Bulletin of the American Physical Society
APS April Meeting 2022
Volume 67, Number 6
Saturday–Tuesday, April 9–12, 2022; New York
Session W03: Next-Generation Observation of High-Energy NeutrinosRecordings Available
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Sponsoring Units: DAP Chair: Tiffany Lewis, NASA Goddard Space Flight Center Room: Salon 1 |
Monday, April 11, 2022 5:45PM - 5:57PM |
W03.00001: EUSO-SPB2 status and science goals Angela V Olinto, James H Adams, Luis A Anchordoqui, Mahdi Bagheri, Johannes Eser, John F Krizmanic, Adam N Otte, Thomas C Paul, Patrick Reardon, Hallsie Reno, Tonia M Venters, Lawrence R Wiencke EUSO-SPB2 (Extreme Universe Space Observatory on a Super Pressure Balloon, 2nd generation) is designed to observe extensive air-showers (EAS) generated by cosmic rays and neutrinos via an air-shower’s fluorescence or optical Cherenkov signals. EUSO-SPB2 consists of two wide-field of view, 1m diameter aperture telescopes, a Fluorescence Telescope (FT) and a Cherenkov Telescope (CT). The two Schmidt telescopes are being assembled in 2022 for a flight campaign in 2023 from Wanaka, New Zealand. The FT records the longitudinal development of an EAS from ultrahigh energy cosmic rays with energies above about 1 EeV. The CT design is designed for detecting the Cherenkov signal from EAS generated either above the Earth’s limb by cosmic rays or below the Earth’s limb by tau-neutrinos that interact as they traverse the Earth. Both telescopes will also study the possible backgrounds for these short timescale signals in the optical and ultraviolet. The CT threshold energy for detection for both the cosmic rays and neutrinos is around a PeV. Built with lessons learned from EUSO-SPB1 and significant advances in telescope design and modeling of the multi-messenger target of opportunity capabilities, the science payload for EUSO-SPB2 will provide pioneering and ground-breaking data to advance the fields of ultra-high energy cosmic rays and neutrino astrophysics. |
Monday, April 11, 2022 5:57PM - 6:09PM |
W03.00002: Development of the Cherenkov Telescope for EUSO-SPB2 Eliza A Gazda Ultrahigh-energy (UHE, >10 PeV) neutrinos provide crucial information to understand cosmic particle accelerators and neutrino physics at the highest energies. We are developing an imaging air-shower Cherenkov Telescope to detect Earth-skimming UHE neutrinos and measure Cherenkov signals from above the limb cosmic rays with around a PeV threshold energy. The telescope has a 0.785 m^2 light collection area and a 512-pixel SiPM camera covering a 12.8° x 6.4° (Horizontal x Vertical) field-of-view with 0.4° resolution. The camera signals are sampled with 100 MS/s and digitized with 12-bit resolution. The telescope will fly in 2023 as part of the Extreme Universe Space Observatory Super Pressure Balloon 2 (EUSO-SPB2), which is a benefit of future space-based missions. The objectives of the flight include: studying sources of background events, validating the performance of the instrument, searching for Earth-skimming tau neutrinos, observing air showers from cosmic rays above the Earth's limb. I present the status of the telescope and results from bench testing the system. |
Monday, April 11, 2022 6:09PM - 6:21PM |
W03.00003: EUSO-SPB2 Telescope Optics and Testing Viktoria Kungel The Extreme Universe Space Observatory - Super Pressure Balloon (EUSO-SPB2) mission will fly two custom telescopes to measure Čerenkov- and fluorescence-emission of extensive air-showers from cosmic rays at the PeV and EeV-scale, and search for tau-neutrinos. Telescope integration and laboratory calibration will be performed in Colorado. To estimate the point spread function and efficiency of the integrated telescopes, a test beam system that delivers a 1-meter diameter parallel beam of light is being fabricated. End-to-end tests of the fully integrated instruments will be carried out in a field campaign at dark sites in the Utah desert. The EUSO-SPB2 optics and laboratory tests will be presented at the APS. |
Monday, April 11, 2022 6:21PM - 6:33PM |
W03.00004: Horizontally Polarized Antennas for the Radio Neutrino Observatory in Greenland Bryan Hendricks Ultra-high energy (UHE) neutrinos (E > 10 PeV) are ideal messengers for the most distant objects in the universe as they travel nearly unimpeded across the cosmos and point directly to their source. However, because they are weakly interacting, they are challenging to detect. At the highest energies, neutrino detectors must monitor extraordinarily large volumes to counter the low interaction cross section and flux that falls steeply with energy. Radio neutrino detectors, taking advantage of the Askaryan effect which produces coherent radio emission, can be massive with sparse detectors due to the long attenuation length of radio waves. The Radio Neutrino Observatory in Greenland (RNO-G) is currently being built at the apex of the ice sheet in Greenland to detect the first UHE neutrinos. It will have 35 stations with both surface and deep components. To reconstruct the energy and direction of neutrinos detected by RNO-G, it must be able to obtain the signal polarization which it can do via the deep components using its horizontally and vertically polarized antennas. I will discuss the design and performance of its horizontally polarized antennas. |
Monday, April 11, 2022 6:33PM - 6:45PM |
W03.00005: An Efficient Detector for Tau Neutrinos at the Highest Energies: The Beamforming Elevated Array for COsmic Neutrinos (BEACON) Andrew J Zeolla When ultrahigh energy tau neutrinos skim the Earth, they can generate tau leptons that then decay in the atmosphere, forming upgoing extensive air showers. The Beamforming Elevated Array for COsmic Neutrinos (BEACON) is a novel detector concept that utilizes a mountaintop radio interferometer to search for the radio emission due to these extensive air showers. The prototype, located at the White Mountain Research Station in California, consists of 4 custom crossed-dipole antennas operating in the 30-80 MHz range and uses a directional interferometric trigger to achieve reduced thresholds and background rejection. The prototype will first be used to detect extensive air showers from down-going cosmic rays to validate the detector model. In this talk, we detail the ongoing cosmic ray search which utilizes both analysis of data collected by the prototype, and simulation. We also discuss recent upgrades made to the BEACON prototype design, as well as the calibration of the antenna array. |
Monday, April 11, 2022 6:45PM - 6:57PM |
W03.00006: Custom Modular Data Acquisition Systems for the BEACON Experiment Zachary Curtis-Ginsberg The Beamforming Elevated Array for COsmic Neutrinos (BEACON) is a new concept targeting the highest tau energy neutrinos (E > 100 PeV). The design uses a compact antenna array on a high elevation mountain to search for radio emission from upgoing tau leptons produced by tau neutrino interactions in the Earth. A prototype for BEACON – located at White Mountain Research Station in California – consists of 4 custom crossed dipole antennas operating in the 30-80 MHz range that are phased in real-time. A novel, modular data acquisition (DAQ) system is being developed to deploy a BEACON station in remote environments. The new DAQ will support up to 32 science instruments, like antennas, while maintaining a small footprint and drawing minimal power. With this new instrumentation and a full deployment, the detector will provide a measurement of the tau flavor of cosmogenic neutrinos, which could be used to set limits on the observed flavor ratios for cosmogenic neutrinos complimentary to the all-flavor flux measurements from other experiments. In this talk I will give a brief overview of BEACON, the development of the new instrumentation for the full array, and discuss how it will be used in the prototype. |
Monday, April 11, 2022 6:57PM - 7:09PM |
W03.00007: Direction Reconstruction for the Radar Echo Telescope for Neutrinos (RET-N) Dylan Frikken The Radar Echo Telescope for Neutrinos (RET-N) is a proposed experiment to detect neutrinos with energies above a few PeV utilizing the radar echo method in Antarctic ice. RET-N will consist of a radio transmitter and an array of receivers, aiming to detect the ionization trail from a ultra-high-energy neutrino interaction in-ice via active radar sounding. A powerful variable for direction reconstruction is the frequency content of the received signal, which changes based on event geometry. This frequency content is dependent on the angles between the cascade momentum direction and array geometry. In this talk, we present a simulation-based reconstruction method utilizing image recognition software to search time-frequency plots for radar echoes. An initial estimate of directional resolution will be reported. This method will be tested in the pathfinder experiment for RET-N, the Radar Echo Telescope for Cosmic Rays (RET-CR). |
Monday, April 11, 2022 7:09PM - 7:21PM |
W03.00008: The low frequency instrument on the PUEO experiment targeting upgoing air showers Yuchieh Ku, Stephanie A Wissel, Valentin Decoene The Payload for Ultrahigh Energy Observations (PUEO) long-duration balloon experiment is designed to observe ultra-high energy (UHE) neutrinos with energy above EeV. These neutrinos are essential tools to probe the extreme-energy universe at all distance scales, such as the production mechanism of UHE cosmic rays. PUEO consists of horn antennas that operate at 300-1200 MHz range as the main instrument and a low frequency (LF) instrument dropped down from the payload. We will present the design of the LF instrument. The LF instrument operates in the 50-300 MHz range, and it is composed of an antenna array that is sensitive to radio waves emitted from air showers. These showers can be initiated by either cosmic rays or tau leptons that are produced from Earth-skimming neutrinos. We will present the expected performance of PUEO to detect tau neutrinos, including both the effective area and expected angular resolution. The LF instrument will be compared to the main instrument and the combined sensitivity of both the LF and the main instrument together. |
Monday, April 11, 2022 7:21PM - 7:33PM |
W03.00009: The Trinity Neutrino Observatory Adam N Otte The detection of astrophysical neutrinos with IceCube has renewed the interest in opening the neutrino window at even higher energies. Trinity is a proposed system of air-shower imaging telescopes to detect Earth-skimming tau neutrinos. The observatory will have 18 novel wide field-of-view telescopes distributed at three different sites on mountain tops. With its high sensitivity from 1 PeV to 10 EeV, Trinity will fill the gap between IceCube and proposed radio UHE-neutrino instruments. In this talk, I will discuss Trinity's concept, design, and sensitivity to diffuse and point sources, highlighting synergies with future radio and in-ice optical observatories. I will close by discussing the Trinity demonstrator we are constructing and planning to deploy in Fall 2022 on Frisco Peak, Utah. |
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