We have re-analyzed the Galactic O-star sample from citet{puls96} by means of line-blanketed NLTE model atmospheres in order to investigate the influence of line-blocking/blanketing on the derived parameters. The analysis has been carried out by fitting the photospheric and wind lines from H and He. In most cases we obtained a good fit, but we have

We present William Herschel Telescope (WHT) and Very Large Telescope (VLT) spectroscopy of MM Ser, the optical counterpart to Ser X-1. We deblend the red spectra of the two close stars identified by Wachter and show that the brighter of the two is responsible for the Hα and He I emission, hence confirming that this is the true counterpart of the X

We present a quantitative morphological analysis of 187 galaxies in a region covering the central 0.28 deg2 of the Coma Cluster. Structural parameters from the best-fitting Sérsic r1/n bulge plus, where appropriate, exponential disk model, are tabulated here. This sample is complete down to a magnitude of R=17 mag. By examining the recent

Echelle spectrophotometry of the planetary nebula NGC 5315 is presented. The data consist of VLT UVES observations in the 3100-10450 Å range. The intensities of 556 emission lines have been measured, including 508 identified permitted lines of H0, He0, C0, C+, N0, N+, N++, O0, O+, Ne0, Ne+, Mg+, Si+, S0, S+, S++, and Ar+. Electron temperatures and

Not Available

We present a summary of high-spatial resolution follow-up observations of the elliptical (E) and lenticular (S0) galaxies in the SAURON survey using the OASIS integral field spectrograph. The OASIS/observations explore the central 8″×10″ regions of these galaxies using a spatial sampling four times higher than SAURON, often revealing previously