivity calculations for the full Trinity Observatory and updates on the Trinity Demonstrator. |
Monday, April 17, 2023 4:09PM - 4:21PM |
Q13.00003: The Low Frequency Instrument for the Payload for Ultrahigh Energy Observations (PUEO) Yuchieh Ku The Payload for Ultrahigh Energy Observations (PUEO) long-duration balloon experiment is designed to observe ultra-high energy (UHE) neutrinos with energies above EeV. These neutrinos can probe the extreme-energy universe at all distance scales. PUEO consists of a Main Instrument on a payload and a Low Frequency (LF) instrument that will be deployed under the payload when the balloon reaches the stratosphere. The Main Instrument includes 108 dual polarized horn antennas that operate in the 300-1200 MHz range, and the 8 sinuous antennas that comprise the LF instrument receive signals in the 50-300 MHz range. The 8-meter tall, 4-meter wide hexagonal LF antenna array is sensitive to impulsive, geomagnetic radio signals emitted from air showers. Either cosmic rays or tau leptons that are produced from Earth-skimming neutrinos can initiate these showers. This talk will focus on the design and construction of the LF instrument, including the antennas, the gondola, the signal chain and the trigger. The expected sensitivity of the Main and the LF instruments to the tau neutrinos and the cosmic rays will also be presented. |
Monday, April 17, 2023 4:21PM - 4:33PM |
Q13.00004: nuSpaceSim: a Comprehensive Simulation Package for Optical Cherenkov and Radio Emission from Neutrino-Sourced Extensive Air Showers Austin Cummings
|
Monday, April 17, 2023 4:33PM - 4:45PM |
Q13.00005: The Fast Flavor Instability as a Catalyst for Neutrino Spin Oscillations in Neutron Star Mergers Henry R Purcell, Sherwood A Richers Recent studies have shown that in anisotropic environments neutrinos can present coherent helicity oscillations which depend directly on the absolute mass scale and Majorana phases. These oscillations are usually too transient to produce important effects in high-energy astrophysical phenomena. However, we demonstrate that a fast flavor instability can substantially increase the characteristic energy of spin oscillations for neutrinos travelling in specific directions, implying a fast flavor instability could 'catalyze' helicity transformation and make it measurable. We find several locations in a neutron star merger simulation where the conditions for a fast flavor instability and for resonant spin oscillations are met simultaneously. We run a particle-in-cell simulation of the fast flavor instability using data from these locations and show the energy of spin oscillations along the direction of maximal neutrino flux is raised by 4 or more orders of magnitude over the course of the instability. We directly solve the Schrodinger Equation using the spin-flavor Hamiltonian from before and after the Instability (setting it to be constant) to qualitatively observe the change in spin oscillations caused by a fast flavor instability. We find that the oscillations are still too transient for all but the lowest energy neutrinos to experience significant spin-flip effects. We conclude nonlinear resonance is likely necessary for spin flip to have an important influence on supernova or merger dynamics, though our proposed mechanism could work in conjuction with other effects to sufficiently raise the energy of spin oscillations. |
Monday, April 17, 2023 4:45PM - 4:57PM |
Q13.00006: Probing extreme astrophysical accelerators through large-scale neutrino anisotropy Marco S Muzio, Noemie Globus We present the extent to which large-scale anisotropies in the ultrahigh energy neutrino sky can probe the distribution of extreme astrophysical accelerators in the universe. In this talk, we discuss the origin of a large-scale neutrino anisotropy and show how observers can use this anisotropy to measure the evolution of ultrahigh energy neutrino sources — and therefore, the sources of ultrahigh energy cosmic rays — for the very first time. |
Monday, April 17, 2023 4:57PM - 5:09PM |
Q13.00007: Predictions of the diffuse supernova neutrino background Shunsaku Horiuchi The diffuse supernova neutrino background (DSNB) arises from the combined flux of neutrinos from all past core-collapse supernovae. The DSNB has not yet been detected, but the predicted DSNB flux is tantalizingly close to current upper limits and detection is anticipated by the now-completed gadonium upgrade at Super-Kamiokande. In this talk, we address critical theoretical uncertainties affecting predictions of the DSNB. First, recent systematic studies of stellar core collapse reveal the quantitative impacts of the progenitor conditions on the collapse process. Second, binary interactions, especially mass transfer and mergers, strongly influence the evolution of massive stars and change their final properties and the occurrence of supernovae. Third, recent core-collapse simulations have begun to model the late-time emission of neutrinos. Then, we put our predictions into the context of experimental sensitivity ongoing searches, finding promising prospects. |
Monday, April 17, 2023 5:09PM - 5:21PM |
Q13.00008: Measuring neutrino properties through the peculiar motion of galaxies Wangzheng ZHANG Neutrinos are believed to be the most abundant fermions in our Universe, but their masses are still one of the biggest puzzles in physics. As the presence of massive neutrinos affects both the cosmic expansion and the gravitational potential of structures, large-scale structures are expected to be a powerful probe to constrain neutrino properties in cosmology. Among these large-scale probes, the galaxy velocity field contains half of the phase space information, and the mean pairwise velocity is potentially a very useful observable to constrain structure formation. Using neutrino-involved N-body simulation, we study the dependences of the halo-halo pairwise velocities on the cosmic neutrino masses and chemical potentials. We found that the neutrino mass effect dominates over the chemical potential effect in these pairwise velocities, and the former always suppresses the structure formation. Finally, we make use of galaxy-galaxy pairwise velocity calculated from the observation (Cosmicflows-3) to constrain neutrino masses and chemical potentials. |
Monday, April 17, 2023 5:21PM - 5:33PM |
Q13.00009: Search for B8 solar neutrino nuclear recoil in XENONnT Dacheng Xu XENONnT is a dark matter direct detection experiment using a liquid xenon time projection chamber. By lowering the energy threshold to ~1 keV, it will be possible to search for the B8 solar neutrinos via coherent elastic neutrino-nucleus scattering (CEvNS). In this talk, I will present the background model in this search and projections for the power to discover B8 CEvNS with XENONnT. |
Follow Us |
Engage
Become an APS Member |
My APS
Renew Membership |
Information for |
About APSThe American Physical Society (APS) is a non-profit membership organization working to advance the knowledge of physics. |
© 2025 American Physical Society
| All rights reserved | Terms of Use
| Contact Us
Headquarters
1 Physics Ellipse, College Park, MD 20740-3844
(301) 209-3200
Editorial Office
100 Motor Pkwy, Suite 110, Hauppauge, NY 11788
(631) 591-4000
Office of Public Affairs
529 14th St NW, Suite 1050, Washington, D.C. 20045-2001
(202) 662-8700