The unified model of active galactic nuclei (AGN) claims that the properties of AGN depend on the viewing angle of the observer with respect to a toroidal distribution of dust surrounding the nucleus. Both the mid-infrared (MIR) attenuation and continuum luminosity are therefore expected to be related to dust associated with the torus. We have

Magneto-acoustic and Alfvénic waves are ubiquitous in solar coronal loops, possibly being excited by photospheric motions. It is not clear, though, how these waves get so high, having obstacles such as the acoustic cut-off frequency, reflection and refraction of fast MHD waves and also the strongly reflecting transition region. In this contribution

In these proceedings we summarize the characteristics and current status of MEGARA, the future optical IFU and MOS for the 10.4 m GTC. MEGARA is being built by a Consortium led by the UCM (Spain) that also includes the INAOE (Mexico), the IAA-CSIC (Spain) and the UPM (Spain). The MEGARA IFU offers two different bundles, one called LCB with a field

We present spectropolarimetric observations in the He I 1083.0 nm multiplet of a quiescent, hedgerow solar prominence. The data were taken with the Tenerife Infrared Polarimeter attached to the German Vacuum Tower Telescope at the Observatorio del Teide (Tenerife; Canary Islands; Spain). The observed He I circular and linear polarization signals

We report observations of the exoplanet host-star HD 80606 using the OSIRIS tunable filter imager. Very-high-precision, narrow-band photometry in four bandpasses around the K I absorption feature was acquired during the January 2010 transit of HD 80606b, with further off-transit observations taken January and April of 2010. We obtained differential

Massive (M_{stellar}≥10^{11} h_{70}^{-2} {M}_{&sun;}) galaxies are privileged probes to explore galaxy evolution, as their high luminosities allow us to track them over a large span of cosmic time. They suffer dramatic modifications in their sizes, star formation histories and number densities from high to low redshift. This must be also reflected