J/A+A/558/A38 FAMA code for stellar parameters and abundances (Magrini+, 2013) ================================================================================ FAMA: An automatic code for stellar parameter and abundance determination. Magrini L., Randich S., Friel E., Spina L., Jacobson H., Cantat-Gaudin T., Donati P., Baglioni R., Maiorca E., Bragaglia A., Sordo R., Vallenari A. =2013A&A...558A..38M ================================================================================ ADC_Keywords: Models ; Abundances Keywords: methods: data analysis - techniques: spectroscopic - stars: abundances - Galaxy: abundances - surveys - open clusters and associations: general Abstract: The large amount of spectra obtained during the epoch of extensive spectroscopic surveys of Galactic stars needs the development of automatic procedures to derive their atmospheric parameters and individual element abundances. Starting from the widely-used code MOOG by C. Sneden, we have developed a new procedure to determine atmospheric parameters and abundances in a fully automatic way. The code FAMA (Fast Automatic MOOG Analysis) is presented describing its approach to derive atmospheric stellar parameters and element abundances. The code, freely distributed, is written in Perl and can be used on different platforms. The aim of FAMA is to render the computation of the atmospheric parameters and abundances of a large number of stars using measurements of equivalent widths (EWs) as automatic and as independent of any subjective approach as possible. It is based on the simultaneous search for three equilibria: excitation equilibrium, ionization balance, and the relationship between logn(FeI) and the reduced EWs. FAMA also evaluates the statistical errors on individual element abundances and errors due to the uncertainties in the stellar parameters. The convergence criteria are not fixed "a priori" but are based on the quality of the spectra. In this paper we present tests performed on the solar spectrum EWs that assess the method's dependency on the initial parameters and we analyze a sample of stars observed in Galactic open and globular clusters. Description: FAMA v.1, July 2013, distributed with MOOGv2013 and Kurucz models. Perl Codes: read_out2.pl read_final.pl driver.pl sclipping_26.0.pl sclipping_final.pl sclipping_26.1.pl confronta.pl fama.pl Model atmopheres and interpolator (Kurucz models): MODEL_ATMO MOOG_files: files to compile MOOG (the most recent version of MOOG can be obtained from http://www.as.utexas.edu/~chris/moog.html) FAMA_moog_files: files to update when compiling MOOG OUTPUT: directory in which the results will be stored, contains a sm macro to produce final plots automoog.par: files with parameters for FAMA 1) OUTPUTdir 2) MOOGdir 3) modelsdir 4) 1.0 (default) percentage of the dispersion of FeI abundances to be considered to compute the errors on the stellar parameters, 1.0 means 100%, thus to compute e.g., the error on Teff we allow to code to find the Teff corresponding to a slope given by {sigma}(FeI)/range(EP). 5) 1.2 (default) {sigma} clipping for FeI lines 6) 1.0 (default) {sigma} clipping for FeII lines 7) 1.0 (default) {sigma} clipping for the other elements 8) 1.0 (default) value of the QP parameter, higher values mean less strong convergence criteria. star.iron: EWs in the correct format to test the code sun.par: initial parameters for the test File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file FAMAv1.tar 512 29460 Tar file with all FAMA codes -------------------------------------------------------------------------------- Acknowledgements: Laura Magrini, laura(at)arcetri.astro.it ================================================================================ (End) Laura Magrini [Arcetri obs.], Patricia Vannier [CDS] 09-Jul-2013