Mid-infrared images of the Seyfert 1 galaxy Mrk 279 obtained with the ISO satellite are presented together with the results of a one-year monitoring campaign of the 2.5-11.7μm spectrum. Contemporaneous optical photometric and spectrophotometric observations are also presented. The galaxy appears as a point-like source at the resolution of the

Results from the third campaign of a ground-based multiband observation of the millimeter emission of the sky from Tenerife (Canary Islands) are presented. The instrument consists of a 0.45 m diameter off-axis telescope equipped with a four-band multimode 3He cooled photometer working at 1.1, 1.3, 2.1, and 3.1 mm wavelengths. The beam is well

HII region catalogue of the barred galaxy NGC 7479. The catalogue contains the position, mean radius and the calibrated H-alpha luminosity of each HII region. The HII region catalogue has been composed using a new semi-automated technique applied to a high quality continuum-subtracted H-alpha image of the galaxy obtained from observations through

We present high-resolution echelle spectroscopy of a sample of H II galaxies. In all galaxies we identify different Hα-emitting knots along the slit crossing the nucleus. All of these have been isolated and separately analyzed through luminosity and size versus σ diagnosis plots. We find that in all cases, for a particular galaxy, the bulk of the

Andredakis et al. (cite{r3}) fit Sersic's law mu (r) ~ r1/n to the bulges of the Balcells & Peletier (cite{r5}) galaxy sample, and infer that n drops with morphological type T from n ~ 4-6 for S0 to n=1 (exponential) for Sc's. We use collisionless N body simulations to test the assumption that initially the surface brightness profiles of all bulges

We report on the discovery of variable circular polarization in the SW Sextantis star LS Pegasi. The observed modulation has an amplitude of ~0.3% and a period of 29.6 minutes, which we assume as the spin period of the magnetic white dwarf. We also detected periodic flaring in the blue wing of Hβ, with a period of 33.5 minutes. The difference