We use asteroid differential photometry gathered in the past decades together with the Gaia stellar catalogue (as photometric standards) to obtain relative magnitudes. The obtained magnitudes are then used to fit the multi-opposition phase curves in several ways depending on data quality.

En este trabajo los resultados obtenidos para un nuevo sensor, el TP3-WFS (por su siglas en inglés Two Pupil Plane Positions Wavefront Sensor). El TP3-WFS utiliza el mismo montaje físico que los sensores de curvatura y geométrico, y comparte con este último el objetivo de obtener las pendientes locales del frente de onda. No obstante, presenta dos

We present near-infrared integral field spectroscopy data obtained with Very Large Telescope/Spectrograph for INtegral Field Observations in the Near Infrared (SINFONI) of `the Teacup galaxy'. The nuclear K-band (1.95-2.45 μm) spectrum of this radio-quiet type-2 quasar reveals a blueshifted broad component of FWHM ˜ 1600-1800 km s-1 in the hydrogen

We present detailed studies of a z = 2.12 submillimeter galaxy, ALESS67.1, using sub-arcsecond resolution ALMA, adaptive optics-aided VLT/SINFONI, and Hubble Space Telescope (HST)/CANDELS data to investigate the kinematics and spatial distributions of dust emission (870 μm continuum), 12CO(J = 3–2), strong optical emission lines, and visible stars

We present new calculations of the Clumpy AGN Tori in a 3D geometry (CAT3D) clumpy torus models, which now include a more physical dust sublimation model as well as active galactic nucleus (AGN) anisotropic emission. These new models allow graphite grains to persist at temperatures higher than the silicate dust sublimation temperature. This

This thesis comprises of a full search in our galaxy for the hidden population of massive stars using the near-infrared photometry with a novel method and a quantitative spectroscopy study of an O star sample in the optical and near-infrared. Massive clusters are those with mass greater than 10^4 Solar Masses . The number of known massive clusters