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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.
| Calán-ESO Proper-Motion Catalog
The Calán-ESO Proper-Motion Catalog (CE Catalog) contains 542stars with proper motions >=0.2" yr-1, identified in 14ESO areas in the southern hemisphere. Proper motions were measured fromred IIIa-F plates taken 6-16 yr apart. Comparing the CE catalog with theLuyten and the Luyten half-second catalogs, we find that both sufferfrom incompleteness, which is particularly serious (<~40% complete)for mR>~13, where many of the astrophysically interestingobject can be found. Proper motions, coordinates, estimated magnitudes,and finding charts for all objects in the catalog are provided. Based onplates obtained with the Schmidt Camera operated by ESO at La Silla,Chile. Project 64.H-0318.
| 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
| Lithium in population I subgiants
We present a lithium survey for a sample of 91 Pop. I stars. JHKLphotometry was also obtained for 61 stars in the sample. Besides Liabundances, [Fe/H] values were derived. Thanks to Hipparcos parallaxes,we could infer absolute V magnitudes for our sample stars and were ableto place them on the color-magnitude diagram, which allowed us toconstrain their evolutionary status. Masses and ages were derived formost of the stars by comparison with evolutionary tracks. The sample wasoriginally selected so to include class IV stars later thanspectral-type F0, but, based on the location on the color-magnitudediagram, we found a posteriori that a fraction of the stars (about 20%)are either main sequence stars or evolved giants. As it is the case fordwarfs and giants, a large spread in lithium abundance is present amongthe subgiants in our sample. As expected, the average lithium decreasesas the stars evolve along the subgiant branch; however, there is not aone-to-one relationship between the position on the color-magnitudediagram and lithium abundance, and the observed dispersion is onlypartially explainable as due to a dispersion in mass, metallicity, andage. In particular, a dispersion in lithium is seen among slightlyevolved subgiants with masses close to solar but in the sameevolutionary stage as the G2 IV star beta Hyi. The comparison of thebeta Hyi-like sample with a sample of non evolved solar-like starsindeed suggests that beta Hyi has most likely evolved from a mainsequence Li-rich star, rather than from a Li-poor star (like the Sun)that has dredged-up previously stored lithium. Our sample includesseveral stars that have completed the first-dredge up lithium dilution,but that have not yet evolved to the evolutionary point whereextra-mixing in the giant phase is thought to occur. A large number ofthem have Li abundances considerably below the theoretical predictionsof first dredge-up dilution. We confirm that this is due to the factthat the progenitors of these stars are most likely stars that havedepleted lithium while on the main sequence; the fraction of post-dredgeup Li rich/poor stars, in fact, is consistent with the observeddistribution of Li abundances among stars that have just left the mainsequence. The signature of the second mixing (or RGB extra-mixing)episode is evident in the log n(Li) vs. B-V and log n(Li) vs. M_boldistributions of the stars in the sample; it seems however that theextra-mixing occurs at luminosities lower than predicted by the modelsof Charbonnel (1994). Finally, a few evolved giants are found thatshould have passed the second mixing episode, but that do not show signsof it. At least half of them are spectroscopic binaries. Based onobservations carried out at the European Southern Observatory, La Silla,Chile
| An analysis of nine moving-blusters.
Not Available
| 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
| 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.
| The orbits of moving clusters in the galactic dynamical models
The orbits of nine moving star clusters distinguished by Agekian andOrlov (1984) are studied in the rotationally symmetric field of theGalaxy. The three galactic models are considered: the potentials of Sala(1987), Allen and Martos (1986), Kutuzov and Osipkov (1989). In thefirst model applied to a local galactic region in the solar circlevicinity, the orbit of each star is periodic in the meridional plane.The presence of two streams of the moving clusters is assumed. Thesuperclusters of Sirius and Hyades are connected with these streams. Forthe two latter global galactic models, the orbits of principal stars inthe moving clusters, as well as the ones of the stars which are probablenon-members of clusters are calculated. A typical lifetime of the movingclusters in the galactic field is estimated.
| Evolved GK stars near the sun. I - The old disk population
A sample of nearly two thousand GK giants with intermediate band, (R,I),DDO and Geneva photometry has been assembled. Astrometric data is alsoavailable for most of the stars. The some 800 members of the old diskpopulation in the sample yield accurate luminosities (from two sources),reddening values and chemical abundances from calibrations of thephotometric parameters. Less than one percent of the objects arepeculiar in the sense that the flux distribution is abnormal. Thepeculiarity is signaled by strong CH (and Ba II) and weak CH. The CH+stars are all spectroscopic binaries, probably with white dwarfcompanions, whereas the CH- stars are not. A broad absorption band,centered near 3500 A, is found in the CH+ stars whereas the CH- objectshave a broad emission feature in the same region. The intensity of theseabsorptions and emissions are independent of the intensity of abnormalspectral features. Ten percent of the old disk sample have a heavyelement abundance from one and a half to three times the solar value.The distribution of the heavy element abundances is nearly a normal onewith a peak near solar abundance and ranges three times to one sixthsolar. The distribution of the (U, V) velocities is independent of theheavy element abundance and does not appear to be random. Ten percent ofthe old disk stars show a CN anomaly, equally divided between CN strongand CN weak. Several stars of individual astrometric or astrophysicalimportance are isolated.
| 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.
| Search for Vega-like nearby stars with 12 micron excess
The identification of Vega-like main-sequence stars with 10-micronexcess would permit important measurements of the spatial extent of theradiating material with ground-based telescopes. In fact, 55 of the 548nearby A, F, G, and K dwarfs with IRAS catalog magnitudes at 12 micronsappear to have excess 12-micron flux. However, for only two of thesestars, Beta Pic and Zeta Lep, was it possible, using small-aperturephotometry at 2.2 and 10 microns, to verify that the 12-micron excess iswith high likelihood associated with the star. For the remaining starsthe apparent 12-micron color of the 106 A, F, G, and K stars in theobserving program is only 0.02 mag. Excess flux due to a Vega-like cloudwhich may surround some of the sources in the observing program, likeAlpha Lyrae, is thus typically not detectable at 10 microns.
| H-alpha absolute chromospheric fluxes in G and K dwarfs and subgiants
High resolution, high S/N H-alpha observations for a sample of 85 dwarfsand subgiants of spectral type F8 to K5 are presented. A calibrationprocedure to convert the observed equivalent widths to absolute fluxesat the stellar surface is developed and these fluxes are compared withthose obtained in the Ca II K line are compared. Within the observedrange of spectral types there is some evidence that the ratio of H-alphato Ca II K line fluxes increases toward cooler stars, suggesting thatthis effect, which is prominent in M dwarfs, is already significant forK stars. For G and early K stars the H-alpha flux is found to increasewith increasing activity more slowly than the Ca II K flux, givingflux-flux relationships that are similar to those observed for solarplages. It is also found that all subgiants in the sample have very lowH-alpha fluxes, typically lower than for dwarfs of the same spectraltype. The survey clearly shows that the H-alpha line, although being auseful diagnostic of stellar chromospheres, and easily accessible tomodern solid-state detectors, is not particularly suitable for anaccurate determination of absolute chromospheric fluxes.
| Walraven photometry of nearby southern OB associations
Homogeneous Walraven (VBLUW) photometry is presented for 5260 stars inthe regions of five nearby southern OB associations: Scorpio Centaurus(Sco OB2), Orion OB1, Canis Major OB1, Monoceros OB1, and Scutum OB2.Derived V and (B - V) in the Johnson system are included.
| 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.
| Chromospheric and transition-region emission from young solar-type stars in clusters, kinematic groups, and the field
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1987AJ.....93..920S&db_key=AST
| DDO Observations of Southern Stars
Not Available
| VRI photometry of nearby stars.
Not Available
| Some Cross-Reference Lists for the Catalog of Possible Nearby Stars
Not Available
| Luminosities, Temperatures, and Kinematics of K-Type Dwarfs
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1971ApJS...22..389E&db_key=AST
| Narrow-Band and Broad-Band Photometry of Red Stars. III. Southern Giants
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1970ApJ...161..199E&db_key=AST
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Observation and Astrometry data
| Constellation: | Centaurus |
| Right ascension: | 13h53m52.20s |
| Declination: | -35°18'52.0" |
| Apparent magnitude: | 6.19 |
| Distance: | 64.392 parsecs |
| Proper motion RA: | -293.4 |
| Proper motion Dec: | -68.6 |
| B-T magnitude: | 7.471 |
| V-T magnitude: | 6.293 |
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