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|Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics|
The Catalogue, available at the Centre de Données Stellaires deStrasbourg, consists of 13 573 records concerning the results obtainedfrom different methods for 7778 stars, reported in the literature. Thefollowing data are listed for each star: identifications, apparentmagnitude, spectral type, apparent diameter in arcsec, absolute radiusin solar units, method of determination, reference, remarks. Commentsand statistics obtained from CADARS are given. The Catalogue isavailable in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (184.108.40.206) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcar?J/A+A/367/521
|The proper motions of fundamental stars. I. 1535 stars from the Basic FK5|
A direct combination of the positions given in the HIPPARCOS cataloguewith astrometric ground-based catalogues having epochs later than 1939allows us to obtain new proper motions for the 1535 stars of the BasicFK5. The results are presented as the catalogue Proper Motions ofFundamental Stars (PMFS), Part I. The median precision of the propermotions is 0.5 mas/year for mu alpha cos delta and 0.7mas/year for mu delta . The non-linear motions of thephotocentres of a few hundred astrometric binaries are separated intotheir linear and elliptic motions. Since the PMFS proper motions do notinclude the information given by the proper motions from othercatalogues (HIPPARCOS, FK5, FK6, etc.) this catalogue can be used as anindependent source of the proper motions of the fundamental stars.Catalogue (Table 3) is only available at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (220.127.116.11) or viahttp://cdsweb.u-strastg.fr/cgi-bin/qcat?J/A+A/365/222
|Ca II activity and rotation in F-K evolved stars|
Ca II H and K high resolution observations for 60 evolved stars in thefield and in 5 open clusters are presented. From these spectrachromospheric fluxes are derived, and a homogeneous sample of more than100 giants is built adding data from the literature. In addition, formost stars, rotational velocities were derived from CORAVELobservations. By comparing chromospheric emission in the cluster starswe confirm the results of Pasquini & Brocato (1992): chromosphericactivity depends on the stellar effective temperature, and mass, whenintermediate mass stars (M ~ 4 Msun) are considered. TheHyades and the Praesepe clump giants show the same level of activity, asexpected from stars with similar masses and effective temperatures. Adifference of up to 0.4 dex in the chromospheric fluxes among the Hyadesgiants is recorded and this sets a clear limit to the intrinsic spreadof stellar activity in evolved giants. These differences in otherwisevery similar stars are likely due to stellar cycles and/or differencesin the stellar initial angular momentum. Among the field stars none ofthe giants with (V-R)o < 0.4 and Ia supergiants observedshows a signature of Ca II activity; this can be due either to the realabsence of a chromosphere, but also to other causes which preclude theappearance of Ca II reversal. By analyzing the whole sample we find thatchromospheric activity scales linearly with stellar rotational velocityand a high power of stellar effective temperature: F'k ~Teff7.7 (Vsini)0.9. This result can beinterpreted as the effect of two chromospheric components of differentnature: one mechanical and one magnetic. Alternatively, by using theHipparcos parallaxes and evolutionary tracks, we divide the sampleaccording to the stellar masses, and we follow the objects along anevolutionary track. For each range of masses activity can simply beexpressed as a function of only one parameter: either theTeff or the angular rotation Omega , with laws F'k~ Omega alpha , because angular velocity decreases witheffective temperature along an evolutionary track. By using theevolutionary tracks and the observed Vsini we investigate the evolutionof the angular momentum for evolved stars in the range 1-5Msun. For the 1.6-3 solar mass stars the data are consistentwith the IOmega =const law while lower and higher masses follow a lawsimilar to IOmega 2=const, where I is the computed stellarmomentum of inertia. We find it intriguing that Vsini remains almostconstant for 1Msun stars along their evolution; if a similarbehavior is shared by Pop II stars, this could explain the relativelyhigh degree of activity observed in Pop II giants. Finally, through theuse of models, we have verified the consistency of the F'k ~Omega alpha and the IOmega beta = Const lawsderived, finding an excellent agreement. This representation, albeitcrude (the models do not consider, for instance, mass losses) representsthe evolution of Ca II activity and of the angular momentum in asatisfactory way in most of the portion of HR diagram analyzed.Different predictions could be tested with observations in selectedclusters. Based on observations collected at ESO, La Silla. Tables 1-3are only available in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (18.104.22.168) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
|A uvbyβ photometric calibration of iron abundances in supergiant stars.|
A photometric reddening-free calibration for [Fe/H] valid for giant andsupergiant stars of intermediate temperature, has been obtained usingthe Stroemgren uvbyβ system. Galactic supergiants, supergiants inthe Magellanic Clouds and Galactic metal deficient red giants withspectroscopic determinations of [Fe/H] were used as calibrators. Thecalibration can be used to predict [Fe/H] with an accuracy of 0.33 dex,valid for stars with 0.14<[m_1_]<0.70 in the iron abundance range-2.5<[Fe/H]<+0.3. This shows the potential of supergiant stars astracers of iron abundances in other galaxies. Evidence that Galacticluminous F-G stars are intrinsically bluer than their counterparts inthe Magellanic Clouds is offered.
|Colour excesses of F-G supergiants and Cepheids from Geneva photometry.|
A reddening scale for F-G supergiants and Cepheids is presented.Supergiants with low reddenings or in clusters form the basis of thecalibration. In this sense, it is entirely empirical. The data have beenobtained in the Geneva photometric system. Comparisons with otherreddening scales show no disagreement. The only problem is with Fernie'sscale for Cepheids (1990), where a systematic trend exists. Its originis not clear. It is suggested to extend the number of supergiants withindependently obtained colour excesses in order to test the existence ofa possible luminosity dependence of the calibration. A period-colourrelation for Cepheids is deduced, on the basis of the present reddeningcorrections. It gives strong support for V473 Lyr being a secondovertone pulsator.
|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.
|Second astrolabe catalogue of Santiago.|
Positions for 350 FK5 and 164 FK5 Extension stars as determined with theDanjon astrolabe of Santiago and differences astrolabe-catalogue aregiven for Equinox J2000.0 and for the mean observation epoch of eachstar. The average mean error in alpha is +/-0.005s and +/-0.07" indelta. The mean epoch of observation of the catalogue is J1979.96.
|Calibrations of Mv, (Fe/H), and log G for yellow supergiant stars from O I 7774 and uvby-beta data|
New calibrations of the absolute magnitude Mv from O I 7774data are derived from narrow-band photometry and low dispersionspectroscopy for AO-G2 low and high luminosity stars. The nonlineardependence of Mv from the equivalent width W(OI) and therelevance of the stellar temperature in the calibration are confirmed inagreement with previous calibrations obtained from high resolutionspectroscopy. Also functional formulas to estimate (Fe/H) and log g fromuvby-beta data for FO-G3 supergiants are offered. These calibrationspredict iron abundances and gravities for yellow supergiants withuncertainties not much higher than good spectroscopic determinations.
|Photometry of F-K type bright giants and supergiants. I - Intermediate band and H-Beta observations|
Over 1500 observations of 560 bright giants and supergiants of types F-Kare presented and compared to the observations by Gray and Olsen (1991).The present results include intermediate-band which is slightlydifferent from the Stromgren data by Gray and Olsen due to a differentwidth for the v filter. A systematic difference in m(1) - M(1) withdecreasing temperature is noted in the two H-Beta data sets, and thecorrelations are defined.
|Santiago Fundamental Catalogue - A catalogue of 1105 FK5 stars (equinox J2000.0)|
The positions in right ascension and declination of 1105 FK5 stars,observed with a Meridian Circle during the period 1979 to 1991, aregiven. The average mean square error of a position, for the wholecatalog, is +/- 0.009 s in right ascension and +/- 0.10 arcsec indeclination. The mean epoch of the catalog is 1983.148.
|Chromospheric activity and stellar evolution - Clues from IUE data|
We investigate the dependence of chromospheric activity on stellarphysical parameters in a sample of cool giants and supergiants. Ca IIsurface fluxes for stars of known masses and evolutionary status arederived from published IUE Mg II observations. Adding these data to thesample of Pasquini et al. (1990) we find that chromospheric activity inevolved stars is better described by two stellar parameters, and a tightrelationship is found between activity, stellar Teff and Mass. Wediscuss this relationship arguing that the stellar evolutionary statuscould play a 'hidden' but fundamental role in determining the activitylevel of evolved late type stars.
|Santiago declination catalogue. II - A declination catalogue of 493 FK5 stars (equinox J2000.0)|
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1991A&AS...90..109C&db_key=AST
|The calibration of the Stromgren photometric system for A, F and early G supergiants. I - The observational data|
An empirical calibration of the Stromgren uvby-beta photometric systemfor the A, F, and early G supergiants is being derived. This paperexplains the observational program and the photometric reductiontechniques used and presents a catalog of new Stromgren photometry forover 600 A, F, and G supergiants.
|The calibration of Stromgren photometry for A, F and early G supergiants. II - The F and early G supergiants|
The technique for calibration of the uvby-beta photometric system isdeveloped empirically for the supergiants and tested for errors.Parameters are derived for gravity and temperature which indicate theintrinsic color, and color excesses are calculated for classicalCepheids. The values compare favorably with previous estimates, althoughthe calibration is found to be sensitive to metal abundance.
|Physical data of the fundamental stars.|
|Groups of stars with common motion in the Galaxy - Groups of red supergiants of the luminosity classes I and II|
|A survey of Balmer-line profiles and IRAS fluxes in forty yellow supergiants|
Results of a survey of yellow supergiants (predominantly F and G) thatwas undertaken to search for distorted Balmer lines are presented. Acomparison between the photometrically variable and nonvariablesupergiants is made with respect to the distorted and undistortedBalmer-line profiles. To complement the analysis, IRAS data are used todetect excess infrared emission, to infer circumstellar dust, and tosuggest a possible prior M supergiant evolutionary phase. Plans forfuture work are briefly discussed.
|Large and Kinematically Unbiased Samples of G- and K-Type Stars. III. Evolved Young Disk Stars in the Bright Star Sample|
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1989PASP..101...54E&db_key=AST
|Large and kinematically unbiased samples of G- and K-type stars. II - Observations of evolved stars in the Bright Star sample. III - Evolved young disk stars in the Bright Star sample|
Four color and RI observations were obtained for a large sample ofG-type and K-type stars in the Bright Star Catalogue. Data are firstpresented for 110 evolved stars. Photometry of evolved young diskpopulation stars have then been calibrated for luminosity, reddening,and metallicity on the basis of results for members of the Hyades andSirius superclusters. New DDO results are given for 120 stars.
|Absolute flux calibration of the H and K lines of CA II - Chromospheric radiative losses in F and G-type stars|
Ca II H and K spectra of 81 (mainly Southern) F and G stars are analyzedusing two different calibration methods. It is shown that, for spectraof sufficiently high resolution, and for stars of relatively lowrotation rates, the calibrations of Linsky et al. (1979) and of Pasquiniet al. (1988) give essentially the same results. These calibrations areused to derive absolute surface fluxes in the H and K lines of Ca II for64 stars. It is shown that several late-F and early-G giants andsupergiants have Ca II H and K fluxes in excess of about 10 to the 6therg/sq cm s, much larger than those typically observed for normal giantsof later spectral types.
|Atomic and molecular line emission from early-type high-luminosity stars|
The paper presents intermediate resolution 1.0-2.5 micron spectra of 13southern early-type peculiar emission line stars. Attention is given tothe NIR line spectra of this class of stars as well as the complexnature of their circumstellar envelopes. Spectra are presented for AGCar, HR Car, HD 87643, HD 316285, CPD -52 deg 9243, CPD -57 deg 2874, GGCar, CD -42 deg 11721, He 3-1359, HD 326823, BI Cru, and HD 45677.Emission lines of H I and He I dominate the NIR spectra, while emissionlines of forbidden Fe II, Mg II, Na I, and Fe II are also seen in someobjects. The Brackett decrement indicates that Br-gamma is opticallythick in all objects studied.
|A photometric survey of the bright southern Be stars|
Repeated UBV photometric measurements were made of the 86 bright Bestars south of declination -20 deg, and a network of comparison starswas set up. From a statistical study of the differential photometry itwas found that short- or intermediate-term variability seems to beoccurring in about half of the Be stars, and to be more evident in thestars of earlier spectral type. It was also possible to identify 11individual short- or intermediate-term variables. Four of these (all ofearly B spectral type) appear to exhibit significant variability on atime-scale of a day or less. More intensive observations of one of thesestars, 28 Omega CMA, indicate short-term variations consistent with thepublished spectroscopic period of 1.37 day.
|Santiago declination catalogue - A declination catalogue of 412 FK4 stars (equinox 1950.0)|
This catalog contains the positions in declination, of 412 FK4 stars.The observations were carried out with the Repsold Meridian Circle atCerro Calan National Astronomical Observatory, during the period1963-1968. The average mean square error of one observation (for thewhole catalog) is + or - 0.13 arcsec. The mean epoch of observation ofthe catalog is 1965.75.
|The near-infrared spectrum of Eta Carinae|
Spectroscopy of the luminous star Eta Carinae has been performed in theatmospheric windows between 1.0 and 2.3 microns. The spectral resolutionemployed, up to about 1200, is the highest yet used at these wavelengthson this object. More than 80 emission lines have been recorded, andidentifications are offered for 90 percent of them, mostly with speciesalso seen at optical wavelengths. In comparison with other wave bands,the emission lines are little affected by either circumstellar reddeningor optical depth effects. Evidence is found that the central star ishotter than 40,000 K. It has also been possible to estimate abundancesfor some species. Eta Car is found to be clearly overabundant in helium,but probably underabundant in iron in the gaseous state. A table ofidentifications of the emission lines will serve as a finding list insubsequent analysis of the IR spectra of emission-line systems.
|Concentrations in the local association. III - Late-type bright giants, ages and abundances|
Late-type, bright giants and supergiants in southern and northernconcentrations and in the general field, the ages of the stars fromstellar models, and the abundances, based on intermediate bandphotometric indices, are investigated. It is found that the brightgiants and supergiants of types F to K among association members in theconcentrations and in the general field are overabundant in metals, withP(Fe/H) approximately equal to 0.25. These bright giants, and theearly-type association members brighter than about M(V) = -1 mag (mode Bstars), are determined to be younger than 5-6 x 10 to the 7th yr. Thefainter (mode A) main-sequence members of the association are shown tobe near 2 x 10 to the 8th yr with P(Fe/H) approximately equal to 0.
|New UBVRI photometry for 900 supergiants|
A description is presented of the results obtained in connection with asystematic program of supergiant photometry on the Johnson UBVRI system.During the eight years after the start of the program, almost 1000 starshave been observed, about 400 three or more times each. The originalselection of stars used the spectral type catalog of Jaschek et al.(1964) to choose supergiants. Since observations were possible from bothChile and Canada, no declination limits were imposed, and no particularselection criteria were imposed other than to eliminate carbon stars.These are so red as to require enormous extrapolations of thetransformation equations.
|Urby-beta photometry of visual double stars - A comparison with stellar models and isochrones|
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1982A&A...110..215O&db_key=AST
|DDO Observations of Southern Stars|
|The region of NGC 2287 and CR 121|
Intermediate band and H-beta observations of 135 stars in the regions ofthe clusters NGC 2287 and Cr 121 are discussed, and a luminositycalibration of photometric parameters for late G- to early K-type brightgiants and supergiants is introduced. Results indicate that NGC 2287 isat a distance of 740 pc, very little reddened, 100-million years old,and contains three or four G8-K2 bright giants and supergiants and ablue straggler. Cr 121 is 1.17 kpc distant, very little reddened, 1.5million years old and an extension of CMa OB1. Cr 121 contains a nearerconcentration of stars at the same distance as NGC 2287, and theassociation appears to be the same age as CMa OB1, although presequencestars may exist. Intermingling of stars in CMa OB2 and NGC 2287 is alsoconsidered possible, and a test of the calibration of two methods ofluminosity determination of early A-type stars using photometricparameters shows them to be entirely consistent.
|CA II H and K chromospheric emission in F- and G-type stars|
A survey of representative Ca II H and K line profiles (the mostpronounced chromospheric indicators observable from the ground) ispresented to illustrate the chromospheric emission of different types ofF and G stars. Of the 90 stars observed, a typical one is selected foreach spectral type, leaving a sample of 47. The spectral types are takenfrom Jaschek (1978), except when superseded by Keenan and Pitts (1980).For BS 3591 the Bright Star Catalog classification of F 8 III isretained, and data for the sun (G 2 V) refer to observations ofskylight, which is almost equal to integrated sunlight. General trendsin the changing appearance of chromospheric emission, as well as thephysical scatter of chromospheric activity levels among stars of similarphotospheric properties, are presented. It is shown that the sun's levelof chromospheric activity does not deviate much from what is typical forfield stars of a similar spectral class.
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