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Stochastic influxes of IGW also lead to minimum core rotation rates, which may be realized given very efficient prior core spin-down via IGW/magnetic torques. Such a spin-down is not unreasonable, especially given that the cores of low mass red giant stars rotate slower than can be accounted for using hydrodynamic mechanisms or magnetic torques via the Tayler-Spruit dynamo \citep{cantiello:14}. It is thus quite plausible that massive star cores are efficiently spun down via waves/magnetic torques, after which they are stochasticly spun up via waves launched during O/Si burning. If this mechanism determines the core spin rate before death, it entails a Maxwellian distribution in spin frequency, with typical spin periods of $300 \, {\rm s} \lesssim P \lesssim 10^4 \, {\rm s}$. We thus find it extremely unlikely that magnetic torques can enforce very large pre-collapse spin periods as claimed by \cite{spruit:98}.   If AM is conserved during the supernova, stochastic IGW spin-up entails NS birth periods of $20 \, {\rm ms} \lesssim P \lesssim 400 \, {\rm ms}$, albeit with significant uncertainty. These estimates are comparable to spin periods of typical young, slowly rotating NSs (\citealt{lai:96,gotthelf:13}), and for the broad inferred birth spin period distribution of $P \lesssim 500 \, {\rm ms}$ for ordinary pulsars (\citealt{faucher:06,popov:10,gullon:14}). Therefore, stochastic wave spin-up could be the dominant mechanism in determining the rotation periods of pre-collapse SN cores and newborn NSs. In this scenario, there is little or no correlation between the spin of the progenitor and the spin of the NS it spawns. We note that this scenario is very similar to the stochastic spin-up scenario proposed by \cite{spruit:98}, except that the AM depostion occurs before core-collapse, and the source of the AM (convectively excited IGW) is somewhat better understood. We also express a word of caution, as Si burning isa  notoriously difficult for stellar evolution codes to handle, and the properties of Si burning produced by our MESA evolutions cannot be completely trusted. % We note that the AM deposited by IGW also entails a characteristic momentum deposition of $P_{\rm ex} \sim I_c \Omega_{\rm ex}/r_c$, which corresponds to a core velocity of $v_{\rm ex} \sim P_{\rm ex}/M_c$. Our calculations entail typical ``kick" velocities of $ 10^2 \, {\rm km} \, {\rm s}^{-1} \lesssim v_{\rm ex} \lesssim 7 \times 10^2 \, {\rm km} {\rm s}^{-1} $, very similar to typical NS kick velocities ***REF***. It may therefore be possible that stochastic momentum/AM deposition accounting for NS kicks/spins occurs in a similar fashion outlined in \cite{spruit:98}, but with the momentum deposition occuring {\it before} core collapse via IGW excited by vigorous shell burning.