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Pulkovo compilation of radial velocities for 35495 stars in a common system.
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| Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc-The Southern Sample
We are obtaining spectra, spectral types, and basic physical parametersfor the nearly 3600 dwarf and giant stars earlier than M0 in theHipparcos catalog within 40 pc of the Sun. Here we report on resultsfor 1676 stars in the southern hemisphere observed at Cerro TololoInter-American Observatory and Steward Observatory. These resultsinclude new, precise, homogeneous spectral types, basic physicalparameters (including the effective temperature, surface gravity, andmetallicity [M/H]), and measures of the chromospheric activity of ourprogram stars. We include notes on astrophysically interesting stars inthis sample, the metallicity distribution of the solar neighborhood, anda table of solar analogs. We also demonstrate that the bimodal nature ofthe distribution of the chromospheric activity parameterlogR'HK depends strongly on the metallicity, andwe explore the nature of the ``low-metallicity'' chromosphericallyactive K-type dwarfs.
| 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.
| Multiplicity among solar-type stars. III. Statistical properties of the F7-K binaries with periods up to 10 years
Two CORAVEL radial velocity surveys - one among stars in the solarneighbourhood, the other in the Pleiades and in Praesepe - are merged toderive the statistical properties of main-sequence binaries withspectral types F7 to K and with periods up to 10 years. A sample of 89spectroscopic orbits was finally obtained. Among them, 52 relate to afree-of-bias selection of 405 stars (240 field stars and 165 clusterstars). The statistics corrected for selection effects yield thefollowing results: (1) No discrepancy is found between the binariesamong field stars and the binaries in open cluster. The distributions ofmass ratios, of periods, the period-eccentricity diagram and the binaryfrequencies are all within the same error intervals. (2) Thedistribution of mass ratios presents two maxima: a broad peak from q ~0.2 to q ~ 0.7, and a sharp peak for q > 0.8 (twins). Both arepresent among the early-type as well as among the late-type part of thesample, indicating a scale-free formation process. The peak for q >0.8 gradually decreases when long-period binaries are considered.Whatever their periods, the twins have eccentricities significantlylower than the other binaries, confirming a difference in the formationprocesses. Twins could be generated by in situ formation followed byaccretion from a gaseous envelope, whereas binaries with intermediatemass ratios could be formed at wide separations, but they are madecloser by migration led by interactions with a circumbinary disk. (3)The frequency of binaries with P<10 years is about 14%. (4) About0.3% of binaries are expected to appear as false positives in a planetsearch. Therefore, the frequency of planetary systems among stars ispresently 7+4-2%. The extension of thedistribution of mass ratios in the planetary range would result in avery sharp and very high peak, well separated from the binary stars withlow mass ratios. Based on photoelectric radial-velocity measurementscollected at Haute-Provence observatory and on observations made withthe ESA Hipparcos astrometry satellite.
| 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.
| Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics
The Catalogue, available at the Centre de Données Stellaires deStrasbourg, consists of 13 573 records concerning the results obtainedfrom different methods for 7778 stars, reported in the literature. Thefollowing data are listed for each star: identifications, apparentmagnitude, spectral type, apparent diameter in arcsec, absolute radiusin solar units, method of determination, reference, remarks. Commentsand statistics obtained from CADARS are given. The Catalogue isavailable in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcar?J/A+A/367/521
| Homogeneous photometry and metal abundances for a large sample of Hipparcos metal-poor stars*
Homogeneous photometric data (Johnson V, B-V, V-K, Cousins V-I andStrömgren b-y), radial velocities, and abundances of Fe, O, Mg, Si,Ca, Ti, Cr and Ni are presented for 99 stars with high-precisionparallaxes measured by the Hipparcos satellite. These data have beenpreviously used to assist the derivation of accurate distances and agesof Galactic globular clusters. Magnitudes and colours for the programmestars were obtained by combining and standardizing carefully selectedliterature data available in the Simbad data base, and V and B-V valuesmeasured by the Hipparcos/Tycho mission. Comparison of colours for ourtargets suggests: (i) ground-based and Tycho B-V values agree well forcolours bluer than 0.75 mag, but have a lot of scatter for reddercolours; (ii) the Hipparcos V-I colours have a very large scatter and azero-point offset of +0.02 mag compared to the literature values.The programme stars have metal abundances in the range-2.5<[Fe/H]<0.2. The spectroscopic observational data set consistsof high-dispersion (15 000200) spectraobtained at the Asiago and McDonald Observatories for 66 stars. Theanalysis is carried out following the same precepts as those used inprevious papers of this series, and includes corrections for departuresfrom LTE in the formation of the O lines. The main results are: (i) theequilibrium of ionization of Fe is well satisfied in late F-early Kdwarfs; (ii) oxygen and α-elements are overabundant by ~0.3 dex.This large homogeneous abundance data set has been used to recalibratethe abundance scales of Schuster & Nissen, Ryan & Norris andCarney et al. (1994).
| Ages of Globular Clusters from HIPPARCOS Parallaxes of Local Subdwarfs
We report here initial but strongly conclusive results for absolute agesof Galactic globular clusters (GGCs). This study is based onhigh-precision trigonometric parallaxes from the HIPPARCOS satellitecoupled with accurate metal abundances ([Fe/H], [O/Fe], and [ alpha/Fe]) from high-resolution spectroscopy for a sample of about thirtysubdwarfs. Systematic effects due to star selection (Lutz-Kelkercorrections to parallaxes) and the possible presence of undetectedbinaries in the sample of bona fide single stars are examined, andappropriate corrections are estimated. They are found to be small forour sample. The new data allow us to reliably define the absolutelocation of the main sequence (MS) as a function of metallicity. Theseresults are then used to derive distances and ages for a carefullyselected sample of nine globular clusters having metallicitiesdetermined from high-dispersion spectra of individual giants accordingto a procedure totally consistent with that used for the fieldsubdwarfs. Very precise and homogeneous reddening values have also beenindependently determined for these clusters. Random errors for ourdistance moduli are +/-0.08 mag, and systematic errors are likely of thesame order of magnitude. These very accurate distances allow us toderive ages with internal errors of ~12% (+/-1.5 Gyr). The main resultsare: 1. HIPPARCOS parallaxes are smaller than corresponding ground-basedmeasurements, leading, in turn, to longer distance moduli (~0.2 mag) andyounger ages (~2.8 Gyr). 2. The distance to NGC 6752 derived from our MSfitting is consistent with that determined using the white dwarf coolingsequence. 3. The relation between the zero-age HB (ZAHB) absolutemagnitude and metallicity for the nine program clusters isMV({ZAHB})=(0.22+/-0.09)([{Fe}/{H}]+1.5)+(0.49+/-0.04) . Thisrelation is fairly consistent with some of the most recent theoreticalmodels. Within quoted errors, the slope is in agreement with that givenby the Baade-Wesselink (BW) analysis of RR Lyrae stars by Fernley andClementini et al., while it is somewhat shallower than the relationgiven by Sandage. The zero-point is 0.2 to 0.3 mag brighter than thatobtained with BW, while it agrees fairly well with that given bySandage. A comparison with alternative relationships is brieflydiscussed. 4. The corresponding LMC distance modulus is (m - M)0 = 18.60+/- 0.07, in good agreement with the recent values of 18.70 +/- 0.10 and18.54 +/- 0.2 derived by Feast & Catchpole and van Leeuwen et al.,respectively, from HIPPARCOS parallaxes of Galactic Cepheid and Miravariables. 5. The age of the bona fide old globular clusters (OosterhoffII and BHB), based on the absolute magnitude of the turnoff (atheoretically robust indicator) is {Age}=11.8^{+2.1}_{-2.5} {Gyr} ,wherethe error bar is the 95% confidence range. The rms scatter of individualages around the mean value is ~10%, in agreement with expectations fromobservational errors alone (that is, we do not find it necessary tointroduce a real age scatter among these clusters). A reliable study ofthe relative ages requires the use of age indicators better suited tothis purpose and data for a larger sample of GGCs. 6. Allowing for aminimum delay of 0.5 Gyr from the birth of the universe until theformation of globular clusters, our age estimate is compatible with anEinstein-de Sitter model if H0 <= 64 km s-1 Mpc-1, or H0 <= 83 kms-1 Mpc-1 in a flat universe with Omega m = 0.2. Since these upperlimits are well within the confidence range of most determinations ofH0, we conclude that the present age of globular clusters does notconflict with standard inflationary models of the universe.
| The catalogue of nearby stars metallicities.
Not Available
| Classification of Population II Stars in the Vilnius Photometric System. I. Methods
The methods used for classification of Population II stars in theVilnius photometric system are described. An extensive set of standardswith known astrophysical parameters compiled from the literature sourcesis given. These standard stars are classified in the Vilnius photometricsystem using the methods described. The accuracy of classification isevaluated by a comparison of the astrophysical parameters derived fromthe Vilnius photometric system with those estimated from spectroscopicstudies as well as from photometric data in other systems. For dwarfsand subdwarfs, we find a satisfactory agreement between our reddeningsand those estimated in the uvbyscriptstyle beta system. The standarddeviation of [Fe/H] deter mined in the Vilnius system is about 0.2 dex.The absolute magnitude for dwarfs and subdwarfs is estimated with anaccuracy of scriptstyle <=0.5 mag.
| The Age of the Galactic Globular Cluster System
A careful assessment of current uncertainties in stellar physics(opacities, nuclear reaction rates, equation of state effects,diffusion, rotation, and mass loss), in the chemistry of globularcluster (GC) stars, and in the cluster distance scale, suggests that themost metal-poor (presumably the oldest) of the Galaxy's GCs have agesnear 15 Gyr. Ages below 12 Gyr or above 20 Gyr appear to be highlyunlikely. If these {approximately equal to} 2σ limits areincreased by {approximately} 1 Gyr to account for the formation time ofthe globulars, and if standard Friedmann cosmologies with thecosmological constant set to zero are assumed, then the GC constraint onthe present age of the Universe (to > 13 Gyr) implies that the Hubbleconstant Ho <51 km s-1 Mpc-1 if the density parameter Omega = 1 or< than} 62 km s-1 Mpc-1 if Omega = 0.3.
| 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
| Empirical Calibration of Absolute Magnitudes for G-K Dwarfs and Subdwarfs in the Vilnius Photometric System
Calibrations giving l M_V as functions of [Fe/H] and various intrinsiccolor indices of the Vilnius photometric system are derived for G--Kdwarfs and subdwarfs. The calibrations are based only on the stars withknown trigonometric parallaxes and allow one to estimate the absolutemagnitudes with a standard deviation of +/- 0.6 mag. Comparisons of ourcalibrations with the absolute magnitude estimates in the literatureshow a satisfactory agreement.
| The importance of surface inhomogeneities for K and M dwarf chromospheric fluxes
We present published and archived spectroscopic and spectrophotometricdata of H-alpha, Ca II, Mg II, and X-rays for a large sample of K and Mdwarfs. The data set points to the importance that surfaceinhomogeneities have in the flux luminosity diagrams in these late-typedwarfs, irrespective of whether the Balmer lines are in emission orabsorption. Although supporting the fact that cooler stars exhibitincreasing levels of surface activity, evident through an increasingincidence of Balmer emission, surface inhomogeneities, or variations inthe local temperature and density structure, at the chromospheric level,dominate the total Ca II and Mg II fluxes. We show that the flux-fluxand luminosity-luminosity relations indicate differing extents ofinhomogeneity from the chromosphere through to the corona. A goodcorrelation between Ca II and Mg II fluxes indicates that they areformed in overlapping regions of the chromosphere, so that thecontribution of surface inhomogeneities is not evident from thisparticular flux-flux diagram. In the region of the upper chromospherethrough to the transition and corona, the correlation between Ly-alphaand X-ray fluxes indicates regions with similar levels of arealinhomogeneity. This appears to be uncorrelated with that at thechromospheric level.
| Parallaxes and proper motions. XIX - The subdwarf sequence
Parallaxes and proper motions are presented for 19 stars in 15 starfields. Four of the stars were discovered in the course of the measuresto have significantly large proper motions and the data for them areincluded in the tables. The other 15 are all stars considered to besubluminous. Photometric and metallicity data for most of them arepresented. They appear not to conform to a straight linear relationbetween (FE/H) determined from the measured ultraviolet excess and theabsolute magnitude corrected to a B-V color of 0.6.
| BVRI photometry of the Gliese Catalogue stars
Photoelectri BVRI photometry on the Cousins (Kron-Cape) system has beenobtained for many of the southern faint stars in the Gliese Catalog(1969). This extends the work of Cousins (1980) and provides a uniformset of data for the nearby stars. Several red dwarfs are noted, whichwere used to define the red end of the Cousins system.
| H-alpha photometry of dwarf K and M stars - Chromospheric activity
H-alpha photometry of 118 K and M dwarfs are presented, with H-alphaequivalent width measures accurate to about 0.05 A. The data arecombined with the spectroscopic surveys of Stauffer and Hartmann (1986)and Fleming et al. (1988) to study the main features of thechromospheric activity versus mass relation for low-mass stars. An upperbound to the H-alpha equivalent width is found to be a function of themass relation (R-I). H-alpha luminosities and surface fluxes arecalculated for active stars, showing that both quantities generallydecline with R-I. The upper bound to the fraction of a star's bolometricluminosity, however, is independent of R-I. The results suggest that thechromospheres of most dMe stars with R-I less than 1.1 are in anactivity-saturated state. Also, H-alpha variability, probably due toflares, is detected in several stars.
| UBV (RI)c photometry of faint nearby stars.
Not Available
| Luminosities, abundances, and motions of stars brighter than visual magnitude 15.1 and annual proper motions larger than one-half arcsecond
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1987AJ.....93..393E&db_key=AST
| Catalog of proper-motion stars. III - Stars brighter than visual magnitude 15.1, south of declination +30 deg, and with annual proper motion between 0.5 and 0.7 arcsec
A catalog of (VRI) photometry for the some one thousand stars withannual proper motion between 0.5 and 0.7 arcsec, brighter than visualmagnitude 15.1, and south of declination +30 deg is presented. Theavailable proper-motion and radial-velocity data are also summarized.
| Photometry of dwarf K and M stars
Broadband photometry in BVRI colors for 120 nearby dwarf K and M starsis presented. The apparent magnitude distributions of Vyssotsky and VanVleck stars with photometry and without photometry are studied. Therelationship between apparent and photoelectric magnitudes is analyzed.The proper motion and transverse velocity of the two star types areexamined and compared.
| Dwarf K and M stars of high proper motion found in a hemispheric survey
A recently completed visual/red spectral region objective-prism surveyof more than half the sky found some 2200 dwarf K and M stars ofnegligible proper motion (Stephenson, 1986). The present paper adds the1800-odd spectroscopically identified dwarfs that did prove to havesignificant proper motions. About half of these had previous spectralclassifications of some sort, especially by Vyssotsky (1952, 1956). Forthe great majority, the present coordinates are more accurate thanprevious data. The paper includes about 50 stars with unpublishedparallaxes, likely to have parallaxes of 0.05 arcsec or more. Combiningthe present data with the first paper suggests that the number oflow-proper-motion stars in that paper was not unreasonable.
| G. P. Kuiper's spectral classifications of proper-motion stars
Spectral classifications are listed for over 3200 stars, mainly of largeproper motion, observed and classified by Kuiper during the years1937-1944 at the Yerkes and McDonald Observatories. While Kuiper himselfpublished many of his types, and while improved classifications are nowavailable for many of these stars, much of value remains. For many ofthe objects, no other spectral data exist.
| UBVRI photoelectric photometry of nearby stars
In order to complete the photometric data of the Gliese (1969) 'Catalogof Nearby Stars', and in addition use these data for the Hipparcos spaceastrometry mission, program stars have been selected from the catalogand its supplements on the basis of their having an incomplete set ofUBVRI photometric data of magnitude lower than 13. The program developedrejects determinations of any magnitude or color index having a residualgreater than 2(sigma-prime), where sigma-prime is the standard deviationfor the determinations of unit weight.
| Predicted infrared brightness of stars within 25 parsecs of the sun
Procedures are given for transforming selected optical data intoinfrared flux densities or irradiances. The results provide R, T(eff)blackbody approximations for about 2000 of the stars in Woolley et al.'sCatalog of Stars (1970) within 25 pc of the sun, and additional whitedwarfs, with infrared flux densities predicted for them at ninewavelengths from 2.2 to 101 microns including the Infrared AstronomySatellite bands.
| The degree of completeness of nearby stars and the stellar luminosity function
The aim of this study is the determination of the degree of completenessof nearby star catalogs for stars of as many spectral classes aspossible, by means of a novel method which eliminates giants, subgiantsand white dwarfs from the data sample. It is shown that main-sequencestars earlier than M0 are essentially complete and identified withinabout 20 pc of the sun, by determining V/V(max) as a function of B-V forthe main sequence stars. The luminosity function produced by the M0stars has been known to differ from the commonly accepted and smoothedluminosity function, which increases monotonically with absolutemagnitude, between the absolute visual magnitudes +6 and +9. It isconcluded that the deficiency between these magnitude limits is real,suggesting either (1) that stars of masses equivalent to this absolutemagnitude range are rarer than those of greater mass, or (2) that themass-luminosity relation is not as linear as is believed at present.
| Optical polarization of stars of galactic latitudes b-45 degres.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1976A&AS...23..125S&db_key=AST
| Dwarf K and M stars in the southern hemisphere.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1972AJ.....77..486U&db_key=AST
| Photoelectric Three Colour Magnitudes for Southern Stars
Not Available
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Datos observacionales y astrométricos
| Constelación: | Ballena |
| Ascensión Recta: | 01h17m34.03s |
| Declinación: | -15°30'12.0" |
| Magnitud Aparente: | 9.767 |
| Distancia: | 30.139 parsecs |
| Movimiento Propio en Ascensión Recta: | 281.9 |
| Movimiento Propio en Declinación: | -479.6 |
| B-T magnitude: | 10.934 |
| V-T magnitude: | 9.864 |
Catálogos y designaciones:
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