The Open Cluster Chemical Analysis and Mapping (OCCAM) survey aims to produce a comprehensive, uniform, infrared-based data set for hundreds of open clusters, and constrain key Galactic dynamical and chemical parameters from this sample. This first contribution from the OCCAM survey presents analysis of 141 members stars in 28 open clusters with

Aims: The association of Type Ic supernovae (SNe) with long-duration gamma-ray bursts (GRBs) is well established. We endeavor, through accurate ground-based observational campaigns, to characterize these SNe at increasingly high redshifts. Methods: We obtained a series of optical photometric and spectroscopic observations of the Type Ic SN 2012bz

The Kepler mission has made an important observation: the first detection of photons from a terrestrial planet by observing its phase curve (Kepler-10b). This opens a new field in exoplanet science: the possibility of obtaining information about the atmosphere and surface of rocky planets, objects of prime interest. In this Letter, we apply the

There is a long-lasting debate, started in the nineteenth century by d‟Arbois de Jubainville and Jullian, among others, regarding the pan-Celtic nature of the mid-season (or rather, start of season) feasts known from the Mediaeval Ireland (set on 1st November, February, May and August). D‟Arbois indicated that one of these feasts coincided with the

The Very Small Array (VSA) detected a cold spot in the Cosmic Microwave Background (CMB) towardsthe Corona Borealis supercluster of galaxies. The origin of this spot remains unclear as itis not obviously associated to any known cluster of galaxies. We present here recent observationalresults (GTC, WHT, SDSS) and theoretical (N-body simulations)

We present a complete study of the diffuse ionized gas (DIG) in a sample of six spiral galaxies (NGC 157, NGC 3359, NGC 3631, NGC 6764, NGC 6951, NGC 7479) using very high quality Hα images which allow analysis down to very low surface brightness (between 0.3 and 2 pc cm-6). Separation of the diffuse Hα emission from that of the H II regions was