of 45 stars, mainly Vega-type and pre-main sequence (CTTs, ETTs and
Herbig Ae/Be), have been determined. These are crucial parameters necessary
for understanding the evolutionary sequence leading from the early stages
of the pre-main sequence evolution to stars with disks and planets already
formed. Future work, already in progress, includes the accurate
determination of the stellar luminosities and metal abundances. The
comparison of all data with those predicted from pre-main sequence
evolutionary tracks will provide further insight into the physics of these
stars.
Acknowledgements
We are grateful to the referee, Prof. Gibor Basri, for his careful reading of the manuscript, suggestions and criticisms that helped us to improve the first version of this paper. We acknowledge the International Scientific Committee of the Canary Islands' Observatories for the allocation of observing time in the International Time programme. The work of C. Eiroa, B. Merín, B. Montesinos, A. Mora and J. Palacios has been supported in part by the Spanish grant ESP 98-1339. A. Mora wishes to thank Dr. J. R. Barnes for valuable discussions about echelle reduction procedures. Part of this research has made use of the SIMBAD database, operated at CDS, Strasbourg, France.
Copyright ESO 2001