Context: Shells in Elliptical Galaxies are faint, sharp-edged features, believed to provide evidence for a merger event. Accurate photometry at high spatial resolution is needed to learn on presence of inner shells, population properties of shells, and dust in shell galaxies. Aims: Learn more about the origin of shells and dust in early type

We present here the outline of the process that any potential GTC observer will need to follow in order to perform their observations. Depending on which of the members of the GTC community the observer belongs to, the details of the different steps and timeline of the process will differ slightly, but in general it will be as follows: first the

Gravity is the key engine for the evolution of the universe and the formation of its main structures: galaxies, clusters of galaxies and filaments. Gravity is also an invaluable tool for exploring the universe through the relativistic effect of gravitational lensing. The gravitational potentials of clusters of galaxies turn these bodies into

In this work we present merger fractions from galaxy samples selected by either Ks-luminosity, or B-band luminosity, from the GOYA photometric survey of the Groth strip using asymmetry indices to identify merging galaxies. The merger fraction in B-band can be approximated by the function F_{mg}(z) = 0.006(1 + z)^{3.2}. The merger fraction in Ks

Using the UBVIJK photometry from the GOYA Survey of the Groth strip, we have built a catalog with photometric redshifts for 2000 sources (0 z 5). For z 1.5, excellent agreement is found with spectroscopic redshifts ( dz/(1+z) >= 0.07). Such catalog will provide a robust determination of the evolution of the K-band luminosity function, as well as

We present the results obtained from our deep survey of lensing clusters aimed at constraining the abundance of star-forming galaxies at z ˜ 6-11. Lensing magnification improves the search efficiency and subsequent spectroscopic studies with the new generation of NIR multi-object spectrographs (e.g. EMIR/GTC). The UV Luminosity Function derived