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The best observational constraints stem from measurements of the rotation rates of the compact remnants following CC. For instance, a few low-mass black hole X-ray binary systems have been measured to have large spins that can only be accounted for by high spins at birth (***REF***). However, the rotation rates of young NSs show little evidence for rapid rotation ($P \lesssim 10 \, {\rm ms}$) at birth. The most rapidly rotating young pulsars include PSR J0537-6910 ($P=16\,{\rm ms}$) and the Crab pulsar ($P=33\,{\rm ms}$), whose birth periods have been estimated to be $P_i \lesssim 10\,{\rm ms}$ \citep{marshall:98} and $P_i \sim 19 \, {\rm ms}$ \citep{kaspi:02}, respectively. Many young NSs appear to rotate much more slowly, with typical periods of hundreds of ms \citealt{lai:96,gotthelf:13}. In general, pulsar observations seem to indicate a broad range of initial birth periods in the vicinity of tens to hundreds of milliseconds \citealt{faucher:06,popov:10,gullon:14}. Hence, rapidly rotating young NSs appear to be the exception rather than the rule.   Theoretical efforts have struggled to produce slow rotation rates. In the absence of strong AM transport mechanisms within the massive star progenitor, NSs would invariably be born rotating near break-up. \citet{Heger_2005} and \citet{Suijs_2008} examined the effect of magnetic torques generated via the Tayler-Spruit dynamo \citep[TS,][]{spruit:02}, and found typical NS spin periods at birth (assuming AM conservation during core-collapse and the ensuing supernova) of several milliseconds. \citet{wheeler:14} implemented magnetic torques due to MRI and the TS dynamo, and were able to reach iron core rotation rates of $P_{c} \sim 500 \, {\rm s}$, corresponding to NS spin periods of $P \sim 25 \, {\rm ms}$. These efforts are promising, however, the operation of both mechanisms within stars has been debated (***REFS***), \citep[e.g.]{Zahn_2007},  and theoretical uncertainties abound. Recent asteroseismic advances have allowed for the measurement of core rotation rates in low mass red giant stars (\citealt{beck:12,beck:14,mosser:12,deheuvels:12,deheuvels:14}). The measurements indicate that the cores of these stars rotate much slower than can be explained via hydrodynamic AM transport mechanisms or magnetic torques via the TS dynamo \citep{cantiello:14}. Although the cores rotate much faster than the surface (and one cannot assume nearly rigid rotation as suggested in \citealt{spruit:98}), the slow core rotation rate suggests that cores of massive stars may rotate slower than expected.