We have performed a new abundance analysis of Carina red giant (RG) stars from spectroscopic data collected with UVES (high spectral resolution) and FLAMES/GIRAFFE (high and medium resolution) at ESO/VLT. The former sample includes 44 RGs, while the latter consists of 65 (high-resolution) and ~800 (medium-resolution) RGs, covering a significant

Microvariability consists of small timescale variations of low amplitude in the photometric light curves of quasars and represents an important tool to investigate their inner core. Detection of quasar microvariations is challenging because of their non-periodicity, as well as the need for high monitoring frequency and a high signal-to-noise ratio

In this review I will tour through the most recent findings on the internal kinematic properties of Local Group dwarf galaxies, as determined from extensive spectroscopic surveys of their stellar component.I will also discuss the current status on determinations of the dark matter content and distribution in these objects, with particular focus on

We present a suite of cosmological radiation-hydrodynamical simulations of the assembly of galaxies driving the reionization of the intergalactic medium (IGM) at z ≳ 6. The simulations account for the hydrodynamical feedback from photoionization heating and the explosion of massive stars as supernovae (SNe). Our reference simulation, which was

Seven-stone antas are a group of megalithic monuments that were built in the southwest of the Iberian Peninsula for a period of some one thousand years in the 4th millennium B.C. They were constructed with a pattern of orientations that certainly situate them among the oldest monuments on Earth with undisputable astronomical orientations. They were

Borlaff et al. (2014) found that the characteristic photometric parameters of antitruncated discs in S0 galaxies follow tight scaling relations. Now, we have investigated if these scaling relations are satisfied by Type-III galaxies of other morphological types using published data in the R and Spitzer 3.6 microns bands. We have found that the