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The N2K Consortium. VI. Doppler Shifts without Templates and Three New Short-Period Planets
We present a modification to the iodine cell Doppler technique thateliminates the need for an observed stellar template spectrum. For agiven target star, we iterate toward a synthetic template spectrumbeginning with an existing template of a similar star. We then perturbthe shape of this first-guess template to match the program observationof the target star taken through an iodine cell. The elimination of aseparate template observation saves valuable telescope time, a featurethat is ideally suited for the quick-look strategy employed by the``Next 2000 Stars'' (N2K) planet search program. Tests using Keck HIRES(High Resolution Echelle Spectrometer) spectra indicate that synthetictemplates yield a short-term precision of 3 m s-1 and along-term, run-to-run precision of 5 m s-1. We used this newDoppler technique to discover three new planets: a 1.50MJplanet in a 2.1375 day orbit around HD 86081; a 0.71MJ planetin circular, 26.73 day orbit around HD 224693; and a Saturn-mass planetin an 18.179 day orbit around HD 33283. The remarkably short period ofHD 86081b bridges the gap between the extremely short period planetsdetected in the Optical Gravitational Lensing Experiment (OGLE) surveyand the 16 Doppler-detected hot Jupiters (P < 15 days), which have anorbital period distribution that piles up at about 3 days. We haveacquired photometric observations of two of the planetary host starswith the automated photometric telescopes at Fairborn Observatory. HD86081 and HD 224693 both lack detectable brightness variability on theirradial velocity periods, supporting planetary-reflex motion as the causeof the radial velocity variability. HD 86081 shows no evidence ofplanetary transits in spite of a 17.6% transit probability. We have toofew photometric observations to detect or rule out transits for HD224693.Based on observations obtained at the W. M. Keck Observatory, which isoperated jointly by the University of California and the CaliforniaInstitute of Technology.
| 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
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| Takýmyýldýz: | Altilik |
| Sað Açýklýk: | 09h46m43.20s |
| Yükselim: | -03°12'40.9" |
| Görünürdeki Parlaklýk: | 7.504 |
| Uzaklýk: | 73.692 parsek |
| özdevim Sað Açýklýk: | -15.7 |
| özdevim Yükselim: | 56.7 |
| B-T magnitude: | 7.936 |
| V-T magnitude: | 7.54 |
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