EDP Sciences
Free Access
Volume 417, Number 3, April III 2004
Page(s) 1055 - 1062
Section Stellar structure and evolution
DOI https://doi.org/10.1051/0004-6361:20034324
Published online 26 March 2004

A&A 417, 1055-1062 (2004)
DOI: 10.1051/0004-6361:20034324

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

T. Zwitter1, F. Castelli2, 3 and U. Munari4, 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 Attività Spaziali dell'Università di Padova, Italy

(Received 16 September 2003 / Accepted 24 December 2003)

A library of 183 588 synthetic spectra based on Kurucz's ATLAS9 models is presented for the far red spectral interval (7653-8747 Å). It is characterized by  $3500~{\rm K} \le T_{\rm eff} \le 47\,500$ K, $0.0 \le \log g \le 5.0$, $-3.0 \le [{\rm M}/{\rm H}] \le +0.5$, $0 \le V_{\rm rot} \le 500$ km s -1, $\xi = 2$ km s -1. The whole grid of spectra is calculated for resolving powers 8500, 11 500 and 20 000. A section of the grid is also computed for [ $\alpha/{\rm Fe}]=+0.4$ 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: miscellaneous -- stars: fundamental parameters -- surveys -- stars: atmospheres

Offprint request: T. Zwitter, tomaz.zwitter@fmf.uni-lj.si

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© ESO 2004

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