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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.
| 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
| A new UBV and proper motion survey in the anticentre direction at intermediate galactic latitude: Kinematics of the Galaxy's stellar populations
We present the results from a new complete absolute proper motion surveyin the direction of intermediate galactic latitude (L = 167.5 deg, b =47.4 deg) with respect to background galaxies and quasars, using a setof Tautenburg and OCA (Observatoire de la Cote d'Azur) Schmidt plates,obtained at different epochs separated by approximately 25 years.Photometric U, B and V survey has been done for 4167 objects covering18.8 square degree field and proper motions have been calculated for1888 objects for a 8.6 deg2 area. The resulting catalogs arecomplete down to V = 17, B = 19 and U = 16.5. An average proper motionaccuracy of 0.25 sec per century was achieved for stars brighter than V= 16, with the uncertainties increasing to approximately 0.4 sec percentury at V greater than 16. The photometric accuracy ranges between0.07 to 0.10 in the three bands. We utilize our photometric and absoluteproper motions data to investigate the structure and kinematics of theGalaxy. We have determined ultraviolet excesses and distances for asub-sample of 2685 stars in the color range 0.3 less than or equal to(B-V) less than or equal to 0.9 and with V less than or equal to 17.Thus we have been able to probe the kinematical distribution of F andG-type stars to distances up to 3.5 kpc from the plane. We obtain avalue -0.21 +/- 0.1/kpc for the galactic radial gradient of velocitydispersion. By comparing the ratio of stars in this direction to thenumber of stars towards galactic center at intermediate latitude (l =3deg, b = 47 deg), give a strong evidence that the scale length of olddisk is rather short (2-2.5 kpc). Because of the kinematical biasesinherent in our data sample, we can not present definite kinematicalparameters for the intermediate population, but reasonable estimateswould be an asymmetric drift of 57 +/- 4 km/s and velocity dispersion of60 +/- 3 km/s at a mean distance (above the plane) of z = 2 kpc.
| Hyades and Sirius supercluster members brighter than magnitude (V) 7.1. II - Right ascension six to twelve hours
The present star sample is contained in the Bright Star Catalogue andits Supplement, augmented with a further supplement of 788 stars foundduring various observing programs over the past 40 years. Accurate,four-color and H-beta, or (RI), photometry is available for most of thesupercluster members. The criteria for membership are the comparisons ofthe proper motion, radial velocity, and luminosity obtained from thesupercluster parameters with the observed motions and the luminosityderived from the photometric parameters. New proper motions, based onall available catalogs, have been derived for the additional 788 starsdiscussed here, as well as all supercluster members.
| A catalogue of four-color photometry of late F-type stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1969AJ.....74..705P&db_key=AST
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| Takýmyýldýz: | Buyuk Ayi |
| Sað Açýklýk: | 09h35m50.73s |
| Yükselim: | +48°29'29.8" |
| Görünürdeki Parlaklýk: | 7.03 |
| Uzaklýk: | 93.897 parsek |
| özdevim Sað Açýklýk: | -47.6 |
| özdevim Yükselim: | 23.8 |
| B-T magnitude: | 7.55 |
| V-T magnitude: | 7.073 |
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