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We follow the microlensing approach and quantify the occurrence of Keplerexoplanets as a function of planet-to-star mass ratio, q, rather than planetradius or mass. For planets with radii ~1-6 R_earth and periods <100 days, wefind that, except for a normalization factor, the occurrence rate vs q can bedescribed by the same broken power law with a break at ~3 x10^{-5} independentof host type for hosts below 1 M_sun. These findings indicate that theplanet-to-star mass ratio is a more fundamental quantity in planet formationthan planet mass. We then compare our results to those from microlensing forwhich the overwhelming majority satisfies the M_host<1 M_sun criterion. Thebreak in q for the microlensing planet population, which mostly probes theregion outside the snowline, is 3-10 times higher than that inferred fromKepler. Thus, the most common planet inside the snowline is ~3-10 times lessmassive than the one outside. With rocky planets interior to gaseous planets,the Solar System broadly follows the combined mass-ratio function inferred fromKepler and microlensing. However, the exoplanet population has a less extremeradial distribution of planetary masses than the Solar System. Establishingwhether the mass-ratio function beyond the snowline is also host typeindependent will be crucial to build a comprehensive theory of planetformation.

A Universal Break in the Planet-to-Star Mass-Ratio Function of Kepler MKG stars