Spectrophotometric properties of galaxies at intermediate redshifts (z ~ 0.2–1.0)

I. Sample description, photometric properties and spectral measurements

¹ Laboratoire d'Astrophysique de Toulouse et Tarbes (LATT - UMR 5572), Observatoire Midi-Pyrénées, 14 avenue E. Belin, 31400 Toulouse, France e-mail: flamare@ast.obs-mip.fr
² Max-Planck Institut für Astrophysik, Karl-Schwarzschild-Strasse 1 Postfach 1317, 85741 Garching, Germany
³ Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal
⁴ Institut d'Astrophysique de Paris, CNRS, 98 bis boulevard Arago, 75014 Paris, France

Received: 9 June 2005
Accepted: 29 October 2005

Abstract

We present the spectrophotometric properties of a sample of 141 emission-line galaxies at redshifts in the range with a peak around . The analysis is based on medium resolution (), optical spectra obtained at VLT and Keck. The targets are mostly “Canada-France Redshift Survey” emission-line galaxies, with the addition of field galaxies randomly selected behind lensing clusters. We complement this sample with galaxy spectra from the “Gemini Deep Deep Survey” public data release. We have computed absolute magnitudes of the galaxies and measured the line fluxes and equivalent widths of the main emission/absorption lines. The last two have been measured after careful subtraction of the fitted stellar continuum using the platefit software originally developed for the SDSS and adapted to our data. We present a careful comparison of this software with the results of manual measurements. The pipeline has also been tested on lower resolution spectra, typical of the “VIMOS/VLT Deep Survey” (), by resampling our medium resolution spectra. We show that we can successfully deblend the most important strong emission lines. These data are primarily used to perform a spectral classification of the galaxies in order to distinguish star-forming galaxies from AGNs. Among the initial sample of 141 emission-line galaxies, we find 7 Seyfert 2 (narrow-line AGN), 115 star-forming galaxies and 16 “candidate” star-forming galaxies. Scientific analysis of these data, in terms of chemical abundances, stellar populations, etc., will be presented in subsequent papers of this serie.