In this contribution we review some of the most relevant results of the PhD thesis awarded with the XIV SEA PhD prize in 2018. The thesis is aimed at characterising the ionised gas abundance distribution in spiral galaxies by using two sets of high-quality integral field spectroscopic data from the CALIFA and AMUSING surveys. We observe that

We present results of an ongoing project dedicated to reassess the shape of the radial abundance gradient of O in the Milky Way based on deep spectroscopy of H II regions. Most of he data have been obtained with spectrographs attached to 8-10 m telescopes. The actual sample comprises 35 objects located at Galactocentric distances, R_{G}, from 5.1

We present the first detailed kinematic analysis of the proper motions (PMs) of stars in the Magellanic Bridge, from both the Gaia Data Release 2 catalog and from Hubble Space Telescope (HST) Advanced Camera for Surveys data. For the Gaia data, we identify and select two populations of stars in the Bridge region, young main-sequence (MS) and red

We studied the Class I protostar 2MASS 22352345 + 7517076 whose dramatic brightening between the IRAS, Akari, and WISE surveys was reported by Onozato et al. 2MASS 22352345+7517076 is a member of a small group of low-mass young stellar objects, associated with IRAS 22343 + 7501 in the molecular cloud Lynds 1251. The IRAS, ISO, Spitzer, Akari

OTELO (OSIRIS Tunable filter Emission Line Objects) is an emission-line object survey covering a spectral range between 9070 and 9280Å in a window of reduced airglow emission. The first pointing of OTELO, in the Extented Groth Strip, consists of 36 tomographic slices sampled at 6Å, obtained with the red tunable filter of OSIRIS at the Gran

The evolution of galaxies across the cosmic time are observationally studied by means of extragalactic surveys that cover significant volumes of Universe, with a wealth of multi-wavelength ancillary data. OTELO survey provides the deepest narrow band survey to date, in terms of minimum detectable flux, and emission line equivalent width, that has