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\section{Introduction}  \label{intro}   Rotation is a key player in the drama that unfolds upon the death of a massive star. The angular momentum (AM) contained in the iron core and overlying layers determines the rotation rate at core collapse (CC), which could have a strong impact on the dynamics of CC and the subsequent supernova \cite[See e.g][]{MacFadyen_1999,Woosley_2002,Woosley_2006}. Rotation may help determine the nature of the compact remnant, which could range from a slowly rotating neutron star (NS) to a millisecond magnetar or rapidly rotating black hole \cite[See e.g.][]{Heger:00,Heger_2005}. e.g.][]{heger:00,Heger_2005}.  The former may evolve into an ordinary pulsar, while the latter two outcomes offer exciting prospects for the production of long gamma-ray bursts (GRB) and superluminous supernovae. In each of these phenomena, rotating central engines are suspected to be the primary source of power. Despite the important influence of rotation, little is known about the rotation rates of the inner cores of massive stars nearing CC. %Although rapid rotation leaves an imprint in the gravitational wave spectrum produced at core bounce (Ott et al. 2012, Abdikamalov et al. 2014, Klion et al. 2015, Fuller et al. 2015), a gravitational wave detection of a galactic supernovae is likely decades away.