Contents
Images
Upload your image
DSS Images Other Images
Related articles
Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available
| Speckle interferometry of nearby multiple stars. III.
Not Available
| Speckle interferometry of nearby multiple stars. II.
This paper is a continuation of diffraction-limited speckleinterferometry of binary and multiple stars carried out at the 6-mtelescope of the Special Astrophysical Observatory in Zelenchuk. Theprogram has concentrated on nearby (π>10 mas) close binariesdiscovered or measured during the Hipparcos mission. Here, we present132 measurements of relative positions and magnitude differences for 99pairs and 8 measurements for 6 triple systems. 54 entries in the paperare new Hipparcos binaries. New triple systems with late-type dwarfcomponents, discovered in the course of observations, are HIP 8533 andHIP 25354.Based on data collected at the Special Astrophysical Observatory,Russia.{Tables 1-3 are 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?/A+A/422/627
| 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
| Astrometric radial velocities. III. Hipparcos measurements of nearby star clusters and associations
Radial motions of stars in nearby moving clusters are determined fromaccurate proper motions and trigonometric parallaxes, without any use ofspectroscopy. Assuming that cluster members share the same velocityvector (apart from a random dispersion), we apply a maximum-likelihoodmethod on astrometric data from Hipparcos to compute radial and spacevelocities (and their dispersions) in the Ursa Major, Hyades, ComaBerenices, Pleiades, and Praesepe clusters, and for theScorpius-Centaurus, alpha Persei, and ``HIP 98321'' associations. Theradial motion of the Hyades cluster is determined to within 0.4 kms-1 (standard error), and that of its individual stars towithin 0.6 km s-1. For other clusters, Hipparcos data yieldastrometric radial velocities with typical accuracies of a few kms-1. A comparison of these astrometric values withspectroscopic radial velocities in the literature shows a good generalagreement and, in the case of the best-determined Hyades cluster, alsopermits searches for subtle astrophysical differences, such as evidencefor enhanced convective blueshifts of F-dwarf spectra, and decreasedgravitational redshifts in giants. Similar comparisons for the ScorpiusOB2 complex indicate some expansion of its associations, albeit slowerthan expected from their ages. As a by-product from the radial-velocitysolutions, kinematically improved parallaxes for individual stars areobtained, enabling Hertzsprung-Russell diagrams with unprecedentedaccuracy in luminosity. For the Hyades (parallax accuracy 0.3 mas), itsmain sequence resembles a thin line, possibly with wiggles in it.Although this main sequence has underpopulated regions at certaincolours (previously suggested to be ``Böhm-Vitense gaps''), suchare not visible for other clusters, and are probably spurious. Futurespace astrometry missions carry a great potential for absoluteradial-velocity determinations, insensitive to the complexities ofstellar spectra. Based on observations by the ESA Hipparcos satellite.Extended versions of Tables \ref{tab1} and \ref{tab2} are available inelectronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr(130.79.125.8) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/381/446
| A Hipparcos study of the Hyades open cluster. Improved colour-absolute magnitude and Hertzsprung-Russell diagrams
Hipparcos parallaxes fix distances to individual stars in the Hyadescluster with an accuracy of ~ 6 percent. We use the Hipparcos propermotions, which have a larger relative precision than the trigonometricparallaxes, to derive ~ 3 times more precise distance estimates, byassuming that all members share the same space motion. An investigationof the available kinematic data confirms that the Hyades velocity fielddoes not contain significant structure in the form of rotation and/orshear, but is fully consistent with a common space motion plus a(one-dimensional) internal velocity dispersion of ~ 0.30 kms-1. The improved parallaxes as a set are statisticallyconsistent with the Hipparcos parallaxes. The maximum expectedsystematic error in the proper motion-based parallaxes for stars in theouter regions of the cluster (i.e., beyond ~ 2 tidal radii ~ 20 pc) isla 0.30 mas. The new parallaxes confirm that the Hipparcos measurementsare correlated on small angular scales, consistent with the limitsspecified in the Hipparcos Catalogue, though with significantly smaller``amplitudes'' than claimed by Narayanan & Gould. We use the Tycho-2long time-baseline astrometric catalogue to derive a set of independentproper motion-based parallaxes for the Hipparcos members. The newparallaxes provide a uniquely sharp view of the three-dimensionalstructure of the Hyades. The colour-absolute magnitude diagram of thecluster based on the new parallaxes shows a well-defined main sequencewith two ``gaps''/``turn-offs''. These features provide the first directobservational support of Böhm-Vitense's prediction that (the onsetof) surface convection in stars significantly affects their (B-V)colours. We present and discuss the theoretical Hertzsprung-Russelldiagram (log L versus log T_eff) for an objectively defined set of 88high-fidelity members of the cluster as well as the delta Scuti startheta 2 Tau, the giants delta 1, theta1, epsilon , and gamma Tau, and the white dwarfs V471 Tau andHD 27483 (all of which are also members). The precision with which thenew parallaxes place individual Hyades in the Hertzsprung-Russelldiagram is limited by (systematic) uncertainties related to thetransformations from observed colours and absolute magnitudes toeffective temperatures and luminosities. The new parallaxes providestringent constraints on the calibration of such transformations whencombined with detailed theoretical stellar evolutionary modelling,tailored to the chemical composition and age of the Hyades, over thelarge stellar mass range of the cluster probed by Hipparcos.
| Structure and colour-magnitude diagrams of Scorpius OB2 based on kinematic modelling of Hipparcos data
All stars in a `moving group' share the same space motion. The presenceof such a coherent structure in velocity space can be used to derive(improved) estimates of the stellar parallaxes from the observedpositions and proper motions. A Lund Observatory group (Dravins et al.)describes an elegant and sophisticated maximum likelihood procedure todo so using Hipparcos data. Their method determines the cluster centroidspace motion, the internal velocity dispersion, which is assumed to beisotropic, and the individual model parallaxes for all member stars,implicitly using the assumption of a `compact' cluster with a `small'velocity dispersion. We implement the Lund procedure, and test itextensively using Monte Carlo simulations. We discuss the effects on thederived parallaxes of a `large' velocity dispersion, as measured forphysically extended, `loose' OB associations. We also investigate theinfluence of an overall expanding motion, which is relevant to suchunbound groups. We conclude that the method is robust against allsystematic effects that we considered, except for the maximum likelihoodestimate of the one-dimensional internal velocity dispersionsigmav, which is always underestimated. The model parallaxaccuracies are limited by the internal velocity dispersion for nearbygroups (mean distance D<~50-150pc, depending on Galactic longitude).We present an application to the nearby association Scorpius OB2, whichconsists of the three subgroups Upper Scorpius (mean distance 145pc),Upper Centaurus Lupus (140 pc), and Lower Centaurus Crux (118pc).Membership of these groups has recently been established by de Zeeuw etal. using Hipparcos data. The resulting model parallaxes are (1)statistically consistent with and (2) more precise by a factor of ~2than the Hipparcos trigonometric parallaxes; they (3) significantlynarrow the locus of stars in the (B-V)0-MV0colour-absolute magnitude diagram, and (4) define a single-star mainsequence which is consistent with Mermilliod's zero-age main-sequencecalibration. We find, after bias correction based on Monte Carlosimulations, that sigmav<~1.0-1.5kms-1 for allthree subgroups; these values are confirmed by the statistics of theresidual (muperp) proper motion components. Whereas, as aresult of their consistency with the Hipparcos values, the modelparallaxes do not improve significantly upon the mean associationdistances derived by de Zeeuw et al. from Hipparcos trigonometricparallaxes, they do resolve the parallax distribution, and thus thespatial structure, for Upper Centaurus Lupus and Lower Centaurus Crux.
| The Hyades: distance, structure, dynamics, and age
{We use absolute trigonometric parallaxes from the Hipparcos Catalogueto determine individual distances to members of the Hyades cluster, fromwhich the 3-dimensional structure of the cluster can be derived.Inertially-referenced proper motions are used to rediscuss distancedeterminations based on convergent-point analyses. A combination ofparallaxes and proper motions from Hipparcos, and radial velocities fromground-based observations, are used to determine the position andvelocity components of candidate members with respect to the clustercentre, providing new information on cluster membership: 13 newcandidate members within 20 pc of the cluster centre have beenidentified. Farther from the cluster centre there is a gradual mergingbetween certain cluster members and field stars, both spatially andkinematically. Within the cluster, the kinematical structure is fullyconsistent with parallel space motion of the component stars with aninternal velocity dispersion of about 0.3 km s(-1) . The spatialstructure and mass segregation are consistent with N-body simulationresults, without the need to invoke expansion, contraction, rotation, orother significant perturbations of the cluster. The quality of theindividual distance determinations permits the cluster zero-age mainsequence to be accurately modelled. The helium abundance for the clusteris determined to be Y =3D 0.26+/-0.02 which, combined with isochronemodelling including convective overshooting, yields a cluster age of625+/-50 Myr. The distance to the observed centre of mass (a conceptmeaningful only in the restricted context of the cluster memberscontained in the Hipparcos Catalogue) is 46.34+/-0.27 pc, correspondingto a distance modulus m-M=3D3.33+/-0.01 mag for the objects within 10 pcof the cluster centre (roughly corresponding to the tidal radius). Thisdistance modulus is close to, but significantly better determined than,that derived from recent high-precision radial velocity studies,somewhat larger than that indicated by recent ground-based trigonometricparallax determinations, and smaller than those found from recentstudies of the cluster convergent point. These discrepancies areinvestigated and explained. } Based on observations made with the ESAHipparcos astrometry satellite. Table~2 is also 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/Abstract.html
| Determination of atmospheric parameters of T Tauri stars.
The inferred effective temperatures (T_eff_) and surface gravities(logg) of T Tauri stars (TTS) are usually contaminated by the presenceof a non stellar continuum emission (veiling) and the strongchromospheric activity characteristic of these objects. In this work, wedevelop a method to determine T_eff_'s and surface gravities of a groupof TTS. This method is based on the comparison between observed andtheoretical molecular and atomic line depth ratios being thereforeinsensitive to the influence of veiling. We show the strong dependenceof our line depth ratios upon gravity and temperature. The resultinggravities, as expected for TTS, average between the values of dwarf andgiant stars. Previously published gravities for each of our stars varywidely due in part to the differences in the adopted visual extinction,veiling (if ever considered) and methods of assessing the stellarluminosity. Our values of T_eff_ and logg have the uniqueness of beingentirely derived from high resolution data and are not affected bycircumstellar extinction or veiling. They therefore serve as morereliable input parameters for future spectral synthesis analyses of TTauri stars requiring model atmospheres. We provide a table relatingtheoretical line depth ratios with T_eff_ and log g for easy assessmentof TTS fundamental parameters.
| ROSAT All-Sky Survey Observations of the Hyades Cluster
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995ApJ...448..683S&db_key=AST
| The Henry Draper Extension Charts: A catalogue of accurate positions, proper motions, magnitudes and spectral types of 86933 stars
The Henry Draper Extension Charts (HDEC), published in the form offinding charts, provide spectral classification for some 87000 starsmostly between 10th and 11th magnitude. This data, being highlyvaluable, as yet was practically unusable for modern computer-basedastronomy. An earlier pilot project (Roeser et al. 1991) demonstrated apossibility to convert this into a star catalogue, using measurements ofcartesian coordinates of stars on the charts and positions of theAstrographic Catalogue (AC) for subsequent identification. We presenthere a final HDEC catalogue comprising accurate positions, propermotions, magnitudes and spectral classes for 86933 stars of the HenryDraper Extension Charts.
| Radio continuum emission from stars: a catalogue update.
An updated version of my catalogue of radio stars is presented. Somestatistics and availability are discussed.
| Low-Mass Stars in the Hyades
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1993MNRAS.265..785R&db_key=AST
| The low mass Hyades and the evaporation of clusters
The 135 single stars and 85 binary systems, redder than R-I = +0.34 magand brighter than V = 17 mag, between alpha = 3.75 h and 5.0 h and delta= +5 deg and + 25 deg show a luminosity function that differsconsiderably from that of the general field stars within 20 pc of theSun. The ratio of double star components to single cluster membersincreases markedly with decreasing luminosity. Forty-three single starsand 16 binary systems that are members of the Hyades supercluster within20 pc of the Sun show the same luminosity function as the field stars inthat region. Fifty percent of the cluster members and 40 percent of thesupercluster members are components of binary stars. The equivalentwidths of H-alpha appear to support a range of ages (approximately 8 to16 x 108 yr) for the cluster stars and demonstrate that theoldest objects are in the supercluster. A list of cluster members, whichmay include the end of the stable main sequence, but for which accurate(R-I) photometry is not available, is included. The half-dozen knownparallax stars of the faintest luminosity contain at least onesupercluster member, TVLM 868-110639, which is probably beyond thestable, nuclear burning main sequence as a 'transitional' or 'brown'dwarf.
| Intensity of Cah Lines in Cool Dwarfs
Abstract image available at:http://adsabs.harvard.edu/abs/1993A&AS..101..409B
| Photometry of dwarf K and M stars
An observational program using UBVRI photometry is presented for 688stars from among the dwarf K and M stars already found spectroscopicallyby Vyssotsky (1958). Of these, 211 have not been observedphotometrically. These observations were obtained over a period ofseveral years at the Kitt Peak National Observatory using a GaAsphotomultiplier with an 0.9 m reflector. Based on night-to-nightvariations in the measures of individual stars, the internal errors maybe estimated to be roughly 0.01 mag for the colors and 0.015 for the Vmagnitudes. The photometric parallaxes reported for each star werecomputed in the manner discussed by Weis (1986).
| Proper motions from Schmidt plates. II - The Hyades
COSMOS scans of photographic plates taken by the Palomar Oschin Schmidttelescope and by the UK Schmidt telescope are used to obtain propermotions for about 450,000 stars within a 112-sq-deg region covering partof the Hyades luster. With epoch differences of 33 to 37 yr, propermotions accurate to 6-12 milliarcsec/yr are obtained, and 393 candidateHyades to a limiting magnitude of about 15.5, including at least two newwhite dwarf candidates, are identified. The main-sequence luminosityfunction determined from this sample is similar to that defined by localfield stars, with a broad maximum at about +12. Both the line-of-sightand surface density distributions show evidence for significant masssegregation; the overall proper motion distribution suggests a tightcore centered within a much broader distribution. A total mass of410-480 solar masses and a gravitational binding radius of about 10.5 pcare derived.
| Four colour and H-beta photometry for low mass members in open clusters. II - The Hyades
Photoelectric uvby and H-beta photometry has been obtained for 28low-mass members in the Hyades cluster. The stars observed are G and Ktype stars of the lower main sequence with colors up to (b-y) = 0.8 mag,selected from the proper motion study of Van Altena (1969) with highprobability of membership. Their position in the related four color andH-beta photometric diagrams is discussed. The derived values for thedistance modulus and metallicity are compatible with the common acceptedvalues for this cluster. The c1-(b-y) plane shows the persistence of theHyades anomaly in the G star range, disappearing for late G and Kspectral types. This result is in good agreement with previous resultsobtained by the authors for the Praesepe star cluster.
| The chromospheric activity of low-mass stars in the Hyades
High-resolution spectra or narrow-band H-alpha photometry of 106 dwarf Kand M stars in the Hyades cluster have been used to determine H-alphaequivalent widths. These data reveal a sequence of Hyades members withH-alpha in absorption for photospheric temperatures hotter than about3500 K. Within this sequence, the dispersion about the mean equivalentwidth-color relation is only slightly larger than the measurementerrors. A second sequence of Hyades members, characterized by H-alphaemission and significant scatter at a given color, appears at effectivetemperatures cooler than about 4000 K. This bifurcation in H-alphaproperties at 4000 K coincides with a bifurcation in the rotationalcharacteristics of Hyades stars: the dispersion in the rotationalvelocities of the hotter Hyades members at a given effective temperatureis small while the cooler stars exhibit significant scatter in theirrotational velocities. On the basis of these data, it is suggested thatlow-mass stars spin down to rotational velocities dependent upon massand age, but independent of premain-sequence angular momentum.
| Hamilton echelle spectra of young stars. I - Optical veiling
An extensive set of veiling measurements of T Tauri stars coveringalmost the entire optical spectrum is presented. These are based onHamilton echelle spectra obtained during 1987-1989. A full range of TTauri stars, from 'weak' to 'continuum' stars is studied; in some cases,several spectra of a given target are seen in which the veiling haschanged, occasionally dramatically. Veilings are determined using twonew methods: one which concentrates on the residual intensities ofselected spectral lines, and the other which compares theautocorrelation functions for a T Tauri star and a veiled standard. Thegeneral shape of the veiling is often as predicted by accretion diskmodels: almost flat in the red and increasing in the blue. Cooler starshave generally higher veiling, implying that the veiling power isrelatively independent of stellar mass. The relation between veiling andthe narrow and broad emission lines supports a nonstellar origin for theveiling and broad line components, and a stellar origin for the narrowlines.
| Identification par des numéros de catalogue ou par une position semi-précise d'étoiles doubles du Catalogue Index (1976. 5)
Not Available
| A radial-velocity survey of the Hyades
Photoelectric radial-velocity measurements, obtained with external erroras small as 0.1 km/s using the 200-inch Hale telescope at PalomarObservatory during the period 1971-1986, are reported for over 400candidate members (with V magnitude between 6 and 14) of the Hyadescluster. The history of Hyades observations is recalled; the Palomarinstrumentation and observing program are described; the data-reductionand standardization procedures are discussed in detail; and the data arepresented in extensive tables and graphs. About 200 of the stars areclassified as cluster members, including 60 spectroscopic binaries.
| Rotational velocities of low-mass stars in the Hyades
High-resolution echelle spectra have been used to estimate rotationalvelocities for K and M dwarfs in the Hyades. All of the K dwarfs haverotational velocities less than the instrumental limit of 10 km/s. Mostof the M dwarfs with (R - I)K larger than 1.0 have detectable rotationalvelocities, with v sin i between 10 and 20 km/s. Combining these datawith results from the younger Pleiades and Alpha Persei clusters, it isfound that G dwarfs spin down from about 100 km/s to about 10 km/s inless than 40 million yr, whereas M dwarfs take an order of magnitudelonger to spin down.
| Photometry of dwarf K and M stars
Broadband photometry in BVRI colors for 120 nearby dwarf K and M starsis presented. The apparent magnitude distributions of Vyssotsky and VanVleck stars with photometry and without photometry are studied. Therelationship between apparent and photoelectric magnitudes is analyzed.The proper motion and transverse velocity of the two star types areexamined and compared.
| Positions of 127 Hyads and 6-cm observations of 320 Hyads
Accurate positions are given for 127 Hyades cluster stars whichpreviously had only approximate positions known. The fields of 320Hyads, including 55 X-ray stars, were observed with the VLA to a 6-cmdetection level of approximately 0.5 mJy. There were no detections.
| Systematic search for members of the Hyades Supercluster. VI - The lower main sequence
Proper motion has served as the basis for identifying 50 members of theHyades Supercluster from a complete sample of stars with visualmagnitude higher than 15 and annual proper motion greater than 0.5arcsec. The resulting main sequence is represented by M(bol) 4.51 + 4.31(R-I), with 0.15 mag dispersion. The supercluster stars may represent 15percent of the star density near the sun. The reddest superclusterdwarfs are noted to be cool to a degree that is nearly comparable tosuch extreme stars to VB 10.
| Infrared photometry of Hyades dwarfs
JHK infrared photometry is presented for 76 main-sequence proper motionmembers brighter than V = 12 in the Hyades. Known binaries are confirmedand new candidates proposed using color-magnitude and color-colordiagrams. The cluster binary frequency (about 40%) is discussed, as wellas its possible effects on the cluster distance modulus and stellarchromospheric/coronal activity.
| Photometry of Possible Members of the Hyades Cluster - Part Four
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1982PASP...94..475W&db_key=AST
| Luminosity distribution and shape of the Hyades cluster
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1979A&A....78..312O&db_key=AST
| Photometry of new possible members of the Hyades cluster.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1977AJ.....82..978U&db_key=AST
|
Submit a new article
Related links
Submit a new link
Member of following groups:
|
Observation and Astrometry data
| Constellation: | おうし座 |
| Right ascension: | 04h26m42.82s |
| Declination: | +12°41'11.8" |
| Apparent magnitude: | 10.659 |
| Distance: | 35.373 parsecs |
| Proper motion RA: | 124.7 |
| Proper motion Dec: | -18.1 |
| B-T magnitude: | 12.259 |
| V-T magnitude: | 10.792 |
Catalogs and designations:
|
INHABITED SKY
