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.
<Astron. Astrophys. 558, A38 (2013)>
=2013A&A...558A..38M 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)
FAMAmoogfiles:
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
σ(FeI)/range(EP).
5) 1.2 (default) σ clipping for FeI lines
6) 1.0 (default) σ clipping for FeII lines
7) 1.0 (default) σ 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:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
FAMAv1.tar 512 29460 Tar file with all FAMA codes
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Acknowledgements:
Laura Magrini, laura(at)arcetri.astro.it
(End) Laura Magrini [Arcetri obs.], Patricia Vannier [CDS] 09-Jul-2013