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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
| NICS-TNG infrared spectroscopy of trans-neptunian objects 2000 EB173 and 2000 WR106
We report complete near-infrared (0.9-2.4 mu m) spectral observations oftrans-neptunian objects (TNOs) 2000 EB173 and 2000 WR106 collected usingthe new Near Infrared Camera Spectrometer (NICS) attached to the 3.56 mTelescopio Nazionale Galileo (TNG). Both spectra are very red and with aquite strong and broad drop extending throughout the K band. However,while 2000 EB173 does not show any evidence of narrow absorptionfeatures, the spectrum of 2000 WR106 has quite deep water ice absorptionat 1.5 and 2.0 mu m. Moreover, the latter object is significantly lessred than the former indicating, therefore, that the surface of 2000WR106 is ``cleaner'' (i.e. less processed by particle irradiation) thanthat of 2000 EB173.
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| Takýmyýldýz: | Kral-Sefe |
| Sað Açýklýk: | 20h36m36.97s |
| Yükselim: | +62°25'55.1" |
| Görünürdeki Parlaklýk: | 7.857 |
| Uzaklýk: | 178.891 parsek |
| özdevim Sað Açýklýk: | 8.2 |
| özdevim Yükselim: | 12.2 |
| B-T magnitude: | 8.333 |
| V-T magnitude: | 7.897 |
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