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The S-Type Asymptotic Giant Branch Stars RS Cnc, ST Her, OP Her And HR Peg
We present FCAPT differential Johnson l BV and Cousins l RI photometryand radial velocities of the S-type AGB stars RS Cnc, ST Her, OP Her andHR Peg. We performed multiperiodic analyses of this photometry to learnabout the frequencies of variability. The l B, V, R, and l I lightcurves are generally in phase. RS Cnc has periods of order 122 and 248days. Repeating the analyses using our data with the extensive l V and lR photometry of Percy et al. (2001) shows several periods near 248 daysand a period near 135 days. The primary period of ST Her appears to beabout 144 days although it is manifested most readily by its 103 dayalias. OP Her and HR Peg exhibit periods, respectively, of about 416 and116 days and of 54 and 74 days. The differences between our data set andthe larger one of Percy et al. (2001) for RS Cnc raises importantquestions about multiperiodic analyses for AGB stars.Tables 2, 4 and 6 are only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html.
| Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs
We present a uniform catalog of stellar properties for 1040 nearby F, G,and K stars that have been observed by the Keck, Lick, and AAT planetsearch programs. Fitting observed echelle spectra with synthetic spectrayielded effective temperature, surface gravity, metallicity, projectedrotational velocity, and abundances of the elements Na, Si, Ti, Fe, andNi, for every star in the catalog. Combining V-band photometry andHipparcos parallaxes with a bolometric correction based on thespectroscopic results yielded stellar luminosity, radius, and mass.Interpolating Yonsei-Yale isochrones to the luminosity, effectivetemperature, metallicity, and α-element enhancement of each staryielded a theoretical mass, radius, gravity, and age range for moststars in the catalog. Automated tools provide uniform results and makeanalysis of such a large sample practical. Our analysis method differsfrom traditional abundance analyses in that we fit the observed spectrumdirectly, rather than trying to match equivalent widths, and wedetermine effective temperature and surface gravity from the spectrumitself, rather than adopting values based on measured photometry orparallax. As part of our analysis, we determined a new relationshipbetween macroturbulence and effective temperature on the main sequence.Detailed error analysis revealed small systematic offsets with respectto the Sun and spurious abundance trends as a function of effectivetemperature that would be inobvious in smaller samples. We attempted toremove these errors by applying empirical corrections, achieving aprecision per spectrum of 44 K in effective temperature, 0.03 dex inmetallicity, 0.06 dex in the logarithm of gravity, and 0.5 kms-1 in projected rotational velocity. Comparisons withprevious studies show only small discrepancies. Our spectroscopicallydetermined masses have a median fractional precision of 15%, but theyare systematically 10% higher than masses obtained by interpolatingisochrones. Our spectroscopic radii have a median fractional precisionof 3%. Our ages from isochrones have a precision that variesdramatically with location in the Hertzsprung-Russell diagram. We planto extend the catalog by applying our automated analysis technique toother large stellar samples.
| The Planet-Metallicity Correlation
We have recently carried out spectral synthesis modeling to determineTeff, logg, vsini, and [Fe/H] for 1040 FGK-type stars on theKeck, Lick, and Anglo-Australian Telescope planet search programs. Thisis the first time that a single, uniform spectroscopic analysis has beenmade for every star on a large Doppler planet search survey. We identifya subset of 850 stars that have Doppler observations sufficient todetect uniformly all planets with radial velocity semiamplitudes K>30m s-1 and orbital periods shorter than 4 yr. From this subsetof stars, we determine that fewer than 3% of stars with-0.5<[Fe/H]<0.0 have Doppler-detected planets. Above solarmetallicity, there is a smooth and rapid rise in the fraction of starswith planets. At [Fe/H]>+0.3 dex, 25% of observed stars have detectedgas giant planets. A power-law fit to these data relates the formationprobability for gas giant planets to the square of the number of metalatoms. High stellar metallicity also appears to be correlated with thepresence of multiple-planet systems and with the total detected planetmass. This data set was examined to better understand the origin of highmetallicity in stars with planets. None of the expected fossilsignatures of accretion are observed in stars with planets relative tothe general sample: (1) metallicity does not appear to increase as themass of the convective envelopes decreases, (2) subgiants with planetsdo not show dilution of metallicity, (3) no abundance variations for Na,Si, Ti, or Ni are found as a function of condensation temperature, and(4) no correlations between metallicity and orbital period oreccentricity could be identified. We conclude that stars with extrasolarplanets do not have an accretion signature that distinguishes them fromother stars; more likely, they are simply born in higher metallicitymolecular clouds.Based on observations obtained at Lick and Keck Observatories, operatedby the University of California, and the Anglo-Australian Observatories.
| Chromospheric Ca II Emission in Nearby F, G, K, and M Stars
We present chromospheric Ca II H and K activity measurements, rotationperiods, and ages for ~1200 F, G, K, and M type main-sequence stars from~18,000 archival spectra taken at Keck and Lick Observatories as a partof the California and Carnegie Planet Search Project. We have calibratedour chromospheric S-values against the Mount Wilson chromosphericactivity data. From these measurements we have calculated medianactivity levels and derived R'HK, stellar ages,and rotation periods from general parameterizations for 1228 stars,~1000 of which have no previously published S-values. We also presentprecise time series of activity measurements for these stars.Based on observations obtained at Lick Observatory, which is operated bythe University of California, and on observations obtained at the W. M.Keck Observatory, which is operated jointly by the University ofCalifornia and the California Institute of Technology. The KeckObservatory was made possible by the generous financial support of theW. M. Keck Foundation.
| 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
| New Metallicity Calibration Down to [Fe/H] = -2.75 dex
We have taken 88 dwarfs, covering the colour-index interval 0.37 <=(B-V)0 <= 1.07mag, with metallicities -2.70 <= [Fe/H]<= +0.26dex, from three different sources for new metallicitycalibration. The catalogue of Cayrel de Stroble et al. (2001), whichincludes 65% of the stars in our sample, supplies detailed informationon abundances for stars with determination based on high-resolutionspectroscopy. In constructing the new calibration we have used as`corner stones' 77 stars which supply at least one of the followingconditions: (i) the parallax is larger than 10mas (distance relative tothe Sun less than 100pc) and the galactic latitude is absolutely higherthan 30° (ii) the parallax is rather large, if the galactic latitudeis absolutely low and vice versa. Contrary to previous investigations, athird-degree polynomial is fitted for the new calibration: [Fe/H]=0.10 -2.76δ - 24.04δ2 + 30.00δ3. Thecoefficients were evaluated by the least-squares method, without regardto the metallicity of Hyades. However, the constant term is in the rangeof metallicity determined for this cluster, i.e.0.08<=[Fe/H]<=0.11dex. The mean deviation and the mean error inour work are equal to those of Carney (1979), for [Fe/H] >= -1.75dexwhere Carney's calibration is valid
| Improved Astrometry and Photometry for the Luyten Catalog. II. Faint Stars and the Revised Catalog
We complete construction of a catalog containing improved astrometry andnew optical/infrared photometry for the vast majority of NLTT starslying in the overlap of regions covered by POSS I and by the secondincremental Two Micron All Sky Survey (2MASS) release, approximately 44%of the sky. The epoch 2000 positions are typically accurate to 130 mas,the proper motions to 5.5 mas yr-1, and the V-J colors to0.25 mag. Relative proper motions of binary components are measured to 3mas yr-1. The false-identification rate is ~1% for11<~V<~18 and substantially less at brighter magnitudes. Theseimprovements permit the construction of a reduced proper-motion diagramthat, for the first time, allows one to classify NLTT stars intomain-sequence (MS) stars, subdwarfs (SDs), and white dwarfs (WDs). We inturn use this diagram to analyze the properties of both our catalog andthe NLTT catalog on which it is based. In sharp contrast to popularbelief, we find that NLTT incompleteness in the plane is almostcompletely concentrated in MS stars, and that SDs and WDs are detectedalmost uniformly over the sky δ>-33deg. Our catalogwill therefore provide a powerful tool to probe these populationsstatistically, as well as to reliably identify individual SDs and WDs.
| Statistical cataloging of archival data for luminosity class IV-V stars. II. The epoch 2001 [Fe/H] catalog
This paper describes the derivation of an updated statistical catalog ofmetallicities. The stars for which those metallicities apply are ofspectral types F, G, and K, and are on or near the main sequence. Theinput data for the catalog are values of [Fe/H] published before 2002February and derived from lines of weak and moderate strength. Theanalyses used to derive the data have been based on one-dimensional LTEmodel atmospheres. Initial adjustments which are applied to the datainclude corrections to a uniform temperature scale which is given in acompanion paper (see Taylor \cite{t02}). After correction, the data aresubjected to a statistical analysis. For each of 941 stars considered,the results of that analysis include a mean value of [Fe/H], an rmserror, an associated number of degrees of freedom, and one or moreidentification numbers for source papers. The catalog of these resultssupersedes an earlier version given by Taylor (\cite{t94b}).Catalog is only available in electronic form at the CDS via anonymousftp cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/398/731
| Statistical cataloging of archival data for luminosity class IV-V stars. I. The epoch 2001 temperature catalog
This paper is one of a pair in which temperatures and metallicitycatalogs for class IV-V stars are considered. The temperature catalogdescribed here is derived from a calibration based on stellar angulardiameters. If published calibrations of this kind are compared by usingcolor-index transformations, temperature-dependent differences among thecalibrations are commonly found. However, such differences are minimizedif attention is restricted to calibrations based on Johnson V-K. Acalibration of this sort from Di Benedetto (\cite{dib98}) is thereforetested and adopted. That calibration is then applied to spectroscopicand photometric data, with the latter predominating. Cousins R-Iphotometry receives special attention because of its high precision andlow metallicity sensitivity. Testing of temperatures derived from thecalibration suggests that their accuracy and precision are satisfactory,though further testing will be warranted as new results appear. Thesetemperatures appear in the catalog as values of theta equiv5040/T(effective). Most of these entries are accompanied by measured orderived values of Cousins R-I. Entries are given for 951 stars.Catalog is only available in electronic form at the CDS via anonymousftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/398/721
| 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
| Photometric and Ca II H and K Spectroscopic Variations in Nearby Sun-like Stars with Planets. III.
We present the results of an analysis of time-series photometry, Ca II Hand K spectrophotometry, and high-dispersion visible spectra of ninenearby Sun-like stars recently identified as having planets. For the sixstars whose presumed planets have orbital periods of less than 4 months(τ Boo, 51 Peg, υ And, ρ1 Cnc, ρ CrB, and70 Vir), sine-curve fits to the photometric data show no variations withsemiamplitude greater than 1 or 2 parts in 104. Photometricvariations in 47 UMa are similarly small, although our photometric dataof this star are slightly affected by variability of the comparisonstar. Nonvariability at this level of precision is sufficient to ruleout surface magnetic activity as the cause of the observedradial-velocity variations in these seven stars and makes nonradialpulsations unlikely as well. Thus, our photometry provides indirect butstrong support for true reflex motions-planets-in these seven stars, butcannot yet so support the planetary hypothesis for the two additionalstars, 16 Cyg B and Gl 411. Continued photometric monitoring of theshort-period systems may soon result in the direct detection of theseplanets in reflected light. We have used our photometric fluxes tosearch for possible transits of the extrasolar planets. Transitsdefinitely do not occur in τ Boo, 51 Peg, υ And, andρ1 Cnc, and probably do not occur in ρ CrB and 70Vir. Our transit-search results are inconclusive for 47 UMa, and wecannot address the issue for 16 Cyg B and Gl 411. The precision of ourphotometry is sufficient to detect transits of planets even if they arenot gas giants, as currently assumed, but much smaller objects withrocky compositions. The chance of finding at least one transit in thesix stars is ~40%. We find significant year-to-year photometricvariability only in τ Boo, which is not only the youngest star inthe sample but also the star with the shallowest convective zone. Theinterseasonal range in its yearly mean photometric flux is ~0.002 mag,roughly twice the 0.0008 mag decadal variation in the Sun's totalirradiance. Monitoring of the relative Ca II H and K fluxes beganbetween 1966 and 1968 for 51 Peg, τ Boo, ρ CrB, and Gl 411,between 1990 and 1993 for 47 UMa, 70 Vir, 16 Cyg B, andρ1 Cnc, and in 1996 for υ And. The data have beennewly recalibrated for improved long-term instrumental stability,resulting in better precision of the Ca II records. Five of the ninestars in this study have little or no detectable year-to-year variationin Ca II flux. The remaining four show moderate or pronouncedvariability: τ Boo, whose radial-velocity and photometric variationshave comparatively high amplitudes; Gl 411, whose planetary companionwas inferred astrometrically, not spectroscopically; ρ1Cnc, which may undergo decadal cyclic activity; and υ And, whichshows moderate year-to-year variability. Except for 47 UMa,intraseasonal variability consistent with rotation was detected in theCa II records of all stars. However, the rotation periods determined forυ And, 70 Vir, and 16 Cyg B are of low confidence. Anexamination of the recalibrated Ca II records for 51 Peg finds arotation period of 22 days, in contrast to our previous result of 37days. Ages have been estimated from the mean Ca II flux and, wherepossible, the rotation period. We find general consistency with the agesdetermined by others comparing properties determined fromhigh-resolution spectroscopy to evolutionary models, although theuncertainties are, in general, large. Based on observations made atMount Wilson Observatory, operated by the Mount Wilson Institute, underan agreement with the Carnegie Institution of Washington and theautomatic photoelectric telescope at Fairborn Observatory in thePatagonia Mountains of southern Arizona.
| Correlated Depletion of Lithium and Beryllium in F Stars
It has been known for over a decade that Hyades F stars have severelydepleted their Li abundances (the "Li gap"), in sharp contrast to thepredictions of the standard stellar evolution theory. We began a Li andBe survey aimed at identifying the physical mechanism that creates theLi gap. We present here the first results of that survey, which includehigh-resolution (R = 48,000-120,000) and high signal-to-noise ratioobservations in 24 stars of the Li I lambda 6707.8 and/or the Be IIlambda 3131 doublets taken at the University of Hawaii 2.2 m,Canada-France-Hawaii 3.6 m, and Keck I 10 m telescopes. Our programstars with detections in both Li and Be define a clear trend thatsuggests (1) the surface Li and Be abundance depletions are correlatedand (2) surface Li diminishes more rapidly than surface Be. Our resultssuggest that correlated Li and Be depletion is a normal process that Fstars undergo. The Li-Be trend argues strongly against the mass-loss anddiffusion mechanisms and strongly supports slow mixing as the cause ofthe surface light-element deficiencies. Moreover, models withrotationally induced mixing are in better agreement with the data thanare models with wave-driven mixing.
| The ROSAT all-sky survey catalogue of optically bright main-sequence stars and subgiant stars
We present X-ray data for all main-sequence and subgiant stars ofspectral types A, F, G, and K and luminosity classes IV and V listed inthe Bright Star Catalogue that have been detected as X-ray sources inthe ROSAT all-sky survey; several stars without luminosity class arealso included. The catalogue contains 980 entries yielding an averagedetection rate of 32 percent. In addition to count rates, sourcedetection parameters, hardness ratios, and X-ray fluxes we also listX-ray luminosities derived from Hipparcos parallaxes. The catalogue isalso available in electronic form via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Properties of Sun-like Stars with Planets: 51 Pegasi, 47 Ursae Majoris, 70 Virginis, and HD 114762
Radial velocity variations have revealed planets orbiting 51 Peg, 47UMa, and 70 Vir, and a low-mass companion orbiting HD 114762. We analyzeparallel records of photometric measurements in Stromgren b and y andJohnson V, R, and I passbands and Ca II H and K fluxes in those stars.In the case of 51 Peg, the high precision of the differentialphotometric measurements made by the 0.75 m Automatic PhotoelectricTelescope and the nonvariability of the star would allow the detectionof a transit of a planet as small as Earth (corresponding to anamplitude of 0.0001 mag) if its orbit were nearly coplanar with our lineof sight. No transits were observed. For 51 Peg and 70 Vir, the upperlimit of nondetection of photometric variability at their companion'sorbital periods is Delta (b + y)/2 < 0.0002 +/- 0.0002 mag. For HD114762, it is Delta V < 0.0007 +/- 0.0004 mag. Such small amplitudesof photometric variability seem to eliminate periodic velocityvariations expected from p-mode oscillations. All four stars aremagnetically quiet; that is, they lack the typical Ca II and photometricvariability due to rotation and activity cycles expected from surfacemagnetic activity in solar-type stars. Such quiescence produces aninteresting observational bias that favors the detection of planets fromlow-amplitude radial velocity or photometric variations by minimizingthe contribution from intrinsic stellar variability. We discuss thecircumstances for which the probability of planet detections is improvedby the reduced level of variability from surface magnetic activity in Gand K stars. Stars with low variability in surface activity should bethe best candidates for planet searches using radial velocity andphotometric techniques. Searches for planets around younger, more activestars will be impeded by variations in velocity or brightness caused bytime-varying surface features. The Ca II H and K fluxes indicate thatall four stars are older than 5 Gyr. Ages were estimated from theaverage levels of Ca II H and K fluxes and an existing relationship ofthe decrease of Ca II fluxes with age on the lower main sequence andwere drawn from previous results based on theoretical isochrone fitting.Values of the projected rotational velocity, v sin i, are determined for70 Vir and 47 UMa from high-resolution spectra.
| A catalogue of [Fe/H] determinations: 1996 edition
A fifth Edition of the Catalogue of [Fe/H] determinations is presentedherewith. It contains 5946 determinations for 3247 stars, including 751stars in 84 associations, clusters or galaxies. The literature iscomplete up to December 1995. The 700 bibliographical referencescorrespond to [Fe/H] determinations obtained from high resolutionspectroscopic observations and detailed analyses, most of them carriedout with the help of model-atmospheres. The Catalogue is made up ofthree formatted files: File 1: field stars, File 2: stars in galacticassociations and clusters, and stars in SMC, LMC, M33, File 3: numberedlist of bibliographical references The three files are only available inelectronic form at the Centre de Donnees Stellaires in Strasbourg, viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5), or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| The photoelectric astrolabe catalogue of Yunnan Observatory (YPAC).
The positions of 53 FK5, 70 FK5 Extension and 486 GC stars are given forthe equator and equinox J2000.0 and for the mean observation epoch ofeach star. They are determined with the photoelectric astrolabe ofYunnan Observatory. The internal mean errors in right ascension anddeclination are +/- 0.046" and +/- 0.059", respectively. The meanobservation epoch is 1989.51.
| 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.
| Analyses of archival data for cool dwarfs. 2: A catalog of temperatures
A calibration presented in a previous paper is used in this paper toderive temperatures for FGK stars near the main sequence. Thecalibration is checked against published counterparts, and it is foundthat previous calibrations have not established K-dwarf temperatures inparticular beyond reasonable doubt. The database assembled to derive thetemperatures is described, and the problems posed by close binaries areevaluated. The newly derived temperatures are used to check a line-depthratio proposed as a thermometer by Gray and Johanson (1991, PASP, 103,439), and it is found that the ratio is metallicity-sensitive.Temperatures are given for a total of 417 stars.
| The local distribution of NA I interstellar gas
We present high-resolution absorption measurements (lambda/Delta lambdaapproximately 75,000) of the interstellar Na I D lines at 5890 A toward80 southern hemisphere early-type stars located in the localinterstellar medium (LISM). Combining these results with other sodiummeasurements taken from the literature, we produce galactic maps of thedistribution of neutral sodium column density for a total of 293 starsgenerally lying within approximately 250 pc of the Sun. These mapsreveal the approximate shape of the mid-plane contours of the rarefiedregion of interstellar space termed the Local Bubble. Its shape is seenas highly asymmetric, with a radius ranging from 30 to 300 pc, and withan average radius of 60 pc. Similar plots of the Galactic mid-planedistribution of sources emitting extreme ultraviolet radiation show thatthey also trace out similar contours of the Local Bubble derived from NaI absorption measurements. We conclude that the Local Bubble absorptioninterface can be represented by a hydrogen column density,NuETA = 2 x 1019 cm-2, which explainsboth the local distribution of Na I absorption and the observed galacticdistribution of extreme ultraviolet sources. The derived mid-planecontours of the Bubble generally reproduce the large-scale featurescarved out in the interstellar medium by several nearby galactic shellstructures.
| Optical Polarization of 1000 Stars Within 50-PARSECS from the Sun
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1993A&AS..101..551L&db_key=AST
| Further high-resolution NA I observations of the local interstellar medium
High-resolution absorption measurements of the interstellar Na I D linesat 5890 A observed toward 27 early-type stars in the local interstellarmedium (LISM) are presented. These results are combined with otherhigh-resolution sodium measurements to map the space distribution ofneutral sodium column density for some 118 stars out to less than 200pc. These measurements indicate an upper limit to the neutral sodiumcolumn density of log N(Na I) less than 10.0/sq cm can be inferred outto a distance of 50 pc in most directions in the LISM. Also, therarefield region of the Local Bubble may extend beyond 60 pc in at least35 percent of the directions sampled thus far. Evidence is shown for aubiquitous, comoving vector for neutral NaI gas clouds in the LISM whichis in a different direction to LISM vectors previously reported for moreionized local gas clouds. A comparison of the measured sodium columnswith those of interstellar Ca II for a sample of 12 stars within 95 pcresults in a ratio of Na I/Ca II less than 0.5 for most stars. Thisvalue implies that there could be warm, neutral gas with T of about12,500 K beyond 50 pc in the LISM.
| Chemical Composition of Open Clusters. II. C/H and C/Fe in F Dwarfs from High-Resolution Spectroscopy
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1990ApJ...351..480F&db_key=AST
| Chemical composition of open clusters. I - Fe/H from high-resolution spectroscopy
Using high-resolution spectroscopy, the abundance ratios Fe/H, C/H, andC/Fe were determined for F dwarfs in the Alpha Per, the Pleiades, andthe Hyades clusters; the UMa, Hyades, and Wolf 630 moving groups; and aselection of bright F field dwarfs. The age span of these objects rangesfrom 5 x 10 to the 7th to 2 x 10 to the 9th yr. No evidence was found ofa trend in Fe/H with age for these clusters and groups, but there wereclear differences in Fe/H among these groups, indicating intrinsicdifferences in the metal content of the local gas out of which thesegroups were formed. No evidence was found for a trend of C/H with age ofthese stellar groups, but there were cluster-to-cluster variations,implying differences in the content of carbon in the precluster gas. TheC/H cluster differences followed the same pattern as the Fe/H clusterdifferences and yield C/Fe values which are constant, and equal to thesolar value, in all the groups.
| A uvby-like photometric system for the WF/PC of the HST
The possibility of combining four filters of the Hubble Space TelescopeWide Field/Planetary Camera into a uvby-like photometric system isdiscussed. On the basis of earth-based observations with appropriatefilters, such a system consisting of WF/PC filters F 368M, F 413M, F492M, and F 547M was calibrated for the determination of fundamentalparameters of F dwarf stars. A good agreement was found between thisempirical calibration and a theoretical one by Bell (1988). Goodestimates of effective temperatures and metallicities can be obtainedwith this system, while gravity determinations require a UV filter atshorter wavelengths.
| Third preliminary catalogue of stars observed with the photoelectric astrolabe of the Beijing Astronomical Observatory.
Not Available
| On the nearest molecular clouds. III - MBM 40, 53, 54, and 55
In an attempt to determine the distances to four high-latitude molecularclouds (HLCs), echelle spectra near the Na I D lines, accurate MKspectral types, and photoelectric photometry for 25 nearby stars havebeen obtained. Fairly firm distance limits may be placed on MBM 40 (dsmaller than or equal to 140 pc) and MBM 53 (d greater than or equal to110 pc and less than or equal to 155 pc), based on the presence orabsence of strong interstellar Na I absorption towards stars projectedon or near those HLCs. Weak interstellar absorption lines observedtoward many of the stars located near MBM 54 and 55 make the distancesto those clouds less certain (about 265 pc for both). Interstellar CHabsorption at 4300 A was detected in the spectrum of HD 218662, locatedbehind MBM 53 with a CH column density of 2.1 x 10 to the 13th per sqcm, thus implying a CH abundance comparable to that observed in othermolecular clouds. Morphological and velocity agreement among COemission, the Na I absorption, the 100 micron infrared cirrus emission,and the 21 cm H I emission near these HLCs suggest a close associationof the interstellar material responsible for those phenomena.
| Lithium in the Hyades, the Hyades moving group, and Praesepe
High-resolution spectra of 35 F main-sequence stars have been obtainedat high SNRs in the region of the Li I resonance line at 6708 A.Fourteen of the stars are members of the Hyades, six are members ofPraesepe, and the remaining 15 stars are members of the Hyades MovingGroup. Equivalent widths of the Li resonance line and of Fe lines in thesame spectral region were measured and Li and Fe abundances werecalculated from spectral synthesis using Kurucz model atmospheres. Amean metallicity of (Fe/H) = + 0.17 + or - 0.06 for the Hyades, + 0.13 +or - 0.07 for Praesepe, and + 0.11 + or - 0.09 for the Hyades MovingGroup is obtained. The Li abundance patterns are consistent with thosefound previously for the Hyades stars and for the Praesepe stars, butsome of the Hyades Moving Group members do not fit this Li-temperatureprofile well. The possibility exists that the Hyades Moving Group is notcoeval and that its members have little in common other than kinematics.
| Radial velocity measurements. II - Ground-based observations of the program stars for the HIPPARCOS satellite
New radial velocities for 446 stars of magnitude 9.0 or brighter in 1616-sq-deg fields of the Northern Hemisphere are determined by automaticPDS measurement of 80-A/mm-dispersion spectra obtained at theObservatoire de Haute Provence using a 17-cm-diameter objective prism.The fields were selected to provide data for the input catalog of theESA Hipparcos astrometric satellite. The measurement techniques andprecision are discussed, and the results are presented in extensivetables and graphs.
| Intermediate band, H-beta, and RI photometry of a large sample of stars unbiased with respect to their motion. I - The F-type stars
Intermediate band and H-beta data from a sample of 1000 stars earlierthan type G2 are presented and discussed relative to the stars'luminosities, metal abundances, and motion. Two groups of stars areconsidered, one within 10 arcsec of the South Galactic Pole and 8.5-8.6mag stars contained in the Moore-Paddock (1950) and Wayman (1960)samples (MP-W). The MP-W stars are mainly old disk population stars withmetal abundances of 4-0.25 solar values. Possible age-abundancedistribution-luminosity connections are explored, as are techniques forseparating old and young disk population objects.
| The Hyades main sequence
Intermediate band, H-beta and RI observations of 72 Hyades cluster starsto V = 11 mag are reported and discussed. A modulus of 3.2 mag isderived on the basis of a comparison with field stars of large parallax.Also presented are observations of 98 main-sequence stars of the Hyadesgroup that were previously found to be group members from kinematicalconsiderations. Parallaxes of the group stars, computed on theassumption that they are members of an extended Hyades cluster, yieldmean values of (U, V, W) = (+40.5, -18.4, -4.9) km/s, with dispersionsof (2.3, 2.3, 6.0) km/s, compared with (+41.7, -18.4, -2.0) and (2.6,1.3, 1.9) km/s for the brightest cluster members. It is noted that allthe stars discussed can be considered as members of a supercluster inwhich only a slight relaxation control of the W velocities is presentfor stars far from the nucleus. Evidence is found, including that of thePraesepe cluster at Z = +80 pc, for some interchange between the U, V,and W velocities in stars farthest from the galactic plane, with thetotal cluster velocity being maintained.
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Membre dels grups següents:
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Dades d'Observació i Astrometria
| Constel·lació: | Pegasus |
| Ascensió Recta: | 23h06m18.20s |
| Declinació: | +18°31'03.0" |
| Magnitud Aparent: | 6.13 |
| Distancia: | 43.178 parsecs |
| Moviment propi RA: | 227.7 |
| Moviment propi Dec: | 60.3 |
| B-T magnitude: | 6.698 |
| V-T magnitude: | 6.2 |
Catàlegs i designacions:
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