Stellar population parameters using MaNGA and MUSE

The stellar initial mass function (IMF) has implications for a wide range of problems in astrophysics and is one of the largest uncertainties when analysing the integrated light of galaxies. The MaNGA IFU survey provides the opportunity to make precise spatially resolved measurements of stellar population properties in galaxies, owing to its unique combination of spatial resolution, wavelength coverage, and sample size. We measure radial gradients in age, metallicity, abundances of various individual elements, and the low-mass IMF slope from stacked spectra. We derive these parameters by fitting stellar population models to a combination of optical and near-infrared absorption features. We compare local and global trends for early- and late-type galaxies, with an attempt to understand the processes that drive the evolution of these objects. Through MUSE we focus on a galaxy-by-galaxy approach to study detailed spatial variations and also obtain results from full spectrum fitting.