Aims: As a new approach to the study of resolved stellar populations in nearby galaxies, our goal is to demonstrate with a pilot study in NGC 300 that integral field spectroscopy with high spatial resolution and excellent seeing conditions reaches an unprecedented depth in severely crowded fields. Methods: Observations by MUSE with seven pointings

We present simultaneous and continuous observations of Hα, Hβ, ion{Na}{1} D1, D2, ion{He}{1} D3 and ion{Ca}{2} H & K lines of the chromospherically active binary HR 1099. We have observed HR 1099 for more than 3 weeks almost continuously and monitored two flares. An increase in Hα and ion{Ca}{2} H & K, Hβ and ion{He}{1} D3 and a strong filling-in

The extension of the highly successful Doppler technique into the near-infrared (0.9-2.5 μm) is opening new parameter domains for extra-solar planet searches in terms of ages and masses of the primary stars. Here we present the current status of NAHUAL, a next generation near-infrared spectrograph for the 10.4-meter Gran Telescopio Canarias (GTC)

We explore the possibility that the steepening observed shortward of 1000 Å in the energy distribution of quasars may result from absorption by dust, being either intrinsic to the quasar environment or intergalactic. We find that a dust extinction curve consisting of nanodiamonds, composed of terrestrial cubic diamonds or with surface impurities as

We present a first study of truncation of the stellar disks of spiral galaxies in the near infrared. Observations of NGC 4013, NGC 4217, NGC 6504 and NGC 5981 were made with the CAIN NIR camera on the CST in Tenerife. This wavelength range provides the best description of the phenomenon, not only because extinction effects are minimized, but also

We report near-infrared K ', L', and M ' band imaging observations of the nearby merging galaxy NGC 6240 with the Infrared Camera and Spectrograph on the Subaru telescope. The observations were performed with the assistance of the Subaru Adaptive Optics System, and the achieved spatial resolutions were around 0{^''.}10-0{^''.}20. We also obtained