IMF-σ: core & power-law galaxies Our analysis reveals a separation in the IMF-σ relation for M87 and NGC7619 (squares), compared to NGC1332 and NGC0307 (circles). Larger symbol sizes indicate smaller radii. The former are pressure-supported core galaxies with luminosity profiles that turn over at a certain radius while the latter are rotation-supported power-law galaxies containing surface brightness profiles with a steep power-law. Power-law galaxies appear to have more bottom-heavy IMFs and higher M/L than core galaxies of the same σ (see also [6]). While σ drives the overall trend for galaxies, offsets are seen in the relation for different galaxies. We are adding more core and power-law galaxies to the sample and aim to explore any differences in radial gradients between them. Method We create high S/N Voronoi binned spectra [1], subtracting emission lines and deriving kinematics using PPXF [2]. We measure optical absorption features as well as perform full spectrum fitting with ALF [3], example fits shown below. We obtain consistent results from both for age, metallicity, Mg abundance using different stellar population models [3][4]. Introduction 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. Through MUSE we focus on a galaxy-by-galaxy approach to study detailed spatial variations in age, metallicity, individual element abundances, and the low-mass IMF slope by fitting the full spectrum with stellar population models. We perform the analysis for galaxies with different kinematics and explore trends with velocity dispersion. M87: elliptical, slow rotator Having masked the contaminated jet and central region, we find a constant age~13 Gyrs, [Mg/Fe]~0.4 dex, strong negative gradients in [Fe/H] and [Na/Fe], and mild negative gradients in the IMF slope and M/L. The IMF is slightly steeper than Salpeter in the centre and Salpeter at 0.5 Re. Comparing M/L from dynamical models for M87 reveals a value of ~6.5 in the centre, which is lower than the results from stellar population analyses (see also [5]). NGC1332: E/S0, fast rotator This galaxy, viewed edge-on, also has an old stellar population with a very shallow gradient out to 1 Re, and a negative metallicity gradient. [Mg/Fe] is lower at ~0.3 dex. A steep negative gradient is found in [Na/Fe] with maximum values of 0.6 dex and a slope of -0.3 dex/Re. The low-mass IMF has a slope of 3.4 in the centre, decreasing to 3 at 1 Re, corresponding to a very high central M/L ~10-15 in the V band. NGC1332 shows an interesting v-h3 correlation which suggests the presence of a bar, viewed end-on. The stellar population maps also show some asymmetry, supporting this. Spatially-Resolved Stellar IMF in a Sample of Kinematically Distinct MUSE Galaxies Taniya Parikh⭑, Roberto Saglia, Jens Thomas, Kianusch Mehrgan, Ralf Bender Max-Planck-Institut für extraterrestrische Physik, Garching, Germany ⭑tparikh@mpe.mpg.de 1 Cappellari & Copin 2003, MNRAS, 342, 345 2 Cappellari 2017, MNRAS, 466, 798 3 Conroy et al. 2018, ApJ, 854, 139 4 Thomas, Maraston & Johansson 2011, MNRAS, 412, 2183 5 Sarzi et al. 2018, MNRAS, 478, 4084 6 Bernardi et al. 2019, MNRAS, 489, 5633