The OTELO project is the extragalactic survey currently under way using the tunable filters of the OSIRIS instrument at the GTC. OTELO is already providing the deepest emission line object survey of the universe up to a redshift 7. In this contribution, the status of the survey and the first results obtained will be presented.

Aims: We systematically study the relations between the Hα luminosity and the near-IR luminosity and temperature of a set of selected HII regions in the disc of M100. Methods: By using the technique of cross-reference between the optical Hα image (the catalogue of HII regions in M100) and the Spitzer IRAC images, we locate the selected HII regions

We summarize recent theoretical results dealing with the formation of massive stellar systems. The key premise is the high stellar density which leads to a very efficient star forming process in the so called positive feedback mode. Multiple implications arise from such models, e.g., much less mechanical energy exits the starburst process and much

In this work we study the physical properties of star-forming galaxies selected in an Hα near-infrared narrow-band survey tuned for redshift z=0.84 (Villar et al. 2008, 2011). Also, we present a sample at z˜1 with mass greater than 10^{10} M_{&sun;} with Hα emission. The observations were carried out with WHT/LIRIS (see Sánchez de Miguel et al

PHI, Polarimetric and Helioseismic Imager, is an instrument for solar observations that will go on board the Solar Orbiter mission (ESA/NASA), to be launched on 2017. This mission will orbit the Sun getting as close as 0.28 AU. It is also an out of the ecliptic mission which will provide a better, more direct observation of high solar latitudes. SO

Spectroscopic and spectropolarimetric observations with high spectral resolution provide extremely rich information on the physical conditions of distant celestial objects; sometimes, even the mere presence of a spectroscopic or polarimetric pattern may offer fundamental insights. But these are photon-starving techniques. Signals are often at the