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The Galileo Project aims to shed light on the nature and characteristics of Unidentified Aerial Phenomena (UAP). We are developing a multi-modal instrumentation suite that will monitor the sky in seven electromagnetic and three audio bands. Computing will play a critical role in this project, enabling the automated collection and processing of data. In this paper, we provide a brief overview of data sources, and describe our plan for computing infrastructure and architecture. We present a proposed real-time pipeline for distinguishing between natural and human-made phenomena, and for detecting objects that fall outside the phenomenological envelope of known phenomena. In addition, we outline the algorithms we will test and evaluate for use in offline data analysis. While preliminary, our work represents a significant step towards a unified data capture and analysis platform for the systematic detection and rigorous scientific study of unusual aerial phenomena in a regional airspace. [ABSTRACT FROM AUTHOR]

The acoustic monitoring, omni-directional system (AMOS) in the Galileo Project is a passive, multi-band, field microphone suite designed to aid in the detection and characterization of aerial phenomena. Acoustic monitoring augments the Project's electromagnetic sensors suite by providing a relatively independent physical signal modality with which to validate the identification of known phenomena and to more fully characterize detected objects. The AMOS system spans infrasonic frequencies down to 0.05 Hz, all of audible, and ultrasonic frequencies up to 190 kHz. It uses three distinct systems with overlapping bandwidths: infrasonic (0.05 Hz – 20 Hz), audible (10 Hz – 20 kHz), and ultrasonic (16 kHz – 190 kHz). The sensors and their capture devices allow AMOS to monitor and characterize the tremendous range of sounds produced by natural and human-made aerial phenomena, and to encompass possible acoustic characteristics of novel sources. Sound signals from aerial objects can be captured and classified with a single microphone under the following conditions: the sound reaches the sensor; the sound level is above ambient noise; and the signal has not been excessively distorted by the transmission path. A preliminary examination of the signal and noise environment required for the detection and characterization of aerial objects, based on theoretical and empirical equations for sound attenuation in air, finds that moderately loud audible sources (100 dB) at 1 km are detectable, especially for frequencies below 1 kHz and in quiet, rural environments. Infrasonic sources are detectable at much longer distances and ultrasonic at much shorter distances. Preliminary aircraft recordings collected using the single, omni-directional audible microphone are presented, along with basic spectral analysis. Such data will be used in conjunction with flight transponder data to develop algorithms and corresponding software for quickly identifying known aircraft and characterizing the sound transmission path. Future work will include multi-sensor audible and infrasonic arrays for sound localization; analysis of larger and more diverse data sets; and exploration of machine learning and artificial intelligence integration for the detection and identification of many more types of known phenomena in all three frequency bands. [ABSTRACT FROM AUTHOR]

In this paper, we review some of the extant literature on the study of interstellar objects (ISOs). With the forthcoming Vera C. Rubin Telescope and Legacy Survey of Space and Time (LSST), we find that 0. 3 8 − 8 4 'Oumuamua-like interstellar objects are expected to be detected in the next 10 years, with 95% confidence. The feasibility of a rendezvous trajectory has been demonstrated in previous work. In this paper, we investigate the requirements for a rendezvous mission with the primary objective of producing a resolved image of an interstellar object. We outline the rendezvous distances necessary as a function of resolution elements and object size. We expand upon current population synthesis models to account for the size dependency on the detection rates for reachable interstellar objects. We assess the trade-off between object diameter and occurrence rate, and conclude that objects with the size range between a third of the size and the size of 'Oumuamua will be optimal targets for an imaging rendezvous. We also discuss expectations for surface properties and spectral features of interstellar objects, as well as the benefits of various spacecraft storage locations. [ABSTRACT FROM AUTHOR]