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We present the characterization of the Kepler-93 exoplanetary system, basedon three years of photometry gathered by the Kepler spacecraft. The durationand cadence of the Kepler observations, in tandem with the brightness of thestar, enable unusually precise constraints on both the planet and its host. Weconduct an asteroseismic analysis of the Kepler photometry and conclude thatthe star has an average density of 1.652+/-0.006 g/cm^3. Its mass of0.911+/-0.033 M_Sun renders it one of the lowest-mass subjects of asteroseismicstudy. An analysis of the transit signature produced by the planet Kepler-93b,which appears with a period of 4.72673978+/-9.7x10^-7 days, returns aconsistent but less precise measurement of the stellar density, 1.72+0.02-0.28g/cm^3. The agreement of these two values lends credence to the planetaryinterpretation of the transit signal. The achromatic transit depth, as comparedbetween Kepler and the Spitzer Space Telescope, supports the same conclusion.We observed seven transits of Kepler-93b with Spitzer, three of which weconducted in a new observing mode. The pointing strategy we employed to gatherthis subset of observations halved our uncertainty on the transit radius ratioR_p/R_star. We find, after folding together the stellar radius measurement of0.919+/-0.011 R_Sun with the transit depth, a best-fit value for the planetaryradius of 1.481+/-0.019 R_Earth. The uncertainty of 120 km on our measurementof the planet's size currently renders it one of the most precisely measuredplanetary radii outside of the Solar System. Together with the radius, theplanetary mass of 3.8+/-1.5 M_Earth corresponds to a rocky density of 6.3+/-2.6g/cm^3. After applying a prior on the plausible maximum densities ofsimilarly-sized worlds between 1--1.5 R_Earth, we find that Kepler-93bpossesses an average density within this group.

Kepler-93b: A Terrestrial World Measured to within 120 km, and a Test Case for a New Spitzer Observing Mode