========================================================================== J/A+A/485/41 NGC 55 blue massive stars VLT-spectroscopy (Castro+, 2008) The following files can be converted to FITS (extension .fit .fgz or .fiZ) tablea[123].dat ========================================================================== Query from: http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/A+A/485/41 ==========================================================================
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Beginning of ReadMe : J/A+A/485/41 VLT spectroscopy of blue massive stars in NGC55 (Castro+, 2008) ================================================================================ The Araucaria Project: VLT-spectroscopy of blue massive stars in NGC55. Castro N., Herrero A., Garcia M., Trundle C., Bresolin F., Gieren W., Pietrzynski G., Kudritzki R.-P., Demarco R. <Astron. Astrophys., 485, 41-50 (2008)> =2008A&A...485...41C ================================================================================ ADC_Keywords: Galaxies, nearby ; Stars, blue ; Spectral types ; Photometry ; Radial velocities Keywords: galaxies: individual: NGC 55 - galaxies: stellar content - stars: early-type - stars: fundamental parameters - catalogs Abstract: This is the first paper of a series devoted to studying the population of blue massive stars in NGC 55, a galaxy of the Sculptor group at a distance of about 2Mpc. We have obtained optical (3300-6210AA), low-resolution spectra of approximately 200 blue massive stars with VLT-FORS2, which we have classified with the aid of Milky Way and Magellanic Cloud standard stars. Description: Targets were selected from existing V- and I-band photometry obtained as part of the ongoing ARAUCARIA Cepheid search project whose results have been reported in Pietrzynski et al. (2006, Cat. J/AJ/132/2556). These data were taken with the Warsaw 1.3m telescope at Las Campanas Observatory. We obtained spectra for 200 objects with FORS2 (FOcal Reducer and low dispersion Spectrograph) at the Very Large Telescope (VLT-UT2), in the Mask eXchange Unit (MXU) mode. The observations, performed in November 2004.
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