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The hundreds of multiple planetary systems discovered by the \textit{Kepler}mission are typically observed to reside in close-in ($\lesssim0.5$ AU),low-eccentricity, and low-inclination orbits. We run N-body experiments tostudy the effect that unstable outer ($\gtrsim1$ AU) giant planets, whose endorbital configurations resemble those in the Radial Velocity population, haveon these close-in multiple super-Earth systems. Our experiments show that thegiant planets greatly reduce the multiplicity of the inner super-Earths and thesurviving population can have large eccentricities ($e\gtrsim0.3$) andinclinations ($i\gtrsim20^\circ$) at levels that anti-correlate withmultiplicity. Consequently, this model predicts the existence of a populationof dynamically hot single-transiting planets with typical eccentricities andinclinations %in the ranges of $\sim 0.1-0.5$ and $\sim 10^\circ-40^\circ$. Weshow that these results can explain the following observations: (i) the recenteccentricity measurements of \textit{Kepler} super-Earths from transitdurations; (ii) the tentative observation that single-transiting systems have awider distribution of stellar obliquity angles compared to themultiple-transiting systems; (iii) the architecture of some eccentricsuper-Earths discovered by Radial Velocity surveys such as HD\,125612c. Futureobservations from \textit{TESS} will reveal many more dynamically hot singletransiting planets, for which follow up Radial Velocity studies will be able totest our models and see whether they have outer giant planets.

Dynamically hot Super-Earths from outer giant planet scattering