FIT3D fits optical spectra to deblend the underlying stellar population and the ionized gas, and extract physical information from each component. FIT3D is focused on the analysis of Integral Field Spectroscopy data, but is not restricted to it, and is the basis of Pipe3D, a pipeline used in the analysis of datasets like CALIFA, MaNGA, and SAMI. It can run iteratively or in an automatic way to derive the parameters of a large set of spectra.

XookSuut models circular and noncircular flows on resolved velocity maps. The code performs nonparametric fits to derive kinematic models without assuming analytical functions on the different velocity components of the models. It recovers the circular and radial motions in galaxies in dynamical equilibrium and can derive the noncircular motions induced by oval distortions, such as that produced by stellar bars. XookSuut explores the full space of parameters on a N-dimensional space to derive their mean values; this combined method efficiently recovers the constant parameters and the different kinematic components.