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Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters
The availability of the Hipparcos Catalogue has triggered many kinematicand dynamical studies of the solar neighbourhood. Nevertheless, thosestudies generally lacked the third component of the space velocities,i.e., the radial velocities. This work presents the kinematic analysisof 5952 K and 739 M giants in the solar neighbourhood which includes forthe first time radial velocity data from a large survey performed withthe CORAVEL spectrovelocimeter. It also uses proper motions from theTycho-2 catalogue, which are expected to be more accurate than theHipparcos ones. An important by-product of this study is the observedfraction of only 5.7% of spectroscopic binaries among M giants ascompared to 13.7% for K giants. After excluding the binaries for whichno center-of-mass velocity could be estimated, 5311 K and 719 M giantsremain in the final sample. The UV-plane constructed from these datafor the stars with precise parallaxes (σπ/π≤20%) reveals a rich small-scale structure, with several clumpscorresponding to the Hercules stream, the Sirius moving group, and theHyades and Pleiades superclusters. A maximum-likelihood method, based ona Bayesian approach, has been applied to the data, in order to make fulluse of all the available stars (not only those with precise parallaxes)and to derive the kinematic properties of these subgroups. Isochrones inthe Hertzsprung-Russell diagram reveal a very wide range of ages forstars belonging to these groups. These groups are most probably relatedto the dynamical perturbation by transient spiral waves (as recentlymodelled by De Simone et al. \cite{Simone2004}) rather than to clusterremnants. A possible explanation for the presence of younggroup/clusters in the same area of the UV-plane is that they have beenput there by the spiral wave associated with their formation, while thekinematics of the older stars of our sample has also been disturbed bythe same wave. The emerging picture is thus one of dynamical streamspervading the solar neighbourhood and travelling in the Galaxy withsimilar space velocities. The term dynamical stream is more appropriatethan the traditional term supercluster since it involves stars ofdifferent ages, not born at the same place nor at the same time. Theposition of those streams in the UV-plane is responsible for the vertexdeviation of 16.2o ± 5.6o for the wholesample. Our study suggests that the vertex deviation for youngerpopulations could have the same dynamical origin. The underlyingvelocity ellipsoid, extracted by the maximum-likelihood method afterremoval of the streams, is not centered on the value commonly acceptedfor the radial antisolar motion: it is centered on < U > =-2.78±1.07 km s-1. However, the full data set(including the various streams) does yield the usual value for theradial solar motion, when properly accounting for the biases inherent tothis kind of analysis (namely, < U > = -10.25±0.15 kms-1). This discrepancy clearly raises the essential questionof how to derive the solar motion in the presence of dynamicalperturbations altering the kinematics of the solar neighbourhood: doesthere exist in the solar neighbourhood a subset of stars having no netradial motion which can be used as a reference against which to measurethe solar motion?Based on observations performed at the Swiss 1m-telescope at OHP,France, and on data from the ESA Hipparcos astrometry satellite.Full Table \ref{taba1} 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/430/165}
| The Dynamics of the Merging Galaxy Cluster System A2256: Evidence for a New Subcluster
We present 236 new radial velocities of galaxies in the cluster A2256measured with the WIYN Hydra Multi-Object Spectrograph. Combined withthe previous work of Fabricant, Kent, & Kurtz, we have velocitiesfor a total of 319 galaxies, of which 277 are cluster members. Inaddition to the new radial velocities, we present a 3×3 imagemosaic in the R band of the central 19'×19'region of A2256, from which we obtained photometry for 861 galaxies.These data provide strong evidence for a merger event between twogroups. In addition, we present evidence for the presence of a thirdgroup, on the outer reaches of the system, that is just now beginning tomerge with the system.
| 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.
| The magnetic activity cycle of II Pegasi: results from twenty-five years of wide-band photometry
We present an analysis of a sequence of light curves of the RS CVn-typebinary II Pegasi extending from 1974 to 1998. The distribution of thespotted area versus longitude is derived by Maximum Entropy and Tikhonovregularized maps, assuming a constant spot temperature (Lanza et al.1998a). The spot pattern on the active K2 IV star can be subdivided intoa component uniformly distributed in longitude and a second unevenlydistributed component, which is responsible for the observed photometricmodulation. The uniformly distributed component appears to be possiblymodulated with an activity cycle of ~ 13.5 yr. The unevenly distributedcomponent is mainly concentrated around three major active longitudes.The spot activity appears practically permanent at one longitude, butthe spot area changes with a cycle of ~ 9.5 yr. On the contrary, thespot activity is discontinuous at the other two longitudes, and itswitches back and forth between them with a cycle of ~ 6.8 yr. However,before each switching is completed, a transition phase of ~ 1.05 yr,during which both longitudes are active, occurs. After this transientphase, spot activity remains localized at one of the two longitudes for~ 4.7 yr untill another switching event occurs, which re-establishesspot activity at the other longitude. The longitude separation betweenthe permanent and the switching active longitudes is closest during theswitching phases and it varies along the ~ 6.8 yr cycle. Different timescales characterize the activity at the permanent longitude and at theswitching longitudes: a period of ~ 9.5 yr is related to the activitycycle at the permanent longitude, and a period of ~ 4.3 yr characterizesthe spot life time at the switching longitudes in between switchingevents. The photometric period of the active star changes from season toseason with a relative amplitude of 1.5% and a period of ~ 4.7 yr. Sucha variation of the photometric period may be likely associated with thephase shift of the light curves produced by the switching of spotactivity from one active longitude to the other. The permanently activelongitude shows a steady migration towards decreasing orbital phases,with an oscillating migration rate along the 9.5 yr cycle period andnearly in phase with the variation of its spotted area. The amplitude ofthe differential rotation derived from such a behaviour is of the orderof ~ 0.023%, about one order of magnitude smaller than estimated byHenry et al. (1995). The other two active longitudes migrates alsotowards decreasing orbital phase, but at a discontinuous rate. Thereappears to be no correlation between the location of the activelongitudes with respect to the line joining the two components of thesystem and their activity level.
| Fundamental plane distances to early-type field galaxies in the South Equatorial Strip. I. The spectroscopic data
Radial velocities and central velocity dispersions are derived for 238E/S0 galaxies from medium-resolution spectroscopy. New spectroscopicdata have been obtained as part of a study of the Fundamental Planedistances and peculiar motions of early-type galaxies in three selecteddirections of the South Equatorial Strip, undertaken in order toinvestigate the reality of large-scale streaming motion; results of thisstudy have been reported in Müller et al. (1998). The new APM SouthEquatorial Strip Catalog (-17fdg 5 < delta < +2fdg 5) was used toselect the sample of field galaxies in three directions: (1) 15h10 -16h10; (2) 20h30 - 21h50; (3) 00h10 - 01h30. The spectra obtained have amedian S/N per Å of 23, an instrumental resolution (FWHM) of ~ 4Å, and the spectrograph resolution (dispersion) is ~ 100 kms-1. The Fourier cross-correlation method was used to derivethe radial velocities and velocity dispersions. The velocity dispersionshave been corrected for the size of the aperture and for the galaxyeffective radius. Comparisons of the derived radial velocities with datafrom the literature show that our values are accurate to 40 kms-1. A comparison with results from Jo rgensen et al. (1995)shows that the derived central velocity dispersion have an rms scatterof 0.036 in log sigma . There is no offset relative to the velocitydispersions of Davies et al. (1987).
| Towards a fundamental calibration of stellar parameters of A, F, G, K dwarfs and giants
I report on the implementation of the empirical surface brightnesstechnique using the near-infrared Johnson broadband { (V-K)} colour assuitable sampling observable aimed at providing accurate effectivetemperatures of 537 dwarfs and giants of A-F-G-K spectral-type selectedfor a flux calibration of the Infrared Space Observatory (ISO). Thesurface brightness-colour correlation is carefully calibrated using aset of high-precision angular diameters measured by moderninterferometry techniques. The stellar sizes predicted by thiscorrelation are then combined with the bolometric flux measurementsavailable for a subset of 327 ISO standard stars in order to determineone-dimensional { (T, V-K)} temperature scales of dwarfs and giants. Theresulting very tight relationships show an intrinsic scatter induced byobservational photometry and bolometric flux measurements well below thetarget accuracy of +/- 1 % required for temperature determinations ofthe ISO standards. Major improvements related to the actual directcalibration are the high-precision broadband { K} magnitudes obtainedfor this purpose and the use of Hipparcos parallaxes for dereddeningphotometric data. The temperature scale of F-G-K dwarfs shows thesmallest random errors closely consistent with those affecting theobservational photometry alone, indicating a negligible contributionfrom the component due to the bolometric flux measurements despite thewide range in metallicity for these stars. A more detailed analysisusing a subset of selected dwarfs with large metallicity gradientsstrongly supports the actual bolometric fluxes as being practicallyunaffected by the metallicity of field stars, in contrast with recentresults claiming somewhat significant effects. The temperature scale ofF-G-K giants is affected by random errors much larger than those ofdwarfs, indicating that most of the relevant component of the scattercomes from the bolometric flux measurements. Since the giants have smallmetallicities, only gravity effects become likely responsible for theincreased level of scatter. The empirical stellar temperatures withsmall model-dependent corrections are compared with the semiempiricaldata by the Infrared Flux Method (IRFM) using the large sample of 327comparison stars. One major achievement is that all empirical andsemiempirical temperature estimates of F-G-K giants and dwarfs are foundto be closely consistent between each other to within +/- 1 %. However,there is also evidence for somewhat significant differential effects.These include an average systematic shift of (2.33 +/- 0.13) % affectingthe A-type stars, the semiempirical estimates being too low by thisamount, and an additional component of scatter as significant as +/- 1 %affecting all the comparison stars. The systematic effect confirms theresults from other investigations and indicates that previousdiscrepancies in applying the IRFM to A-type stars are not yet removedby using new LTE line-blanketed model atmospheres along with the updatedabsolute flux calibration, whereas the additional random component isfound to disappear in a broadband version of the IRFM using an infraredreference flux derived from wide rather than narrow band photometricdata. Table 1 and 2 are only available in the electronic form of thispaper
| Discovery of a Probable CH Star in the Globular Cluster M14 and Implications for the Evolution of Binaries in Clusters
We report the discovery of a probable CH star in the core of theGalactic globular cluster M14 (=NGC 6402 = C1735-032), identified froman integrated-light spectrum of the cluster obtained with the MOSspectrograph on the Canada-France-Hawaii telescope. From ahigh-resolution echelle spectrum of the same star obtained with theHydra fiber positioner and bench spectrograph on the WIYN telescope, wemeasure a radial velocity of -53.0 +/- 1.2 km s-1. Although thisvelocity is inconsistent with published estimates of the systemic radialvelocity of M14 (e.g., v^-r ~ -123 km s-1), we usehigh-precision Hydra velocities for 20 stars in the central 2.'6 of M14to calculate improved values for the cluster mean velocity andone-dimensional velocity dispersion: -59.5 +/- 1.9 km s-1 and 8.2 +/-1.4 km s-1, respectively. Both the star's location near the tip of thered giant branch in the cluster color-magnitude diagram and its radialvelocity therefore argue for membership in M14. Since theintermediate-resolution MOS spectrum shows not only enhanced CHabsorption but also strong Swan bands of C2, M14 joins omega Cen as theonly globular clusters known to contain "classical" CH stars. Althoughevidence for its duplicity must await additional radial velocitymeasurements, the CH star in M14 is probably, like all field CH stars, aspectroscopic binary with a degenerate (white dwarf) secondary. Thecandidate and confirmed CH stars in M14 and omega Cen, and in a numberof Galactic dSph galaxies, may then owe their existence to the longtimescales for the shrinking and coalescence of hard binaries inlow-concentration environments.
| 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.
| Nine Seasons of Velocity Measurements in the Draco and Ursa Minor Dwarf Spheroidal Galaxies with the MMT Echelle
We have used the Multiple Mirror Telescope echelle spectrograph tomeasure 112 velocities of 42 stars in the Draco and Ursa Minor dwarfspheroidal galaxies and three velocities of three foreground starsbetween 1982 April and 1990 September. We used 11 A resolution spectraobtained with the MX multifiber spectrograph at the Steward 90" to findadditional giant candidates; 5 UMi and 13 Draco stars were then observedat the MMT and added to the original sample of velocity members. Inaddition, the MX spectra were used to eliminate 74 stars in thedirection of UMI and 59 stars in Draco as likely foreground dwarfs. Wedetected 7 velocity variables, defined as those stars whose probabilityof exceeding the measured X^2^ by chance is less than 1.5%. Three ofthese stars are Carbon (C) stars (UMi K and VA 335 and Draco C1); twohave emission lines (Draco CI and UMi M). We show that the C star DracoC4, with a proper motion membership probability of 7%, has a velocityconsistent with membership. It is not surprising that these C (mostlikely CH) stars are binaries because McClure has shown that mostGalactic CH stars are in binary systems. Of the remaining 35 stars, only4 are velocity variables, with measured velocity extrema of 29.1 kms^-1^ (UMi M), 7.2 km s^-1^ (Draco XI-2), 9.0 km s^-1^ (Draco 24), and8.3 km s^-1^ (Draco 473). The velocity dispersions are 10.1 +/- 1.7 kms^-1^ for UMi, and 9.9 +/- 1.4 km s^-1^ for Draco. These dispersionschange to 10.5 +/- 2.0 for UMi, and 8.2 +?- 1.3 for Draco if weeliminate the velocity variables. Our dispersion for UMi differs fromthat of Hargreaves et al. [MNRAS, 271,693 (1994b)] by 1.3σ of thecombined errors. These velocities are combined with the one-componentKing models of Pryor & Kormendy [AJ, 100,127 (1990)] to give M/L =73 for UMi, and 77 for Draco.
| Abundances and velocities for open and globular cluster giants: The data.
We present a large dataset consisting of giants in the field, and inopen and globular clusters. A total of 122 giants were observed in thefields of 8 open clusters. A total of 342 giants were observed in thefields of 25 globular clusters. A total of 36 field stars with wellknown abundances and luminosities were also observed. Radial velocitiesare determined for most giants, some of which have no photometryavailable. We have analyzed several spectral features in order to definea grid that will allow the determination of metal abundances for haloand bulge giants. The errors involved in the determination of radialvelocities and [Fe/H] are carefully examined. We find that field andopen cluster stars on one side, and globular cluster giants on the otherside, do not follow the same calibration. This is possibly due toenhanced [α/Fe] abundances in globular clusters. Therefore, wehave defined a calibration based only on globular cluster giants, validfrom [Fe/H]=-2.0 to +0.5. This calibration is carried out with thepurpose of measuring metallicities for bulge and halo giants, with theunderlying assumption that the abundance ratios of the relevant elementsrelative to iron are similar to the calibrating stars. Adopting asstandards the globular clusters NGC 288, NGC 362, NGC 1851, NGC 6356,NGC 6624, 47 Tuc, M 4 , M 3, and M 22 we derive metallicities forglobular clusters with less well known compositions, like M 28, and NGC6637. In particular, we confirm a low metallicity for M 28([Fe/H]=-1.35+/-0.2), a cluster that has a disk orbit.
| BV Photometry and Hα Spectroscopy of the Rs-Canum Binary II-Pegasi
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1993A&A...277..155M&db_key=AST
| Spectroscopy of V471 Tau. I - Review of basic properties
Spectroscopic observations of the eclipsing binary V471 Tau are reportedand analyzed. Data obtained mainly in the red band at Mt. WilsonObservatory and KPNO during the period 1975-1983 are compiled inextensive tables and graphs, and the radial velocity of the K dwarfcomponent is determined using a Griffin-mask technique. Resultsdiscussed include: (1) distance 44 + or - 6 pc, (consistent withmembership in the Hyades), (2) apparent period variation consistent witha third component, (3) emissionlike features affecting theradial-velocity determination, (4) transient features consistent withthe presence of flares, and (5) phase-coherent variation in H-alpha(attributed to the action of the white-dwarf Lyman continuum emission onthe K dwarf).
| Time-resolved spectroscopy of the cataclysmic variable V426 Ophiuchi
The double-lined spectroscopic binary V426 Oph is characterized on thebasis of 94 420-520-nm spectra obtained with dispersion 5.9 nm/mm usinga CCD detector in the ES2 Cassegrain spectrograph on the 2.1-m Struvereflector at McDonald Observatory on July 9-14, 1983. The data arepresented in tables, graphs, and sample spectra and discussed in detail.Parameters determined include orbital period 0.285314 + or - 0.000096 d,white-dwarf mass 0.9 + or - 0.2 solar mass, secondary-star mass 0.7 + or- 0.1 solar mass, inclination 59 + or - 6 deg, distance 202 + or - 33pc, and anomalous velocity shift -100 to -200 km/s. Evidence of flaringis seen in both the continuum and line emission, but the data in generalindicate a simple rotating disk filling about 70 percent of the Rochelobe. The characteristics of V426 Oph and of SS Cyg are compared andanalyzed theoretically.
| Photometry during the End-Phase of a spot Cycle in II Peg
Not Available
| Standard Velocity Stars
Not Available
| HZ 9 - A white-dwarf-red-dwarf spectroscopic binary in the Hyades
It is noted that the star HZ 9, a member of the Hyades, is aspectroscopic binary with a period of 0.56433 day. One component is a DAwhite dwarf and the other is a late main-sequence M star (roughlydM4.5e). The system is similar to V471 Tauri and PG 1413+01; like them,it is probably a post-common-envelope binary.
| Photoelectric radial velocities, paper 6 Heard's IAU standard stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1975MNRAS.171..407G&db_key=AST
| The establishment of 21 new ninth magnitude IAU standard radial velocity stars
Not Available
| Photoelectric photometry of selected AG stars in the 25D to 30D zone.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1968AJ.....73..187B&db_key=AST
| Relationship between CN anomaly and U V W components of space velocity.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1962AJ.....67..757Y&db_key=AST
| Spectral and Luminosity Classifications and Measurements of the Strength of Cyanogen Absorption for Late-Type Stars from Objective-Prism Spectra.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1961ApJ...134..809Y&db_key=AST
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| Takýmyýldýz: | Kanatli At |
| Sað Açýklýk: | 23h46m25.51s |
| Yükselim: | +28°42'13.0" |
| Görünürdeki Parlaklýk: | 6.975 |
| Uzaklýk: | 990.099 parsek |
| özdevim Sað Açýklýk: | -15.3 |
| özdevim Yükselim: | -10.5 |
| B-T magnitude: | 9.086 |
| V-T magnitude: | 7.15 |
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