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A Comprehensive Network for the Discovery and Characterization of Interstellar Objects Like 3I/ATLAS

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An artist’s illustration of a lunar base with potential scientific benefits. An optical interferometer on the atmosphere-free Moon with a baseline of 100 meters can resolve the nucleus of interstellar objects like 3I/ATLAS, at a distance comparable to the Earth-Sun separation. (Image credit: ESA — P.Carril)

Inspired by the unresolved anomalies displayed by the latest interstellar visitor 3I/ATLAS (as listed here), I co-authored a new paper with the brilliant graduate student, Oem Trivedi. The paper is titled: “A Comprehensive Network for the Discovery and Characterization of Interstellar Objects.”

The last decade had ushered-in the discovery of interstellar objects (ISOs), marking the emergence of a genuinely new observational window into our cosmic neighborhood beyond the Solar System, akin to finding objects from the street in our backyard. The discoveries of 1I/‘Oumuamua, IM1, 2I/Borisov, and most recently 3I/ATLAS, have demonstrated unambiguously that the Solar System is not isolated but rather permeated by a substantial flux of objects from our cosmic street. These detections provided the first direct empirical evidence for the physical properties of objects born in environments far removed from our own. In doing so, ISO astronomy has begun to offer insights in a way that was previously accessible only through remote observing and indirect inference.

At the same time, the rapid progress of the field has highlighted how young and structurally incomplete ISO studies are. Current discoveries are rare, observationally constrained and often characterized by substantial degeneracies in physical interpretation. Detection of new ISOs is limited by short visibility windows and survey observing frequency (cadence). Follow-up observations are frequently reactive, fragmented and constrained by atmospheric or scheduling limitations. As a result, many of the most fundamental questions regarding ISO size, shape, composition, internal structure and dynamical history, remain weakly constrained. These challenges imply that the present era represents an early, exploratory phase in which observational capability has outpaced the development of a coherent end-to-end strategy.

This state-of-affairs motivated me and Oem to imagine a future observational architecture for ISO studies that can scale with rising discovery rates and increasing scientific and societal relevance. Aside from the opportunity to learn about asteroids or comets in other planetary systems, the possibility that some ISOs might carry alien technology highlights their potential significance for the future of humanity. In the context of planetary defense, it is imperative to develop a comprehensive detection and characterization scheme that would alert earthlings to a `black swan event’ — in which an interstellar technological probe would pose a potential threat to humanity. The likelihood of this risk can be expressed in the context of the Loeb Classification Scale, as quantified here, here and here.

Despite the rapid growth of time-domain sky surveys, the current searches for ISOs remain constrained by a small number of structural limitations that collectively restrict both the rate of discovery and the depth of physical inference that can be drawn from any individual detection. These limitations do not arise from a lack of observational effort but from the intrinsic mismatch between the transient, fast moving nature of ISOs and the capabilities of existing discovery and follow-up infrastructure. In particular, there are four dominant issues that presently define the boundary of what ISO searches can achieve.

A first and primary limitation is that ISO discovery is inherently a cadence-limited problem, since the visibility window of an ISO is intrinsically short. A second major limitation arises after detection, with the severe degeneracy in photometric (brightness) and astrometric (sky coordinates) inferences — caused by short observational arcs and unfavorable viewing geometry. A third limiting factor is the ambiguity in interpreting non-gravitational accelerations in terms of cometary outgassing, solar radiation pressure or technological thrusters. The fourth, and arguably most fundamental limitation, is the lack of direct spatial resolution of ISOs.

Taken together, these four issues delineate the landscape of unknown physical properties in existing ISO studies. ISO discovery is limited by cadence and visibility windows, physical inference is dominated by photometric and dynamical degeneracies, non-gravitational effects remain fundamentally ambiguous and the absence of rapid, high-resolution characterization prevents the resolution of these degeneracies. These limitations are not independent but mutually reinforcing. They underline the need for an observational architecture that explicitly separates and optimizes discovery and characterization, while preserving information content through rapid response and access to fundamentally new measurement modes.

The above-mentioned limitations point towards an observational architecture in which no single facility, mission class or observational mode can simultaneously satisfy the requirements of ISO discovery, physical characterization, and risk assessment. Instead, a coordinated observational architecture is required, in which different components are explicitly optimized for distinct roles and are coupled through rapid information flow and decision logic.

At the discovery level, the core requirement is maximal sky coverage with high cadence and sufficient depth to detect fast-moving, faint objects over short visibility windows. Constructing a second NSF-DOE Rubin Observatory setup to cover the northern hemisphere is a configuration that naturally satisfies this requirement for the entire sky with two state-of-the-art survey telescopes.

Discovery alone, however, does not address dominant inference degeneracies. The second layer of the architecture consists of rapid response, high angular resolution characterization, triggered automatically by discovery alerts and informed by real time orbital and photometric inferences. The fundamental quantity controlling the diagnostic power of imaging is the achievable resolution length, L = λ ∆ /D, where λ is the observing wavelength, ∆ is the object’s distance from the observatory and D the effective baseline of the observatory. For optical wavelengths λ ∼ 0.5 micrometers and distances ∆ < 1 AU, resolving sub-kilometer scale ISO requires effective baselines >100 meters. This resolution is far more challenging for terrestrial facilities owing to atmospheric turbulence. A lunar-based optical interferometer operating in a vacuum environment with stable thermal and mechanical conditions, naturally reaches this regime as the absence of atmospheric seeing allows diffraction-limited performance, while the lunar surface enables baselines at the required scale. Direct imaging at this resolution removes multiple degeneracies simultaneously by providing constraints on the shape, aspect ratio, binarity and surface structure of ISOs, thereby breaking the size-albedo-shape degeneracy inherent in unresolved images.

The third component of the proposed architecture is an interceptor mission, which occupies a different region of the cost-information space. Interceptors are not discovery instruments but high-cost, information-gathering systems capable of in-situ measurements. Their feasibility depends sensitively on warning time and orbit geometry. The relative velocity between a collocated spacecraft and an ISO must be smaller than the velocity thrust achievable by the spacecraft propulsion system, implying that early discovery and rapid orbit determination are prerequisites. The proposed architecture ensures that only a small subset of ISOs, selected on the basis of high scientific return or potential risk, are escalated to this level. In this sense, ISO interceptors represent the final rung in a hierarchical response ladder rather than a default solution.

This layered architecture directly resolves the four dominant limitations identified earlier. Cadence and visibility constraints are mitigated by dual hemisphere discovery while photometric and astrometric degeneracies are broken by spatially resolved imaging. Ambiguities in non-gravitational acceleration are addressed by high-resolution imaging, rotation and possibly through mass estimates. The fleeting nature of the information about ISOs is countered by an explicit rapid response design that minimizes latency between detection and characterization. Importantly, these solutions do not rely on speculative technologies but on combining existing and planned capabilities into a coherent system.

A coordinated ISO network consisting of Rubin-South and Rubin-North for discovery, lunar interferometry for rapid high-resolution characterization and ISO interceptors for exceptional cases, constitutes a logically consistent, quantitatively justified, and operationally feasible architecture. It directly addresses the structural limitations of current ISO studies, providing rational prioritization based on urgency needs regarding the Loeb scale classification scale for assessing potential threats to Earth from alien technology, and provides a compelling scientific justification for incorporating ISO imaging into the broader objectives of lunar exploration through NASA’s Artemis Program.

This architecture transforms ISO studies from an opportunistic, discovery driven activity into a mature observational discipline with a clear end-to-end strategy. We name this architecture as the “Comprehensive Inter-Stellar Objects Network”, abbreviated as CISON.

The current status of ISO studies is limited not by the absence of discovery facilities, but by the lack of a coherent end-to-end observational architecture that links discovery, characterization and decision making. By identifying the dominant structural issues in present ISO studies and formulating a coordinated response, CISON offers a physically motivated and operationally feasible framework. It separates discovery and characterization into complementary layers, combining dual hemisphere Rubin-class surveys with rapid response, high resolution follow-up and selective escalation to interceptor missions. CISON directly addresses the core limitations of cadence, degeneracy and fleeting information that currently define the field.

The CISON architecture alters not only the quantity but the quality of information available for newly discovered ISOs. Through early detection, spatially resolved imaging and rapid physical discrimination among non-gravitational effects, CISON enables decisive collapse of parameter degeneracies that otherwise persist until late times. When coupled to the differential formulation of the Loeb Scale, this improvement translates into faster, more stable and genuinely predictive classification of interstellar objects. The evolving Loeb score becomes an operational diagnostic rather than a retrospective label, allowing risk assessment and scientific prioritization to proceed on timescales of days to weeks instead of months.

The new paper quantifies the benefits of CISON in the context of discovering and characterizing the hypothetical 100th interstellar object, labeled as 100I/X.

CISON reframes ISO astronomy as a mature, anticipatory discipline rather than an opportunistic byproduct of time domain surveys as it is right now. By naturally motivating the inclusion of ISO imaging within lunar infrastructure within NASA’s Artemis program, the proposed architecture embeds interstellar science within the long-term expansion of observational capabilities beyond Earth. In doing so, CISON establishes a template for how future astronomical frontiers may be explored, through tightly integrated networks that combine wide-field discovery, precision characterization and quantitative decision frameworks.

As ISO detection rates rise in the coming decades from the NSF-DOE Rubin Observatory and its potential northern twin, CISON will be essential not only for maximizing scientific return but also for responsibly assessing rare objects that may carry profound implications for planetary defense, techno-signature searches and the understanding of our broader cosmic environment.

ABOUT THE AUTHOR

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(Image Credit: Chris Michel, National Academy of Sciences, 2023)

Avi Loeb is the head of the Galileo Project, founding director of Harvard University’s — Black Hole Initiative, director of the Institute for Theory and Computation at the Harvard-Smithsonian Center for Astrophysics, and the former chair of the astronomy department at Harvard University (2011–2020). He is a former member of the President’s Council of Advisors on Science and Technology and a former chair of the Board on Physics and Astronomy of the National Academies. He is the bestselling author of “Extraterrestrial: The First Sign of Intelligent Life Beyond Earth” and a co-author of the textbook “Life in the Cosmos”, both published in 2021. The paperback edition of his new book, titled “Interstellar”, was published in August 2024.

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