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Pulkovo compilation of radial velocities for 35495 stars in a common system.
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| Hipparcos red stars in the HpV_T2 and V I_C systems
For Hipparcos M, S, and C spectral type stars, we provide calibratedinstantaneous (epoch) Cousins V - I color indices using newly derivedHpV_T2 photometry. Three new sets of ground-based Cousins V I data havebeen obtained for more than 170 carbon and red M giants. These datasetsin combination with the published sources of V I photometry served toobtain the calibration curves linking Hipparcos/Tycho Hp-V_T2 with theCousins V - I index. In total, 321 carbon stars and 4464 M- and S-typestars have new V - I indices. The standard error of the mean V - I isabout 0.1 mag or better down to Hp~9 although it deteriorates rapidly atfainter magnitudes. These V - I indices can be used to verify thepublished Hipparcos V - I color indices. Thus, we have identified ahandful of new cases where, instead of the real target, a random fieldstar has been observed. A considerable fraction of the DMSA/C and DMSA/Vsolutions for red stars appear not to be warranted. Most likely suchspurious solutions may originate from usage of a heavily biased color inthe astrometric processing.Based on observations from the Hipparcos astrometric satellite operatedby the European Space Agency (ESA 1997).}\fnmsep\thanks{Table 7 is onlyavailable in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/397/997
| Carbon-rich giants in the HR diagram and their luminosity function
The luminosity function (LF) of nearly 300 Galactic carbon giants isderived. Adding BaII giants and various related objects, about 370objects are located in the RGB and AGB portions of the theoretical HRdiagram. As intermediate steps, (1) bolometric corrections arecalibrated against selected intrinsic color indices; (2) the diagram ofphotometric coefficients 1/2 vs. astrometric trueparallaxes varpi are interpreted in terms of ranges of photosphericradii for every photometric group; (3) coefficients CR andCL for bias-free evaluation of mean photospheric radii andmean luminosities are computed. The LF of Galactic carbon giantsexhibits two maxima corresponding to the HC-stars of the thick disk andto the CV-stars of the old thin disk respectively. It is discussed andcompared to those of carbon stars in the Magellanic Clouds and Galacticbulge. The HC-part is similar to the LF of the Galactic bulge,reinforcing the idea that the Bulge and the thick disk are part of thesame dynamical component. The CV-part looks similar to the LF of theLarge Magellanic Cloud (LMC), but the former is wider due to thesubstantial errors on HIPPARCOS parallaxes. The obtained meanluminosities increase with increasing radii and decreasing effectivetemperatures, along the HC-CV sequence of photometric groups, except forHC0, the earliest one. This trend illustrates the RGB- and AGB-tracks oflow- and intermediate-mass stars for a range in metallicities. From acomparison with theoretical tracks in the HR diagram, the initial massesMi range from about 0.8 to 4.0 Msun for carbongiants, with possibly larger masses for a few extreme objects. A largerange of metallicities is likely, from metal-poor HC-stars classified asCH stars on the grounds of their spectra (a spheroidal component), tonear-solar compositions of many CV-stars. Technetium-rich carbon giantsare brighter than the lower limit Mbol =~ -3.6+/- 0.4 andcentered at =~-4.7+0.6-0.9 at about =~(2935+/-200) K or CV3-CV4 in our classification. Much like the resultsof Van Eck et al. (\cite{vaneck98}) for S stars, this confirms theTDU-model of those TP-AGB stars. This is not the case of the HC-stars inthe thick disk, with >~ 3400 K and>~ -3.4. The faint HC1 and HC2-stars( =~ -1.1+0.7-1.0) arefound slightly brighter than the BaII giants ( =~-0.3+/-1.3) on average. Most RCB variables and HdC stars range fromMbol =~ -1 to -4 against -0.2 to -2.4 for those of the threepopulation II Cepheids in the sample. The former stars show the largestluminosities ( <~ -4 at the highest effectivetemperatures (6500-7500 K), close to the Mbol =~ -5 value forthe hot LMC RCB-stars (W Men and HV 5637). A full discussion of theresults is postponed to a companion paper on pulsation modes andpulsation masses of carbon-rich long period variables (LPVs; Paper IV,present issue). This research has made use of the Simbad databaseoperated at CDS, Strasbourg, France. Partially based on data from theESA HIPPARCOS astrometry satellite. Table 2 is only available inelectronic form at the 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/390/967
| The effective temperatures of carbon-rich stars
We evaluate effective temperatures of 390 carbon-rich stars. Theinterstellar extinction on their lines of sights was determined andcircumstellar contributions derived. The intrinsic (dereddened) spectralenergy distributions (SEDs) are classified into 14 photometric groups(HCi, CVj and SCV with i=0,5 and j=1,7). The newscale of effective temperatures proposed here is calibrated on the 54angular diameters (measured on 52 stars) available at present from lunaroccultations and interferometry. The brightness distribution on stellardiscs and its influence on diameter evaluations are discussed. Theeffective temperatures directly deduced from those diameters correlatewith the classification into photometric groups, despite the large errorbars on diameters. The main parameter of our photometric classificationis thus effective temperature. Our photometric < k right >1/2 coefficients are shown to be angular diameters on arelative scale for a given photometric group, (more precisely for agiven effective temperature). The angular diameters are consistent withthe photometric data previously shown to be consistent with the trueparallaxes from HIPPARCOS observations (Knapik, et al. \cite{knapik98},Sect. 6). Provisional effective temperatures, as constrained by asuccessful comparison of dereddened SEDs from observations to modelatmosphere predictions, are in good agreement with the values directlycalculated from the observed angular diameters and with those deducedfrom five selected intrinsic color indices. These three approaches wereused to calibrate a reference angular diameter Phi 0 and theassociated coefficient CT_eff. The effective temperatureproposed for each star is the arithmetic mean of two estimates, one(``bolometric'') from a reference integrated flux F0, theother (``spectral'') from calibrated color indices which arerepresentative of SED shapes. Effective temperatures for about 390carbon stars are provided on this new homogeneous scale, together withvalues for some stars classified with oxygen-type SEDs with a total of438 SEDs (410 stars) studied. Apparent bolometric magnitudes are given.Objects with strong infrared excesses and optically thick circumstellardust shells are discussed separately. The new effective temperaturescale is shown to be compatible and (statistically) consistent with thesample of direct values from the observed angular diameters. Theeffective temperatures are confirmed to be higher than the mean colortemperatures (from 140 to 440 K). They are in good agreement with thepublished estimates from the infrared flux method forTeff>= 3170 K, while an increasing discrepancy is observedtoward lower temperatures. As an illustration of the efficiency of thephotometric classification and effective temperature scale, the C/Oratios and the Merrill-Sanford (M-S) band intensities are investigated.It is shown that the maximum value, mean value and dispersion of C/Oincrease along the photometric CV-sequence, i.e. with decreasingeffective temperature. The M-S bands of SiC2 are shown tohave a transition from ``none'' to ``strong'' at Teff =~(2800+/- 150right ) K. Simultaneously, with decreasing effectivetemperature, the mean C/O ratio increases from 1.04 to 1.36, thetransition in SiC2 strength occurring while 1.07<= C/O<= 1.18. This research has made use of the Simbad database operatedat CDS, Strasbourg, France. Table 10 is 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/369/178
| General Catalog of Galactic Carbon Stars by C. B. Stephenson. Third Edition
The catalog is an updated and revised version of Stephenson's Catalogueof Galactic Cool Carbon Stars (2nd edition). It includes 6891 entries.For each star the following information is given: equatorial (2000.0)and galactic coordinates, blue, visual and infrared magnitudes, spectralclassification, references, designations in the most significantcatalogs and coordinate precision classes. The main catalog issupplemented by remarks containing information for which there was noplace in entries of the main part, as well as some occasional notesabout the peculiarities of specific stars.
| Re-processing the Hipparcos Transit Data and Intermediate Astrometric Data of spectroscopic binaries. I. Ba, CH and Tc-poor S stars
Only 235 entries were processed as astrometric binaries with orbits inthe Hipparcos and Tycho Catalogue (\cite{Hipparcos}). However, theIntermediate Astrometric Data (IAD) and Transit Data (TD) made availableby ESA make it possible to re-process the stars that turned out to bespectroscopic binaries after the completion of the Catalogue. This paperillustrates how TD and IAD may be used in conjunction with the orbitalparameters of spectroscopic binaries to derive astrometric parameters.The five astrometric and four orbital parameters (not already known fromthe spectroscopic orbit) are derived by minimizing an objective function(chi 2) with an algorithm of global optimization. This codehas been applied to 81 systems for which spectroscopic orbits becameavailable recently and that belong to various families ofchemically-peculiar red giants (namely, dwarf barium stars, strong andmild barium stars, CH stars, and Tc-poor S stars). Among these 81systems, 23 yield reliable astrometric orbits. These 23 systems make itpossible to evaluate on real data the so-called ``cosmic error''described by Wielen et al. (1997), namely the fact that an unrecognizedorbital motion introduces a systematic error on the proper motion.Comparison of the proper motion from the Hipparcos catalogue with thatre-derived in the present work indicates that the former are indeed faroff the present value for binaries with periods in the range 3 to ~ 8years. Hipparcos parallaxes of unrecognized spectroscopic binaries turnout to be reliable, except for systems with periods close to 1 year, asexpected. Finally, we show that, even when a complete orbital revolutionwas observed by Hipparcos, the inclination is unfortunately seldomprecise. Based on observations from the Hipparcos astrometric satelliteoperated by the European Space Agency (ESA 1997).
| Infrared observations of peculiar carbon stars.
We present a uniform and high quality set of infrared photometric (JHK)observations of the 6 peculiar carbon giant stars V Ari, UV Cam, BD+34911, TU Gem, BD+57 2161 and BD+34 4134. All of these belong to the smallgroup of known cool CH giants populating the Galactic halo. Comparisonof the J-H and H-K colours to "normal" C stars show our stars to be"bluer" (i.e., having lower values of J-H and H-K) than the bulk of theGalactic C stars. Comparison with synthetic JHK colours reveal 5 of our6 stars as having considerably lower metallicities and/or highertemperatures than the bulk. Using standard assumptions we deriveestimates of their effective temperatures, gravities, luminosities anddistances. Their derived luminosities place them close to (or below) thetheoretical first He shell flash luminosity, although other observationsindicate their carbon excess to be intrinsic.
| Carbon isotope ratio in carbon stars of the galactic halo.
We analysed CN red system (~8000Å) and C_2_ Swan system(~4700Å) to know carbon isotope ratios (^12^C/^13^C) for carbonstars in the Galactic halo, named CH stars. The isotope ratios areobtained for 6 CH stars by the curve-of-growth analysis of the isolated^12^CN and ^13^CN lines. In this analysis, we compared directly ^12^CNand ^13^CN lines of similar intensities (iso-intensity method), and theresulting ^12^C/^13^C ratios are almost independent of the modelatmosphere and its parameters. The ^13^CN lines appear to be too weak insome CH stars, for which we applied the spectral synthesis method to thestronger C_2_ Swan band, obtained ^12^C/^13^C ratios for two stars andestimated the lower limits of ^12^C/^13^C ratios for two stars. In thiscase, however, the results depend on model atmosphere and itsparameters. Results from our present and previous works show that mostof them (12 stars) distribute around ^12^C/^13^C~10 and two stars havevery high values (^12^C/^13^C>=500). The distribution of ^12^C/^13^Cratios in CH stars is different from that of the population I carbonstars as well as population II oxygen-rich giants (G~K types). The CHstars of very high ^12^C/^13^C ratios can be explained by dredge-up of^12^C due to 3α-process as in population I carbon stars (N-type).On the other hand the formation of the CH stars with low ^12^C/^13^Cratios requires the large supply of ^12^C followed by a process ofdecreasing ^12^C/^13^C ratio.
| Abundances in the symbiotic star AG Draconis: the barium-symbiotic connection.
An abundance analysis of the yellow symbiotic system AG Draconis revealsit to be a metal-poor K-giant ([Fe/H]=-1.3) which is enriched in theheavy s-process elements. This star thus provides a link between thesymbiotic stars and the binary barium and CH stars which are alsos-process enriched. These binary systems, which exhibit overabundancesof the heavy elements, owe their abundance peculiarities to masstransfer from thermally-pulsing asymptotic giant branch stars, whichhave since evolved to become white-dwarf companions of the cool stars wenow view as the chemically peculiar primaries. A comparison of theheavy-element abundance distribution in AG Dra with theoreticalnucleosynthesis calculations shows that the s-process is defined by arelatively large neutron exposure (τ=1.3mb^-1^), while an analysisof the rubidium abundance suggests that the s-process occurred at aneutron density of about 2x10^8^cm^-3^. The derived spectroscopic orbitof AG Dra is similar to the orbits of barium and CH stars. Because theluminosity function of low-metallicity K giants is skewed towards higherluminosities by about 2 magnitudes relative to solar-metallicity giants,it is argued that the lower metallicity K giants have larger mass-lossrates. It is this larger mass-loss rate that drives the symbioticphenomena in AG Dra and we suggest that the other yellow symbiotic starsare probably low-metallicity objects as well.
| A New Version of the Catalog of CH and Related Stars (CH95 Catalog)
A new version of the catalog of CH and related stars contains 244 fieldstars and 17 globular cluster stars. Here a list of these stars withtheir coordinates, their positions in the HR diagram and somestatistical diagrams is presented. The catalog will soon be available inthe printed and computerized versions.
| Classification of Population II Stars in the Vilnius Photometric System. I. Methods
The methods used for classification of Population II stars in theVilnius photometric system are described. An extensive set of standardswith known astrophysical parameters compiled from the literature sourcesis given. These standard stars are classified in the Vilnius photometricsystem using the methods described. The accuracy of classification isevaluated by a comparison of the astrophysical parameters derived fromthe Vilnius photometric system with those estimated from spectroscopicstudies as well as from photometric data in other systems. For dwarfsand subdwarfs, we find a satisfactory agreement between our reddeningsand those estimated in the uvbyscriptstyle beta system. The standarddeviation of [Fe/H] deter mined in the Vilnius system is about 0.2 dex.The absolute magnitude for dwarfs and subdwarfs is estimated with anaccuracy of scriptstyle <=0.5 mag.
| 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.
| Nine Seasons of Velocity Measurements in the Draco and Ursa Minor Dwarf Spheroidal Galaxies with the MMT Echelle
We have used the Multiple Mirror Telescope echelle spectrograph tomeasure 112 velocities of 42 stars in the Draco and Ursa Minor dwarfspheroidal galaxies and three velocities of three foreground starsbetween 1982 April and 1990 September. We used 11 A resolution spectraobtained with the MX multifiber spectrograph at the Steward 90" to findadditional giant candidates; 5 UMi and 13 Draco stars were then observedat the MMT and added to the original sample of velocity members. Inaddition, the MX spectra were used to eliminate 74 stars in thedirection of UMI and 59 stars in Draco as likely foreground dwarfs. Wedetected 7 velocity variables, defined as those stars whose probabilityof exceeding the measured X^2^ by chance is less than 1.5%. Three ofthese stars are Carbon (C) stars (UMi K and VA 335 and Draco C1); twohave emission lines (Draco CI and UMi M). We show that the C star DracoC4, with a proper motion membership probability of 7%, has a velocityconsistent with membership. It is not surprising that these C (mostlikely CH) stars are binaries because McClure has shown that mostGalactic CH stars are in binary systems. Of the remaining 35 stars, only4 are velocity variables, with measured velocity extrema of 29.1 kms^-1^ (UMi M), 7.2 km s^-1^ (Draco XI-2), 9.0 km s^-1^ (Draco 24), and8.3 km s^-1^ (Draco 473). The velocity dispersions are 10.1 +/- 1.7 kms^-1^ for UMi, and 9.9 +/- 1.4 km s^-1^ for Draco. These dispersionschange to 10.5 +/- 2.0 for UMi, and 8.2 +?- 1.3 for Draco if weeliminate the velocity variables. Our dispersion for UMi differs fromthat of Hargreaves et al. [MNRAS, 271,693 (1994b)] by 1.3σ of thecombined errors. These velocities are combined with the one-componentKing models of Pryor & Kormendy [AJ, 100,127 (1990)] to give M/L =73 for UMi, and 77 for Draco.
| A very high C-12/C-13 ratio in some CH stars - Implications for dredge-up in AGB evolution during the metal-poor ERA
Abstract image available at:http://adsabs.harvard.edu/abs/1991A&A...252L...1T
| The binary nature of the barium and CH stars. III - Orbital parameters
Results are presented from a 10-year program to monitor the velocityvariations of Ba II and CH stars, showing that all Ba II and CH starsare binaries. Radial-velocity observations for Ba II and CH binaries aregiven. Also, the results of orbit calculations and orbital elementdeterminations are analyzed. It is shown that the eccentricities of BaII star orbits are significantly lower than the eccentricities for asample of normal G and K giants. In addition, the eccentricities of CHstar orbits are significantly lower than those of Ba II stars,suggesting dissipation due to mass exchange, probably from a previousAGB star. The mass functions for Ba II and CH stars indicate that thestars come from samples of binary systems with a small dispersion inmass ratios. If the Ba II and CH stars are assumed to have masses of 1.5and 0.8 solar mass, respectively, then their companions would havemasses near 0.6 solar mass, similar to the values expected for whitedwarfs.
| Catalogue of CH and metal-deficient barium stars
Not Available
| Velocities of stars in remote Galactic satellites and the mass of the Galaxy
Observations of the two most distant known dwarf spheroidal Galacticsatellites, Leo I and II, and of two remote globular clusters, Eridanusand Pal 14, are presented. It is demonstrated that etalon spectra can beused for accurate wavelength calibration across the entire observedspectral range. Measured velocities of three stars in Eridanus, twostars in Pal 14, six stars in Leo I, and five stars in Leo II are usedto derive that the heliocentric systemic velocities of these systems are- 21 + or - 4, 72 + or - 4, 285 + or - 3, and 70 + or - 4 km/s,respectively. The value of the velocity for Leo I is in significantdisagreement with previously published values. Timing arguments are usedto estimate that the mass of the Galaxy is at least 13 x 10 to the 11thsolar. This value is valid only if Leo I is gravitationally bound to theGalaxy, and arguments supporting this assumption are presented.
| A general catalogue of cool carbon stars
Not Available
| Spectrophotometric investigation of carbon stars
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| The absolute spectrophotometry of carbon stars. VI. Abundance of carbon in the atmospheres.
Not Available
| ICCD speckle observations of binary stars. III - A survey for duplicity among high-velocity stars
An analysis of speckle interferometry data for 182 stars has resulted inthe detection of 10 binaries, four of which are newly resolved systems.After correcting for selection effects, the data are found to becompatible with a total frequency for high-velocity long-period doubleswhich is as large as that for low-velocity stars. Based on spectroscopicparallaxes and visual magnitudes, these binaries are found to be within100 pc of the sun, with eight having linear separations of less than 20AU. Four of the binaries are determined to have periods of less than 20yr.
| The absolute spectrophotometry of 18 carbon stars, III
Not Available
| Spectrophotometry of carbon stars. III - Molecular absorption bands: Quantitative analysis
The C2, CN, SiC2, and CH molecular absorption bands of 56 carbon starsare analyzed quantitatively on the basis of the spectroscopicobservations reported by Ogansian et al. (1985); the results arepresented in tables and graphs. Features noted include a separation ofearly and late stars in the C2 Swan-system red/blue index diagram, aseparation of R and N stars in the (C-12)N/(C-13)N index diagram, and acorrelation between the 4976-A Merrill-Sanford band and the 5896/5890-ANa I doublet.
| CH stars as galaxy halo tracers
A spectroscopic survey of high-latitude carbon stars shows that many ofthese stars are CH stars with characteristically high space velocities.Some newly determined CH stars and others compiled from the literatureare employed to determine the local space density and kinematics ofthese stars. For the local space density, the surprisingly high value ofrho = 5.6 x 10 to the -9th/cu pc is obtained for M(V) ranging from -0.25to -2.2. The main result of the present study is that the velocitydispersion perpendicular to the galactic plane sigma(W) is alwaysgreater than approximately 114 km/s, irrespective of how the sample ofknown CH stars and CH star candidates is subdivided.
| The Spectrophotometry of Carbon Stars - Part Two
Not Available
| The Spectrophotometry of Carbon Stars - Part One
Not Available
| The binary nature of the CH stars
Radial velocity observations are presented that indicate that many CHstars are binary systems. This is an important result for severalreasons. (1) CH stars are Population II objects and found on the giantbranches of several globular clusters; these are populations usuallythought of as deficient in binary systems. (2) Their binary natureprobably links them to the Population I Ba II stars which are alsobinaries. (3) Stars used to determine a mass-to-light ratio of the Dracodwarf spheroidal galaxy are probably CH stars which may give aspuriously high velocity dispersion. (4) CH stars are found only inrelatively loosely concentrated systems, probably linking centralconcentration of clusters with their ability to retain soft binaries.
| CH and metal-dificient barium stars and their color excesses
Not Available
| CH-like stars
The properties of CH-like stars are discussed on the basis ofYamashita's (1972) classification of some 290 carbon stars. The CH-likestars are shown to be early-type red carbon stars. Their spectra arefound to be very similar to those of CH stars (typical high-velocityPopulation II carbon stars), but their proper motions and radialvelocities reveal no evidence of high velocity. The spectra are alsofound to be similar to those of Ba II stars with enhanced carbonfeatures. Abundance anomalies in the spectra of various types of oldpeculiar stars are briefly discussed. It is noted that 16 CH-like starshave been discovered thus far.
| Radial Velocities of Nineteen Carbon Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1974PASJ...26..159Y&db_key=AST
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Dades d'Observació i Astrometria
| Constel·lació: | Auriga |
| Ascensió Recta: | 04h49m16.03s |
| Declinació: | +35°00'06.5" |
| Magnitud Aparent: | 8.84 |
| Distancia: | 613.497 parsecs |
| Moviment propi RA: | 13 |
| Moviment propi Dec: | -8.2 |
| B-T magnitude: | 11.604 |
| V-T magnitude: | 9.069 |
Catàlegs i designacions:
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