We analyse the stellar content of almost 300deg^2 of the sky close to the Galactic plane by directly comparing the predictions of the SKY model (Cohen and Wainscoat et al.) with star counts taken from the Two Micron Galactic plane Survey (TMGS: Garzón et al.). Through these comparisons we can examine discrepancies between counts and model and

We present heliocentric radial velocities for a large number of emission lines covering all the optical spectral range for two slit positions of the Galactic H Ii regions M 42 and M 17 and one slit position of M 8. We obtain a fairly similar relation between the heliocentric velocity and the ionization potential of the ions in all the observed slit

We present a comparison of the velocity power spectra between the GOLF and MDI instruments. In addition, this poster outlines work towards creating a GOLF-simulated signal utilizing MDI velocity images. The simulation of the GOLF signal is achieved by integrating spatially weighted masks with MDI LOI-proxy velocity images. The GOLF-simulated signal

We present the photometric history of some Luminous Blue Variable candidate stars in M 33. The search for outbursts was made in photographic plates taken in the B band of the galaxy M 33 and cover an eight year period, 1982-1990. Twenty five plates, separated into seven groups, have been used. CCD UBV magnitudes of the star UIT003 are presented

We report on near-infrared and optical observations of the GRB 970616 error box and of the X-ray sources discovered by ASCA and ROSAT in the region. No optical transient was found either within the IPN band or in the X-ray error boxes, similarly to other bursts, and we suggest that either considerable intrinsic absorption was present (like GRB

We present narrowband imagery and long-slit intermediate-resolution spectroscopy of the multiple-shell planetary nebulae NGC 2438 and NGC 5882. A comparative study of the chemical abundances of the main nebulae and their surrounding halos shows a moderate N/O enrichment of the central regions. The oxygen abundances appear constant throughout the