Abstract This article reviews the short-, medium-, and long-term prospects for characterizing rocky exoplanets, a central goal of contemporary astrophysics. The primary objectives are to determine whether these planets host atmospheres; if so, to constrain their molecular composition and search for potential biosignatures; if not, to infer their surface composition and thereby enabling a form of exo-geology. In the near term, the James Webb Space Telescope ( JWST ) will continue to lead this effort through photometric and spectroscopic observations of transits, eclipses, and phase curves, primarily targeting rocky exoplanets orbiting M dwarfs, including a limited number within their habitable zones. By the early 2030s, Giant Segmented-Mirror Telescopes (GSMTs) will provide the combination of high angular resolution, high contrast, and high spectral resolution needed to characterize rocky exoplanets around nearby M dwarfs via direct imaging, significantly broadening the accessible target sample and enabling detailed atmospheric and surface studies. Extending these investigations to rocky exoplanets orbiting solar-type stars, particularly those within habitable zones, will require the launch of next-generation space observatories in the 2040s, such as the Habitable Worlds Observatory ( HWO ), optimized for ultraviolet-to-near-infrared observations, and the Large Interferometer For Exoplanets ( LIFE ), designed for mid-infrared interferometry. In parallel, characterizing the broader planetary environment — including host stars and additional companions — will provide essential context. Missions such as Gaia (astrometric detection of companions), PLATO , Earth 2.0 (stellar characterization via asteroseismology), and Ariel (population-level atmospheric studies) will offer critical complementary insights into the architectures and habitability of nearby planetary systems.
Lagage et al. (Tue,) studied this question.