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Chemical Compositions of Thin-disk, High-metallicity Red Horizontal-branch Field Stars
We present a detailed abundance analysis and atmospheric parameters of76 stars from a survey to identify field Galactic red horizontal-branch(RHB) stars. High-resolution echelle spectra (R ~= 60,000, S/N >=100) were obtained with the 2.7 m Harlan J. Smith Telescope at McDonaldObservatory. The target stars were selected only by color and parallaxinformation. Overall metallicities and relative abundances ofproton-capture elements (C, N, O, Li), α-elements (Ca and Si), andneutron-capture elements (Eu and La) were determined by eitherequivalent width or synthetic spectrum analyses. We used CN features atthe λλ7995-8040 region in order to determine the12C/13C ratios of our targets. Investigation ofthe evolutionary stages, using spectroscopic T eff and log gvalues along with derived 12C/13C ratios, revealedthe presence of 18 probable RHB stars in our sample. We also derivedkinematics of the stars with available distance information. Taking intoaccount both the kinematics and probable evolutionary stages, weconclude that our sample contains 5 thick-disk and 13 thin-disk RHBstars. Up until now, RHB stars have been considered as members of thethick disk, and were expected to have large space velocities andsub-solar metallicities. However, our sample is dominated bylow-velocity solar-metallicity RHB stars; their existence cannot beeasily explained with standard stellar evolution.
| Bayesian inference of stellar parameters and interstellar extinction using parallaxes and multiband photometry
Astrometric surveys provide the opportunity to measure the absolutemagnitudes of large numbers of stars, but only if the individualline-of-sight extinctions are known. Unfortunately, extinction is highlydegenerate with stellar effective temperature when estimated frombroad-band optical/infrared photometry. To address this problem, Iintroduce a Bayesian method for estimating the intrinsic parameters of astar and its line-of-sight extinction. It uses both photometry andparallaxes in a self-consistent manner in order to provide anon-parametric posterior probability distribution over the parameters.The method makes explicit use of domain knowledge by employing theHertzsprung-Russell Diagram (HRD) to constrain solutions and to ensurethat they respect stellar physics. I first demonstrate this method byusing it to estimate effective temperature and extinction from BVJHKdata for a set of artificially reddened Hipparcos stars, for whichaccurate effective temperatures have been estimated from high-resolutionspectroscopy. Using just the four colours, we see the expected strongdegeneracy (positive correlation) between the temperature andextinction. Introducing the parallax, apparent magnitude and the HRDreduces this degeneracy and improves both the precision (reduces theerror bars) and the accuracy of the parameter estimates, the latter byabout 35 per cent. The resulting accuracy is about 200 K in temperatureand 0.2 mag in extinction. I then apply the method to estimate theseparameters and absolute magnitudes for some 47 000 F, G, K Hipparcosstars which have been cross-matched with Two-Micron All-Sky Survey(2MASS). The method can easily be extended to incorporate the estimationof other parameters, in particular metallicity and surface gravity,making it particularly suitable for the analysis of the 109stars from Gaia.
| Objective-Prism Spectral Classifications of Northern Proper-Motion Stars
Improved spectral classifications are given for 23 fairly brightnorthern stars of large or intermediate proper motion, usingmoderate-dispersion objective-prism plates taken with the BurrellSchmidt telescope. Most are classified as early K dwarfs, 10 for thefirst time.
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Pozíciós és asztrometriai adatok
| Csillagkép: | Sárkány |
| Rektaszcenzió: | 16h45m13.71s |
| Deklináció: | +72°49'34.3" |
| Vizuális fényesség: | 8.926 |
| Távolság: | 129.702 parszek |
| RA sajátmozgás: | -47.6 |
| Dec sajátmozgás: | 120 |
| B-T magnitude: | 9.839 |
| V-T magnitude: | 9.002 |
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