In this thesis, an extensive exploration of the low surface brightness Universe has been undertaken. A special emphasis has been placed on reducing the limitations arising from the use of integrated photometry, such as the residuals due to the observation and reduction of astronomical data, the effects of the point spread function and the presence

Context. Because of the complex physics that governs the formation of chromospheric lines, interpretation of solar chromospheric observations is difficult. The origin and characteristics of many chromospheric features are, because of this, unresolved. Aims: We focus on studying two prominent features: long fibrils and flare ribbons. To model these

We study the rest-frame optical mass-size relation of bulges and discs from z ̃ 2 to z ̃ 0 for a complete sample of massive galaxies in the CANDELS fields using two-component Sérsic models. Discs and star-forming galaxies follow similar mass-size relations. The mass-size relation of bulges is less steep than the one of quiescent galaxies (best

The traditional measurement of the size of galaxies, the effective radius, is a relic of the epoch when shallow imaging was unable to capture the full extension of astronomical sources. However, current deep imaging surveys have revolutionised our view of these objects, allowing us to regard critically our own conventions. In this sense, it is time

Context. Spiral galaxies are very common in the local Universe, but their formation, evolution, and interplay with bars remain poorly understood after more than a century of astronomical research on the topic. Aims: We use a sample of 391 nearby galaxies from the S 4G survey to characterise the winding angle and amplitude of spiral arms as a

Aims: We take advantage of the capabilities of the OSIRIS Tunable Emission Line Object (OTELO) survey to select and study the AGN population in the field. In particular, we aim to perform an analysis of the properties of these objects, including their demography, morphology, and IR luminosity. Focusing on the population of Hα emitters at z ̃ 0.4