INaf-TRIeste Grid Of Synthetic Spectra

INTRIGOSS is a High Resolution (HR) synthetic spectral library designed for studying FGK stars (Franchini et al. 2018 submitted). The library is based on atmosphere models computed with specified individual element abundances and microturbulent velocity (ξ) via ATLAS12 code (Kurucz 2005 and Castelli 2005). Normalized SPectra (NSP) and surface Flux SPectra (FSP), in the 4830-5400 Å wavelength range, were computed with the SPECTRUM code (Gray & Corbally 1994) v2.76f. INTRIGOSS uses the solar composition by Grevesse et al. (2007) and four different [α/Fe] abundance ratios and consists of 7616 NSP and 7616 FSP spectra.

The atmosphere models are computed in the following ranges of atmospheric parameters:

The synthetic spectra are computed using a line list of atomic and molecular transitions containing for a sub-set of lines their astrophysical gf-values derived by comparing synthetic spectra predictions with a very high SNR (~4000) observed solar spectrum and with the UVES-U580 spectra (SNR > 100) of five cool giants.

Use of the archive

You can select intervals of input parameters (Teff, log g, [Fe/H], [α/Fe], and ξ) by introducing the minimum and maximum values in the two boxes at the right side of each parameter. If you choose limits in more than one parameter you will get spectra that match all the criteria. An output table with the selected spectra will be produced. Filenames of the synthetic spectra are straightforward with the following scheme:



is a numerical character;
is the prefix for [alpha/Fe] and the next character p or m differentiates positive or negative values respectively. Values are multiplied by 100.
is the prefix for [Fe/H] and the next character p or m differentiates positive or negative values respectively. Values are multiplied by 100.
is the prefix for Teff in K
is the prefix for log g multiplied by 10
is the prefix for microturbulence in km/s
identifies NPS spectra while f identifies FSP spectra.

You can download the displayed table. From the table, by marking the small box on the left side of each line, you can choose only the spectra you are interested in. You can download one, more than one, or all the FITS file after creating a tar. Each FITS file contains a binary table with the wavelength and the flux and its header lists also all the atmospheric parameters of the corresponding synthetic spectrum.

Auxiliary data

The following auxiliary data are also available:

You are free to use data from the present archive for scientific reasons within the limits of its applicability as described in Franchini et al. (2018). Please acknowledge the use of the database in your publications. Feel free to contact us for any question or feedback.

This research uses the facilities of the Italian Center for Astronomical Archive (IA2) operated by INAF.