Detecting astrophysical neutrinos at the highest known energies will help answer critically important questions in both astronomy and particle physics. While the existence of ultra-high-energy particle accelerators in our universe is well motivated by the decades of cosmic ray detections up to $10^{21}$ eV, not much is known about the sources themselves. Neutrinos are the only known messenger particle capable of both traveling directly from the source and traveling cosmic distances to reach detectors on Earth. However, because neutrinos rarely interact with matter, detectors must be built to survey many square kilometers to have a chance at regularly seeing these rare events. The Askaryan Radio Array (ARA) is one such detector, located at the South Pole and designed to be sensitive to the radio emission created when a neutrino interacts in the Antarctic ice. Over the last decade, five independent ARA Stations have been built, amassing decades of station years worth of data and setting some of the most competitive flux limits between $10^{16}$ and $10^{19.5}$ eV compared to other radio experiments. This thesis is focused on the newest result from ARA: an analysis of one year of data from the newest station, ARA Station 5. This station is equipped with a low threshold trigger capable of triggering on weaker events than previous ARA stations, with a particular improvement in sensitivity at lower energies. This work discusses the hardware design, deployment, calibration, and first analysis of this new station, proving the feasibility of this type of station design, and motivating its use in future full-scale experiments such as the Radio Neutrino Observatory in Greenland (RNO-G), the Payload for Ultrahigh Energy Observations (PUEO) and potentially IceCube-Gen2. This thesis will also discuss other projects; in particular, the Beamforming Elevated Array for Cosmic Neutrinos (BEACON), a mountaintop detector looking specifically for cosmic rays. With so many new experiments coming online in the next few years, this analysis will impact big decisions regarding future detector design and analysis techniques. Contributing to these efforts has been exciting work, as we look to officially enter the era of ultra-high energy neutrino astronomy.