Juq-154

To eliminate false positives (e.g., background eclipsing binaries), the Very Large Array performed high‑resolution imaging, while the Gaia astrometric catalog confirmed the star’s lack of close companions. The community’s consensus—reflected in a series of peer‑reviewed papers (e.g., Rivera et al., 2025; Huang & Patel, 2025)—affirmed JUQ‑154 as a bona fide exoplanet.

The RV solution indicates an eccentricity of e = 0.04 ± 0.01, implying only modest seasonal variations. Dynamical simulations (N‑body integrations spanning 10⁸ yr) show the orbit is dynamically stable, with no resonant perturbations from the distant companion star (a M‑type dwarf at 210 AU) or any detected interior planets. JUQ-154

Subsequent observations with the Space‑Based Photometric Explorer (SBPE) captured three consistent transit events, each with a depth of 84 ppm and a duration of 9.3 hours. The combined RV and transit data yielded a precise planetary radius of 1.02 R⊕ and a bulk density of 5.7 g cm⁻³, indicating a largely silicate‑iron composition akin to Earth’s. To eliminate false positives (e

Mid‑infrared observations with JWST’s MIRI captured a secondary eclipse depth of 35 ppm, translating to a dayside brightness temperature of 298 K. Phase‑curve data reveal a modest day–night temperature contrast (~10 K), implying efficient heat redistribution, likely mediated by a substantial atmosphere and possibly an oceanic heat sink. The RV solution indicates an eccentricity of e = 0