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We present empirical evidence, supported by a planet formation model, to showthat the curve $R/R_\oplus = 1.05\,(F/F_\oplus)^{0.11}$ approximates thelocation of the so-called photo-evaporation valley. Planets below that curveare likely to have experienced complete photo-evaporation, and planets justabove it appear to have inflated radii; thus we identify a new population ofinflated super-Earths and mini-Neptunes. Our N-body simulations are set withinan evolving protoplanetary disk and include prescriptions for orbitalmigration, gas accretion, and atmospheric loss due to giant impacts. Oursimulated systems broadly match the sizes and periods of super-Earths in theKepler catalog. They also reproduce the relative sizes of adjacent planets inthe same system, with the exception of planet pairs that straddle thephoto-evaporation valley. This latter group is populated by planet pairs witheither very large or very small size ratios ($R_{\rm out} / R_{\rm in} \gg 1$or $R_{\rm out} / R_{\rm in} \ll 1$) and a dearth of size ratios near unity. Itappears that this feature could be reproduced if the planet outside thephoto-evaporation valley (typically the outer planet, but some times not) hasits atmosphere significantly expanded by stellar irradiation. This newpopulation of planets may be ideal targets for future transit spectroscopyobservations with the upcoming James Webb Space Telescope.

Identifying inflated super-Earths and photo-evaporated cores