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We perform in-depth dynamical modelling of the luminous and dark matter (DM)content of the elliptical galaxy NGC 1407. Our strategy consists of solving thespherical Jeans equations for three independent dynamical tracers: stars, blueGCs and red GCs in a self-consistent manner. We adopt a maximum-likelihoodMarkov-Chain Monte Carlo fitting technique in the attempt to constrain theinner slope of the DM density profile (the cusp/core problem), and the stellarinitial mass function (IMF) of the galaxy. We find the inner logarithmic slopeof the DM density profiles to be $\gamma = 0.6\pm0.4$, which is consistent witheither a DM cusp ($\gamma = 1$) or with a DM core $(\gamma = 0)$. Our findingsare consistent with a Salpeter IMF, and marginally consistent with a KroupaIMF. We infer tangential orbits for the blue GCs, and radial anisotropy for redGCs and stars. The modelling results are consistent with the virialmass--concentration relation predicted by $\Lambda$CDM simulations. The virialmass of NGC 1407 is $\log$ $M_{\rm vir} = 13.3 \pm 0.2 M_{\odot}$, whereas thestellar mass is $\log M_* = 11.8 \pm 0.1 M_{\odot}$. The overall uncertaintieson the mass of NGC 1407 are only 5 per cent at the projected stellar effectiveradius. We attribute the disagreement between our results and previous X-rayresults to the gas not being in hydrostatic equilibrium in the central regionsof the galaxy. The halo of NGC 1407 is found be DM dominated, with a dynamicalmass-to-light ratio of $M/L=260_{-100} ^{+174} M_{\odot}/L_{\odot, B}$.However, this value can be larger up to a factor of 3 depending on the assumedprior on the DM scale radius.

The SLUGGS Survey: Multi-population dynamical modelling of the elliptical galaxy NGC 1407 from stars and globular clusters