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Публикации по объекту
A catalog of bright calibrator stars for 200-m baseline near-infrared stellar interferometry
We present in this paper a catalog of reference stars suitable forcalibrating infrared interferometric observations. In the K band,visibilities can be calibrated with a precision of 1% on baselines up to200 meters for the whole sky, and up to 300 meters for some part of thesky. This work, extending to longer baselines a previous catalogcompiled by Bordé et al. (2002, A&A, 393, 183), isparticularl y well adapted to hectometric-class interferometers such asthe Very Large Telescope Interferometer (VLTI, Glindemann et al. 2003,Proc. SPIE, 4838, 89) or the CHARA array (ten Brummelaar et al. 2003,Proc. SPIE, 4838, 69) when one is observing well-resolved, high-surfacebrightness objects (K 8). We use the absolute spectro-photometriccalibration method introduced by Cohen et al. (1999, AJ, 117, 1864) toderive the angular diameters of our new set of 948 G8-M0 calibratorstars extracted from the IRAS, 2MASS and MSX catalogs. Angular stellardiameters range from 0.6 mas to 1.8 mas (median is 1.1 mas) with amedian precision of 1.35%. For both the northern and southernhemispheres, the closest calibrator star is always less than 10°away.
| 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
| The Globular Cluster Systems of the Sculptor Group
We use CTIO 4 m Mosaic II images taken with the Washington CM and HarrisR filters to identify candidate globular clusters in the six majorgalaxies of the Sculptor group: NGC 45, 55, 247, 254, 300, and 7793.From follow-up spectroscopy with Hydra-CTIO, we find 19 new globularclusters in NGC 55, 247, 253, and 300, bringing the total number ofknown Sculptor group globular clusters to 36. The newly discoveredclusters have spectroscopic ages consistent with those of old Milky Wayglobular clusters, and the majority are metal-poor. Their luminosityfunction closely resembles that of the Milky Way's globular clusters;their metallicity distribution is somewhat more metal-rich, but this maybe the result of our color selection of candidates. The mean[α/Fe] ratio in the clusters is -0.2+/-0.3, which is lower thanthe Milky Way average. The specific frequencies SN aresimilar to those of other late-type galaxies. However, if we calculatethe specific frequency using the K-band total magnitudes of the hostgalaxies, we find values that are more than a factor of 2 higher. Thekinematics of the globular cluster systems are consistent with rotationwith the H I disk in each of the four galaxies; however, only in NGC 253is this result based on more than seven objects. We suggest that theSculptor group galaxies add to evidence indicating that many of thefirst-generation globular clusters formed in disks, not halos.
| The Evolution of Massive Stars. I. Red Supergiants in the Magellanic Clouds
We investigate the red supergiant (RSG) content of the SMC and LMC usingmultiobject spectroscopy on a sample of red stars previously identifiedby BVR CCD photometry. We obtained high-accuracy (<1 kms-1) radial velocities for 118 red stars seen toward the SMCand 167 red stars seen toward the LMC, confirming most of these (89% and95%, respectively) as red supergiants. Spectral types were alsodetermined for most of these RSGs. We find that the distribution ofspectral types is skewed toward earlier type at lower metallicities: theaverage (median) spectral type is K5-K7 I in the SMC, M1 I in the LMC,and M2 I in the Milky Way. Our examination of the Kurucz ATLAS9 modelatmospheres suggests that the effect that metallicity has on theappearance on the TiO lines is probably sufficient to account for thiseffect, and we argue that RSGs in the Magellanic Clouds are 100 K (LMC)and 300 K (SMC) cooler than Galactic stars of the same spectral types.The colors of the Kurucz models are not consistent with thisinterpretation for the SMC, although other models (e.g., Bessell et al.)show good agreement. A finer grid of higher resolution synthetic spectraappropriate to cool supergiants is needed to better determine theeffective temperature scale. We compare the distribution of RSGs in theH-R diagram to that of various stellar evolutionary models; we find thatnone of the models produce RSGs as cool and luminous as what is actuallyobserved. This result is much larger than any uncertainty in theeffective temperature scale. We note that, were we to simply adopt theuncorrected Galactic effective scale for RSGs and apply this to oursample, then the SMC's RSGs would be underluminous compared with theLMC's, contrary to what we expect from stellar evolution considerations.In all of our H-R diagrams, however, there is an elegant sequence ofdecreasing effective temperatures with increasing luminosities;explaining this will be an important test of future stellar evolutionarymodels. Finally, we compute the blue-to-red supergiant ratio in the SMCand LMC, finding that the values are indistinguishable (~15) for the twoClouds. We emphasize that ``observed'' B/R values must be carefullydetermined if a comparison with that predicted by stellar models is tobe meaningful. The nonrotation Geneva models overestimate the number ofblue to red supergiants for the SMC, but underestimate it for the LMC;however, given the inability to produce high-luminosity RSGs in themodels that match what is observed in the H-R diagram, such adisagreement is not surprising.
| Sixth Catalogue of Fundamental Stars (FK6). Part III. Additional fundamental stars with direct solutions
The FK6 is a suitable combination of the results of the HIPPARCOSastrometry satellite with ground-based data, measured over a longinterval of time and summarized mainly in the FK5. Part III of the FK6(abbreviated FK6(III)) contains additional fundamental stars with directsolutions. Such direct solutions are appropriate for single stars or forobjects which can be treated like single stars. Part III of the FK6contains in total 3272 stars. Their ground-based data stem from thebright extension of the FK5 (735 stars), from the catalogue of remainingSup stars (RSup, 732 stars), and from the faint extension of the FK5(1805 stars). From the 3272 stars in Part III, we have selected 1928objects as "astrometrically excellent stars", since their instantaneousproper motions and their mean (time-averaged) ones do not differsignificantly. Hence most of the astrometrically excellent stars arewell-behaving "single-star candidates" with good astrometric data. Thesestars are most suited for high-precision astrometry. On the other hand,354 of the stars in Part III are Δμ binaries in the sense ofWielen et al. (1999). Many of them are newly discovered probablebinaries with no other hitherto known indication of binarity. The FK6gives, besides the classical "single-star mode" solutions (SI mode),other solutions which take into account the fact that hidden astrometricbinaries among "apparently single-stars" introduce sizable "cosmicerrors" into the quasi-instantaneously measured HIPPARCOS proper motionsand positions. The FK6 gives, in addition to the SI mode, the "long-termprediction (LTP) mode" and the "short-term prediction (STP) mode". TheseLTP and STP modes are on average the most precise solutions forapparently single stars, depending on the epoch difference with respectto the HIPPARCOS epoch of about 1991. The typical mean error of anFK6(III) proper motion in the single-star mode is 0.59 mas/year. This isa factor of 1.34 better than the typical HIPPARCOS errors for thesestars of 0.79 mas/year. In the long-term prediction mode, in whichcosmic errors are taken into account, the FK6(III) proper motions have atypical mean error of 0.93 mas/year, which is by a factor of about 2better than the corresponding error for the HIPPARCOS values of 1.83mas/year (cosmic errors included).
| Kinematics of the Galactic Globular Cluster System: New Radial Velocities for Clusters in the Direction of the Inner Galaxy
The High-Resolution Echelle Spectrometer (HIRES) on the Keck I telescopehas been used to measure the first radial velocities for stars belongingto 11 heavily reddened globular clusters in the direction of the innerGalaxy. The sample consists of the clusters Terzan 3, NGC 6256, IC 1257,NGC 6380 (=Ton 1), Ton 2 (=Pismis 26), Djorg 1, NGC 6540 (=Djorg 3), IC1276 (=Pal 7), Terzan 12, NGC 6749, and Pal 10. Candidate clustermembers were selected from a combination of previously publishedcolor-magnitude diagrams (CMDs) and new instrumental CMDs obtained withthe Palomar 1.5 m telescope. The systemic velocities of Djorg 1 and Pal10 should be considered provisional, since velocities are available foronly two stars. For the remaining nine clusters, we have measured radialvelocities for three to nine member stars. Using our HIRES spectra, weestimate metallicities of [Fe/H]~=-0.75 for both Terzan 3 and IC 1276,two clusters lacking previous metallicity estimates. The question ofkinematic substructuring among the Galactic globular clusters isinvestigated using an updated catalog of globular cluster distances,metallicities, and velocities. It is found that the population ofmetal-rich globular clusters shows significant rotation at allGalactocentric radii. For the metal-rich clusters within 4 kpc of theGalactic center, the measured rotation velocity and line-of-sightvelocity dispersion are similar to those of bulge field stars. Weinvestigate claims that the metal-rich clusters are associated with thecentral Galactic bar by comparing the kinematics of the innermostclusters to that of the atomic hydrogen in the inner Galaxy. Thelongitude-velocity diagram of both metal-rich and metal-poor clustersbears a remarkable similarity to that of the gas, including the samenoncircular motions that have traditionally been interpreted as evidencefor a Galactic bar, or, alternatively, a nonaxisymmetric bulge. However,uncertainties in the existing three-dimensional Galactocentric positionsfor most of the clusters do not yet allow an unambiguous discriminationbetween the competing scenarios of membership in a rigidly rotating baror in a bulge that is an oblate isotropic rotator. We conclude that themajority of metal-rich clusters within the central ~4 kpc of the Galaxyare probably associated with the bulge/bar, and not the thick disk.
| Radial velocities. Measurements of 2800 B2-F5 stars for HIPPARCOS
Radial velocities have been determined for a sample of 2930 B2-F5 stars,95% observed by the Hipparcos satellite in the north hemisphere and 80%without reliable radial velocity up to now. Observations were obtainedat the Observatoire de Haute Provence with a dispersion of 80Ä,mm(-1) with the aim of studying stellar and galactic dynamics.Radial velocities have been measured by correlation with templates ofthe same spectral class. The mean obtained precision is 3.0 km s(-1)with three observations. A new MK spectral classification is estimatedfor all stars. Based on observations made at the Haute ProvenceObservatory, France and on data from The Hipparcos Catalogue, ESA.Tables 4, 5 and 6 are only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr or viahttp://cdsweb.u-strasbg.fr/Abstract.htm
| Catalogs of temperatures and [Fe/H] averages for evolved G and K stars
A catalog of mean values of [Fe/H] for evolved G and K stars isdescribed. The zero point for the catalog entries has been establishedby using differential analyses. Literature sources for those entries areincluded in the catalog. The mean values are given with rms errors andnumbers of degrees of freedom, and a simple example of the use of thesestatistical data is given. For a number of the stars with entries in thecatalog, temperatures have been determined. A separate catalogcontaining those data is briefly described. Catalog only available atthe CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Spectroscopy of the optical Einstein ring 0047-2808
We present optical and near-infrared spectroscopic observations of theoptical Einstein ring 0047-2808. We detect both [O III] lineslambdalambda4959, 5007 near ~2.3mum, confirming the redshift of thelensed source as z=3.595. The Lyalpha line is redshifted relative to the[O III] line by 140+/-20kms^-1. Similar velocity shifts have been seenin nearby starburst galaxies. The [O III] line is very narrow, 130kms^-1FWHM. If the ring is the image of the centre of a galaxy, theone-dimensional stellar velocity dispersion sigma=55kms^-1 isconsiderably smaller than the value predicted by Baugh et al. for thesomewhat brighter Lyman-break galaxies. The Lyalpha line issignificantly broader than the [O III] line, probably due to resonantscattering. The stellar central velocity dispersion of the early-typedeflector galaxy at z=0.485 is 250+/-30kms^-1. This value is in goodagreement both with the value predicted from the radius of the Einsteinring (and a singular isothermal sphere model for the deflector), andwith the value estimated from the D_n-sigma relation.
| The Kinematics, Orbit, and Survival of the Sagittarius Dwarf Spheroidal Galaxy
\Sgr\ galaxy, the closest satellite galaxy of the Milky Way, hassurvived for many orbits about the Galaxy. Extant numerical calculationsmodeled this galaxy as a system with a centrally-concentrated massprofile, following the light, and found that it should lose more thanone-half of its mass every 2-4 orbits and be completely disrupted longbefore now. Apparently \sgr, and by implication other dSph galaxies, donot have a centrally-concentrated profile for their dark matter. Wedevelop a model in which the stars of the Sgr dwarf are embedded in aconstant-density dark matter halo, representing the core of atidally-limited system, and show that this is consistent with itssurvival. We present new photometric and kinematic observations of \sgr\and show these data are consistent with this explanation for thecontinued existence of this galaxy. \Sgg\ is being tidally distorted andis tidally limited, but is not disrupted as yet. The correspondingminimum total mass is 10(9) msun , while the central mass to visuallight ratio ~ 50 in Solar units. Our new photographic photometry allowsthe detection of main-sequence stars of \sgg\ over an area of 22deg x8deg . \Sgg\ is prolate, with axis ratios ~ 3:1:1. For an adopteddistance of 16 +/- 2 kpc from the Galactic center on the opposite sideof the Galaxy to the Sun, the major axis is gta 9 kpc long and isaligned approximately normal to the plane of the Milky Way Galaxy,roughly following the coordinate line l=5(deg) . The central velocitydispersion of giant stars which are members of \sgg\ is 11.4 +/- 0.7 kmsand is consistent with being constant over the face of the galaxy. Thegradient in mean line-of-sight velocity with position along the majoraxis, dv/db, is ~ 0 kms /degree in the central regions and increases inamplitude to dv/db=-3 kms /degree over the outermost three degrees forwhich we have data. A first measurement of the proper motion of Sgrdetermines the component of its space velocity parallel to its majoraxis to be 250 +/- 90 kms , directed towards the Galactic Plane. Wemodel these kinematic data to determine the orbit of \sgg. Our best fitmodel has an orbital period of lta 1 Gyr and has \sgr close toperigalacticon. This period is shorter, by about a factor of ~ gt 10,than the age of the bulk of its stellar population.
| Core velocity dispersions for 25 Galactic and 10 old Magellanic globular clusters.
We present, for 25 Galactic and 10 old Magellanic globular clusters,projected velocity dispersion (σ_p_) measurements obtained byapplying a cross-correlation technique to integrated-light spectra. Inorder to understand and estimate the statistical errors of thesemeasurements due to small numbers of bright stars dominating theintegrated light, we provide an extensive discussion based on detailednumerical simulations. These errors are smaller if the integration areais larger and/or the cluster concentration higher. The simulations showthat measurements are reliable when the integrated light within theintegration area is brighter than a given magnitude. The statisticalerrors on the σ_p_ measurements of Magellanic globular clustersare small because of a physically large integration area, whereas theycan be important for measurements carried out over small central areasin Galactic clusters. The present observational results are used tooutline a few characteristics of the globular cluster fundamental plane.In this respect, the old Magellanic globular clusters appear similar tothe Galactic clusters.
| 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.
| The position corrections of 1400 stars observed with PA II in San Juan.
Not Available
| High resolution kinematics of galactic globular clusters.
We present integrated central velocity dispersions for 7 globularclusters, three of which known to be post core-collapsed. Discussion ofthe statistical significance of the measurements is presented. For oneof the clusters, M30, we also provide radial velocities of 16 stars,which help mapping the inner velocity dispersion profile. Our datasuggest that M30 has more likely an isothermal core, at variance withthe behavior of its closest twin M15.
| Fifth fundamental catalogue. Part 2: The FK5 extension - new fundamental stars
The mean positions and proper motions for 3117 new fundamental starsessentially in the magnitude range about 4.5 to 9.5 are given in thisFK5 extension. Mean apparent visual magnitude is 7.2 and is on average2.5 magnitudes fainter then the basic FK5 which has a mean magnitude of4.7. (The basic FK5 gives the mean positions and proper motions for theclassical 1535 fundamental stars). The following are discussed: theobservational material, reduction of observations, star selection, andthe system for the FK5 extension. An explanation and description of thecatalog are given. The catalog of 3117 fundamental stars for the equinoxand epoch J2000.0 and B1950.0 is presented. The parallaxes and radialvelocities for 22 extension stars with large forecasting effects aregiven. Catalogs used in the compilation of the FK5 fundamental catalogare listed.
| A critical appraisal of published values of (Fe/H) for K II-IV stars
'Primary' (Fe/H) averages are presented for 373 evolved K stars ofluminosity classes II-IV and (Fe/H) values beween -0.9 and +0.21 dex.The data define a 'consensus' zero point with a precision of + or -0.018 dex and have rms errors per datum which are typically 0.08-0.16dex. The primary data base makes recalibration possible for the large(Fe/H) catalogs of Hansen and Kjaergaard (1971) and Brown et al. (1989).A set of (Fe/H) standard stars and a new DDO calibration are given whichhave rms of 0.07 dex or less for the standard star data. For normal Kgiants, CN-based values of (Fe/H) turn out to be more precise than manyhigh-dispersion results. Some zero-point errors in the latter are alsofound and new examples of continuum-placement problems appear. Thushigh-dispersion results are not invariably superior to photometricmetallicities. A review of high-dispersion and related work onsupermetallicity in K III-IV star is also given.
| A search for lithium-rich giant stars
Lithium abundances or upper limits have been determined for 644 brightG-K giant stars selected from the DDO photometric catalog. Two of thesegiants possess surface lithium abundances approaching the 'cosmic' valueof the interstellar medium and young main-sequence stars, and eight moregiants have Li contents far in excess of standard predictions. At leastsome of these Li-rich giants are shown to be evolved to the stage ofhaving convectively mixed envelopes, either from the direct evidence oflow surface carbon isotope ratios, or from the indirect evidence oftheir H-R diagram positions. Suggestions are given for the uniqueconditions that might have allowed these stars to produce or accrete newlithium for their surface layers, or simply to preserve from destructiontheir initial lithium contents. The lithium abundance of the remainingstars demonstrates that giants only very rarely meet the expectations ofstandard first dredge-up theories; the average extra Li destructionrequired is about 1.5 dex. The evolutionary states of these giants andtheir average masses are discussed briefly, and the Li distribution ofthe giants is compared to predictions of Galactic chemical evolution.
| DDO, Cousins R-I, and photomultiplier scanner data for an analysis of very strong lined K giants
New DDO photometry and photomultiplier scanner data on a number ofsuper-metal-rich K giants are presented. The data provide information onblanketing, feature strengths, and stellar temperatures. Some of thescanner data are transformed to the Cousins R-I system and given withpreviously published measurements using this system.
| E. W. Fick Observatory stellar radial velocity measurements. I - 1976-1984
Stellar radial velocity observations made with the large vacuumhigh-dispersion photoelectric radial velocity spectrometer at FickObservatory are reported. This includes nearly 2000 late-type starsobserved during 585 nights. Gradual modifications to this instrumentover its first eight years of operation have reduced the observationalerror for high-quality dip observations to + or - 0.8 km/s.
| An analysis of the radial-velocity performance of the image-tube spectrograph on the CTIO 1-meter telescope
An analysis of the radial-velocity performance of the 120 A/mmconfiguration of the image-tube spectrograph on the CTIO/Yale 1-metertelescope is presented. The instrument is found to be stable within agiven run but to be susceptible to small changes from run to run. Theremay be systematic changes in velocity residual with declination; noneare found with zenith angle or hour angle. A typical precision of plusor minus 10 km/sec for a single spectrum of a Population I star isachieved for the spectrograph configuration. Rest wavelengths derivedfor F0-K4 Population I stars observed with this spectrograph/image-tubeconfiguration are presented. A table of radial velocities and residualsfor IAU radial-velocity standard stars, as well as some other brightstars, is also presented.
| Observations of Standard Velocity Stars
Not Available
| Standard Velocity Stars
Not Available
| The binary nature of the barium stars. II - Velocities, binary frequency, and preliminary orbits
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1983ApJ...268..264M&db_key=AST
| Photoelectric observations of lunar occultations. XIII
Occultation observations made with the 0.76 m reflector at McDonaldObservatory are presented, for 319 events occurring between Jan. 15,1981 and Feb. 7, 1982. One table reports timings, and a second recordsobservations of 16 double stars, in particular, Nu Gem observationsreveal that the two close components are similar in color. This allowsan estimation of individual visible magnitudes (near 4.60 and 5.32)suggesting that the secondary is a late B-type main-sequence star. SAO158929 observations reveal systematic differences in angular diametervalues. Of the 16 observed double stars, 9 appear to be new discoveries,including SAO 93067, SAO 94595, and SAO 98770. A third table gives fullydarkened angular diameters for the stars SAO 158929, SAO 77516 Y Tau,and SAO 119035 Nu Vir.
| The binary nature of the barium stars
Radial-velocity spectrometer observations are presented that indicatethat Ba II stars are binary systems. The secondary stars of thesesystems have low masses, consistent with their being degenerate objectswhich have lost mass onto their primaries in a previous stage ofevolution. It is suggested that the Population II equivalents, the CHstars, may also be binary systems. This may be related to the fact thatthey are found only in globular clusters of the lowest centralconcentration.
| Radial velocities of IAU standard stars
Radial velocities of 52 IAU Radial Velocity Standard stars, obtainedfrom 358 spectra of 12 and 20 A/mm dispersion during the 1970-1978period, are presented. Some discrepancies between the present resultsand those of the IAU are discussed.
| Absolute dimensions and masses of the remarkable spotted dM4e eclipsing binary flare star CM Draconis
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1977ApJ...218..444L&db_key=AST
| The stellar aggregate surrounding HD 101205 (IC 2944).
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1977A&A....54..233A&db_key=AST
| Spectrographic and photometric observations of supergiants and foreground stars in the direction of the Large Magellanic Cloud
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1972A&AS....6..249A&db_key=AST
| La mesure des vitesses radiales AU spectrographe coude DU telescope de 152 CM de l'Observatoire de Hte Provence.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1972A&A....19..427F&db_key=AST
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Наблюдательные данные и астрометрия
| Созвездие: | Водолей |
| Прямое восхождение: | 23h48m32.50s |
| Склонение: | -06°22'50.0" |
| Видимая звёздная величина: | 6.07 |
| Расстояние: | 221.729 парсек |
| Собственное движение RA: | 0.7 |
| Собственное движение Dec: | -19.5 |
| B-T magnitude: | 7.984 |
| V-T magnitude: | 6.24 |
Каталоги и обозначения:
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INHABITED SKY
