J/A+A/392/1129ivo://CDS.VizieR/J/A+A/392/1129doi:10.26093/cds/vizier.33921129CDSNg Y.K.Brogt E.Chiosi C.Bertelli G.2002-09-28T14:06:57Z2002-09-28T14:06:49ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frstellar-evolutionary-modelsphotometryA new method, AMORE (AutoMatic Observation REnderer) - based on a genetic algorithm optimizer, is presented for the automated study of colour-magnitude diagrams. The method combines several stellar population synthesis tools developed in the last decade by or in collaboration with the Padova group. Our method is able to recover, within the uncertainties, the parameters - distance, extinction, age, metallicity, index of a power-law initial mass function and the index of an exponential star formation rate - from a reference synthetic stellar population. No a priori information is inserted to recover the parameters, which is done simultaneously and not one at a time. Examples are given to demonstrate and to better understand biases in the results, if one of the input parameters is deliberately set fixed to a non-optimum value.2002A&A...392.1129Nhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/392/1129CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/392/1129https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/392/1129http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/392/1129https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/392/1129https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/392/1129http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/392/1129GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/392/1129/tablea1AMORE results with the test population as specified in Sect. 4.3.1 of the paperrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNmodel[1/162] Model numbermeta.id;stat.fitintprimarypcrosscrossover probabilitystat.paramfloatrcrossmulti-point crossover ratestat.paramfloatrbroodamount of offspring two parents can havestat.paramfloatpcreepcreep mutation ratestat.paramfloatpcorrcorrelated mutation ratestat.paramfloatfAFitness valuestat.paramdoubleGenGeneration number (1)stat.paramintJ/A+A/392/1129/tablea2Results of running AMORE with one of the astrophysical parameters fixed at its original valuerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintParamParameter namemeta.id;stat.fit.paramcharNmodelModel numbermeta.id;stat.fitintfAFitness valuestat.paramdoublelogdDistancepcpos.distancedoubleAVExtinctionmagphys.absorptionfloatlogtlLower age limitlog(Gyr)time.agedoublelogthUpper age limitlog(Gyr)time.agedouble[Z]lLower metallicity limitlog(Sun)phys.abund.Fedouble[Z]hUpper metallicity limitlog(Sun)phys.abund.FedoublealphaSlope for the Initial Mass Function power-lawstat.fit.paramfloatbetaIndex for the Star Formation Rate exponentialstat.fit.paramfloatJ/A+A/392/1129/tablea3AMORE with one of the parameters fixed at one sigma from its original valuerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintParamParameter namemeta.id;stat.fit.paramcharOffsetOffset in {sigma} unitsstat.paramintNmodelModel numbermeta.id;stat.fitintfA? Fitness valuestat.paramdoublenullablelogd? Distancepcpos.distancedoublenullableAV? Extinctionmagphys.absorptionfloatnullablelogtl? Lower age limitlog(Gyr)time.agedoublenullablelogth? Upper age limitlog(Gyr)time.agedoublenullable[Z]l? Lower metallicity limitlog(Sun)phys.abund.Fedoublenullable[Z]h? Upper metallicity limitlog(Sun)phys.abund.Fedoublenullablealpha? Slope for the Initial Mass Function power-lawstat.fit.paramfloatnullablebeta? Index for the Star Formation Rate exponentialstat.fit.paramfloatnullable