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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.
| Boron Benchmarks for the Galactic Disk
Sixteen Population I solar-type dwarfs have been selected to ascertainthe baseline B abundance in the Galactic disk for a range of a factor of4 in metallicity: from [Fe/H] of -0.5 to +0.1. All the stars selectedare undepleted in Be, which ensures that they have also retained theirfull initial abundance of B. Evaluation of the trend of B with Feprovides a means to study the evolution of B in the Galactic disk. Weobserved 16 bright stars around the B I 2497 Å line, using theSTIS echelle spectrograph on HST. New observations of Li and Be in somestars were made, and previous abundance studies of Li and Be in thesestars were reevaluated using revised parameters and a modified spectralsynthesis code for consistency with the B measurements. Abundances of Bwere calculated by spectrum synthesis with the revised MOOG code, whichaccounts for the increased opacity in the UV due to metals; the LTE Babundances were then corrected for non-LTE effects. Four additionalstars with undepleted Be have HST B observations, which increase oursample to 20. For these disk stars there is a shallow slope for B versusFe and Be versus Fe, such that as Fe increases by a factor of 4, B andBe increase by 1.7 times. The slope for BLTE versus Fe is0.31+/-0.09, for BNLTE versus Fe 0.40+/-0.12, and for Beversus Fe 0.38+/-0.14. We have estimated the effect of additional UVopacity from Mg and find that an increase of 0.3 dex in Mg results in ahigher B abundances by 0.1 dex for all the disk stars. Individual starsare not consistently above (or below) the mean in both B and Be,implying that the star-to-star differences are not due to variations inthe elemental content of the ``natal'' clouds. We find that the trend ofB abundance with [Fe/H] is consistent with the general trend observed inhalo stars. If we connect the halo and disk stars, then an increase inthe Fe abundance by 103 is accompanied by increases of 100times in B and 550 times in Be. However, fitting two separate relationsfor the disk and the halo stars results in a somewhat steeper slope forBe for the halo stars (1.08+/-0.07) relative to the disk stars(0.38+/-0.14). This is the case for B also in LTE, with Bhalo(0.90+/-0.07) versus Bdisk (0.32+/-0.12). However, the NLTE Babundance increases more slowly for halo stars than the Be abundancedoes; since this is not predicted by light-element synthesis ordepletion, we suggest that a full NLTE analysis would be preferable tomaking the (small) corrections to the LTE abundances. Some of the lowestmetallicity stars are thought to have only upper limits on the Babundance; if that is the case, the NLTE B slope is steeper, nearing1.0. The abundance of B in the disk stars is observed to be a factor of~15+7-5 more than the abundance of Be in thesestars, a result consistent with the predictions of Galactic cosmic-ray(GCR) spallation, B/Be=15+/-5. The upper envelope for Li versus Feyields Li/B and Li/Be ratios that, when coupled with models andpredictions, indicate that 20%-45% of Li might be produced by GCRs.While there is no evidence to support the production of B by neutrinospallation, we cannot rule it out.Based on observations obtained with the NASA/ESA Hubble Space Telescope(HST) through the Space Telescope Science Institute, which is operatedby the Association of Universities for Research in Astronomy, Inc.,under NASA contract NAS5-26555.
| The Brown Dwarf Desert at 75-1200 AU
We present results of a comprehensive infrared coronagraphic search forsubstellar companions to nearby stars. The research consisted of (1) a178-star survey at Steward and Lick observatories, with opticalfollow-up from Keck Observatory, capable of detecting companions withmasses greater than 30 MJ, and semimajor axes between about140 to 1200 AU; (2) a 102-star survey using the Keck Telescope, capableof detecting extrasolar brown dwarfs and planets typically more massivethan 10 MJ, with semimajor axes between about 75 and 300 AU.Only one brown dwarf companion was detected, and no planets. Thefrequency of brown dwarf companions to G, K, and M stars orbitingbetween 75 and 300 AU is measured to be 1%+/-1%, the most precisemeasurement of this quantity to date. The frequency of massive (greaterthan 30 MJ) brown dwarf companions at 120-1200 AU is found tobe f=0.7%+/-0.7%. The frequency of giant planet companions with massesbetween 5 and 10 MJ orbiting between 75 and 300 AU ismeasured here for the first time to be no more than ~3%. Together withother surveys that encompass a wide range of orbital separations, theseresults imply that substellar objects with masses between 12 and 75MJ form only rarely as companions to stars. Theories of starformation that could explain these data are only now beginning toemerge.
| 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
| HIPPARCOS age-metallicity relation of the solar neighbourhood disc stars
We derive age-metallicity relations (AMRs) and orbital parameters forthe 1658 solar neighbourhood stars to which accurate distances aremeasured by the HIPPARCOS satellite. The sample stars comprise 1382 thindisc stars, 229 thick disc stars, and 47 halo stars according to theirorbital parameters. We find a considerable scatter for thin disc AMRalong the one-zone Galactic chemical evolution (GCE) model. Orbits andmetallicities of thin disc stars show now clear relation each other. Thescatter along the AMR exists even if the stars with the same orbits areselected. We examine simple extension of one-zone GCE models whichaccount for inhomogeneity in the effective yield and inhomogeneous starformation rate in the Galaxy. Both extensions of the one-zone GCE modelcannot account for the scatter in age - [Fe/H] - [Ca/Fe] relationsimultaneously. We conclude, therefore, that the scatter along the thindisc AMR is an essential feature in the formation and evolution of theGalaxy. The AMR for thick disc stars shows that the star formationterminated 8 Gyr ago in the thick disc. As already reported by Grattonet al. (\cite{Gratton_et.al.2000}) and Prochaska et al.(\cite{Prochaska_et.al.2000}), thick disc stars are more Ca-rich thanthin disc stars with the same [Fe/H]. We find that thick disc stars showa vertical abundance gradient. These three facts, the AMR, verticalgradient, and [Ca/Fe]-[Fe/H] relation, support monolithic collapseand/or accretion of satellite dwarf galaxies as likely thick discformation scenarios. Tables 2 and 3 are only available in electronicform at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5)or via http:/ /cdsweb.u-strasbg.fr/ cgi-bin/qcat?J/ A+A/394/927
| Rotational velocities of A-type stars in the northern hemisphere. II. Measurement of v sin i
This work is the second part of the set of measurements of v sin i forA-type stars, begun by Royer et al. (\cite{Ror_02a}). Spectra of 249 B8to F2-type stars brighter than V=7 have been collected at Observatoirede Haute-Provence (OHP). Fourier transforms of several line profiles inthe range 4200-4600 Å are used to derive v sin i from thefrequency of the first zero. Statistical analysis of the sampleindicates that measurement error mainly depends on v sin i and thisrelative error of the rotational velocity is found to be about 5% onaverage. The systematic shift with respect to standard values fromSlettebak et al. (\cite{Slk_75}), previously found in the first paper,is here confirmed. Comparisons with data from the literature agree withour findings: v sin i values from Slettebak et al. are underestimatedand the relation between both scales follows a linear law ensuremath vsin inew = 1.03 v sin iold+7.7. Finally, thesedata are combined with those from the previous paper (Royer et al.\cite{Ror_02a}), together with the catalogue of Abt & Morrell(\cite{AbtMol95}). The resulting sample includes some 2150 stars withhomogenized rotational velocities. Based on observations made atObservatoire de Haute Provence (CNRS), France. Tables \ref{results} and\ref{merging} are only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.125.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/393/897
| Photoelectric observations of the complex low-amplitude red variable, UX Dra
Photoelectric V-band observations of the carbon star and low- amplitudevariable UX Dra show periods of 175+/-1 and 334+/-2 days when combinedwith the Hipparcos data. The 175 day period is very stable over 11 yearsbut the longer period shows some variation.
| The use of modern catalogue data for variable star comparisons: a practical investigation
Visual and photometric V band light curves are compared. The visual dataare recalibrated using the Johnson V magnitudes contained in the TychoCatalogue and the effect of this substitution assessed. The exerciseemphasises the fact that modern catalogue data is too contextual in itsnature to be plucked from its source and forced into service on anarbitrary basis.
| The ROSAT all-sky survey catalogue of optically bright main-sequence stars and subgiant stars
We present X-ray data for all main-sequence and subgiant stars ofspectral types A, F, G, and K and luminosity classes IV and V listed inthe Bright Star Catalogue that have been detected as X-ray sources inthe ROSAT all-sky survey; several stars without luminosity class arealso included. The catalogue contains 980 entries yielding an averagedetection rate of 32 percent. In addition to count rates, sourcedetection parameters, hardness ratios, and X-ray fluxes we also listX-ray luminosities derived from Hipparcos parallaxes. The catalogue isalso available in electronic form via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| A catalogue of [Fe/H] determinations: 1996 edition
A fifth Edition of the Catalogue of [Fe/H] determinations is presentedherewith. It contains 5946 determinations for 3247 stars, including 751stars in 84 associations, clusters or galaxies. The literature iscomplete up to December 1995. The 700 bibliographical referencescorrespond to [Fe/H] determinations obtained from high resolutionspectroscopic observations and detailed analyses, most of them carriedout with the help of model-atmospheres. The Catalogue is made up ofthree formatted files: File 1: field stars, File 2: stars in galacticassociations and clusters, and stars in SMC, LMC, M33, File 3: numberedlist of bibliographical references The three files are only available inelectronic form at the Centre de Donnees Stellaires in Strasbourg, viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5), or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Identification of a complete sample of northern ROSAT All-Sky Survey X-ray sources. II. The optical observations
We describe a program for the optical identification of a representativesample of RASS sources contained in six study areas north of delta = -9deg, with |bII| >~ 20 deg including one region near theNorth Galactic pole (NGP) and one near the North Ecliptic pole (NEP) andpresent some preliminary results. A full identification has been carriedout for a count-rate and area-limited complete subsample comprising 674sources. The ratio of ``extragalactic'' ( e.g. AGN, clusters ofgalaxies) to ``stellar'' (e.g. coronal emitters, active binaries)counterparts was found to depend on the galactic neutral hydrogen columndensity, NH. In the area near the NGP (low NH)``extragalactic'' counterparts dominate, while in the area with thehighest NH most X-ray sources are identified with stellarcounterparts.
| Observations of Low-amplitude Late-Type Variables
Not Available
| The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995ApJS...99..135A&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.
| A catalogue of Fe/H determinations - 1991 edition
A revised version of the catalog of Fe/H determinations published by G.Cayrel et al. (1985) is presented. The catalog contains 3252 Fe/Hdeterminations for 1676 stars. The literature is complete up to December1990. The catalog includes only Fe/H determinations obtained from highresolution spectroscopic observations based on detailed spectroscopicanalyses, most of them carried out with model atmospheres. The catalogcontains a good number of Fe/H determinations for stars from open andglobular clusters and for some supergiants in the Magellanic Clouds.
| UBV photometry of stars whose positions are accurately known. VI
Results are presented from UBV photometric observations of 1000 stars ofthe Bright Star Catalogue and the faint extension of the FK5.Observations were carried out between July 1987 and December 1990 withthe 40-cm Cassegrain telescope of the Kvistaberg Observatory.
| Lithium in early F dwarfs
The Canada-France-Hawaii telescope and Reticon detector fitted with acoude spectrograph was used to obtain spectra of 7 F0-F5 dwarf stars inorder to determine the Li abundances in early Pop I stars. The spectrawere collected witha 0.11 A resolution at a S/N ratio of 400-600. Thecosmic abundance ratio of Li/H = 1/1 billion was found in a third of thestars observed, i.e., the hottest and youngest objects. Furtherdepletions by factors of 3-10 were detected with 17 percent of thedwarfs, and 53 percent were depleted by factors of 10-150. The objectswere divided into those which were Li-rich and under 2 billion yr oldand those which were older and were depleted by factors of over 40 timesthe cosmic abundance. The oldest stars were most depleted. Curiously,the Li-rich stars had high rotation rates and the Li-poor stars had slowrotation rates, except for the Hyades-like dwarfs, which had low Liabundances and temperatures around 6400 K.
| Spectral classification of the bright F stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1976PASP...88...95C&db_key=AST
| MK Spectral Types for Some Bright F Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1974PASP...86...70C&db_key=AST
| Rotation of evolving A and F stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1972A&A....18..428D&db_key=AST
| Photographic magnitudes of stars brighter than 7m.75 between +75° and +80° declination (Errata: 11 270)
Not Available
| Yerkes actinometry. Zone +73deg to +90deg.
Not Available
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Pozíciós és asztrometriai adatok
| Csillagkép: | Sárkány |
| Rektaszcenzió: | 18h57m57.20s |
| Deklináció: | +77°03'03.0" |
| Vizuális fényesség: | 6.54 |
| Távolság: | 60.753 parszek |
| RA sajátmozgás: | -36.8 |
| Dec sajátmozgás: | -65.4 |
| B-T magnitude: | 7.023 |
| V-T magnitude: | 6.609 |
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