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An HI interstellar bubble surrounding WR85 and RCW118
We analyse the distribution of the interstellar matter in the environsof the Wolf-Rayet star LSS3982 (= WR85, WN6+OB?) linked to the opticalring nebula RCW118. Our study is based on neutral hydrogen 21-cm linedata belonging to the Southern Galactic Plane Survey (SGPS).The analysis of the HI data allowed the identification of a neutralhydrogen interstellar bubble related to WR85 and the 25-arcmin-diameterring nebula RCW118. The HI bubble was detected at a systemic velocity of-21.5 km s-1, corresponding to a kinematical distance of 2.8+/- 1.1 kpc, compatible with the stellar distance. The neutral structureis about 25 arcmin in radius or 21 +/- 8 pc, and is expanding at 9 +/- 2km s-1. The associated ionized and neutral masses amount to3000 Msolar. The carbon monoxide (CO) emission distributiondepicts a region lacking CO coincident in position and velocity with theHI structure. The 9.3-arcmin-diameter inner optical nebula appears to berelated to the approaching part of the neutral atomic shell. The HI voidand shell are the neutral gas counterparts of the optical bubble andhave very probably originated in the action of the strong stellar windof the central star during the O-type and WR phases on the surroundinginterstellar medium. The HI bubble appears to be in the momentumconserving stage.
| 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
| Dynamical masses of young star clusters in NGC 4038/4039
In order to estimate the masses of the compact, young star clusters inthe merging galaxy pair, NGC 4038/4039 (``the Antennae''), we haveobtained medium and high resolution spectroscopy using ISAAC on VLT-UT1and UVES on VLT-UT2 of five such clusters. The velocity dispersions wereestimated using the stellar absorption features of CO at 2.29 mu m andmetal absorption lines at around 8500 Å, including lines of theCalcium Triplet. The size scales and light profiles were measured fromHST images. From these data and assuming Virial equilibrium, weestimated the masses of five clusters. The resulting masses range from6.5 x 105 to 4.7 x 106 Msun. Thesemasses are large, a factor of a few to more than 10 larger than thetypical mass of a globular cluster in the Milky Way. The mass-to-lightratios for these clusters in the V- and K-bands in comparison withstellar synthesis models suggest that to first order the IMF slopes areapproximately consistent with Salpeter for a mass range of 0.1 to 100Msun. However, the clusters show a significant range ofpossible IMF slopes or lower mass cut-offs and that these variations maycorrelate with the interstellar environment of the cluster. Comparisonwith the results of Fokker-Planck simulations of compact clusters withproperties similar to the clusters studied here suggest that they arelikely to be long-lived and may lose a substantial fraction of theirtotal mass. This mass loss would make the star clusters obtain masseswhich are comparable to the typical mass of a globular cluster. Based onobservations collected at the European Southern Observatory, Chile.
| 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 (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcar?J/A+A/367/521
| The ROSAT all-sky survey catalogue of optically bright late-type giants and supergiants
We present X-ray data for all late-type (A, F, G, K, M) giants andsupergiants (luminosity classes I to III-IV) listed in the Bright StarCatalogue that have been detected in the ROSAT all-sky survey.Altogether, our catalogue contains 450 entries of X-ray emitting evolvedlate-type stars, which corresponds to an average detection rate of about11.7 percent. The selection of the sample stars, the data analysis, thecriteria for an accepted match between star and X-ray source, and thedetermination of X-ray fluxes are described. Catalogue only available atCDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| The yellow hypergiants
We list the main stellar data of known hypergiants and similarlyluminous stars, and then concentrate on a review of the yellowhypergiants. These stars are post-red supergiants evolving alongblueward loops in the Hertzsprung-Russell diagram. Their properties,their location in the Hertzsprung-Russell diagram and their occasionalmass ejections are related to a region of atmospheric instability in theH-R diagram, the Yellow Void. The `bouncing against the border of theVoid' of three objects: ρ Cas, HR8752 and IRC+10420, is described.The apparent atmospheric instability of yellow hypergiants is related tothe atmospheric pulsations. There are indications that the approach tothe Void is associated with an increased amplitude of the pulsation andwith enhanced mass loss. The observed small-scale motion field is onlyapparently strongly supersonic; the observed large stochastic velocitiesare the quasi-stochastically varying thermal motions in the many hotsheets that occur in the wakes of many small shocks, while the realhydrodynamic velocity component is small and subsonic. This shock-wavefield is also responsible for the observed rate of mass loss and foremission in the wings of Hα . Most yellow hypergiants haveenvelopes containing gas and dust, but a thick extended envelope,presumably dissipating and showing bipolar outflow, is only known aroundIRC+10420. At the interface of the bipolar wind and the interstellarmedium one or more stationary shocks may develop as is observed in thecase of IRC+10420 and suspected with ρ Cas.
| 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.
| An IRAS-based Search for New Dusty Late-Type WC Wolf-Rayet Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995ApJS..100..413C&db_key=AST
| A spectroscopic database for Stephenson-Sanduleak Southern Luminous Stars
A database of published spectral classifications for objects in theStepenson-Sanduleak Luminous Stars in the Southern Milky Way catalog hasbeen compiled from the literature. A total of 6182 classifications for2562 stars from 139 sources are incorporated.
| 1612 MHz OH survey of IRAS point sources. I - Observations made at Dwingeloo, Effelsberg and Parkes
The data from a large sky survey are presented including a northernpilot study and a detailed southern study in which detections are biasedtoward the most evolved sources and distant sources. Both areinvestigated at the 1612-MHz transition of OH to take advantage of thestrongest line for AGB stars with optically thick dust shells. The IRASsources are chosen by considering their IR colors related to fluxes at12, 25, and 60 microns. Observations are reported for 2703 IRAS pointsources at the 1612-MHz transition, and 738 OH/IR stars are detected.The survey identifies 597 of the sources as previously unidentified, and95 percent of the OH profiles observed have twin-peak masercharacteristics which are related to emission from expandingcircumstellar shells. The other 5 percent of the sources are concludedto be transition objects between OH/IR stars and planetary nebulae.
| Near infrared spectra of RV Tauri stars
Medium resolution spectrograms of the near infrared spectral region in asample of RV Tauri stars with spectral types F and early G have beencompared with those of a sample of population I objects. It is shownthat the equivalent widths of Ca II infrared triplet and Paschen linesallow to separate RV Tauri stars from population I supergiants.Moreover, the possibility of using the O I triplet at 7774 A as a toolfor testing the period-luminosity relation for RV Tauri stars isdiscussed.
| 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.
| Colour excesses and absolute magnitudes for non-Cepheid F-G supergiants from uvbybeta photometry
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1990A&A...239..205A&db_key=AST
| A list of MK standard stars
Not Available
| Supergiants and the Galactic metallicity gradient. II - Spectroscopic abundances for 64 distant F- to M-type supergiants
The metallicity gradient in the Galactic disk from in situ stars withvisual magnitude ranging from 6 to 10 is analyzed. Atmosphericparameters and detailed chemical abundances for 64 Population Isupergiants of spectral types F through M and luminosity classes Iathrough II have been determined. The derived Fe/H ratios ranging from-0.5 to + 0.7 show a mean value of +0.13 with an estimated uncertaintyof + or - 0.2. A subset of 25 supergiants fainter than 7th magnitudelying in the direction of the Galactic center shows a Fe/H mean of +0.18+ or - 0.04, while a similar sample of 15 faint supergiants lying in thedirection of the Galactic anticenter shows a lower Fe/H mean of +0.07 +or - 0.06. For a sample of bright supergiants analyzed by Luck andLambert (1985), the mean abundance pattern for all 64 stars showed thefollowing: deficient C and O along with enhancement of N, indicatingmixing of CNO-cycled material to the stellar surfaces; an apparent Srenhancement attributed to departures from LTE; and an essentially solarpattern of other chemical elements.
| 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.
| Narrowband photometry of luminosity class I stars
Observational data in the alpha(16)Lambda(9) photometric system arepresented for 60 supergiant stars of luminosity class I, from O5 to K3.The results show a good affinity between the equivalent widths of thehydrogen H-alpha line and of the O I triplet at a wavelength of 7774 Awith the alpha(16) and Lambda(9) indices. The comparison betweenspectral type and each photometric index is also illustrated. Allsupergiant stars except four are separated from main-sequence stars, inthe alpha(16)Lambda(9) array.
| A multifrequency study of circumstellar envelopes of cool giants and supergiants
A multifrequency study of all parts of circumstellar envelopes of coolgiants and supergiants is presented. In order to investigate theinfluence of stellar parameters on spectral features of these envelopes,a sample of 77 cool giants and supergiants that occupies a horizontalstrip in the Hertzsprung-Russell diagram was observed. Spectroscopic andphotometric observations at optical, infrared and radio wavelengths ledto the following results: (1) for giants there exists a strongcorrelation between H-alpha emission and SiO masers, which led to thesuggestion that SiO masers are triggered by shock-waves and can bepumped by collisions, (2) the SiO expansion velocity was found to besystematically lower by 2 km/s compared to the CO expansion velocity,and (3) a relation between the asymmetry of the light curve and theintensity of the dust emission at 9.7 microns has been confirmed for awide range of periods. Rather than luminosity alone, pulsationalproperties of the variable play a dominant role for the structure ofcircumstellar envelopes of cool giants and supergiants.
| 1988 Revised MK Spectral Standards for Stars GO and Later
Not Available
| Optical properties of circumstellar silicates in the visible and the near-infrared
The results of Papoular and Pegourie (1983) and Pegourie and Papoular(1985) on modeling the IR emission of a sample of O-rich giants andsupergiants are used to deduce the optical properties of circumstellarsilicates in the visible and the near-IR. It is shown that the energybalance between the total energy radiated by the shell and that which itabsorbs from the star makes it possible to stongly constrain the opticalproperties of the grain material and to determine the refraction index.Planck mean efficiencies both for emissivity and radiation pressure arecalculated for the temperature and grain radius ranges of interest forcomputations of a red giant environment.
| Ultraviolet survey for hot companions among nonvariable yellow supergiants
Twenty nonvariable yellow supergiants have been observed for the firsttime with the International Ultraviolet Explorer satellite, with the aimof discovering hot companions. Two newly discovered systems areannounced: HD 74395 (G2 I + B9.5 IV-V) and HD 193469 (later than G0 + B8IV-V). The Cepheid HD 9250 was also observed, but no hot companion wasfound. Some stars independently known to have a hot companion wereincluded in order to study the properties of the companions and tocompare with previous work. Atmospheric models were used to fit theoverall energy distribution of the binary system, allowing an estimateof Te, log g, and the spectral type of the companion. The magnitudedifferences, in the V band, between the yellow supergiants and theircompanions were calculated. The possibility of using this magnitudedifference and the spectral type determined for the hot companions toestimate M(v) for the yellow supergiants and the distance to the systemsis explored. Comparison of the binaries' positions in the H-R diagramwith theoretical evolutionary tracks suggests that the masses of theprimaries are contained between 5 and 9 solar masses and that, onaverage, they are about twice as massive as their hot companions.
| An IRAS survey of IR excesses in G-type stars
The IRAS Point Source Catalog has been searched for infrared sourcesassociated with G-type stars. Of the 3803 IRAS sources identified inthis way, 28 were found to have enhanced emission at lambda greater than25 microns characteristic of circumstellar material. The majority of theIR-excess stars were supergiants whose inferred mass loss rates werefound to be comparable to those of red giants. One of the stars, IRAS11059-7721, is a G main-sequence star whose circumstellar medium (CSM)has 20,000 times the optical depth of Vega's CSM. The physicalcharacteristics of the circumstellar emission for this sample aredescribed, and several scenarios for its existence are examined in lightof the IRAS data.
| 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.
| A photometric determination of the metal content for F-G type supergiants in the Large Magellanic Cloud
A VBLUW photometric analysis is used to derive the metal content of some100 F- and G type supergiants in the LMC. Using the empirical locus ofPel in the V-B/B-L diagram in conjunction with the relative dependenceof theoretical colors on the metal abundance, a metal deficiency of1.4-1.6 is found for the LMC stars in comparison with those in the solarneighborhood. With an average UBV system foreground reddening of E(B-V)= 0.05 for the LMC, these stars have a metal content of 0.66 + 0.11,-0.03 of the solar abundance. Agreement is found with the result ofprevious studies. Application to the derivation of the reddenings ofmost of the galactic supergiants is noted.
| IRAS observations of the cool galactic hypergiants
Not Available
| The optical properties of dust in the mid-IR silicate bands
A study of the emission silicate features of 10 supergiants and S Lep,which are all in the solar region of the Galaxy, is discussed. Theoptical efficiency of the circumstellar grain material of M stars isdeduced over the range 8-30 microns. It is shown that the efficiencyclearly peaks at 10 microns and is analogous to that of amorphousMg2SiO4. A similar procedure, using 13 available spectra of protostellarobjects, shows that the dust in molecular clouds and in the ISM, iscomposed of small (less than 1 micron) grains with an optical extinctionefficiency peaking at 9.5 microns and practically identical to that ofamorphous MgSiO3. Combining the two kinds of dust, and allowing forgrain sizes greater than 1 micron, it is possible to reproduce the wide10-micron features emitted by M giants with more or less thick shells.Using the results of meteoritic chemical analysis and of the theory ofcomposite gas condensation, the likelihood of amorphous MgSiO4 andMgSiO3 being present in circumstellar and interstellar dust,respectively, is evaluated.
| Wolf-Rayet stars in clusters - The initial stellar masses and evolutionary connections between subtypes
The membership of Wolf-Rayet stars in open clusters and OB associationsis used to determine the initial mass Mi of stars becoming WR stars. Adetailed discussion of the relation between the spectral types of thecluster turnoff and the initial mass of WR stars is made on the basis ofstellar models. Lower limits 18 solar mass for WN stars and 35 solarmass for WC stars are obtained. From the study of WR stars in clustersand associations evolutionary connections are established between WRsubtypes. The most massive stars (Mi greater than about 60 solar mass)evolve via WN7 into WC4-WC8 stars. In the mass range Mi = 35-60 solarmass an evolutionary sequence WN5, WN6 to WC8.5, WC9 to WO is found.From initial masses lower than 35 solar mass mainly WN3, WN4, and WN5stars can be formed. Binary evolution appears to have a negligibleeffect on the lower limit of initial mass but introduces a systematicdeviation into the evolutionary sequences mentioned above. Particularly,the WR subtypes formed by close binaries are generally earlier thanthose formed by single stars of the same initial mass.
| 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.
| The spectra of Wolf-Rayet stars. I - Optical line strengths and the hydrogen-to-helium ratios in WN type stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1983ApJ...268..228C&db_key=AST
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| Csillagkép: | Skorpió |
| Rektaszcenzió: | 17h14m27.70s |
| Deklináció: | -39°46'01.0" |
| Vizuális fényesség: | 6.6 |
| Távolság: | 10000000 parszek |
| RA sajátmozgás: | -1.2 |
| Dec sajátmozgás: | -2.4 |
| B-T magnitude: | 9.576 |
| V-T magnitude: | 6.737 |
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