in the central part of the galaxy due to dynamical friction.'
author:
- 'Anil C. Seth, Robert D. Blum, Nate Bastian , Nelson Caldwell, Victor P. Debattista, Thomas H. Puzia'
title: The Rotating Nuclear Star Cluster in NGC 4244
---

Introduction
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Prominent nuclear star clusters (NSCs) are found in $\sim$75% of late-type spiral galaxies [@boker02] and early-type galaxies [@cote06]. These NSCs are intrinsically very luminous, with typical $M_I \sim -12$, and sizes similar to globular clusters [$r_{eff} \sim 5$pc; @boker04a]. Recently, multiple studies [@ferrarese06; @wehner06; @rossa06] have shown that NSC masses are coupled to the mass of their host galaxy, following a similar $M$-$\sigma$ relation as massive black holes (MBHs) and extending this relation to lower mass galaxies. This result suggests that the formation of both types of objects are linked to the formation of their host galaxies. Some galaxies host both NSCs and MBHs, but the relationship between these two types of objects is unknown [@seth08]. Unlike black holes, the assembly history of NSCs can, in principle, be inferred from studies of their stellar populations and kinematics. Thus NSCs provide important tools for studying the history of galaxy centers and their connection to the galaxies as a whole.

