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We present spatially resolved measurements of the stellar initial massfunction (IMF) in NGC 1399, the largest elliptical galaxy in the FornaxCluster. Using data from the Multi Unit Spectroscopic Explorer (MUSE) andupdated state-of-the-art stellar population synthesis models from Conroy et. al2018, we use full spectral fitting to measure the low-mass IMF, as well as anumber of individual elemental abundances, as a function of radius in thisobject. We find that the IMF in NGC 1399 is heavier than the Milky Way in itscentre and remains radially constant at a super-salpeter slope out to 0.7R$_{e}$. At radii larger than this, the IMF slope decreases to becomemarginally consistent with a Milky Way IMF just beyond R$_{e}$. The inferredcentral V-band M/L ratio is in excellent agreement with the previously reporteddynamical M/L measurement from Houghton et. al 2006. The measured radial formof the M/L ratio may be evidence for a two-phase formation in this object, withthe central regions forming differently to the outskirts. We also reportmeasurements of a spatially resolved filament of ionised gas extending 4arcseconds (404 pc at $D_{\mathrm{L}}=21.1$ Mpc) from the centre of NGC 1399,with very narrow equivalent width and low velocity dispersion ($65\pm14$ \kms).The location of the emission, combined with an analysis of the emission lineratios, leads us to conclude that NGC 1399's AGN is the source of ionisingradiation.

The stellar population and initial mass function of NGC 1399 with MUSE