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Aims: We developed a new method of estimating the stellar parameters Teff,log g, [M/H], and elemental abundances. This method was implemented in a newcode, SP_Ace (Stellar Parameters And Chemical abundances Estimator). This is ahighly automated code suitable for analyzing the spectra of large spectroscopicsurveys with low or medium spectral resolution (R=2,000-20,000). Methods: Afterthe astrophysical calibration of the oscillator strengths of 4643 absorptionlines covering the wavelength ranges 5212-6860\AA\ and 8400-8924\AA, weconstructed a library that contains the equivalent widths (EW) of these linesfor a grid of stellar parameters. The EWs of each line are fit by a polynomialfunction that describes the EW of the line as a function of the stellarparameters. The coefficients of these polynomial functions are stored in alibrary called the "$GCOG$ library". SP_Ace, a code written in FORTRAN95, usesthe GCOG library to compute the EWs of the lines, constructs models of spectraas a function of the stellar parameters and abundances, and searches for themodel that minimizes the $\chi^2$ deviation when compared to the observedspectrum. The code has been tested on synthetic and real spectra for a widerange of signal-to-noise and spectral resolutions. Results: SP_Ace derivesstellar parameters such as Teff, log g, [M/H], and chemical abundances of up toten elements for low to medium resolution spectra of FGK-type stars withprecision comparable to the one usually obtained with spectra of higherresolution. Systematic errors in stellar parameters and chemical abundances arepresented and identified with tests on synthetic and real spectra. Stochasticerrors are automatically estimated by the code for all the parameters. A simpleWeb front end of SP_Ace can be found at http://dc.g-vo.org/SP_ACE, while thesource code will be published soon.

SP_Ace: a new code to derive stellar parameters and elemental abundances