EMIR is the NIR imager and multiobject spectrograph being built as a common user instrument for the 10-m class GTC. Big cryogenic instruments demand a reliable design and a specific hardware and software to increase its safety and productivity. EMIR vacuum, cooling and heating systems are monitored and partially controlled by a Programmable Logic

AOLI, Adaptive Optics Lucky Imager, is the next generation of extremely high resolution instruments in the optical range, combining the two more promising techniques: Adaptive optics and lucky imaging. The possibility of reaching fainter objects at maximum resolution implies a better use of weak energy on each lucky image. AOLI aims to achieve this

A C60 fullerene/tetracene adduct was synthesized and studied by electronic absorption spectroscopy and FT-IR spectroscopy. Essentially the mono-adduct was obtained as suggested by the spectroscopic analysis and by the thermogravimetric analysis (TGA). The stability and the retro Diels-Alder reaction of the C60/tetracene adduct was studied by TGA

One of the most important features in active galactic nuclei (AGN) is the variability of their emission. Variability has been discovered at X-ray, UV, and radio frequencies on time scales from hours to years. Among the AGN family and according to theoretical studies, Low-Ionization Nuclear Emission Line Region (LINER) nuclei would be variable

Variability in active galactic nuclei (AGN) has been discovered at X-ray, UV, and radio frequencies on timescales from hours to years, being one of their most important features. Among the AGN family and according to theoretical studies, low-ionization nuclear emission line region (LINER) nuclei would be variable objects at long timescales because

We present the surface brightness profile fitting of a sample of double nucleus disk galaxies, minor merger candidates. We have decomposed these systems into two compact nuclear components and one or two extended galaxy disk components and estimated the luminosity of the primary and secondary nucleus and of the host galaxy and the separation