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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}
| 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 74th Special Name-list of Variable Stars
We present the Name-list introducing GCVS names for 3153 variable starsdiscovered by the Hipparcos mission.
| High-resolution spectroscopy of Vega-like stars - I. Effective temperatures, gravities and photospheric abundances
Vega-like stars are young main-sequence stars exhibiting an excessemission of infrared radiation. Modelling this excess depends not onlyon the parameters assigned to the grains, but on those assigned to thestars themselves. In an effort to update and improve the informationavailable on this class of star, we have analysed 13 stars classed asVega-like, having an infrared excess attributable to dust emission,along with two spectral standards which have also been found to showexcess emission from dust. In this, the first of two papers, we derivestellar properties (spectral type, effective temperature and log g) andphotospheric abundances. The spectral types derived revealed that one ofthe sample was a luminosity class III giant, ruling it out of theVega-like class, and two others underwent a significantreclassification. The remainder had their type confirmed. All but twoprogramme stars have been found to be emission-line stars - theiremission-line properties are discussed in Paper II. Attention hasrecently been drawn to the possible link between Vega-like stars and thephotospheric metal-depleted class of A-type stars, the lambda Bootisstars. These latter stars are hypothesized to have obtained theirunderabundances by the accretion of depleted circumstellar gas on to thephotosphere of the star. Since Vega-like stars are expected to havediscs of dust, it might be expected that accretion may cause this samephenomenon. We have analysed four A-type stars in our sample and twoA-type standards, deriving photospheric abundances for up to 10elements. No pattern of underabundance similar to lambda Bootis starswas found, although a depletion of silicon was found in two stars (up to0.86 dex below solar) and of magnesium in one star (0.56 dex lower). Thedepletion could be attributable to the accretion of those elements on tograins in the circumstellar environment of these stars.
| The Tokyo PMC catalog 90-93: Catalog of positions of 6649 stars observed in 1990 through 1993 with Tokyo photoelectric meridian circle
The sixth annual catalog of the Tokyo Photoelectric Meridian Circle(PMC) is presented for 6649 stars which were observed at least two timesin January 1990 through March 1993. The mean positions of the starsobserved are given in the catalog at the corresponding mean epochs ofobservations of individual stars. The coordinates of the catalog arebased on the FK5 system, and referred to the equinox and equator ofJ2000.0. The mean local deviations of the observed positions from theFK5 catalog positions are constructed for the basic FK5 stars to comparewith those of the Tokyo PMC Catalog 89 and preliminary Hipparcos resultsof H30.
| Supplement to the Arecibo 1612 MHz survey of color-selected IRAS sources
The completeness of the Arecibo 1612 MHz survey of color-selected IRASsources is extended to (25-12) micrometer greater than -0.7. In addition(1) most IR sources with spectral types normally associated with OH/IRstars and colors outside the coverage of the original survey have beenexamined; (2) most ambiguous observations during the survey have beenreobserved; (3) most single peaked sources have been reexamined, and 17found with second peaks. We report 39 new 1612 MHz detections, of which34 are original. These are also surveyed in the mainlines. Analysis ofthe complete flux-limited survey confirms the existence of a longitudesensitivity effect in the detection of sources, which reduces the totalnumber detected by approximately equals 4%. This analysis sets an upperlimit of 16% on the proportion of a color-selected sample that may beidentified with carbon stars and/or star-formation regions.
| South galactic CAP G and K stars with infrared excesses
Near-infrared and IRAS photometry is discussed for 13 G and K stars inthe south galactic cap. Five of them show a strong flux excess at 12microns as would be expected from dust shells emitting at temperaturesof several hundred Kelvin. One of them (XY Tau) has previously beenclassified as a 206-d Mira, but the new observations suggest it isactually a variable F or G star. The most likely explanation is that theoriginal classification was wrong and that it is in fact apremain-sequence star. The other four stars are either in very unusualevolutionary states or they are binary systems. The presence oflong-term variations in the near-infrared flux of the flare star CC Eriis reported. The colors are redder when the star is fainter, and thevariations might be associated with the star spot cycle.
| A survey for infrared excesses among high galactic latitude SAO stars
This project involves extending the previous analysis of infraredexcesses among a volume-limited sample of 134 nearby A-K main-sequencestars to a magnitude-limited sample of stars, culled from the SAOCatalog, with excesses determined from the IRAS Point Source Catalogflux density ratios. This new sample includes 5706 B-M type stars, 379of which have infrared excesses. The objective involved use of astatistically complete survey of objects in a standard catalog in orderto assess the frequency with which different physical processes canaffect the infrared output of stars. These processes include, but arenot limited to, orbiting cold particle clouds and the onset of rapidmass loss. It is concluded that cold disks are consistent with theinfrared excesses found among A-G dwarfs and G-K giants in the sample.
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Pozíciós és asztrometriai adatok
| Csillagkép: | Halak |
| Rektaszcenzió: | 00h29m54.18s |
| Deklináció: | +08°48'22.5" |
| Vizuális fényesség: | 7.876 |
| Távolság: | 364.964 parszek |
| RA sajátmozgás: | 8.7 |
| Dec sajátmozgás: | 2.3 |
| B-T magnitude: | 10.076 |
| V-T magnitude: | 8.058 |
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