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The N2K Consortium. VII. Atmospheric Parameters of 1907 Metal-rich Stars: Finding Planet-Search Targets
We report high-precision atmospheric parameters for 1907 stars in theN2K low-resolution spectroscopic survey, designed to identify metal-richFGK dwarfs likely to harbor detectable planets. Of these stars, 284 arein the ideal temperature range for planet searches,Teff<=6000 K, and have a 10% or greater probability ofhosting planets based on their metallicities. The stars in thelow-resolution spectroscopic survey should eventually yield >60 newplanets, including 8-9 hot Jupiters. Short-period planets have alreadybeen discovered orbiting the survey targets HIP 14810 and HD 149143.
| Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available
| Abundance difference between components of wide binaries
We present iron abundance analysis for 23 wide binaries with mainsequence components in the temperture range 4900-6300 K, taken from thesample of the pairs currently included in the radial velocity planetsearch on going at the Telescopio Nazionale Galileo (TNG) using the highresolution spectrograph SARG. The use of a line-by-line differentialanalysis technique between the components of each pair allows us toreach errors of about 0.02 dex in the iron content difference. Most ofthe pairs have abundance differences lower than 0.02 dex and there areno pairs with differences larger than 0.07 dex. The four cases ofdifferences larger than 0.02 dex may be spurious because of the largererror bars affecting pairs with large temperature difference, cold starsand rotating stars. The pair HD 219542, previously reported by us tohave a different composition, here is shown to be normal. Fornon-rotating stars warmer than 5500 K, characterized by a thinnerconvective envelope and for which our analyis appears to be of higheraccuracy, we are able to exclude in most cases the consumption of morethan 1 Earth Mass of iron (about 5 Earth masses of meteoritic material)during the main sequence lifetime of the stars, placing more stringentlimits (about 0.4 Earth masses of iron) in five cases of warm stars.This latter limit is similar to the estimates of rocky material accretedby the Sun during its main sequence lifetime. Combining the results ofthe present analysis with those for the Hyades and Pleiades, we concludethat the hypothesis that pollution by planetary material is the onlymechanism responsible for the highest metallicity of the stars withplanets may be rejected at more than 99% level of confidence if theincidence of planets in these samples is as high as 8% and similar tothe field stars included in current radial velocity surveys. However,the significance of this result drops considerably if the incidence ofplanets around stars in binary systems and clusters is less than a halfof that around normal field stars.Based on observations made with the Italian Telescopio Nazionale Galileo(TNG) operated on the island of La Palma by the Centro Galileo Galileiof the INAF (Istituto Nazionale di Astrofisica) at the SpanishObservatorio del Roque de los Muchachos of the Instituto de Astrofisicade Canarias.The equivalent widths 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/420/683
| 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
| Non-interacting main-sequence binaries with different chemical compositions: Evidences of infall of rocky material?
We performed a careful differential abundance analysis of individualcomponents of six main sequence binaries with separations of a fewhundreds of AU. To reduce analysis concerns, we selected systems withalmost equal mass components. We were able to derive differentialabundances of several elements with errors down to 0.01 dex in the bestcases. We found that in four systems the two components have the samechemical composition, within these very severe limits. However, cleardifferences were found for the two remaining systems (HD 219542 and HD200466), in both cases the primaries being more Fe-rich than thesecondaries, by 0.091+/- 0.009 and 0.053+/- 0.024 dex respectively.Similar differences were found for most of the elements considered inour analysis; however, we found no appreciable difference for volatileelements and a trend for increasing abundance differences withincreasing condensation temperature for individual elements, a resultsimilar to that found for some single stars with planets by Smith et al.(\cite{Smith01}). Finally, we note that HD 219542A has a Li-abundancecomparable to those of Li-rich stars in old open clusters, while no Liis detected in the slightly cooler HD 219542B. We suggest that theprimaries of these two systems have accreted rocky planets or the innerdust-rich part of a protoplanetary disk, likely due to gravitationalperturbation caused by the presence of the companion. Based onobservations made with the Italian Telescopio Nazionale Galileo (TNG)operated on the island of La Palma by the Centro Galileo Galilei of theCNAA (Consorzio Nazionale per l'Astronomia e l'Astrofisica) at theSpanish Observatorio del Roque de los Muchachos of the Instituto deAstrofisica de Canarias. Table 1 is only available in electronic form atthe CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp: //cdsweb .u-strasbg .fr/ cgi-bin/qcat?J/A+A/377/123
| Speckle Interferometry at the US Naval Observatory. V.
The results of 1544 speckle interferometric observations of 637 binarystars, ranging in separation from 0.25" to 5.25", are tabulated. Theseobservations were obtained using the 66 cm refractor at the US NavalObservatory in Washington, DC, with an intensified CCD detector. This isthe fifth in a series of papers presenting measures obtained with thissystem and covers the period 1998 January 1 through December 31. Randomerrors for all measures are estimated to be 17.6 mas in separation and0.55d/ρ in position angle, where ρ is the separation inarcseconds.
| Speckle Interferometry at the US Naval Observatory. IV.
The results of 1314 speckle interferometric observations of 625 binarystars, ranging in separation from 0.2" to 5.2" with a limiting secondarymagnitude of V=11, are tabulated. These observations were obtained usingthe 66 cm refractor at the US Naval Observatory in Washington, DC, withan intensified CCD detector. This is the fourth in a series of paperspresenting measures obtained with this equipment and covers the period1997 January 1 through December 31. Random errors for all measures areestimated to be 18 mas in separation and 0.57d/rho in position angle,where rho is the separation in arcseconds.
| CCD astrometry and instrumental {DELTA}V photometry of wide visual double stars. IV. Differential measurements of northern pairs.
We present relative positions and instrumental visual magnitudedifferences ({DELTA}V) of 101 northern wide double star components. Themean accuracy of the magnitude differences is 0.01 magnitudes, of theangular separation 0.04 arcseconds, and of position angle 0.13 degrees.Most of the programme pairs are targets of the HIPPARCOS mission andthey have been often observed during the last 150 years.
| Stroemgren photometry of F- and G-type stars brighter than V = 9.6. I. UVBY photometry
Within the framework of a large photometric observing program, designedto investigate the Galaxy's structure and evolution, Hβ photometryis being made for about 9000 stars. As a by-product, supplementary uvbyphotometry has been made. The results are presented in a cataloguecontaining 6924 uvby observations of 6190 stars, all south ofδ=+38deg. The overall internal rms errors of one observation(transformed to the standard system) of a program star in the interval6.5
| A preliminary compilation of DS-programme star positions
A catalog is presented of the double-star-program (DS-program) starpositions, listing right ascensions for 930 DSs and declinations for1225 DSs of the program. The positions were compiled from the observedvalues obtained between 1980 and 1987 with the meridian circles of sixUSSR observatories (the Moscow, Kazan', Kiev, Khar'kov, Odessa, andTashkent Observatories) and the Belgrade Observatory. The measurementsand the treatment of the observational material were performed using therelative method, and the FK-4 system stars were used as reference stars.
| Photographic Measures of Visual Double Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1983A&AS...51...63P&db_key=AST
| Photographic measures of double stars. II
Measures are presented for 302 double stars photographed on 657 plateswith the 36-in. Lick refractor in the period between 1945 and 1962. Thedata provided include the observing epochs, the rectangular coordinatesof the secondary components with reference to the respective primaries,the mean errors of a single measurement, the computed mean errors, thedouble-star separations, and the position angles both for the observingepoch and reduced to the equator of 2000. An additional 561 unmeasuredplates of acceptable quality obtained between 1948 and 1960 are listed.
| Stars with large proper motions in the astrographic zones +32° and + 33° (List V)
Not Available
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Наблюдательные данные и астрометрия
| Созвездие: | Возничий |
| Прямое восхождение: | 05h10m59.10s |
| Склонение: | +32°02'19.7" |
| Видимая звёздная величина: | 8.063 |
| Расстояние: | 46.751 парсек |
| Собственное движение RA: | -135.5 |
| Собственное движение Dec: | 16.7 |
| B-T magnitude: | 8.926 |
| V-T magnitude: | 8.135 |
Каталоги и обозначения:
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