T-PHOT extracts accurate photometry from low-resolution images of extragalactic fields, where the blending of sources can be a serious problem for accurate and unbiased measurement of fluxes and colors. It gathers data from a high-resolution image of a region of the sky and uses the source positions and morphologies to obtain priors for the photometric analysis of the lower resolution image of the same field. T-PHOT handles different types of datasets as input priors, including a list of objects that will be used to obtain cutouts from the real high-resolution image, a set of analytical models (as .fits stamps), and a list of unresolved, point-like sources, useful for example for far-infrared wavelength domains. T-PHOT yields accurate estimations of fluxes within the intrinsic uncertainties of the method when systematic errors are taken into account (which can be done using a flagging code given in the output), and handles multiwavelength optical to far-infrared image photometry. T-PHOT was developed as part of the ASTRODEEP project (www.astrodeep.eu).

FiCUS (FItting the stellar Continuum of Uv Spectra) fit the stellar continuum of extragalactic ultraviolet (UV) spectra. The code takes observed-frame wavelength, flux density (with errors) and user-defined mask arrays as inputs, and returns an estimation of the galaxy stellar age, metallicity and dust extinction, as well as other secondary Spectral Energy Distribution (SED) parameters. FiCUS has two scripts; the first reads the INPUT file provided by the user and performs the fit according to selected options. It then gives the best-fit parameters and creates the OUTPUT files and figures. The second script includes pre-defined routines for spectral analysis, loading INPUT files and handling with data and models, as well as functions for the fitting routine, SED-parameters calculations and plotting, and imports functions into the first script.