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Mid-late M stars are opportunistic targets for the study of low-massexoplanets in transit because of the high planet-to-star radius ratios of theirplanets. Recent studies of such stars have shown that, like their early-Mcounterparts, they often host multi-resonant networks of small planets. Here,we reanalyze radial velocity measurements of YZ Ceti, an active M4 dwarf forwhich the HARPS exoplanet survey recently discovered three exoplanets onshort-period (P = 4.66, 3.06, 1.97 days) orbits. Our analysis finds that theorbital periods of the inner two planets cannot be uniquely determined usingthe published HARPS velocities. In particular, it appears likely that the3.06-day period of YZ Ceti c is an alias, and that its true period is 0.75days. If so, the revised minimum mass of this planet is less than 0.6 Earthmasses, and its geometric transit probability increases to 10%. We encourageadditional observations to determine the true periods of YZ Ceti b and c, andsuggest a search for transits at the 0.75-day period in TESS lightcurves.

Aliasing in the Radial Velocities of YZ Ceti: An Ultra-Short Period for YZ Ceti c?