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Statistical Constraints for Astrometric Binaries with Nonlinear Motion
Useful constraints on the orbits and mass ratios of astrometric binariesin the Hipparcos catalog are derived from the measured proper motiondifferences of Hipparcos and Tycho-2 (Δμ), accelerations ofproper motions (μ˙), and second derivatives of proper motions(μ̈). It is shown how, in some cases, statistical bounds can beestimated for the masses of the secondary components. Two catalogs ofastrometric binaries are generated, one of binaries with significantproper motion differences and the other of binaries with significantaccelerations of their proper motions. Mathematical relations betweenthe astrometric observables Δμ, μ˙, and μ̈ andthe orbital elements are derived in the appendices. We find a remarkabledifference between the distribution of spectral types of stars withlarge accelerations but small proper motion differences and that ofstars with large proper motion differences but insignificantaccelerations. The spectral type distribution for the former sample ofbinaries is the same as the general distribution of all stars in theHipparcos catalog, whereas the latter sample is clearly dominated bysolar-type stars, with an obvious dearth of blue stars. We point outthat the latter set includes mostly binaries with long periods (longerthan about 6 yr).
| 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
| New periodic variables from the Hipparcos epoch photometry
Two selection statistics are used to extract new candidate periodicvariables from the epoch photometry of the Hipparcos catalogue. Theprimary selection criterion is a signal-to-noise ratio. The dependenceof this statistic on the number of observations is calibrated usingabout 30000 randomly permuted Hipparcos data sets. A significance levelof 0.1 per cent is used to extract a first batch of candidate variables.The second criterion requires that the optimal frequency be unaffectedif the data are de-trended by low-order polynomials. We find 2675 newcandidate periodic variables, of which the majority (2082) are from theHipparcos`unsolved' variables. Potential problems with theinterpretation of the data (e.g. aliasing) are discussed.
| 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).
| On the Variability of K5-M Stars
I investigate the Hipparcos Satellite photometry of K5-M stars to seethe pattern of activity of these stars. A few stars for which furtherstudy is desirable are identified.
| The 74th Special Name-list of Variable Stars
We present the Name-list introducing GCVS names for 3153 variable starsdiscovered by the Hipparcos mission.
| Revision and Calibration of MK Luminosity Classes for Cool Giants by HIPPARCOS Parallaxes
The Hipparcos parallaxes of cool giants are utilized in two ways in thispaper. First, a plot of reduced parallaxes of stars brighter than 6.5,as a function of spectral type, for the first time separates members ofthe clump from stars in the main giant ridge. A slight modification ofthe MK luminosity standards has been made so that luminosity class IIIbdefines members of the clump, and nearly all of the class III stars fallwithin the main giant ridge. Second, a new calibration of MK luminosityclasses III and IIIb in terms of visual absolute magnitudes has beenmade.
| Circumstellar shells and mass loss rates: Clues to the evolution of S stars
It is the purpose of this paper to rediscuss the circumstellarproperties of S stars and to put these properties in perspective withour current understanding of the evolutionary status of S stars, inparticular the intrinsic/extrinsic dichotomy. This dichotomy states thatonly Tc-rich (``intrinsic'') S stars are genuine thermally-pulsingasymptotic giant branch stars, possibly involved in the M-S-Cevolutionary sequence. Tc-poor S stars are referred to as ``extrinsic''S stars, because they are the cooler analogs of barium stars, and likethem, owe their chemical peculiarities to mass transfer across theirbinary system. Accordingly, an extensive data set probing thecircumstellar environment of S stars (IRAS flux densities, maseremission, CO rotational lines) has been collected and criticallyevaluated. This data set combines new observations (9 stars have beenobserved in the CO J=2-1 line and 3 in the CO J=3-2 line, with four newdetections) with existing material (all CO and maser observations of Sstars published in the literature). The IRAS flux densities of S starshave been re-evaluated by co-adding the individual scans, in order tobetter handle the intrinsic variability of these stars in the IRASbands, and possible contamination by Galactic cirrus. In the (K - [12],[25] - [60]) color-color diagram, S stars segregate into five distinctregions according to their Tc content and ZrO/TiO, C/O and IR spectralindices. Stars with photospheric colors (populating ``Region A'') may beidentified with extrinsic S stars. For the other regions characterizedby different excess levels in the 12, 25 and 60 mu m bands, severaldiagnostics (like the IRAS spectral class, maser emission, and shape ofCO rotational lines) have been collected to infer the physicalproperties of the dust shell. A simple radiative-transfer code has alsobeen used to infer the chemical nature (carbonaceous or silicate) of thedust grains from the observed IR colors. S stars with large K - [12]excesses and moderate [25] - [60] excesses (populating Regions B and C)exhibit the signatures of oxygen-rich shells (9.7 mu m silicate emissionand SiO maser emission). The situation is less clear for S stars withsmall K - [12] and moderate [25]-[60] indices (populating Regions D andE). Their IR colors are consistent with carbonaceous grains (as is theirfeatureless IRAS spectrum, and absence of silicate or SiO maseremission), but these features may equally well be explained by adetached shell. For many of these stars with a large 60 mu m excess, theshell is indeed resolved by the IRAS beam at 60 mu m. The prototypicalSC star FU Mon is among these. Since SC stars are believed to be in avery short-lived evolutionary phase where C/O = 1 within 1%, FU Mon maybe a good candidate for the ``interrupted mass-loss'' scenario advocatedby \cite[Willems & de Jong (1988).]{Wi88} The CO line profile of FUMon is also peculiar in being quite narrow (V_e = 2.8 km ssp {-1}),suggesting that the mass loss has just resumed in this star. Mass lossrates or upper limits have been derived for all S stars observed in theCO rotational lines, and range from < 2;10(-8) Msb ȯ y(-1) forextrinsic S stars to 1;10(-5) Msb ȯ y(-1) (the Mira S star W Aql).These mass-loss rates correlate well with the K - [12] color index,which probes the dust loss rate, provided that mathaccent 95 M ga 10({-)8} Msb ȯ y(-1) . Small mass-loss rates are found for extrinsic Sstars, consistent with their not being so evolved (RGB or Early-AGB) asthe Tc-rich S stars. This result does not support the claim often madein relation with symbiotic stars that binarity strongly enhances themass-loss rate. Based on observations carried out at the CaltechSubmillimeter Observatory (Mauna Kea, Hawaii).
| Classification and Identification of IRAS Sources with Low-Resolution Spectra
IRAS low-resolution spectra were extracted for 11,224 IRAS sources.These spectra were classified into astrophysical classes, based on thepresence of emission and absorption features and on the shape of thecontinuum. Counterparts of these IRAS sources in existing optical andinfrared catalogs are identified, and their optical spectral types arelisted if they are known. The correlations between thephotospheric/optical and circumstellar/infrared classification arediscussed.
| A catalogue of associations between IRAS sources and S stars.
Cross identifications between the General Catalogue of Galactic S Stars(GCGSS), the IRAS Point Source Catalogue (PSC), and the Guide StarCatalogue (GSC) are presented. The purpose of the present catalogue isi) to provide a clean sample of S stars with far-IR data, and ii) toprovide accurate GSC positions for S stars, superseding those listed inthe GCGSS. The IRAS colour-colour diagram and the galactic distributionof S stars associated with an IRAS source are presented. Several S starshaving extended images in at least one IRAS band have also beenidentified.
| Circumstellar Properties of S Stars. I. Dust Features
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1993ApJ...416..769C&db_key=AST
| Asymptotic giant branch stars near the sun
Available red and near-infrared photometry and apparent motions of M, S,and C asymptotic giant branch (AGB) stars in the Bright Star Catalogueare tabulated and discussed. It is shown that the red and near infraredindices normally used for late-type stars are interchangeable except forcarbon stars. The M-type giants are variable with visual amplitudegreater than 0.05 mag. The reddening-free parameter m2 from Genevaphotometry is essentially a temperature parameter for M giants, whilethe reddening-free parameter d is a sensitive detector of blue stellarcompanions. The space density of AGB stars near the sun decreases by afactor of 35 in a temperature range 3800 to 3400 K. Two of the S starsnear the sun were found to have nearly equal space motions and may becomembers of the Arcturus group.
| Third list of corrections to the identifications of IRAS sources in Astron. & Astrophys Suppl. 65, 607 and Astron. J. 98, 931
Not Available
| The Perkins catalog of revised MK types for the cooler stars
A catalog is presented listing the spectral types of the G, K, M, and Sstars that have been classified at the Perkins Observatory in therevised MK system. Extensive comparisons have been made to ensureconsistency between the MK spectral types of stars in the Northern andSouthern Hemispheres. Different classification spectrograms have beengradually improved in spite of some inherent limitations. In thecatalog, the full subclasses used are the following: G0, G5, G8, K0, K1,K2, K3, K4, K5, M0, M1, M2, M3, M4, M5, M6, M7, and M8. Theirregularities are the price paid for keeping the general scheme of theoriginal Henry Draper classification.
| Radial velocity monitoring of a sample of barium and S stars using CORAVEL - Towards an evolutionary link between barium and S stars?
The paper presents the preliminary results of a radial velocitymonitoring of a sample of 27 southern Ba II and 9 northern S stars,extending over three seasons, and performed with the CORAVELspectrometer. Both samples contained a large number of stars withvariable radial velocities. At least five S stars show velocityvariations originating in orbital motions, while Mira-type pulsations ofsmall amplitude may be a possibility for three more S stars displayingvelocity variations with dispersions in the interval of 1.0-1.5 km/s. Abinary scenario involving mass transfer and accounting for the dualorigin of S stars is suggested.
| IRAS catalogues and atlases - Atlas of low-resolution spectra
Plots of all 5425 spectra in the IRAS catalogue of low-resolutionspectra are presented. The catalogue contains the average spectra ofmost IRAS poiont sources with 12 micron flux densities above 10 Jy.
| Radial velocities of southern stars obtained with the photoelectric scanner CORAVEL. III - 790 late-type bright stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1985A&AS...59...15A&db_key=AST
| A General Catalogue of Galactic S-Stars - ED.2
Not Available
| The radial velocities of 116 southern red stars
Using a photoelectric speedometer based on the radial velocityspectrometer of Griffin (1967), radial velocities of 116 southern redstars, many of them semi-regular variables, were measured. Theinstrument was placed at the Newtonian focus of the 130-inch (4.2-m)camera of the Coude spectrograph of the Mount Stromlo 74-inch (1.88-m)reflector. The stellar spectrum was focused on a mask 50 mm in length,designed to match the spectrum of the M-giant Beta Pegasi. The inversedispersion was 2.5 angstroms per millimeter in the second order. Thewavelength range used (5338-5449 angstroms) was chosen because it isbetween two TiO bands and so suffers less blanketing in M stars. Resultsare tabulated and compared with standard values.
| Narrow-Band and Broad-Band Photometry of Red Stars. III. Southern Giants
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1970ApJ...161..199E&db_key=AST
| Estrellas Rojas entre Popa y Cruz.
Not Available
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Pozíciós és asztrometriai adatok
| Csillagkép: | Hajófar |
| Rektaszcenzió: | 08h23m17.20s |
| Deklináció: | -38°17'09.0" |
| Vizuális fényesség: | 6.32 |
| Távolság: | 429.185 parszek |
| RA sajátmozgás: | 0.7 |
| Dec sajátmozgás: | 0.4 |
| B-T magnitude: | 8.421 |
| V-T magnitude: | 6.502 |
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