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An extensive library of synthetic spectra covering the far red, RAVE and GAIA wavelength ra.pdf

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An extensive library of synthetic spectra covering the far red, RAVE and GAIA wavelength ra

a r X i v : a s t r o - p h / 0 4 0 1 0 6 9 v 2 2 0 J a n 2 0 0 4 Astronomy Astrophysics manuscript no. synthe˙asaccepted February 2, 2008 (DOI: will be inserted by hand later) An extensive library of synthetic spectra covering the far red, RAVE and GAIA wavelength ranges Tomaz? Zwitter 1 , Fiorella Castelli 2,3 , and Ulisse Munari 4,5 1 University of Ljubljana, Department of Physics, Jadranska 19, 1000 Ljubljana, Slovenia 2 CNR-Istituto di Astrofisica Spaziale e Fisica Cosmica, Via del Fosso del Cavaliere, 00133, Roma, Italy 3 INAF-Osservatorio Astronomico di Trieste, Via G.B. Tiepolo 11, 34131, Trieste, Italy 4 Osservatorio Astronomico di Padova, Sede di Asiago, 36012 Asiago (VI), Italy 5 CISAS, Centro Interdipartimentale Studi ed Attivita? Spaziali dell’Universita? di Padova, Italy Received date..............; accepted date................ Abstract. A library of 183 588 synthetic spectra based on Kurucz’s ATLAS9 models is presented for the far red spectral interval (7653 – 8747 ?). It is characterized by 3 500 K ≤ Teff ≤ 47 500 K, 0.0 ≤ log g ≤ 5.0, ?3.0 ≤ [M/H] ≤ +0.5, 0 ≤ Vrot ≤ 500 km s ?1 , ξ = 2 km s?1. The whole grid of spectra is calculated for resolving powers 8 500, 11 500 and 20 000. A section of the grid is also computed for [α/Fe]=+0.4 and for microturbulent velocities 0 and 4 km s?1. The library covers the wavelength ranges and resolutions of the two ambitious spectroscopic surveys by the ground experiment RAVE and the space mission GAIA. Cross-sections across the multi-dimensional data-cube are used to illustrate the behaviour of the strongest spectral lines. Interpretation of real data will have to include interpolation to grid substeps. We present a simple estimate of the accuracy of such a procedure. Key words. Astronomical data bases: spectroscopic – Stars: fundamental parameters – Surveys:GAIA – Surveys:RAVE 1. Introduction Observations in the far red interval (7650–8750 ?) are becom- ing increasingly used for determination of basic stell