A5108015232- Astrophysics and Cosmic Phenomena
- Neutrino Physics Research
- Radio Astronomy Observations and Technology
- Solar and Space Plasma Dynamics
- Geophysics and Gravity Measurements
- Methane Hydrates and Related Phenomena
- Particle accelerators and beam dynamics
- Gamma-ray bursts and supernovae
University of Kansas
2023-2024
The Radio Neutrino Observatory – Greenland (RNO-G) seeks discovery of ultra-high energy neutrinos from the cosmos through their interactions in ice. science program extends beyond particle astrophysics to include radioglaciology and, as we show herein, solar observations, well. Currently seven 35 planned radio-receiver stations (24 antennas/station) are operational. These sensitive impulsive radio signals with frequencies between 80 and 700 MHz feature a neutrino trigger threshold for...
The Radio Neutrino Observatory in Greenland (RNO-G) is the first in-ice radio array northern hemisphere for detection of ultra-high energy neutrinos via coherent emission from neutrino-induced particle cascades within ice. currently phased construction near Summit Station on ice sheet, with 7~stations deployed during two boreal summer field seasons 2021 and 2022. In this paper, we describe installation system design these initial RNO-G stations, discuss performance as 2024.
The science program of the Radio Neutrino Observatory-Greenland (RNO-G) extends beyond particle astrophysics to include radioglaciology and, as we show herein, solar physics, well. Impulsive flare observations not only permit direct measurements light curves, spectral content, and polarization on time scales significantly shorter than most extant dedicated observatories, but also offer an extremely useful above-surface calibration source, with pointing precision order tens arc-minutes. Using...
We develop an in-situ index of refraction profile using the transit time radio signals broadcast from englacial transmitter to 2-5 km distant radio-frequency receivers, deployed at depths up 200 m. Maxwell's equations generally admit two ray propagation solutions a given transmitter, corresponding direct path (D) and refracted (R); measured D vs. R (dt(D,R)) timing differences provide constraints on near South Pole, where Askaryan Radio Array (ARA) neutrino observatory is located. constrain...
The Askaryan Radio Array (ARA) is a gigaton-size neutrino radio telescope situated near the geographic South Pole, which has been in operation since 2011. It specifically designed to detect emissions resulting from interaction between ultra-high energy neutrinos ($>10$ PeV) and Antarctic ice. Each of five ARA stations equipped with 16 antenna clusters arranged cubic configuration, approximately ${\sim}200$~m deep In this analysis, we utilize data two total livetime ${\sim}10.5$ years,...
The Askaryan Radio Array Station 1 (A1), the first among five autonomous stations deployed for ARA experiment at South Pole, is a unique ultra-high energy neutrino (UHEN) detector based on effect that uses Antarctic ice as medium. Its 16 radio antennas (distributed across 4 strings, each with 2 Vertically Polarized (VPol), Horizontally (HPol) receivers), and strings of transmitting (calibration pulsers, CPs), VPol HPol channel, are depths less than 100 m within shallow firn zone 2.8 km thick...
The Askaryan Radio Array (ARA) is an in-ice ultrahigh energy (UHE, $>10$ PeV) neutrino experiment at the South Pole that aims to detect radio emissions from neutrino-induced particle cascades. ARA has five independent stations which together have collected nearly 24 station-years of data. Each these search for UHE neutrinos by burying clusters antennas $\sim 200$ m deep in a roughly cubical lattice with side length 15$ m. Additionally, fifth station (A5) beamforming trigger, referred as...