We present the spectral extension of our stellar population synthesis models based on the MILES and CaT empirical stellar spectral libraries. For this purpose we combine these two libraries with the Indo-US to construct composite stellar spectra to feed our models. The spectral energy distributions (SEDs) computed with these models and the

The origin of the gas in between the Magellanic Clouds (MCs)—known as the "Magellanic Bridge" (MB)—is puzzling. Numerical simulations suggest that the MB formed from tidally stripped gas and stars in a recent interaction between the MCs. However, the apparent lack of stripped intermediate- or old-age stars associated with the MB is at odds with

Studying the properties of the few compact massive galaxies that exist in the local Universe might provide a closer look to the nature of their high redshift (z ≥ 1.0) massive counterparts. By this means we have characterized their kinematics, structural properties, stellar populations and star formation histories with a set of new high quality

Recent results on the non-universality of the Initial Mass Function (IMF) have shown strong evidence of IMF variations with galaxy velocity dispersion, with a corresponding impact on other stellar population parameters, line indices and colours. Using a set of stellar population models with varying IMF slopes, we provide additional caveats on the

Using Herschel data from the deepest SPIRE and PACS surveys (HerMES and PEP) in COSMOS, GOODS-S and GOODS-N, we examine the dust properties of infrared (IR)-luminous (LIR > 1010 L&sun;) galaxies at 0.1 z 2 and determine how these evolve with cosmic time. The unique angle of this work is the rigorous analysis of survey selection effects, making

Using a large compilation of massive (stellar mass M≥10^{11} M_&sun;) earlytype galaxies (ETGs), we have probed, up to z˜1, whether the presence of satellites within a projected distance of 100 kpc of these objects depends on the size of the host massive galaxies. We do not find any evidence for satellites with a mass ratio down to 1:10 neither