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Two distinct halo populations in the solar neighborhood. II. Evidence from stellar abundances of Mn, Cu, Zn, Y, and Ba
Context. Current models of galaxy formation predict that the Galactichalo was assembled hierarchically. By measuring abundance ratios instars it may be possible to identify substructures in the halo resultingfrom this process. Aims: A previous study of 94 dwarf stars with-1.6 < [Fe/H] < -0.4 in the solar neighborhood has revealed theexistence of two distinct halo populations with a systematic differencein [?/Fe] at a given metallicity. In continuation of that work,abundances of Mn, Cu, Zn, Y, and Ba are determined for the same sampleof stars. Methods: Equivalent widths of atomic lines are measuredfrom high resolution VLT/UVES and NOT/FIES spectra and used to deriveabundance ratios from an LTE analysis based on MARCS model atmospheres.The analysis is made relative to two thick-disk stars, HD22879 and HD 76932, such that very precisedifferential values are obtained. Results: Systematic differencesbetween the "high-?" and "low-?" halo populations are foundfor [Cu/Fe], [Zn/Fe], and [Ba/Y], whereas there is no significantdifference in the case of [Mn/Fe]. At a given metallicity, [Cu/Fe] showsa large scatter that is closely correlated with a corresponding scatterin [Na/Fe] and [Ni/Fe]. Conclusions: The metallicity trends of[Cu/Fe], [Zn/Fe], and [Ba/Y] can be explained from existingnucleosynthesis calculations if the high-? stars formed in regionswith such a high star formation rate that only massive stars and type IIsupernovae contributed to the chemical enrichment. The low-?stars, on the other hand, most likely originate from systems with aslower chemical evolution, characterized by additional enrichment fromtype Ia supernovae and low-mass AGB stars.Based on observations made with the Nordic Optical Telescope on LaPalma, and on data from the European Southern Observatory ESO/ST-ECFScience Archive Facility (programs 65.L-0507, 67.D-0086, 67.D-0439,68.D-0094, 68.B-0475, 69.D-0679, 70.D-0474, 71.B-0529, 72.B-0585,76.B-0133 and 77.B-0507).Tables 1, 2, and excerpt of Table 3 areavailable in electronic form at http://www.aanda.orgTables 1, 2, andfull Table 3 are also available at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/530/A15
| The origin of palladium and silver
Context. In recent years, progress has been made in understanding therapid neutron-capture process (r-process) and current studies suggestthe need for a second, so-called weak r-process. Observational proof ofthis possible second branch of the r-process may come from a detailedknowledge of the formation and evolution of silver (Ag) and to someextent palladium (Pd) abundances in halo stars. Aims: We studythe silver and palladium abundances of a large sample of stars (only afew measurements have been made so far) to gain insight into theformation process of lighter neutron-capture elements. Methods:We analysed a sample of stars (including both dwarfs and giants), forwhich we determined in a consistent manner stellar parameters andabundances. The abundances were derived via spectrum synthesis, makinguse of the MOOG synthetic spectrum code (1D LTE) and MARCS stellar modelatmospheres (1D LTE). Results: We derived the Ag and Pdabundances of 56 stars, the largest sample to date for which both Pd andAg have been studied. The stars span a metallicity range of 2.5 dex,from the metal-poor giants at [Fe/H] ~ -3.2 to the more metal-richdwarfs at [Fe/H] ~ -0.6. Both elements display rather flat trends withmetallicity, with some dispersion being present at the lowestmetallicities. Conclusions: The similarity detected in theevolutionary trends of both Ag and Pd is indicative of a common origin.Qualitative comparisons with some theoretical calculations seem toconfirm the need for a second r-process, responsible for theirformation. Further abundance studies (exploring more light n-captureelements) and comparisons with a wider variety of theoretical models areneeded to fully characterise the details and site of the formationmechanism(s).Appendix is only available in electronic form at http://www.aanda.org
| Stellar atmosphere parameters with MA?, a MAssive compression of ?2 for spectral fitting
MA? is a new tool to estimate parameters from stellar spectra. It isbased on the maximum likelihood method, with the likelihood compressedin a way that the information stored in the spectral fluxes isconserved. The compressed data are given by the size of the number ofparameters, rather than by the number of flux points. The optimumspeed-up reached by the compression is the ratio of the data set to thenumber of parameters. The method has been tested on a sample oflow-resolution spectra from the Sloan Extension for GalacticUnderstanding and Exploration (SEGUE) survey for the estimate ofmetallicity, effective temperature and surface gravity, with accuraciesof 0.24 dex, 130 K and 0.5 dex, respectively. Our stellar parameters andthose recovered by the SEGUE Stellar Parameter Pipeline agree reasonablywell. A small sample of high-resolution VLT-UVES spectra is also used totest the method and the results were compared to a more classicalapproach. The speed and multi-resolution capability of MA? combinedwith its performance compared with other methods indicates that it willbe a useful tool for the analysis of upcoming spectral surveys.
| Two distinct halo populations in the solar neighborhood. Evidence from stellar abundance ratios and kinematics
Aims: Precise abundance ratios are determined for 94 dwarf starswith Teff K, -1.6 < [Fe/H] < -0.4, and distances D? 335 pc. Most of them have halo kinematics, but 16 thick-disk starsare included. Methods: Equivalent widths of atomic lines aremeasured from VLT/UVES and NOT/FIES spectra with resolutions R? 55000 and R ? 40 000, respectively. An LTE abundance analysis basedon MARCS models is applied to derive precise differential abundanceratios of Na, Mg, Si, Ca, Ti, Cr, and Ni with respect to Fe. Results: The halo stars fall into two populations, clearly separated in[?/Fe], where ? refers to the average abundance of Mg, Si,Ca, and Ti. Differences in [Na/Fe] and [Ni/Fe] are also present with aremarkably clear correlation between these two abundance ratios. Conclusions: The “high-?” stars may be ancient disk orbulge stars “heated” to halo kinematics by merging satellitegalaxies or they could have formed as the first stars during thecollapse of a proto-Galactic gas cloud. The kinematics of the“low-?” stars suggest that they have been accretedfrom dwarf galaxies, and that some of them may originate from the? Cen progenitor galaxy.Based on observations made with the Nordic Optical Telescope on LaPalma, and on data from the European Southern Observatory ESO/ST-ECFScience Archive Facility.Tables 3 and 4 are also 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/511/L10Figures5-8 and Tables 1-4 are only available in electronic form at http://www.aanda.org
| A New Color-Magnitude Diagram for 47 Tucanae: A Statistical Analysis
We present a statistical analysis of color-magnitude diagrams of 47 Tucderived from original and archival BVI photometry that produces the mostprobable locus for single stars. After adopting E(B-V) = 0.04, we derivean apparent distance modulus (m - M) V = 13.375 andachieve good matches to the most probable locus in the [B - V, V],[V - I, I], and [B - I, I] planes with 12 Gyr, [?/Fe]= +0.3, [Fe/H] = -0.83 isochrones from the Victoria-Regina models.This metallicity is generally lower than recent spectroscopicallyderived estimates for the cluster, but it is reinforced by themain-sequence match with a sample of subdwarfs.Based in part on observations made with the European SouthernObservatory (ESO) telescopes and obtained from the ESO/ST-ECF ScienceArchive facility.
| Beryllium abundances and star formation in the halo and in the thick disk
Context: Beryllium is a pure product of cosmic ray spallation. Thisimplies a relatively simple evolution in time of the beryllium abundanceand suggests its use as a time-like observable. Aims: Our goal is toderive abundances of Be in a sample of 90 stars, the largest sample ofhalo and thick disk stars analyzed to date. We study the evolution of Bein the early Galaxy and its dependence on kinematic and orbitalparameters, and investigate its use as a cosmochronometer. Abundances ofBe, Fe, and α-elements of 73 stars are employed to study theformation of the halo and the thick disk of the Galaxy. Methods:Beryllium abundances are determined from high-resolution, highsignal-to-noise UVES spectra with spectrum synthesis. Atmosphericparameters and abundances of α-elements are adopted from theliterature. Lithium abundances are used to eliminate mixed stars fromthe sample. The properties of halo and thick disk stars are investigatedin diagrams of log(Be/H) vs. [ α/H] , log(Be/H) vs. [Fe/H], and [α/Fe] vs. log(Be/H) and with orbital and kinematic parameters. Results: We present our observational results in various diagrams. (i)In a log(Be/H) vs. [Fe/H] diagram we find a marginal statisticaldetection of a real scatter, above what is expected from measurementerrors, with a larger scatter among halo stars. The detection of thescatter is further supported by the existence of pairs of stars withidentical atmospheric parameters and different Be abundances; (ii) in alog(Be/H) vs. [ α/Fe] diagram, the halo stars separate into twocomponents; one is consistent with predictions of evolutionary models,while the other has too high α and Be abundances and is chemicallyindistinguishable from thick disk stars. This suggests that the halo isnot a single uniform population where a clear age-metallicity relationcan be defined; (iii) In diagrams of R_min vs. [ α/Fe] andlog(Be/H), the thick disk stars show a possible decrease in [α/Fe] with R_min, whereas no dependence of Be with R_min is seen.This anticorrelation suggests that the star formation rate was lower inthe outer regions of the thick disk, pointing towards an inside-outformation. The lack of correlation for Be indicates that it isinsensitive to the local conditions of star formation.Based on observations made with ESO VLT, at Paranal Observatory, underprograms 076.B-0133 and 077.B-0507, and on data obtained from theESO/ST-ECF Science Archive Facility and the UVES Paranal ObservatoryProject 266.D-5655.Tables 1-3, 6 and Appendices A-C are only available in electronic format http://www.aanda.org
| Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available
| Metallicity and absolute magnitude calibrations for UBV photometry
Calibrations are presented here for metallicity ([Fe/H]) in terms of theultraviolet excess, [δ(U - B) at B - V = 0.6, hereafterδ0.6], and also for the absolute visual magnitude(MV) and its difference with respect to the Hyades(ΔMHV) in terms of δ0.6 and(B - V), making use of high-resolution spectroscopic abundances from theliterature and Hipparcos parallaxes. The relation[Fe/H]-δ0.6 has been derived for dwarf plus turn-offstars, and also for dwarf, turn-off, plus subgiant stars classifiedusing the MV-(B - V)0 plane of Fig. 11, which iscalibrated with isochrones from Bergbusch & VandenBerg (and alsoVandenBerg & Clem). The [Fe/H]-δ0.6 relations inour equations (5) and (6) agree well with those of Carney, as can beseen from Fig. 5(a). Within the uncertainties, the zero-points,+0.13(+/-0.05) of equation (5) and +0.13(+/-0.04) of equation (6), arein good agreement with the photometric ones of Cameron and of Carney,and close to the spectroscopic ones of Cayrel et al. and of Boesgaard& Friel for the Hyades open cluster. Good quantitative agreementbetween our estimated [Fe/H] abundances with those from uvby-βphotometry and spectroscopic [Fe/H]spec values demonstratesthat our equation (6) can be used in deriving quality photometric metalabundances for field stars and clusters using UBV data from variousphotometric surveys.For dwarf and turn-off stars, a new hybrid MV calibration ispresented, based on Hipparcos parallaxes withσπ/π <= 0.1 and with a dispersion of +/-0.24in MV. This hybrid MV calibration containsδ0.6 and (B - V) terms, plus higher order cross-termsof these, and is valid for the ranges of +0.37 <= (B - V)0<= +0.88,- 0.10 <= δ0.6 <= +0.29 and 3.44<= MV <= 7.23. For dwarf and turn-off stars, therelation for ΔMHV is revised and updated interms of (B - V) and δ0.6, for the ranges of -0.10<= δ0.6 <= +0.29, and +0.49 <= (B -V)0 <= +0.89, again making use of Hipparcos parallaxeswith σπ/π <= 0.1. These parallaxes formetal-poor dwarf and turn-off stars in our sample reveal that thedifference of ΔMHV(B - V) relative to Hyadesat (B - V) = +0.70 should be 1.37mag, instead of the 1.58mag given byLaird et al. In general, Hipparcos parallaxes are larger thanground-based ones, causing a divergence of ourΔMHV(B - V,δ0.6) relation(the solid line in Fig. 15b), from the one of Laird et al. (the dashedline) for the range +0.10 <= δ0.6 <= +0.29 ourabsolute magnitudes are fainter, as has been confirmed for localsubdwarfs by Reid. Our final calibrations forΔMHV(B - V, δ0.6),equations (16) and (17), are third-order polynomials inδ0.6, pass through the origin, and provide photometricdistances in reasonable agreement with those obtained directly fromHipparcos parallaxes (Fig. 18).
| Sulphur abundance in Galactic stars
We investigate sulphur abundance in 74 Galactic stars by using highresolution spectra obtained at ESO VLT and NTT telescopes. For the firsttime the abundances are derived, where possible, from three opticalmultiplets: Mult. 1, 6, and 8. By combining our own measurements withdata in the literature we assemble a sample of 253 stars in themetallicity range -3.2 [Fe/H] +0.5. Two important features,which could hardly be detected in smaller samples, are obvious from thislarge sample: 1) a sizeable scatter in [S/Fe] ratios around [Fe/H]-1; 2) at low metallicities we observe stars with [S/Fe] 0.4, aswell as stars with higher [S/Fe] ratios. The latter do not seem to bekinematically different from the former ones. Whether the latter findingstems from a distinct population of metal-poor stars or simply from anincreased scatter in sulphur abundances remains an open question.
| Abundance trends in kinematical groups of the Milky Way's disk
We have compiled a large catalogue of metallicities and abundance ratiosfrom the literature in order to investigate abundance trends of severalalpha and iron peak elements in the thin disk and the thick disk of theGalaxy. The catalogue includes 743 stars with abundances of Fe, O, Mg,Ca, Ti, Si, Na, Ni and Al in the metallicity range -1.30 < [Fe/H]< +0.50. We have checked that systematic differences betweenabundances measured in the different studies were lower than randomerrors before combining them. Accurate distances and proper motions fromHipparcos and radial velocities from several sources have been retreivedfor 639 stars and their velocities (U, V, W) and galactic orbits havebeen computed. Ages of 322 stars have been estimated with a Bayesianmethod of isochrone fitting. Two samples kinematically representative ofthe thin and thick disks have been selected, taking into account theHercules stream which is intermediate in kinematics, but with a probabledynamical origin. Our results show that the two disks are chemicallywell separated, they overlap greatly in metallicity and both showparallel decreasing alpha elements with increasing metallicity, in theinterval -0.80 < [Fe/H] < -0.30. The Mg enhancement with respectto Fe of the thick disk is measured to be 0.14 dex. An even largerenhancement is observed for Al. The thick disk is clearly older than thethin disk with tentative evidence of an AMR over 2-3 Gyr and a hiatus instar formation before the formation of the thin disk. We do not observea vertical gradient in the metallicity of the thick disk. The Herculesstream has properties similar to that of the thin disk, with a widerrange of metallicity. Metal-rich stars assigned to the thick disk andsuper-metal-rich stars assigned to the thin disk appear as outliers inall their properties.
| The [Zn/Fe] - [Fe/H] trend for disk and halo stars
Zn abundances, derived from a model atmosphere analysis of theλ6362.35 Å Zn I line, are presented for 44 thin disk, 10thick disk and 8 halo dwarf stars in the metallicity range -1.0 <[Fe/H] < +0.2. It is found that [Zn/Fe] in thin disk stars shows aslight increasing trend with decreasing metallicity reaching a value[Zn/Fe] ≃ +0.1 at [Fe/H] = -0.6. The thick disk stars in themetallicity range -0.9 < [Fe/H] < -0.6 have an average [Zn/Fe]≃ +0.15 dex, whereas five alpha-poor and Ni-poor halo stars in thesame metallicity range have [Zn/Fe] ≃ 0.0 dex. These resultsindicate that Zn is not an exact tracer of Fe as often assumed inabundance studies of damped Lyman-alpha systems (DLAs). A betterunderstanding of the nucleosynthesis of Zn is needed in order to obtainmore detailed information on the past history of star formation in DLAsfrom e.g. the observed sulphur/zinc ratio.Based on observations collected at the National AstronomicalObservatories, Xinglong, China and the European Southern Observatory, LaSilla, Chile (ESO No. 67.D-0106).
| Stellar Chemical Signatures and Hierarchical Galaxy Formation
To compare the chemistries of stars in the Milky Way dwarf spheroidal(dSph) satellite galaxies with stars in the Galaxy, we have compiled alarge sample of Galactic stellar abundances from the literature. Whenkinematic information is available, we have assigned the stars tostandard Galactic components through Bayesian classification based onGaussian velocity ellipsoids. As found in previous studies, the[α/Fe] ratios of most stars in the dSph galaxies are generallylower than similar metallicity Galactic stars in this extended sample.Our kinematically selected stars confirm this for the Galactic halo,thin-disk, and thick-disk components. There is marginal overlap in thelow [α/Fe] ratios between dSph stars and Galactic halo stars onextreme retrograde orbits (V<-420 km s-1), but this is notsupported by other element ratios. Other element ratios compared in thispaper include r- and s-process abundances, where we find a significantoffset in the [Y/Fe] ratios, which results in a large overabundance in[Ba/Y] in most dSph stars compared with Galactic stars. Thus, thechemical signatures of most of the dSph stars are distinct from thestars in each of the kinematic components of the Galaxy. This resultrules out continuous merging of low-mass galaxies similar to these dSphsatellites during the formation of the Galaxy. However, we do not ruleout very early merging of low-mass dwarf galaxies, since up to one-halfof the most metal-poor stars ([Fe/H]<=-1.8) have chemistries that arein fair agreement with Galactic halo stars. We also do not rule outmerging with higher mass galaxies, although we note that the LMC and theremnants of the Sgr dwarf galaxy are also chemically distinct from themajority of the Galactic halo stars. Formation of the Galaxy's thickdisk by heating of an old thin disk during a merger is also not ruledout; however, the Galaxy's thick disk itself cannot be comprised of theremnants from a low-mass (dSph) dwarf galaxy, nor of a high-mass dwarfgalaxy like the LMC or Sgr, because of differences in chemistry.The new and independent environments offered by the dSph galaxies alsoallow us to examine fundamental assumptions related to thenucleosynthesis of the elements. The metal-poor stars ([Fe/H]<=-1.8)in the dSph galaxies appear to have lower [Ca/Fe] and [Ti/Fe] than[Mg/Fe] ratios, unlike similar metallicity stars in the Galaxy.Predictions from the α-process (α-rich freeze-out) would beconsistent with this result if there have been a lack of hypernovae indSph galaxies. The α-process could also be responsible for thevery low Y abundances in the metal-poor stars in dSph's; since [La/Eu](and possibly [Ba/Eu]) are consistent with pure r-process results, thelow [Y/Eu] suggests a separate r-process site for this light(first-peak) r-process element. We also discuss SNe II rates and yieldsas other alternatives, however. In stars with higher metallicities([Fe/H]>=-1.8), contributions from the s-process are expected; [(Y,La, and Ba)/Eu] all rise as expected, and yet [Ba/Y] is still muchhigher in the dSph stars than similar metallicity Galactic stars. Thisresult is consistent with s-process contributions from lower metallicityAGB stars in dSph galaxies, and is in good agreement with the slowerchemical evolution expected in the low-mass dSph galaxies relative tothe Galaxy, such that the build-up of metals occurs over much longertimescales. Future investigations of nucleosynthetic constraints (aswell as galaxy formation and evolution) will require an examination ofmany stars within individual dwarf galaxies.Finally, the Na-Ni trend reported in 1997 by Nissen & Schuster isconfirmed in Galactic halo stars, but we discuss this in terms of thegeneral nucleosynthesis of neutron-rich elements. We do not confirm thatthe Na-Ni trend is related to the accretion of dSph galaxies in theGalactic halo.
| Abundances for metal-poor stars with accurate parallaxes. I. Basic data
We present element-to-element abundance ratios measured from highdispersion spectra for 150 field subdwarfs and early subgiants withaccurate Hipparcos parallaxes (errors <20%). For 50 stars new spectrawere obtained with the UVES on Kueyen (VLT UT2), the McDonald 2.7 mtelescope, and SARG at TNG. Additionally, literature equivalent widthswere taken from the works by Nissen & Schuster, Fulbright, andProchaska et al. to complement our data. The whole sample includes boththick disk and halo stars (and a few thin disk stars); most stars havemetallicities in the range -2<[Fe/H]<-0.6. We found our data, thatof Nissen & Schuster, and that of Prochaska to be of comparablequality; results from Fulbright scatter a bit more, but they are stillof very good quality and are extremely useful due to the large size ofhis sample. The results of the present analysis will be used inforthcoming papers to discuss the chemical properties of thedissipational collapse and accretion components of our Galaxy.Based in part on data collected at the European Southern Observatory,Chile, at the MacDonald Observatory, Texas, USA, and at the TelescopioNazionale Galileo, Canary Island, INAF,Italy-Spain.}\fnmsep\thanks{Table 1 is only available in electronic format the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) orvia\resizebox{8.8cm}{2.2mm}htpp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/404/187}
| 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.
| New Metallicity Calibration Down to [Fe/H] = -2.75 dex
We have taken 88 dwarfs, covering the colour-index interval 0.37 <=(B-V)0 <= 1.07mag, with metallicities -2.70 <= [Fe/H]<= +0.26dex, from three different sources for new metallicitycalibration. The catalogue of Cayrel de Stroble et al. (2001), whichincludes 65% of the stars in our sample, supplies detailed informationon abundances for stars with determination based on high-resolutionspectroscopy. In constructing the new calibration we have used as`corner stones' 77 stars which supply at least one of the followingconditions: (i) the parallax is larger than 10mas (distance relative tothe Sun less than 100pc) and the galactic latitude is absolutely higherthan 30° (ii) the parallax is rather large, if the galactic latitudeis absolutely low and vice versa. Contrary to previous investigations, athird-degree polynomial is fitted for the new calibration: [Fe/H]=0.10 -2.76δ - 24.04δ2 + 30.00δ3. Thecoefficients were evaluated by the least-squares method, without regardto the metallicity of Hyades. However, the constant term is in the rangeof metallicity determined for this cluster, i.e.0.08<=[Fe/H]<=0.11dex. The mean deviation and the mean error inour work are equal to those of Carney (1979), for [Fe/H] >= -1.75dexwhere Carney's calibration is valid
| Revised Coordinates and Proper Motions of the Stars in the Luyten Half-Second Catalog
We present refined coordinates and proper-motion data for the highproper-motion (HPM) stars in the Luyten Half-Second (LHS) catalog. Thepositional uncertainty in the original Luyten catalog is typicallygreater than 10" and is often greater than 30". We have used the digitalscans of the POSS I and POSS II plates to derive more accurate positionsand proper motions of the objects. Out of the 4470 candidates in the LHScatalog, 4323 objects were manually reidentified in the POSS I and POSSII scans. A small fraction of the stars were not found because of thelack of finder charts and digitized POSS II scans. The uncertainties inthe revised positions are typically ~2" but can be as high as ~8" in afew cases, which is a large improvement over the original data.Cross-correlation with the Tycho-2 and Hipparcos catalogs yielded 819candidates (with mR<~12). For these brighter sources, theposition and proper-motion data were replaced with the more accurateTycho-2/Hipparcos data. In total, we have revised proper-motionmeasurements and coordinates for 4040 stars and revised coordinates for4330 stars. The electronic version of the paper5 contains the updated information on all 4470stars in the LHS catalog.
| A search for previously unrecognized metal-poor subdwarfs in the Hipparcos astrometric catalogue
We have identified 317 stars included in the Hipparcos astrometriccatalogue that have parallaxes measured to a precision of better than 15per cent, and the location of which in the(MV,(B-V)T) diagram implies a metallicitycomparable to or less than that of the intermediate-abundance globularcluster M5. We have undertaken an extensive literature search to locateStrömgren, Johnson/Cousins and Walraven photometry for over 120stars. In addition, we present new UBV(RI)C photometry of 201of these candidate halo stars, together with similar data for a further14 known metal-poor subdwarfs. These observations provide the firstextensive data set of RCIC photometry ofmetal-poor, main-sequence stars with well-determined trigonometricparallaxes. Finally, we have obtained intermediate-resolution opticalspectroscopy of 175 stars. 47 stars still lack sufficient supplementaryobservations for population classification; however, we are able toestimate abundances for 270 stars, or over 80 per cent of the sample.The overwhelming majority have near-solar abundance, with theirinclusion in the present sample stemming from errors in the colourslisted in the Hipparcos catalogue. Only 44 stars show consistentevidence of abundances below [Fe/H]=-1.0. Nine are additions to thesmall sample of metal-poor subdwarfs with accurate photometry. Weconsider briefly the implication of these results for clustermain-sequence fitting.
| Catalogue of [Fe/H] determinations for FGK stars: 2001 edition
The catalogue presented here is a compilation of published atmosphericparameters (Teff, log g, [Fe/H]) obtained from highresolution, high signal-to-noise spectroscopic observations. This newedition has changed compared to the five previous versions. It is nowrestricted to intermediate and low mass stars (F, G and K stars). Itcontains 6354 determinations of (Teff, log g, [Fe/H]) for3356 stars, including 909 stars in 79 stellar systems. The literature iscomplete between January 1980 and December 2000 and includes 378references. The catalogue is made up of two tables, one for field starsand one for stars in galactic associations, open and globular clustersand external galaxies. The catalogue is distributed through the CDSdatabase. Access to the catalogue with cross-identification to othersets of data is also possible with VizieR (Ochsenbein et al.\cite{och00}). The catalogue (Tables 1 and 2) is only available inelectronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr(130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/373/159 and VizieRhttp://vizier.u-strasbg.fr/.
| Lithium abundances for 185 main-sequence stars: Galactic evolution and stellar depletion of lithium
We present a survey of lithium abundances in 185 main-sequence fieldstars with 5600 <~ Teff <~ 6600 K and -1.4 <~ [Fe/H]<~ +0.2 based on new measurements of the equivalent width of thelambda 6708 Li I line in high-resolution spectra of 130 stars and areanalysis of data for 55 stars from Lambert et al. (\cite{Lambert91}).The survey takes advantage of improved photometric and spectroscopicdeterminations of effective temperature and metallicity as well as massand age derived from Hipparcos absolute magnitudes, offering anopportunity to investigate the behaviour of Li as a function of theseparameters. An interesting result from this study is the presence of alarge gap in the log varepsilon (Li) - Teff plane, whichdistinguishes ``Li-dip'' stars like those first identified in the Hyadescluster by Boesgaard & Tripicco (\cite{Boesgaard86}) from otherstars with a much higher Li abundance. The Li-dip stars concentrate on acertain mass, which decreases with metallicity from about 1.4Msun at solar metallicity to 1.1 Msun at [Fe/H] =~-1.0. Excluding the Li-dip stars and a small group of lower mass starswith Teff < 5900 K and log varepsilon (Li) < 1.5, theremaining stars, when divided into four metallicity groups, may show acorrelation between Li abundance and stellar mass. The dispersion aroundthe log varepsilon (Li)-mass relation is about 0.2 dex below [Fe/H] =~-0.4 and 0.3 dex above this metallicity, which cannot be explained byobservational errors or differences in metallicity. Furthermore, thereis no correlation between the residuals of the log varepsilon (Li)-massrelations and stellar age, which ranges from 1.5 Gyr to about 15 Gyr.This suggests that Li depletion occurs early in stellar life and thatparameters other than stellar mass and metallicity affect the degree ofdepletion, e.g. initial rotation velocity and/or the rate of angularmomentum loss. It cannot be excluded, however, that a cosmic scatter ofthe Li abundance in the Galaxy at a given metallicity contributes to thedispersion in Li abundance. These problems make it difficult todetermine the Galactic evolution of Li from the data, but a comparisonof the upper envelope of the distribution of stars in the log varepsilon(Li) - [Fe/H] plane with recent Galactic evolutionary models by Romanoet al. (\cite{Romano99}) suggests that novae are a major source for theLi production in the Galactic disk; their occurrence seems to be theexplanation for the steep increase of Li abundance at [Fe/H] =~ -0.4.Based on observations carried out at Beijing Astronomical Observatory(Xinglong, PR China) and European Southern Observatory, La Silla, Chile.Table 1 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/371/943 and athttp://www.edpsciences.org
| Non-LTE Abundances and Consequences for the Evolution of the α-Elements in the Galaxy
Abundances of α-elements such as Ca and Mg in disk and halo starsare usually derived from equivalent width lines measured onhigh-resolution spectra and assuming local thermodynamic equilibrium(LTE). In this paper, we present non-LTE differential abundances derivedby computing the statistical equilibrium of Ca I and Mg I atoms, usinghigh-resolution equivalent widths available in the literature for 252dwarf to subgiant stars. These non-LTE abundances, combined with recentdetermination of non-LTE abundances of iron, seem to remove thedispersion of the [Ca/Fe] and [Mg/Fe] ratios in the galactic halo anddisk phases, revealing new and surprising structures. These results haveimportant consequences for chemical evolution models of the Galaxy. Inaddition, non-LTE abundance ratios for stars belonging to the M92cluster apparently have the same behavior. More high-resolutionobservations, mainly of globular clusters, are urgently needed toconfirm our results.
| Sc and Mn abundances in disk and metal-rich halo stars
Sc and Mn abundances are determined for 119 F and G main-sequence starswith -1.4 < [Fe/H] < +0.1, representing stars from the thin disk,the thick disk and the halo. The results indicate that Sc behaves likean alpha element, showing a decreasing [Sc/Fe] with increasingmetallicity in disk stars and a dual pattern in the kinematicallyselected halo stars. In contrast, Mn shows an increase from [Mn/Fe] =~-0.5 at [Fe/H] = -1.4 to zero at solar metallicity. There appears to bea discontinuity or sharp increase of [Mn/Fe] at [Fe/H] =~ -0.7corresponding to the transition between the thick and the thin disk. Itis discussed if supernovae of Type Ia are a major source of Mn in theGalactic disk or if the trend of [Mn/Fe] vs. [Fe/H] can be explained bynucleosynthesis in Type II supernovae with a strong metallicitydependence of the yield. Based on observations carried out at theEuropean Southern Observatory, La Silla, Chile, and Beijing AstronomicalObservatory, Xinglong, China
| Chemical composition of halo and disk stars with overlapping metallicities.
High resolution (R=60000), high S/N spectra have been obtained for 13halo stars and 16 disk stars with 5400<~T_eff_<~6500K,4.0<~logg<~4.6 and overlapping metallicities in the range-1.3<~[Fe/H]<~-0.5. Equivalent widths of weak FeI and FeII linesare used to determine differential values of T_eff_ and logg. Relativeabundances of O, Na, Mg, Si, Ca, Ti, Cr, Fe, Ni, Y and Ba are determinedto a precision ranging from 0.02 to 0.07dex. Kinematical data have beencollected and used to calculate the stellar orbital parameters, R_max_,the maximum distance from the Galactic center, and z_max_, the maximumdistance from the Galactic plane. A group of 8 halo stars havesignificantly lower [α/Fe] values than disk stars of the samemetallicity (α= O, Mg, Si, Ca or Ti). These stars are alsounderabundant in Na and Ni and maybe in Cr. [Na/Fe] ranges from -0.4 to+0.1, and [Ni/Fe] is surprisingly well correlated with [Na/Fe]. Thesmallest values of [α/Fe] and [Na/Fe] are found for the stars withthe largest values of R_max_ and z_max_. This may indicate that theanomalous halo stars have been accreted from dwarf galaxies with achemical evolution history different from that of the inner halo and thedisk. In any case the data show that abundance ratios in stars are notuniversal functions of [Fe/H] and that the chemical evolution of theGalaxy at [Fe/H]=~-1.0 is more complicated than assumed in many models.One halo star, HD 106038, is found to be strongly overabundant in Si,Ni, Y and Ba relative to Fe.
| Astrometric positions of stars with high proper motions in the Southern Hemisphere
Several stars with large proper motions, cited by W.J. Luyten, wereincluded in the preliminary programme for the HIPPARCOS mission. Whenperforming preparatory measurements of plates, difficulties wereencountered in identifying certain of these stars when relying only onpublished coordinates. We have taken advantage of this work whichrelates to the southern sky in order to determine the astrometricposition of the greatest possible number of these objects, even forthose which were not included in the programme. Catalogue is onlyavailable in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Uvby-β photometry of high-velocity and metal-poor stars. IX. Effects of orbital chaos in the Galactic halo.
Galactic orbits have been integrated using the Galactic potential modelof Allen & Santillan (1991RMxAA..22..255A) for 280 halo starsidentified in the V_rot_, [Fe/H] diagram. The effects of chaos upontheir orbital structure have been investigated. A "vertical" surface ofsection is defined, where Z is plotted versus z each time the orbitcrosses the cylinder ˜ω=8.5kpc; this surface of sectionallows a more complete visualization of the Galactic orbits in phasespace, a better understanding of the orbital chaos, and a more directcomparison with observations. "Horizontal" surfaces of section andmeridional orbits have also been plotted for all of these halo stars,and have been used to classify the Galactic orbits into the categoriesbox, chaotic, and resonant; 44.3% of the halo orbits are found to showsome evidence of chaos. The observed |W'| velocities of the halo starsgive poor measures of z_max_ for the box orbits, and especially for thechaotic orbits. Regressions of [Fe/H] against R_max_ and z_max_, for thetotal sample and for the chaotic and non-chaotic subsets, show littleevidence for a metallicity gradient in the Galactic halo. The surfacesof section for many of the halo stars (~ a third) show some evidence ofstructure within chaos. Part of this structure is due to the"stickiness" that chaotic orbits experience near the outer KAM tori offamilies of periodic and quasiperiodic orbits. This "stickiness" hasbeen discussed extensively in the literature. The phase-space clumpinessproduced by this "stickiness" may help to explain the "moving groups"found in the solar vicinity and the non-Gaussian velocity distributionsobserved at the Galactic poles. Also, the "confinement" of the chaoticorbits by a 1:1 resonant family of tube orbits, which passes a few kpcabove the Sun, may explain part of the halo duality which has beendetected in several studies, such as those of Hartwick (1987, in TheGalaxy, eds. G.Gilmore & B. Carswell. Reidel, dordrecht, 281) and ofKinman et al. (1994AJ....108.1722K). Histograms of the observed |W'|velocity and of the calculated orbital parameter z_max_ have beenplotted for the 280 halo stars. Structure is seen in both histograms,due mainly to the chaotic orbits; the |W'| histogram is non-Gaussianwith two peaks, and the z_max_ histogram has three peaks. Remarkably thestructure in these two histograms is correlated and can be explained inrelation to the details of the surfaces of section and the "confinement"and "stickiness" phenomena of the chaotic orbits.
| Vitesses radiales. Catalogue WEB: Wilson Evans Batten. Subtittle: Radial velocities: The Wilson-Evans-Batten catalogue.
We give a common version of the two catalogues of Mean Radial Velocitiesby Wilson (1963) and Evans (1978) to which we have added the catalogueof spectroscopic binary systems (Batten et al. 1989). For each star,when possible, we give: 1) an acronym to enter SIMBAD (Set ofIdentifications Measurements and Bibliography for Astronomical Data) ofthe CDS (Centre de Donnees Astronomiques de Strasbourg). 2) the numberHIC of the HIPPARCOS catalogue (Turon 1992). 3) the CCDM number(Catalogue des Composantes des etoiles Doubles et Multiples) byDommanget & Nys (1994). For the cluster stars, a precise study hasbeen done, on the identificator numbers. Numerous remarks point out theproblems we have had to deal with.
| Ca II H and K Filter Photometry on the UVBY System. II. The Catalog of Observations
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995AJ....109.2828T&db_key=AST
| The general catalogue of trigonometric [stellar] paralaxes
Not Available
| Subdwarf Studies. III. The Halo Metallicity Distribution
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1991AJ....101.1865R&db_key=AST
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| Takýmyýldýz: | Pupa |
| Sað Açýklýk: | 07h34m18.60s |
| Yükselim: | -45°16'43.1" |
| Görünürdeki Parlaklýk: | 10.483 |
| özdevim Sað Açýklýk: | -310.2 |
| özdevim Yükselim: | 443.4 |
| B-T magnitude: | 11.284 |
| V-T magnitude: | 10.55 |
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