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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.
| 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
| Non-radial pulsation of the δ Scuti star UV Trianguli
We present the results of a three-year photometric study of the δScuti star UV Trianguli. Our data sets consist of 9378 differentialmeasurements in Johnson V together with a few data collected into theStrömgren uvbyβ system. UV Tri is at least a biperiodicvariable. The two best-fitting frequencies, f1= 9.3298d-1 and f2= 10.8513 d-1, are still notthe complete set of pulsation frequencies representing the lightvariations of the star. A suspected third frequency might present in thestar. Several `anomalous cycles' are observed in the light curves. Theyseem real, but are aperiodic. We derive the colour indices and physicalparameters for the variable and conclude that it is a Population Iδ Sct star with normal metal abundance ([Me/H]= 0.0 +/- 0.1 dex)evolving on its main-sequence stage at an early evolutionary phasebefore the turn-off point. Finally, we compare the observed oscillationfrequencies with theoretical models. The two pulsation modes of UV Triare likely to be non-radial gravity modes.
| Photometric Observations of the δ Scuti Star UV Trianguli and its Evolutionary Status
UV Tri was observed photometrically from 1999 to 2000 at the XinglongStation of the National Astronomical Observatories, Chinese Academy ofSciences, and was also observed with Strömgren uvbyHβ filter system at the Sierra Nevada Observatory(Spain) in 2000. From period analyses of the data, three pulsationfrequencies, 9.3299 c d-1, 10.8483 c d-1 and3.6035 c d-1 were obtained. We derived color indices: b-y =0.215, m1 = 0.169, c1 = 0.783, and β = 2.775.With these indices and some calibrations, we obtain: Mv =2.44, Mbol = 2.27, logL /Lȯ = 0.99, and logTeff = 3.875. Evolutionary sequences of stellar models with1.00-2.00 solar masses, at steps of 0.05 Msun, are computed. Eachsequence consists of 220 evolutionary intervals. From a comparisonbetween the observed and calculated physical parameters we conclude thatUV Tri is in an early evolutionary phase before the turn-off point.
| 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 galactic foreground reddening in the direction of the nearby triangulum galaxy M33
Observations of 314 stars with the uvby-beta photometric system are usedto establish the reddening in the direction of the nearby Triangulumgalaxy M33. Color excesses are obtained for 151 A and F type stars in a1 deg radius centered around the galaxy. A color excess of E(b-y) =0.057 mag /E(B-V) = 0.077 mag/ is obtained for a distance modulus m - M= 10. A secondary result of this investigation is the discovery of sixsuspected variable stars, as well as ten observations of V Triangulum, aBeta Lyrae eclipsing variable.
| Catalog of Indidual Radial Velocities, 0h-12h, Measured by Astronomers of the Mount Wilson Observatory
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1970ApJS...19..387A&db_key=AST
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Datos observacionales y astrométricos
| Constelación: | Piscis, Peces |
| Ascensión Recta: | 01h27m29.93s |
| Declinación: | +30°30'42.0" |
| Magnitud Aparente: | 7.977 |
| Distancia: | 89.445 parsecs |
| Movimiento Propio en Ascensión Recta: | 79.5 |
| Movimiento Propio en Declinación: | 8.2 |
| B-T magnitude: | 8.491 |
| V-T magnitude: | 8.02 |
Catálogos y designaciones:
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