The spiral galaxy NGC 3359 has been observed in the Hα line with the TAURUS II Fabry-Perot interferometer at the William Herschel Telescope within the BARS programme on the Canary Island telescopes in order to study the kinematics of the ionized gas. We have produced maps of velocity and velocity dispersion, and computed the rotation curve out to ~

The far-UV spectrum of the T Tauri stars (TTSs) provides important clues about the structure of the stellar atmospheres, winds and accretion shocks. The IUE (International Ultraviolet Explorer) Final Archive contains the most complete data base for such studies. A new extraction system, the IUE Newly Extracted Spectra (ines), has been developed to

The planetary nebula M2-9 has drastically changed its shape since its discovery by Minkwoski. Although the outline of the nebula seems to be stationary, most of the knots and bright features (N1, N2, S1, and S2) have moved laterally from the west to the east edges of both lobes. These features and their changes have reflection, not point, symmetry

We present an analysis of radii of giant stars with 6200 K>= T_eff >= 3800 K based on angular diameters obtained by means of the IRFM and distances computed from Hipparcos parallaxes. In order to asses the reliability of IRFM diameters we have considered a selected sample of stars whose diameters have been directly measured by interferometric

We present new long-slit William Herschel Telescope spectroscopic observations of the lens galaxy G1 associated with the double-imaged QSO 0957+561A,B. The central stellar velocity dispersion obtained, σl=310+/-20 km s-1, is in reasonable agreement with other measurements of this dynamical parameter. Using all updated measurements of the stellar

We present the first spectropolarimetric observations of the symbiotic nova HM Sge. We first note that marked spectral changes occurred: in the near IR the spectrum of the Mira in the system has clearly appeared. The nebular emission line spectrum remains largely unchanged but we detect for the first time the Raman line at lambda 6825. These