The NEO Physical Observations and Properties Simulation (NEOPOPS) project

Near-Earth Objects (NEOs) provide key insights for understanding the primordial structure of planetesimals and the compositional gradient of the solar nebula. They carry information about the processes that shaped the early Solar System as a function of heliocentric distance. Furthermore, NEOs may have been instrumental in delivering water and organic-rich material to Earth, potentially contributing to the emergence of life [1].

These objects can even pose a threat to our civilization. Terrestrial impact craters attest to the catastrophic effects of past asteroid collisions with our planet (e.g. the K-Pg event which occurred approximately 65 million years ago, attributed to the impact of an asteroid of about 10 km in size). Such events can produce changes in biodiversity, such as species extinction (or mass extinction) and drastic climate changes.  More recently, the Chelyabinsk meteor event in February 2013 highlighted that even relatively small objects (less than 100m) can cause significant harm to human safety and infrastructure [2]. The blast created by this 20-m meteor's air burst produced extensive ground damage, and almost 1500 people sought medical attention because of the event. The overall majority of the injuries were caused by the secondary blast effects of glass which shattered and fell inward.

Accurate knowledge of a target's physical properties is essential for effective mitigation measures in any potential impact scenario, as this information is crucial for planning and successfully implementing appropriate response strategies. In this context, the NEO Physical Observations and Properties Simulation (NEOPOPS) was established, building on the success of previous international research programs dedicated to the study of NEOs (NEOShield,  NEOShield-2, and NEOROCKS). NEOPOPS is an European project funded by the EU Horizon Europe Programme and implemented by ESA for the period 2025-2028. Its objectives are multiple:

• to efficiently organize follow-up astronomical observations of NEOs, to obtain high-quality data for deriving their physical properties, with priority given to the timely characterization of potentially hazardous objects;
• to significantly improve statistical analyses, modeling, and numerical simulations aimed at understanding the physical nature of NEOs, with a particular focus on small-sized objects, which are of paramount importance for designing effective mitigation measures both in space and on the ground;
• to foster European and international cooperation in NEO physical characterization, providing scenarios and roadmaps with the scale up the experience gained during the project to a global level;
• to collaborate with ESA to significantly improve public understanding and perception of the asteroid hazards, counteracting the spread of misinformation and unwarranted alarm.

 

Our team consists of six partners from four countries (Italy, France, the Czech Republic, and UK) employing diverse and complementary observational techniques to consolidate and further enhance physical characterization of NEOs. The team also contributes to rapid-response exercises aimed at characterizing newly discovered objects, thereby addressing the challenge posed by imminent impactors. In particular, we participated in recent observational campaigns to characterize 2024 YR4 [3] and 2025 FA22 [4].

The INAF-OAR is responsible for several working packages, including overall project coordination (WP1), spectroscopic observations (WP4) and rapid-response activities (WP6). In this presentation, we will describe the structure of NEOPOPS as well as its spectroscopic component. We will also present some recent results and statistics obtained during the first year of the project.

 

Acknowledgments: The NEOPOPS observations were funded by a program of the European Union and implemented by ESA (agreement No.4000147191/25/D/MRP)

 

References

• Bottke W.F., Cellino A., Paolicchi P., et al., 2002, Asteroid III, University of Arizona Press, p. 3-15, 2002.
• Perna D., Barucci M.A., Drube L., et al., 2015, P&SS, 118, P. 311-317
• Devogèle, M., Hainaut, O. R., Micheli, M. et al., 2026, JAnSc, 73, 31.
• Ieva, S., Bourdelle de Micas, J., Farina, A. et al., in preparation