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Statistical cataloging of archival data for luminosity class IV-V stars. II. The epoch 2001 [Fe/H] catalog
This paper describes the derivation of an updated statistical catalog ofmetallicities. The stars for which those metallicities apply are ofspectral types F, G, and K, and are on or near the main sequence. Theinput data for the catalog are values of [Fe/H] published before 2002February and derived from lines of weak and moderate strength. Theanalyses used to derive the data have been based on one-dimensional LTEmodel atmospheres. Initial adjustments which are applied to the datainclude corrections to a uniform temperature scale which is given in acompanion paper (see Taylor \cite{t02}). After correction, the data aresubjected to a statistical analysis. For each of 941 stars considered,the results of that analysis include a mean value of [Fe/H], an rmserror, an associated number of degrees of freedom, and one or moreidentification numbers for source papers. The catalog of these resultssupersedes an earlier version given by Taylor (\cite{t94b}).Catalog is only available in electronic form at the CDS via anonymousftp cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/398/731
| Statistical cataloging of archival data for luminosity class IV-V stars. I. The epoch 2001 temperature catalog
This paper is one of a pair in which temperatures and metallicitycatalogs for class IV-V stars are considered. The temperature catalogdescribed here is derived from a calibration based on stellar angulardiameters. If published calibrations of this kind are compared by usingcolor-index transformations, temperature-dependent differences among thecalibrations are commonly found. However, such differences are minimizedif attention is restricted to calibrations based on Johnson V-K. Acalibration of this sort from Di Benedetto (\cite{dib98}) is thereforetested and adopted. That calibration is then applied to spectroscopicand photometric data, with the latter predominating. Cousins R-Iphotometry receives special attention because of its high precision andlow metallicity sensitivity. Testing of temperatures derived from thecalibration suggests that their accuracy and precision are satisfactory,though further testing will be warranted as new results appear. Thesetemperatures appear in the catalog as values of theta equiv5040/T(effective). Most of these entries are accompanied by measured orderived values of Cousins R-I. Entries are given for 951 stars.Catalog is only available in electronic form at the CDS via anonymousftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/398/721
| Improved Astrometry and Photometry for the Luyten Catalog. II. Faint Stars and the Revised Catalog
We complete construction of a catalog containing improved astrometry andnew optical/infrared photometry for the vast majority of NLTT starslying in the overlap of regions covered by POSS I and by the secondincremental Two Micron All Sky Survey (2MASS) release, approximately 44%of the sky. The epoch 2000 positions are typically accurate to 130 mas,the proper motions to 5.5 mas yr-1, and the V-J colors to0.25 mag. Relative proper motions of binary components are measured to 3mas yr-1. The false-identification rate is ~1% for11<~V<~18 and substantially less at brighter magnitudes. Theseimprovements permit the construction of a reduced proper-motion diagramthat, for the first time, allows one to classify NLTT stars intomain-sequence (MS) stars, subdwarfs (SDs), and white dwarfs (WDs). We inturn use this diagram to analyze the properties of both our catalog andthe NLTT catalog on which it is based. In sharp contrast to popularbelief, we find that NLTT incompleteness in the plane is almostcompletely concentrated in MS stars, and that SDs and WDs are detectedalmost uniformly over the sky δ>-33deg. Our catalogwill therefore provide a powerful tool to probe these populationsstatistically, as well as to reliably identify individual SDs and WDs.
| HIPPARCOS age-metallicity relation of the solar neighbourhood disc stars
We derive age-metallicity relations (AMRs) and orbital parameters forthe 1658 solar neighbourhood stars to which accurate distances aremeasured by the HIPPARCOS satellite. The sample stars comprise 1382 thindisc stars, 229 thick disc stars, and 47 halo stars according to theirorbital parameters. We find a considerable scatter for thin disc AMRalong the one-zone Galactic chemical evolution (GCE) model. Orbits andmetallicities of thin disc stars show now clear relation each other. Thescatter along the AMR exists even if the stars with the same orbits areselected. We examine simple extension of one-zone GCE models whichaccount for inhomogeneity in the effective yield and inhomogeneous starformation rate in the Galaxy. Both extensions of the one-zone GCE modelcannot account for the scatter in age - [Fe/H] - [Ca/Fe] relationsimultaneously. We conclude, therefore, that the scatter along the thindisc AMR is an essential feature in the formation and evolution of theGalaxy. The AMR for thick disc stars shows that the star formationterminated 8 Gyr ago in the thick disc. As already reported by Grattonet al. (\cite{Gratton_et.al.2000}) and Prochaska et al.(\cite{Prochaska_et.al.2000}), thick disc stars are more Ca-rich thanthin disc stars with the same [Fe/H]. We find that thick disc stars showa vertical abundance gradient. These three facts, the AMR, verticalgradient, and [Ca/Fe]-[Fe/H] relation, support monolithic collapseand/or accretion of satellite dwarf galaxies as likely thick discformation scenarios. Tables 2 and 3 are only available in electronicform at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5)or via http:/ /cdsweb.u-strasbg.fr/ cgi-bin/qcat?J/ A+A/394/927
| Aluminium in metal-poor stars.
Previous calculations of the statistical equilibrium of aluminium in thesolar photosphere have shown that NLTE populations hardly affect Al lineformation in the Sun; however, in metal-poor stars the influence ofelectron collisions is reduced, and a UV radiation field enhanced due tosmaller background line opacity results in more pronounced NLTE effects.Thus analyses based on NLTE populations lead to significantly higher Alabundances than those calculated from LTE. For stars of intermediatemetallicity between -1.0<[Fe/H]<-0.5 some overabundance relativeto iron is found. For more metal-poor stars the overabundance disappearsand approaches the solar ratio, [Al/Fe]=0. Only a weak overabundance inthe [Al/Mg] ratio is detected for stars with intermediate metallicityand a small underabundance of -0.2 to -0.3dex for the metal-poor stars.From investigation of both solar and stellar Al spectra the influence ofhydrogen collisions could be better estimated. The previously definedatomic model thus had to be slightly modified to fit both metal-rich andmetal-poor stars. Compared with LTE analyses the present resultscompletely change the chemical enrichment scenario with [Al/Fe] nowfollowing the trend of primary elements for all metal-poor stars. Thehump of enhanced Al/Fe values for stars between -1.0<[Fe/H]<-0.5does not seem to be an artefact. It nearly vanishes for the [Mg/Fe]abundance ratios. It may not necessarily have to be explained in termsof stellar nucleosynthesis because it could result from our reference toLTE abundances for Mg and Fe.
| A catalogue of [Fe/H] determinations: 1996 edition
A fifth Edition of the Catalogue of [Fe/H] determinations is presentedherewith. It contains 5946 determinations for 3247 stars, including 751stars in 84 associations, clusters or galaxies. The literature iscomplete up to December 1995. The 700 bibliographical referencescorrespond to [Fe/H] determinations obtained from high resolutionspectroscopic observations and detailed analyses, most of them carriedout with the help of model-atmospheres. The Catalogue is made up ofthree formatted files: File 1: field stars, File 2: stars in galacticassociations and clusters, and stars in SMC, LMC, M33, File 3: numberedlist of bibliographical references The three files are only available inelectronic form at the Centre de Donnees Stellaires in Strasbourg, viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5), or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Spectroscopic analyses of metal-poor stars. III. Magnesium abundances.
We present magnesium abundances and Mg/Fe ratios for 56 metal-poordwarfs and subgiants based on differential LTE model atmosphere analysesof spectra that have a typical S/N of 50-100 and a resolution of about20000-30000. The distribution of Mg/Fe abundance ratios with Feabundances is characterized by a steep increase of [Mg/Fe] near[Fe/H]=-0.6. At that iron abundance we recognize an abrupt change from asolar value for stars with [Fe/H]>=-0.6 to an upper limit of +0.4dexfor the metal-poor stars. Our data suggest that this step in the Mg/Feabundance ratio at [Fe/H]=-0.6 is the result of the onset of Galacticdisk formation, whereas [Mg/Fe]=+0.4 apparently is an upper limitarising from the constraints of nucleosynthesis in massive SN II eventsduring the first stellar generations, the yields of which we observe inthe most metal-poor halo stars.
| Spectroscopic analyses of metal-poor stars. II. The evolutionary stage of subdwarfs.
Models of post-main sequence stellar evolution of VandenBerg & Bell(???) have been applied to determine spectroscopic masses and distancesfor metal-poor stars. Careful consideration of the most important errorsources published in more recent papers such as VandenBerg (???) for thefirst time allow us to draw firm statistical conclusions. It is shownthat the evolutionary calculations qualitatively fit to the observedstellar parameters whereas quantitatively they predict too high ages formetal-poor stars. As an important result we confirm that evolutionarysequences need to be calibrated with respect to their metal abundance inorder to use their absolute predictions of temperature and luminosity.It turns out that this can be achieved by a simple shift of theevolutionary tracks and isochrones in effective temperature with values{DELTA}log T_eff_<~0.03 which accounts for possible changes of themixing-length and the O/Fe ratio with metallicity. The stellarluminosities and surface gravities obtained from evolutionary models aremuch more reliable than their effective temperatures. Therefore weconclude that the accuracy of the corresponding spectroscopic stellargravities is systematically affected by deviations from LTE, inparticular along the subgiant sequence where systematic errors less than{DELTA}log g =~0.3 must be ascribed to the non-LTE ionizationequilibrium of Fe II/Fe I. In our spectroscopic analyses the strongdependence between surface gravity and abundances determined from Fe Ilines restricts the accuracy of Fe abundances in subgiants to 0.1 dex atbest. The most remarkable result of our evolutionary and kinematicinvestigations of halo stars refers to the large fraction of slightlyevolved subgiants among the so-called subdwarfs. Since conventionalphotometric approaches often assume that the great majority ofmetal-poor stars are dwarfs this results in distances that aresystematically too low for their samples. Consequently, significantdifferences are found when comparing evolutionary and kinematicparameters obtained from either photometric or spectroscopic data. Wedemonstrate this by comparing the space velocities of the stars. Itappears that stars with particularly high space velocities derived fromspectroscopic distances show very often much lower velocities based ontheir main sequence parallaxes. We find that results refering to mainsequence parallaxes are doubtful and can be used only with greatestcare. An advantageous side-effect of the application of spectroscopicdata to evolutionary calculations is the possibility to identify binarysystems that are either standing out from the Toomre diagram with theirunusually high space velocities, or from a log g - log T_eff_ diagramwith apparently contradictory luminosities.
| Spectroscopic analyses of metal-poor stars. 1: Basic data and stellar parameters
Accurate stellar parameters have been obtained from the analyses of morethan thousand spectra of 115 metal-poor dwarfs and subgiants with visualmagnitudes brighter than V approximately equal to 12. The stellar samplewas selected mainly by high proper motion, with additional restrictionsfrom B-V colors and U-B excesses. The effective temperatures cover arange from 5000 to 6500 K while abundances are found between (M/H) =-0.1 and -0.3 dex. Based on homogeneous ODF blanketed model atmospheresin local thermodynamic equilibrium (LTE) and working differentially withrespect to the Sun we derive a consistent set of stellar parameters,effective temperature, surface gravity, metal abundance andmicroturbulence velocity. Individual profile synthesis is applied to anumber of spectral lines for each star, which has led as a rule toaccuracies in Teff of better than 100 K, in log g of betterthan 0.15, and in (Fe/H) of better than 0.1 dex. Because of theconsistent treatment with only one type of model atmosphere, this sampleprovides an oppurtunity to examine the individual parametersstatistically and investigate in detail their relation to the formationand evolution of the Galaxy. One aspect of this analysis is a generalshift to higher iron abundances for the most metal-poor stars. Alongwith the recently preferred meteoritic solar iron abundance andeffective temperatures from conistent Balmer line profile fits that tendto be 100-200 K hotter than found from photometric calibrations,discrepancies of up to 0.5 dex in (Fe/H) can be explained in comparisonwith other abundance analyses. The most important results refer to theevolutionary status of the bona fide subdwarf sample. Irrespective ofthe different effective temperatures found here, there exists a severeproblem when comparing post main sequence evolutionary models of coolstars with our observed parameters. Even more interesting is the fact,demonstrated by the results of a consistent analysis of the ironionization equilibrium, that roughly half of the subdwarfs aresubgiants, some of them having nearly reached the bottom of the giantbranch.
| Balmer lines in cool dwarf stars II. Effective temperatures and calibration of colour indices
Effective temperatures obtained from synthesis of the extended profilewings of the first four Balmer lines are presented for more than 100dwarfs and subgiants of different metal abundances and surface gravitiesin the temperature range from 5000 to 6500 K. Line formation is based onhomogeneous ODF blanketed model atmospheres in LTE. The resultingtemperatures of the more metal-rich stars differ systematically fromthose determined by reference to synthetic broad- or intermediate-bandcolours such as B-V , b-y , R-I or V-K . While the Balmer linetemperatures give room to only very small individual errors and resultin a convincingly small mean error for all four lines, the scatteragainst temperatures determined from broad-band colours is by faroutside the internal errors claimed in recent applications. This may beattributed to either (a) observational errors, (b) dependence on therelative mixture of metal abundances, (c) unknown line blocking in mostof the visible and near-infrared spectrum or (d) the inhomogeneity foundin the granular patterns of stellar surfaces. Our results suggest thatbroad-band colours are insufficient individual temperature indicators,reliable only in a statistical sense.
| Early type high-velocity stars in the solar neighborhood. IV - Four-color and H-beta photometry
Results are presented from photometric obaservations in the Stromgrenuvby four-color and H-beta systems of early-type high-velocity stars inthe solar neighborhood. Several types of photometrically peculiar starsare selected on the basis of their Stromgren indices and areprovisionally identified as peculiar A stars, field horizontal-branchstars, metal-poor stars near the Population II and old-disk turnoffs,metal-poor blue stragglers, or metallic-line A stars. Numerousphotometrically normal stars were also found.
| Early-type high-velocity stars in the solar neighborhood. I - List of candidates
Suspected nearby high-velocity stars of spectral types B and A areidentified by their proper motions, which are generally too small forthe stars to have been included in previous catalogs of high-velocitystars. The same selection process is then extended to spectral type Fstars, in order to both provide a companion sample and investigatewhether the hypothetical high-velocity, metal-rich population continuesto later spectral types. Of the presented list of 371 stars withconfirmed proper motions, 168 are of A and B spectral types. Photometricand spectroscopic observations of these stars are required to eliminatethose with misclassified spectra and convert proper motions into spacevelocities. The identification of type of stars is important forunderstanding apparent exceptions to the correlation between stellarages, metal abundances, and kinematic properties.
| Luminosities and motion of the F-type stars. II. Metal-deficient stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1972ApJ...175..787E&db_key=AST
| UBV Photometry of 500 Southern Stars [erratum: 1973MNSSA..32...48C]
Not Available
| Radial Velocities and three-colour photometry of 52 stars with large proper motions
Abstract image available at:http://adsabs.harvard.edu/abs/1965MNRAS.129...63P
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