7 Conclusion

We have presented an archive of 908 spectra of 709 stars at two resolutions, $R=10\,000$ and $R=42\,000$, and in the wavelength range $\lambda\lambda = 410{-}680$ nm. The high resolution version is archived normalized to its pseudo-continuum while the low resolution is given in physical flux (above the earth atmosphere) normalized to one at $\lambda = 555$ nm.

The mean S/N per pixel in the high resolution version of the archive is 150 ( $S/N \approx 700$ per 0.1 nm), the photometric precision of the strengthening of the orders of the echelle spectra is better than 0.5%, the precision in bands of about 10-20 nm is 0.5% and the overall (broad-band) precision is 2.5%, limited by the effect of differential refraction.

The stars in this archive cover a large range of the parameter space, though the mapping is still crude for hot and very cool stars.

This archive supersedes the TGMET (1996) library and is being used for automatic determination of the stellar parameters ( $T_{\rm eff}$, $\log~g$, [Fe/H]) by direct comparison of spectra with interpolations in the archive. The new version of the TGMET program, still under development, will enable determinations of the parameters from any $R>10\,000$ spectra, independently of the detailed observational setup. It will be presented in a future paper.

The archive will also be used to synthesize extragalactic stellar populations and to use these high resolution synthetic spectra as kinematical templates to determine simultaneously the parameters of the stellar population and the line-of-sight velocity distribution.

The archive itself will be completed with new observations and spectra from the OHP archive with the goal of improving the mapping of the parameter space and the quality of the photometric calibration.

Acknowledgements

We thank the director and technical staff of Observatoire de Haute-Provence for their constant support of our observing programs and for providing some spectra retrieved from the ELODIE archive. We thank all the observers who provided their observations to complete the database, especially the COROT team: D. Ballereau, J.-C. Bouret, C. Catala, T. Hua, D. Katz, F. Lignieres, T. Lueftinger and C. Van't Veer. We acknowlegde, with gratitude, financial support from the GDR Galaxies, CNRS, France. This work made extensive use of the SIMBAD and VIZIER databases, operated at CDS, Strasbourg, France.