In the young universe, galaxies were blobby conglomerations of stars whose irregular structures were products of their dynamically violent environments.  Over time, star formation in these systems declined as the gas fraction dropped, and galaxies evolved into the spiral and elliptical structures with which we are familiar today.  I will review state-of-the-art developments in our understanding of the evolution of the modern-day Hubble sequence, many of which have been provided by integral-field unit (IFU) spectroscopy that probes the internal kinematics and chemistry of galaxies.

Additionally, I will discuss the promise of the upcoming MaNGA IFU galaxy survey to address the formation history of galactic subcomponents and the nature of present-day galaxy growth via merging and gas accretion.  Operating as a part of the 4th generation Sloan Digital Sky Survey (SDSS-IV), the MaNGA program will answer such questions by obtaining optical integral field spectroscopy for a statistically large sample of 10,000 nearby galaxies, delivering two-dimensional maps of stellar and gas velocities, gas-phase abundances, star formation rates, and many other quantities.  This legacy data set will additionally provide a robust local anchor for interpreting studies of galaxies in the distant universe enabled by next-generation facilities such as TMT and JWST.