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Near-Infrared Spectroscopy of Carbon-Enhanced Metal-Poor Stars. I. A SOAR/OSIRIS Pilot Study
We report on an abundance analysis for a pilot study of sevencarbon-enhanced metal-poor (CEMP) stars, based on medium-resolutionoptical and near-infrared spectroscopy. The optical spectra are used toestimate [Fe/H], [C/Fe], [N/Fe], and [Ba/Fe] for our program stars. Thenear-infrared spectra, obtained during a limited early science run withthe new SOAR 4.1 m telescope and the Ohio State Infrared Imager andSpectrograph, are used to obtain estimates of [O/Fe] and12C/13C. The chemical abundances of CEMP stars areof importance for understanding the origin of CNO in the early Galaxy,as well as for placing constraints on the operation of the astrophysicals-process in very low metallicity asymptotic giant branch stars. Thispilot study includes a few stars with previously measured [Fe/H],[C/Fe], [N/Fe], [O/Fe], 12C/13C, and [Ba/Fe],based on high-resolution optical spectra obtained with large-aperturetelescopes. Our analysis demonstrates that we are able to achievereasonably accurate determinations of these quantities for CEMP starsfrom moderate-resolution optical and near-infrared spectra. This opensthe pathway for the study of significantly larger samples of CEMP starsin the near future. Furthermore, the ability to measure [Ba/Fe] for (atleast the cooler) CEMP stars should enable one to separate stars thatare likely to be associated with s-process enhancements (the CEMP-sstars) from those that do not exhibit neutron-capture enhancements (theCEMP-no stars).
| Radiative decay of the 4d5(6S)5p z5,7Po states in TcII: comparison along the homologous and isoelectronic sequences. Application to astrophysics
Using three independent theoretical approaches (CA, HFR + CP,AUTOSTRUCTURE), oscillator strengths have been calculated for a set ofTcII transitions of astrophysical interest and the reliability of theirabsolute scale has been assessed. The examination of the spectra emittedby some Ap stars has allowed the identification of TcII transitions inHD 125248. This TcII detection should however await confirmation fromspectral synthesis relying on dedicated model atmospheres. New partitionfunctions are also provided for TcI, TcII and TcIII for temperaturesranging between 4000 and 13000 K.
| s-Process in low metallicity Pb stars.
We consider a sample of very metal-poor, C-rich, s-rich and lead-richstars observed at high-resolution spectroscopy, and some recentspectroscopic data of C+s-rich stars obtained at moderate resolution.The spectroscopic data of these stars are interpreted with AGBtheoretical models of different 13C-pocket efficiencies,initial mass and initial r-enrichment. When lead is not measured we giveour theoretical prediction. The observed stars are not on the AGB phase,but are main sequence or giant stars. They acquired the C and senrichments by mass transfer in a close binary system from the moremassive companion while on the AGB (now a white dwarf). A considerablefraction of the stars show both high s and r enrichments. To explain thes+r enriched stars we assume a parental cloud already enriched inr-elements. The measurement of Nb is an indicator of an extrinsic AGB ina binary system. The intrinsic indicator [hs/ls] constrains the initialmass, while [Pb/hs] and [Pb/ls] are a measure of the s-processefficiency. The apparent discrepancies of C and N abundances may bereconciled by assuming a strong cool bottom process occurring during theAGB. An important primary production of light elements, from Ne to Si,increasing with the star mass, is predicted for AGB models at very lowmetallicity, induced by n capture on primary 22Ne and itsprogenies.
| Carbon Stars in the Infrared Telescope in Space Survey
We have identified 139 cool carbon stars in the near-infraredspectrophotometric survey of the Infrared Telescope in Space (IRTS) fromthe conspicuous presence of molecular absorption bands at 1.8, 3.1, and3.8 μm. Among them, 14 are new bright (K~4.0-7.0) carbon stars. Wefind a trend relating the 3.1 μm band strength to the K-L'color index, which is known to correlate with mass-loss rate. This couldbe an effect of a relation between the depth of the 3.1 μm featureand the degree of development of the extended stellar atmosphere wheredust starts to form.
| Forty Years of Spectroscopic Stellar Astrophysics in Japan
The development of Japanese spectroscopic stellar astrophysics in therecent 40 years is reviewed from an observational point of view. In thisarticle, the research activities are provisionally divided into fourfields: hot stars, hot emission-line (Be) stars, cool stars, and otherstars. Historical developments of the observational facilities atOkayama Astrophysical Observatory (spectrographs and detectors) are alsosummarized in connection with the progress in scientific researchactivities.
| CHARM2: An updated Catalog of High Angular Resolution Measurements
We present an update of the Catalog of High Angular ResolutionMeasurements (CHARM, Richichi & Percheron \cite{CHARM}, A&A,386, 492), which includes results available until July 2004. CHARM2 is acompilation of direct measurements by high angular resolution methods,as well as indirect estimates of stellar diameters. Its main goal is toprovide a reference list of sources which can be used for calibrationand verification observations with long-baseline optical and near-IRinterferometers. Single and binary stars are included, as are complexobjects from circumstellar shells to extragalactic sources. The presentupdate provides an increase of almost a factor of two over the previousedition. Additionally, it includes several corrections and improvements,as well as a cross-check with the valuable public release observationsof the ESO Very Large Telescope Interferometer (VLTI). A total of 8231entries for 3238 unique sources are now present in CHARM2. Thisrepresents an increase of a factor of 3.4 and 2.0, respectively, overthe contents of the previous version of CHARM.The catalog is only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/431/773
| First stars IV. CS 29497-030: Evidence for operation of the s-process at very low metallicity
We present an abundance analysis of the very metal-poor, carbon-enhancedstar CS 29497-030. Our results indicate that this unusually hot turnoffstar (Teff = 6650 K, log g = 3.5) has a metallicity [Fe/H] =-2.8, and exhibits large overabundances of carbon ([C/Fe] = +2.38),nitrogen ([N/Fe] = +1.88), and oxygen ([O/Fe] = +1.67). This star alsoexhibits a large enhancement in its neutron-capture elements; thepattern follows that expected to arise from the s-process. Inparticular, the Pb abundance is found to be very high with respect toiron ([Pb/Fe] = +3.5), and also with respect to the second peaks-process elements (e.g., Ba, La, Ce, Nd), which fits into the newlyintroduced classification of lead (Pb) stars. The known spectroscopicbinary status of this star, along with the observed s-process abundancepattern, suggest that it has accreted matter from a companion, whichformerly was an Asymptotic Giant-Branch (AGB) star. In a preliminaryanalysis, we have also identified broad absorption lines of metallicspecies that suggest a large axial rotational velocity for this star,which may be the result of spin-up associated with the accretion ofmaterial from its previous AGB companion. In addition, this star isclearly depleted in the light element Li. When considered along with itsrather high inferred temperature, these observations are consistent withthe expected properties of a very low metallicity halo blue straggler.Based on observations made with the ESO Very Large Telescope at ParanalObservatory, Chile (program ID 165.N-0276(A)).Table \ref{tab6} is only available in electronic form athttp://www.edpsciences.org
| Lead and mathbf s-process elements in stars of various metallicities: AGB predictions compared with observation
We present AGB predictions for all heavy elements within a large rangeof 13C-pocket efficiencies for stars of differentmetallicities, and compare them in detail with a number of spectroscopicobservations of s-rich and lead-rich in the Galaxy. The current conceptof the s-process efficiency, specified by the [hs/ls] index, is shown tobe inappropriate for the metal poor AGB stars and a second independentindex, [Pb/hs] or [Pb/ls], needs to be introduced. The state-of-the-artconcerning the interpretation of lead stars allows a very large spreadof [Pb/hs] in metal poor stars, as typically observed. We discussagreements and discrepancies for a large range of elements.
| Beobachtungsergebnisse Bundesdeutsche Arbeitsgemeinschaft fur Veranderlichen Serne e.V.
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| More lead stars
The standard model for the operation of the s-process in asymptoticgiant branch (AGB) stars predicts that low-metallicity ([Fe/H] <~ -1)AGB stars should exhibit large overabundances of Pb and Bi as comparedto other s-elements. The discovery of the first three such ``leadstars'' (defined as stars enriched in s-elements with [Pb/hs] >~ 1,hs being any of Ba, La or Ce) among CH stars has been reported in aprevious paper (Van Eck et al. \cite{VanEck-01}). Five more CH stars(with [Fe/H] ranging from -1.5 to -2.5) are studied in the presentpaper, and two of them appear to be enriched in lead (with [Pb/Ce] =~0.7). The Pb I line at lambda4057 .812 Å is detected and clearlyresolved thanks to high-resolution spectra (R = lambda /Delta lambda =135ts000 ). The abundances for these two stars (HD 198269 and HD 201626)are consistent with the predictions for the s-process operating inlow-metallicity AGB stars as a consequence of the ``partial mixing'' ofprotons below the convective hydrogen envelope. Another two stars (HD189711 and V Ari) add to a growing number of low-metallicity stars (alsoincluding LP 625-44 and LP 706-7, as reported by Aoki et al.\cite{Aoki2001}) which do not conform to these predictions. Variationson the canonical proton-mixing scenario for the operation of thes-process in low-metallicity stars, that could account for thesediscrepant stars, are briefly discussed.Based on observations carried out at the European Southern Observatory(La Silla, Chile; Program 65.L-0354) and at the Observatoire de HauteProvence (operated by CNRS, France).
| Reprocessing the Hipparcos data of evolved stars. III. Revised Hipparcos period-luminosity relationship for galactic long-period variable stars
We analyze the K band luminosities of a sample of galactic long-periodvariables using parallaxes measured by the Hipparcos mission. Theparallaxes are in most cases re-computed from the Hipparcos IntermediateAstrometric Data using improved astrometric fits and chromaticitycorrections. The K band magnitudes are taken from the literature andfrom measurements by COBE, and are corrected for interstellar andcircumstellar extinction. The sample contains stars of several spectraltypes: M, S and C, and of several variability classes: Mira, semiregularSRa, and SRb. We find that the distribution of stars in theperiod-luminosity plane is independent of circumstellar chemistry, butthat the different variability types have different P-L distributions.Both the Mira variables and the SRb variables have reasonablywell-defined period-luminosity relationships, but with very differentslopes. The SRa variables are distributed between the two classes,suggesting that they are a mixture of Miras and SRb, rather than aseparate class of stars. New period-luminosity relationships are derivedbased on our revised Hipparcos parallaxes. The Miras show a similarperiod-luminosity relationship to that found for Large Magellanic CloudMiras by Feast et al. (\cite{Feast-1989:a}). The maximum absolute Kmagnitude of the sample is about -8.2 for both Miras and semi-regularstars, only slightly fainter than the expected AGB limit. We show thatthe stars with the longest periods (P>400 d) have high mass lossrates and are almost all Mira variables.Based on observations from the Hipparcos astrometric satellite operatedby the European Space Agency (ESA \cite{Hipparcos}).Table \ref{Tab:data1} is 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/403/993
| 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
| The pulsation modes and masses of carbon-rich long period variables
Following our study of the carbon-rich giants in the HR diagram and oftheir luminosity function (Paper III), we investigate the pulsation dataof the long period variables (LPVs) included in our sample. Pulsationmodes (fundamental, overtone(s)) for carbon LPVs are identified in theperiod-radius diagram, making use of observed bi-periodicity in a smallsubsample of those stars, and of comparison to models. Mean pulsationmasses are then deduced from theoretical PMR-relations, with dueattention paid to a possible bias while averaging. Mean (present)pulsation masses (0.6 - 4.0 Msun) are found to increase alongthe group sequence HC5 to CV6, with still larger masses possiblyassociated with cool extreme CV7-objects with strong mass loss and thickcircumstellar shells. This is consistent with the 0.8-4 Msunrange of initial masses found in Paper III for the majority ofcarbon-rich giants affected by mass loss during their evolution. Thepulsation masses found for a few HC-stars (Mle0 .8 Msun) areconsistent with their low initial masses (Mi<~ 1.1Msun), as inferred from their thick disk membership (age =~11 Gyr?) and locus in the HR diagram. A mean pulsation mass of =~ 0.6Msun is found for the three population II Cepheids in thesample. A mass-luminosity diagram is proposed for the Galactic carbongiants. The data from observations is found consistent with theoreticalpredictions from AGB modeling, specially the third dredge-up (TDU)through thermal pulses (TP) with a carbon star formation line (CSFL) forTP-AGB stars. It appears that the CV-giants are close to the tip and endof their evolutionary tracks in the TP-AGB of the HR diagram. It isconfirmed that this end shifts toward lower effective temperatures andhigher luminosities, with increasing masses. It is shown that the C/Oabundance ratios do correlate with effective temperatures, according tothree distinct distributions (halo CH stars, thick disk HC-stars, andthin disk CV-stars). The mean stellar density decreases along theHC5-CV7 sequence, while the surface gravity remains nearly constant atabout 0.5 CGS unit (log g =~ -0.3; 5 x 10-3 SI). The natureof (thin disk) CV-stars as TP-AGB objects being confirmed, thediscussion is focused on (thick disk) HC-stars since the origin of theseold low-mass giants remains unclear. Unpredicted extra mixing on RGBand/or E-AGB is favored. Evolution from (old, low O/H) dwarf carbonstars is also considered since observations of metal-poor stars andrecent calculations point to large supersolar [C/Fe] ratios inPopulation III objects and contamination through rapid cycling in theinterstellar medium. This research has made use of the Simbad databaseoperated at CDS, Strasbourg, France. Partially based on data from theESA HIPPARCOS astrometry satellite.
| 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
| CHARM: A Catalog of High Angular Resolution Measurements
The Catalog of High Angular Resolution Measurements (CHARM) includesmost of the measurements obtained by the techniques of lunaroccultations and long-baseline interferometry at visual and infraredwavelengths, which have appeared in the literature or have otherwisebeen made public until mid-2001. A total of 2432 measurements of 1625sources are included, along with extensive auxiliary information. Inparticular, visual and infrared photometry is included for almost allthe sources. This has been partly extracted from currently availablecatalogs, and partly obtained specifically for CHARM. The main aim is toprovide a compilation of sources which could be used as calibrators orfor science verification purposes by the new generation of largeground-based facilities such as the ESO Very Large Interferometer andthe Keck Interferometer. The Catalog is 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/386/492, and from theauthors on CD-Rom.
| Thick disk and old disk carbon-rich giants in the Sun vicinity
Making use of the HIPPARCOS data and refining a previous study of thespace distribution of the carbon-rich giant stars located in thevicinity of the Sun (Paper I), we fully investigate their spacedistributions and space velocities on the basis of our photometricgrouping (CVi i.e. carbon variable stars with i=1 to 7; HCj i.e. hotcarbon stars with j=0 to 5). As expected, the CH stars (a subset of theHC stars delineated on the grounds of spectroscopic criteria) need to beconsidered separately. We also used groupings according to variabilityclasses. The various biases affecting the use of the data are taken intoaccount as far as possible. The mean distance to the Galactic plane ofthe faint ( >= -3.5) HC-stars amounts to 0.5kpc compared to 0.15 kpc for the bright <=-3.5) CV-stars. Exponentially decreasing distributions are fit withdistance scales of 0.95+/-0.06 kpc and 0.19 kpc respectively, and anormalization factor of 5.2% to 7.3% for the former component,compatible with a thick disk and thin disk respectively. Projectedsurface densities on the Plane are given with a total of about 76kpc-2, including 6% of CH stars and at least 18% for theother HC-stars (namely the HC'-sample). While halo-type velocities arefound for CH stars with a substantial drift of -112 km s-1,the solar reflex velocities and residual-velocity dispersions for theHC'-sample are about twice those of the CV-sample, close to thick diskand thin disk values respectively. In summary, we identify the HC-sampleas a component of the thick disk contaminated by the CH stars which area spheroidal contribution, and possibly by CV-stars at HC5. As expected,the CV-sample is a component of the old (thin) disk, dated from AVR, (3+/- 1 ) Gyr on average, but with a likely spread from a few108 Myr up to 8-12 Gyr. While the former (HC) represents veryold low mass stars (initial masses less than 1.15 Msun butsubject to mass-loss), the latter (CV) are younger stars with higherinitial masses on average (up to a few solar masses). The high frequencyof HC'-stars rules out models requiring rare events. Better modeling ofmixing events in low mass stars on the RGB and AGB could help. Lessdragged up carbon is needed to transform the low-mass stars with a lowO/H ratio into carbon giants. This research has made use of the Simbaddatabase operated at CDS, Strasbourg, France. Partially based on datafrom the ESA HIPPARCOS astrometry satellite.
| Nucleosynthesis and Mixing on the Asymptotic Giant Branch. III. Predicted and Observed s-Process Abundances
We present the results of s-process nucleosynthesis calculations forasymptotic giant branch (AGB) stars of different metallicities anddifferent initial stellar masses (1.5 and 3 Msolar), and wepresent comparisons of them with observational constraints fromhigh-resolution spectroscopy of evolved stars over a wide metallicityrange. The computations were based on previously published stellarevolutionary models that account for the third dredge-up phenomenonoccurring late on the AGB. Neutron production is driven by the13C(α,n)16O reaction during the interpulseperiods in a tiny layer in radiative equilibrium at the top of the He-and C-rich shell. The neutron source 13C is manufacturedlocally by proton captures on the abundant 12C; a few protonsare assumed to penetrate from the convective envelope into the radiativelayer at any third dredge-up episode, when a chemical discontinuity isestablished between the convective envelope and the He- and C-richzones. A weaker neutron release is also guaranteed by the marginalactivation of the reaction 22Ne(α,n)25Mgduring the convective thermal pulses. Owing to the lack of a consistentmodel for 13C formation, the abundance of 13Cburnt per cycle is allowed to vary as a free parameter over a wideinterval (a factor of 50). The s-enriched material is subsequently mixedwith the envelope by the third dredge-up, and the envelope compositionis computed after each thermal pulse. We follow the changes in thephotospheric abundance of the Ba-peak elements (heavy s [hs]) and thatof the Zr-peak ones (light s [ls]), whose logarithmic ratio [hs/ls] hasoften been adopted as an indicator of the s-process efficiency (e.g., ofthe neutron exposure). Our model predictions for this parameter show acomplex trend versus metallicity. Especially noteworthy is theprediction that the flow along the s-path at low metallicities drainsthe Zr and Ba peaks and builds an excess at the doubly magic208Pb, which is at the termination of the s-path. We thendiscuss the effects on the models of variations in the crucialparameters of the 13C pocket, finding that they are notcritical for interpreting the results. The theoretical predictions arecompared with published abundances of s-elements for AGB giants ofclasses MS, S, SC, post-AGB supergiants, and for various classes ofbinary stars, which supposedly derive their composition by mass transferfrom an AGB companion. This is done for objects belonging both to theGalactic disk and to the halo. The observations in general confirm thecomplex dependence of neutron captures on metallicity. They suggest thata moderate spread exists in the abundance of 13C that isburnt in different stars. Although additional observations are needed,it seems that a good understanding has been achieved of s-processoperation in AGB stars. Finally, the detailed abundance distributionincluding the light elements (CNO) of a few s-enriched stars atdifferent metallicities are examined and satisfactorily reproduced bymodel envelope compositions.
| Long period variable stars: galactic populations and infrared luminosity calibrations
In this paper HIPPARCOS astrometric and kinematic data are used tocalibrate both infrared luminosities and kinematical parameters of LongPeriod Variable stars (LPVs). Individual absolute K and IRAS 12 and 25luminosities of 800 LPVs are determined and made available in electronicform. The estimated mean kinematics is analyzed in terms of galacticpopulations. LPVs are found to belong to galactic populations rangingfrom the thin disk to the extended disk. An age range and a lower limitof the initial mass is given for stars of each population. A differenceof 1.3 mag in K for the upper limit of the Asymptotic Giant Branch isfound between the disk and old disk galactic populations, confirming itsdependence on the mass in the main sequence. LPVs with a thin envelopeare distinguished using the estimated mean IRAS luminosities. The levelof attraction (in the classification sense) of each group for the usualclassifying parameters of LPVs (variability and spectral types) isexamined. Table 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/cgi-bin/qcat?J/A+A/374/968 or via ASTRIDdatabase (http://astrid.graal.univ-montp2.fr).
| 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
| Stars with the Largest Hipparcos Photometric Amplitudes
A list of the 2027 stars that have the largest photometric amplitudes inHipparcos Photometry shows that most variable stars are all Miras. Thepercentage of variable types change as a function of amplitude. Thiscompilation should also be of value to photometrists looking forrelatively unstudied, but large amplitude stars.
| 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.
| Dust extinction and intrinsic SEDs of carbon-rich stars. II. The hot carbon stars
The present work is an extension of a recent study by Knapik &Bergeat (\cite{knapik}, henceforth called Paper I) of the spectralenergy distributions (SEDs) of about 300 cool carbon-rich variables andof the interstellar extinction observed on their line of sights. Themethods were originally developed for Semi-Regular (SR) and Irregular(L)-variables. Shortly, this is a kind of a pair method making usesimultaneously of the whole SED from UV to IR. Our approach is appliedhere to the galactic carbon-rich giants with bluer SEDs, namely the hotcarbon (HC) stars, including many ``constant'' stars and a minority ofvariables: AC Her a RV Tau star, the R Coronae Borealis (RCB) stars andothers. Some HdC (i.e. carbon-rich hydrogen deficient stars) and Ba IIstars are also considered. The total number of studied HC stars amountsto about 140. With few exceptions, the colour excesses for interstellarextinction are found in good agreement with the field values from mapspublished in the literature, taking into account the approximatedistances to our stars from HIPPARCOS data (\cite{esa}, henceforthcalled ESA) or binarity. We propose a classification scheme with sixphotometric groups (or boxes: HC0 to HC5) from the bluest to the reddestSEDs. Oxygen-rich SEDs earlier than HC0, are attributed to the hotteststars (AC Her, most RCB-variables and a few others). Previous findingsare confirmed of a junction between oxygen-rich and carbon-rich SEDs atspectral type G. The latest (HC5) group is immediately close to theearliest one in Paper I, namely CV1. The sequence of groups then goesregularly from HC0 to CV6. Substantial infrared excesses with respect toour solutions are found in HD 100764 a HC1 carbon star, AC Her a G0g RVTau star, and the RCB stars classified in either HC or oxygen-groups.The colour excesses at maximum light can usually be attributed tointerstellar reddening, with neutral circumstellar (CS) reddening (largegrains) or no CS extinction at all on the line of sight (non sphericalgeometry) as possible explanations. The latter model (disc or patchydistribution through successive puffs) is favoured. Two RCB variablesfor which we exploit SEDs on a rising branch (V CrA) or minimum light(RS Tel), show CS laws, respectively a selective extinction compatiblewith small grains and an extinction partly neutral indicative of largegrains on the line of sight. This research has made use of the Simbaddatabase operated at CDS, Strasbourg, France.}\fnmsep\thanks{Partiallybased on data from the ESA HIPPARCOS astrometrysatellite}\fnmsep\thanks{Tables~3 and 4 are only available in electronicform at the CDS via anonymous ftp 130.79.128.5
| Absolute magnitudes of carbon stars from HIPPARCOS parallaxes
Hipparcos trigonometric parallaxes and photometric data for about 40bright carbon stars have been analysed. Individual absolute visual andbolometric magnitudes, normal color indices (B-V)_0, absorption valuesand distance moduli were determined. By comparison with stellarevolutionary tracks for initial mass 1<= M/M_ȯ<=4 it is foundthat the majority of CH- and R-stars are on the giant and subgiantbranches, but N-stars occupy a region -4
| The PL relation of galactic carbon LPVs. The distance modulus to LMC
We present a period-luminosity (PL) diagram of 115 galactic carbon-richlong period variables (LPVs) observed by the HIPPARCOS satellite, in theform of the (MK,log P) relation. Our plot is compared to thediagram of carbon variables observed in the Large Magellanic Cloud(LMC). Both diagrams are found very similar and three samples aredelineated: long period variables close to the PL relation of Feast etal. (1989), short period-overluminous variables and a few underluminousLPVs, respectively Samples 1, 2 and 3. The used data were deduced fromexpectations of true parallaxes (Knapik et al. 1997) which arestatistically free of the Lutz-Kelker effect. The remaining bias due tothe non-gaussian distribution of absolute magnitudes is avoided: anon-linear parametric method is applied in Sect. 4 to the analysis ofthe PL relation for Sample 1 (72 LPVs). We obtainMK=(-3.99+/-0.13)log P+(2.07+/-0.15), in good agreement withthe slope found for LMC variables by Reid et al. (1995). The LMCdistance modulus then derived is mu =18.50+/-0.17. A well-defined upperlimit (ul) for long period stars in Sample 1 is found, with similarslopes in both the Galaxy (-4.85) and LMC (-4.72). No correction formetallicity was applied to the results. This research has made use ofthe Simbad database operated at CDS, Strasbourg, France.
| Lunar occultation measurements of stellar angular diameters
Not Available
| Interstellar extinction and the intrinsic spectral distribution of variable carbon stars.
We present a new method of evaluation of the extinction by interstellardust on cool carbon variables. These late-type stars show no markedrelationship between spectral classification (the R, N- and C-types) andphotometric colour indices. The pair method is thus ruled out, at leastin the form currently in use for early-type or intermediate stars. Ourmethod makes use of the whole spectral energy distributions from UV toIR. A sample of 60 unreddened carbon variables is delineated and newcolour-colour diagrams are proposed where the reddening vector is nearlyperpendicular to their narrow intrinsic locus. Six photometric groups(or boxes : CV1 to 6) are derived among unreddened stars. They show acontinuous range of spectral energy distributions from "bluer" to"redder", and mean colour indices are obtained. A pair method isdescribed where each presumably reddened star is compared to these meanunreddened stars, a given extinction law being assumed. As anillustration, the results are shown for a sample of 133 well-documentedstars. The mean extinction law usually adopted for the diffuseinterstellar medium (R_V_=~3.1) is shown to provide good fits. Thethreshold for reddening detection turns to be E(B-V)=~0.02-0.03A goodcorrelation is observed when the derived colour excesses are compared tovalues from maps in the literature. The mean rate of visual extinctionamounts to =~1.25+/-1.1 , ranging from 0.37 nearl=~240° (intercloud) to 2.1 (cloud + intercloud) in two structurescorrelated with Gould's belt.
| 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.
| A Moderate-Resolution Spectral Atlas of Carbon Stars: R, J, N, CH, and Barium Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1996ApJS..105..419B&db_key=AST
| Chemical composition of metal-poor carbon stars in the halo.
In an attempt to increase the sample of metal-deficient late-type (i.e.cool) halo carbon stars analysed (only 3 such stars have previously beenanalysed spectroscopically), we obtained high-resolution visual spectraof 5 more candidates (and analysed in addition existing archive IRspectra for one of the stars) from the recent catalogue of Sleivyt e& Bartkevicius (1990), HD 25408 (C5,3J), HD 42272 (C5,4 CH), HD59643 (C6,2CH), HD 189711 (C4,3 CH) and HD 197604 (C4,2 CH). From thespectra we have derived C/O ratios, N/C ratios, and metal abundances. Ifthe oxygen abundance was fixed at logA(O)=7.4/8.3 (assuming that itfollows the trend of oxygen overabundance relative to iron found in halostars in general) we can furthermore derive [C/Fe] and [N/Fe]. New modelatmospheres of metal-poor carbon stars were calculated with continuumopacity sources and molecular lines of CO, CN, C_2_, HCN, C_2_H_2_ andC_3_. Two of the stars, HD 25408 and HD 42272, turned out not to be CHstars. The other three stars, although late-type, showed the C/O and[Fe/H] ratios common in early-type CH stars. From the total sample ofthe six confirmed cool halo-CH stars now analysed, we find evidence thatnot all metal-poor low mass halo carbon stars can have formed due tomass transfer in binary systems, as is usually assumed. At least 3 ofthe stars, and possible more, are likely to have formed as intrinsiccarbon stars, with some similarities to the carbon star population inthe dwarf galaxies.
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Observation and Astrometry data
| Constellation: | Aries |
| Right ascension: | 02h15m00.08s |
| Declination: | +12°14'23.6" |
| Apparent magnitude: | 8.525 |
| Distance: | 689.655 parsecs |
| Proper motion RA: | 59.5 |
| Proper motion Dec: | 44 |
| B-T magnitude: | 11.28 |
| V-T magnitude: | 8.753 |
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