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The Ca II infrared triplet as a stellar activity diagnostic. II. Test and calibration with high resolution observations
Aims.We report on our analysis of the high resolution spectra (R≈86000) of a sample of 42 late-type active stars (with measured{log{R'_HK}} spanning from ≈{ -}3 to ≈{ -}5) acquired with theItalian 3.6 m Telescopio Nazionale Galileo (TNG) using the SARGspectrometer in the 4960-10 110 Å range. The high quality of thespectra and the good activity-level coverage allow us to measure twodifferent chromospheric indicators that can be derived from the Ca iiinfrared triplet (Ca ii IRT) lines: the residual equivalent width (EQW)and the chromospheric indicator {R_IRT}. The aim of this work isdetermine and test the best way of deriving activity-level informationand errors from the Ca ii IRT lines, in preparation of the GAIACornerstone mission by ESA, by which the Ca ii IRT spectral range willbe spectroscopically observed for millions of stars. Methods: The{R_IRT} index is calculated for each observed star as the differencebetween the calculated NLTE photospheric central intensity and theobserved one. The residual EQW, {Δ W_IRT}, is calculated as thearea of the positive profile obtained as the difference between thecalculated NLTE photospheric and the observed profiles. We correlate{log{R'_HK}} with {R_IRT} and the {Δ W_IRT}. Results: Thisanalysis indicates that Ca ii IRT lines are good chromosphericdiagnostics. We find that both {Δ W_IRT} and the {R_IRT}quantities can be used as chromospheric indicators, although the formerexhibits a tighter correlation with the {log{R'_HK}} index. Furthermore,we find that the total chromospheric excess EQW in the Ca ii IRT isalmost linearly correlated with the excess in the Ca ii H & Kdoublet, as estimated through the {log{R'_HK}} index.Based on observations made with the Italian Telescopio Nazionale Galileo(TNG) operated on the island of La Palma by the Centro Galileo Galileiof the Consorzio Nazionale per l'Astronomia e l'Astrofisica at theSpanish Observatorio del Roque de los Muchachos of the Instituto deAstrofísica de Canarias. Table 4 is only available in electronicform at http://www.aanda.org
| Effective temperature scale and bolometric corrections from 2MASS photometry
We present a method to determine effective temperatures, angularsemi-diameters and bolometric corrections for population I and II FGKtype stars based on V and 2MASS IR photometry. Accurate calibration isaccomplished by using a sample of solar analogues, whose averagetemperature is assumed to be equal to the solar effective temperature of5777 K. By taking into account all possible sources of error we estimateassociated uncertainties to better than 1% in effective temperature andin the range 1.0-2.5% in angular semi-diameter for unreddened stars.Comparison of our new temperatures with other determinations extractedfrom the literature indicates, in general, remarkably good agreement.These results suggest that the effective temperaure scale of FGK starsis currently established with an accuracy better than 0.5%-1%. Theapplication of the method to a sample of 10 999 dwarfs in the Hipparcoscatalogue allows us to define temperature and bolometric correction (Kband) calibrations as a function of (V-K), [m/H] and log g. Bolometriccorrections in the V and K bands as a function of T_eff, [m/H] and log gare also given. We provide effective temperatures, angularsemi-diameters, radii and bolometric corrections in the V and K bandsfor the 10 999 FGK stars in our sample with the correspondinguncertainties.
| Synthetic Lick Indices and Detection of α-enhanced Stars. III. F, G, and K Stars with [Fe/H] > 0.00
A sample of 119 F, G, and K solar neighborhood stars, selected under thecondition [Fe/H]>0.00, is investigated in order to detect which ofthem, if any, present α-enhanced characteristics. According to thekinematics, the sample represents stars of the thin-disk component ofthe Galaxy. The search of α-enhanced characteristics is performedby adopting an already tested procedure that does not require previousknowledge of the stellar main atmospheric parameters. The analysis isbased on the comparison of spectral indices in the Lick IDS system,coming from different observational data sets, with synthetic onescomputed with solar-scaled abundances and with α-elementenhancement. The main result of the analysis is the extreme paucity(likely just one in 119) of α-enhanced stars in our sample, thussuggesting [α/Fe]=0.0 for thin-disk stars with [Fe/H]>0.00.This result, which is in agreement with the standard evolutionarypicture of the disk of the Galaxy, is compared with recent results fromhigh-resolution analysis reported in the literature. The role of theatmospheric parameter assumptions in the analysis of high-resolutionspectroscopic data is discussed, and a possible explanation ofdiscrepant results about α-enhancement for stars with[Fe/H]>0.00 is presented.
| A new Böhm-Vitense gap in the temperature range 5560 to 5610 K in the main sequence hm-Vitense gap in the main sequence
Highly precise temperatures (σ = 10-15 K) have been determinedfrom line depth ratios for a set of 248 F-K field dwarfs of about solarmetallicity (-0.5 < [Fe/H] < +0.4), based on high resolution (R=42000), high S/N echelle spectra. A new gap has been discovered in thedistribution of stars on the Main Sequence in the temperature range 5560to 5610 K. This gap coincides with a jump in the microturbulent velocityVt and the well-known Li depression near 5600 K in fielddwarfs and open clusters. As the principal cause of the observeddiscontinuities in stellar properties we propose the penetration of theconvective zone into the inner layers of stars slightly less massivethan the Sun and related to it, a change in the temperature gradient.Based on spectra collected with the ELODIE spectrograph at the 1.93-mtelescope of the Observatoire de Haute-Provence (France).Full Table 1 is only available in electronic form athttp://www.edpsciences.org
| The Indo-US Library of Coudé Feed Stellar Spectra
We have obtained spectra for 1273 stars using the 0.9 m coudéfeed telescope at Kitt Peak National Observatory. This telescope feedsthe coudé spectrograph of the 2.1 m telescope. The spectra havebeen obtained with the no. 5 camera of the coudé spectrograph anda Loral 3K×1K CCD. Two gratings have been used to provide spectralcoverage from 3460 to 9464 Å, at a resolution of ~1 Å FWHMand at an original dispersion of 0.44 Å pixel-1. For885 stars we have complete spectra over the entire 3460 to 9464 Åwavelength region (neglecting small gaps of less than 50 Å), andpartial spectral coverage for the remaining stars. The 1273 stars havebeen selected to provide broad coverage of the atmospheric parametersTeff, logg, and [Fe/H], as well as spectral type. The goal ofthe project is to provide a comprehensive library of stellar spectra foruse in the automated classification of stellar and galaxy spectra and ingalaxy population synthesis. In this paper we discuss thecharacteristics of the spectral library, viz., details of theobservations, data reduction procedures, and selection of stars. We alsopresent a few illustrations of the quality and information available inthe spectra. The first version of the complete spectral library is nowpublicly available from the National Optical Astronomy Observatory(NOAO) via ftp and http.
| The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of 14 000 F and G dwarfs
We present and discuss new determinations of metallicity, rotation, age,kinematics, and Galactic orbits for a complete, magnitude-limited, andkinematically unbiased sample of 16 682 nearby F and G dwarf stars. Our63 000 new, accurate radial-velocity observations for nearly 13 500stars allow identification of most of the binary stars in the sampleand, together with published uvbyβ photometry, Hipparcosparallaxes, Tycho-2 proper motions, and a few earlier radial velocities,complete the kinematic information for 14 139 stars. These high-qualityvelocity data are supplemented by effective temperatures andmetallicities newly derived from recent and/or revised calibrations. Theremaining stars either lack Hipparcos data or have fast rotation. Amajor effort has been devoted to the determination of new isochrone agesfor all stars for which this is possible. Particular attention has beengiven to a realistic treatment of statistical biases and errorestimates, as standard techniques tend to underestimate these effectsand introduce spurious features in the age distributions. Our ages agreewell with those by Edvardsson et al. (\cite{edv93}), despite severalastrophysical and computational improvements since then. We demonstrate,however, how strong observational and theoretical biases cause thedistribution of the observed ages to be very different from that of thetrue age distribution of the sample. Among the many basic relations ofthe Galactic disk that can be reinvestigated from the data presentedhere, we revisit the metallicity distribution of the G dwarfs and theage-metallicity, age-velocity, and metallicity-velocity relations of theSolar neighbourhood. Our first results confirm the lack of metal-poor Gdwarfs relative to closed-box model predictions (the ``G dwarfproblem''), the existence of radial metallicity gradients in the disk,the small change in mean metallicity of the thin disk since itsformation and the substantial scatter in metallicity at all ages, andthe continuing kinematic heating of the thin disk with an efficiencyconsistent with that expected for a combination of spiral arms and giantmolecular clouds. Distinct features in the distribution of the Vcomponent of the space motion are extended in age and metallicity,corresponding to the effects of stochastic spiral waves rather thanclassical moving groups, and may complicate the identification ofthick-disk stars from kinematic criteria. More advanced analyses of thisrich material will require careful simulations of the selection criteriafor the sample and the distribution of observational errors.Based on observations made with the Danish 1.5-m telescope at ESO, LaSilla, Chile, and with the Swiss 1-m telescope at Observatoire deHaute-Provence, France.Complete Tables 1 and 2 are only available in electronic form at the CDSvia anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/418/989
| 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
| The Vienna-KPNO search for Doppler-imaging candidate stars. I. A catalog of stellar-activity indicators for 1058 late-type Hipparcos stars
We present the results from a spectroscopic Ca ii H&K survey of 1058late-type stars selected from a color-limited subsample of the Hipparcoscatalog. Out of these 1058 stars, 371 stars were found to showsignificant H&K emission, most of them previously unknown; 23% withstrong emission, 36% with moderate emission, and 41% with weak emission.These spectra are used to determine absolute H&K emission-linefluxes, radial velocities, and equivalent widths of theluminosity-sensitive Sr ii line at 4077 Ä. Red-wavelengthspectroscopic and Strömgren y photometric follow-up observations ofthe 371 stars with H&K emission are used to additionally determinethe absolute Hα -core flux, the lithium abundance from the Li i6708 Å equivalent width, the rotational velocity vsin i, theradial velocity, and the light variations and its periodicity. Thelatter is interpreted as the stellar rotation period due to aninhomogeneous surface brightness distribution. 156 stars were found withphotometric periods between 0.29 and 64 days, 11 additional systemsshowed quasi-periodic variations possibly in excess of ~50 days. Further54 stars had variations but no unique period was found, and four starswere essentially constant. Altogether, 170 new variable stars werediscovered. Additionally, we found 17 new SB1 (plus 16 new candidates)and 19 new SB2 systems, as well as one definite and two possible new SB3systems. Finally, we present a list of 21 stars that we think are mostsuitable candidates for a detailed study with the Doppler-imagingtechnique. Tables A1--A3 are only available in electronic form at theCDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Abundances in metal-rich stars. Detailed abundance analysis of 47 G and K dwarf stars with [Me/H] > 0.10 dex
We have derived elemental abundances of O, Na, Mg, Al, Si, Ca, Ti, Cr,Mn, Fe, Co, Ni as well as for a number of s-elements for 47 G and Kdwarf, with [Me/H]>0.1 dex. The selection of stars was based on theirkinematics as well as on their uvby-beta photometry. One sample of starson rather eccentric orbits traces the chemical evolution interior to thesolar orbit and another, on circular orbits, the evolution around thesolar orbit. A few Extreme Population I stars were included in thelatter sample. The stars have -0.1 dex < [Fe/H] < 0.42 dex. Thespectroscopic [Fe/H] correlate well with the [Me/H] derived fromuvby-beta photometry. We find that the elemental abundances of Mg, Al,Si, Ca, Ti, Cr and Ni all follow [Fe/H]. Our data put furtherconstraints on models of galactic chemical evolution, in particular ofCr, Mn and Co which have not previously been studied for dwarf starswith [Me/H] >0.1 dex. The increase in [Na/Fe] and [Al/Fe] as afunction of [Fe/H] found previously by \cite[Edvardsson et al.(1993a)]{Edv93} has been confirmed for [Na/Fe]. This upturning relation,and the scatter around it, are shown not to be due to a mixture ofpopulations with different mean distances to the galactic centre. We donot confirm the same trend for aluminium, which is somewhat surprisingsince both these elements are thought to be produced in the sameenvironments in the pre-supernova stars. Nor have we been able to traceany tendency for relative abundances of O, Si, and Ti relative to Fe tovary with the stellar velocities, i.e. the stars present mean distanceto the galactic centre. These results imply that there is no significantdifference in the chemical evolution of the different stellarpopulations for stars with [Me/H]>0.1 dex. We find that [O/Fe]continue to decline with increasing [Fe/H] and that oxygen and europiumcorrelate well. However [Si/Fe] and [Ca/Fe] seem to stay constant. Areal (``cosmic'') scatter in [Ti/Fe] at given [Fe/H] is suggested aswell as a decreasing abundance of the s-elements relative to iron forthe most metal-rich dwarf stars. We discuss our results in the contextof recent models of galactic chemical evolution. In our sample we haveincluded a few very metal rich stars, sometimes called SMR (super metalrich) stars. We find these stars to be among the most iron-rich in oursample but far from as metal-rich as indicated by their photometricmetallicities. SMR stars on highly eccentric orbits, alleged to tracethe evolution of the chemical evolution in the galactic Bulge, havepreviously been found overabundant in O, Mg and Si. We have includedthree such stars from the study by \cite[Barbuy & Grenon(1990)]{Bar90}. We find them to be less metal rich and the otherelemental abundances remain puzzling. Detailed spectroscopic abundanceanalyses of K dwarf stars are rare. Our study includes 5 K dwarf starsand has revealed what appears to be a striking example ofoverionization. The overionization is especially prominent for Ca, Crand Fe. The origin of this apparent overionization is not clear and wediscuss different explanations in some detail. Based on observations atthe McDonald Observatory.
| Stroemgren photometry of F- and G-type stars brighter than V = 9.6. I. UVBY photometry
Within the framework of a large photometric observing program, designedto investigate the Galaxy's structure and evolution, Hβ photometryis being made for about 9000 stars. As a by-product, supplementary uvbyphotometry has been made. The results are presented in a cataloguecontaining 6924 uvby observations of 6190 stars, all south ofδ=+38deg. The overall internal rms errors of one observation(transformed to the standard system) of a program star in the interval6.5
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