We present broadband photometry and provide a quantitative analysis of the structure of galaxies in the inner region of the Abell Cluster 2443 (z~0.1). The galaxy parameters have been derived by fitting a two-component model (Sérsic r1/n bulge and exponential disk) to a magnitude-limited sample. Using a new method of analysis that takes into

We present the photometric history of some luminous blue variable candidate stars of M 33. The search was made with the plates collection of the Bulgarian National Astronomical Observatory. We found that 1, of 6 objects studied, showe d photometric variations consistent with the LBV phase. These new data, together with the LBV type spectrum of the

Oxygen abundances have been derived in a sample of very metal-poor stars from observations of the Oi triplet at /λλ 7771-5 Å and OH lines in the near UV. Iron abundances derived in LTE were corrected for NLTE effects following Thévenin and Idiart [ApJ 521 (1999) 753]. Furthermore, a detailed NLTE analysis of iron lines has been carried out for one

OSIRIS (Optical System for Imaging and low/intermediate-Resolution Integrated Spectroscopy) will be one of the Day One instruments for the Spanish 10.4m telescope GTC at La Palma. One of the scientific projects to be addressed with OSIRIS is the study of the galaxy population in clusters of galaxies at high redshift. Part of the cluster sample

We report complete near-infrared (0.9-2.4 mu m) spectral observations of trans-neptunian objects (TNOs) 2000 EB173 and 2000 WR106 collected using the new Near Infrared Camera Spectrometer (NICS) attached to the 3.56 m Telescopio Nazionale Galileo (TNG). Both spectra are very red and with a quite strong and broad drop extending throughout the K band

We present high resolution (15'' and 2.5 km/s) HI observations of the S0 gal axy NGC 404. We derive an HI mass of MHI = 6.7 × 107 Msolar, in good agreement with previous measurements. The HI is distributed in a broad annulus and extends out to a diameter of 9', well beyond the optical diameter of 6'. The velocity field is regular and shows