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Radial velocity measurements of stellar reflex motion have revealed manyextrasolar planets, but gaps in the observations produce aliases, spuriousfrequencies that are frequently confused with the planets' orbital frequencies.In the case of Gl 581 d, the distinction between an alias and the truefrequency was the distinction between a frozen, dead planet and a planetpossibly hospitable to life (Udry et al. 2007; Mayor et al. 2009). To improvethe characterization of planetary systems, we describe how aliases originateand present a new approach for distinguishing between orbital frequencies andtheir aliases. Our approach harnesses features in the spectral window functionto compare the amplitude and phase of predicted aliases with peaks present inthe data. We apply it to confirm prior alias distinctions for the planets GJ876 d and HD 75898 b. We find that the true periods of Gl 581 d and HD 73526b/c remain ambiguous. We revise the periods of HD 156668 b and 55 Cnc e, whichwere afflicted by daily aliases. For HD 156668 b, the correct period is 1.2699days and minimum mass is (3.1 +/- 0.4) Earth masses. For 55 Cnc e, the correctperiod is 0.7365 days -- the shortest of any known planet -- and minimum massis (8.3 +/- 0.3) Earth masses. This revision produces a significantly improved5-planet Keplerian fit for 55 Cnc, and a self-consistent dynamical fitdescribes the data just as well. As radial velocity techniques push toever-smaller planets, often found in systems of multiple planets,distinguishing true periods from aliases will become increasingly important.

Radial velocity planets de-aliased. A new, short period for Super-Earth 55 Cnc e