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Multi-planet systems provide important laboratories for exploring dynamicalinteractions within the range of known exoplanetary system architectures. Onesuch system is GJ 357, consisting of a low-mass host star and three orbitingplanets, the outermost (planet d) of which does not transit but lies within theHabitable Zone (HZ) of the host star. The minimum mass of planet d causes itsnature to be unknown, both in terms of whether it is truly terrestrial and ifit is a candidate for harboring surface liquid water. Here, we use threesectors of photometry from the Transiting Exoplanet Survey Satellite (TESS) toshow that planets c and d do not transit the host star, and therefore may havemasses higher than the derived minimum masses. We present the results for asuite of dynamical simulations that inject an Earth-mass planet within the HZof the system for three different orbital and mass configurations of planet d.These results show that planet d, rather than being a potentially habitableplanet, is likely a source of significant orbital instability for otherpotential terrestrial planets within the HZ. We find that relatively smalleccentricities of planet d cause a majority of the HZ to be unstable for anEarth-mass planet. These results highlight the importance of dynamicalstability for systems that are prioritized in the context of planetaryhabitability.

GJ 357 d: Potentially Habitable World or Agent of Chaos?