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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}
| Absolute proper motion and space motion of the globular cluster M15
We have separated cluster members and field stars for stars in a regionaround the globular cluster M15. The membership of ultraviolet brightstars of M15 is discussed. The absolute proper motion of M15 has beendetermined with respect to the PPM catalog. An extragalactic calibrationof the proper motions has been performed. The calibration was done bymeasurements of galaxies on the Palomar Sky Survey glass copies andplates from the Schmidt telescope of the Observatoire de la Cote d'Azur(CERGA). We compare the three different methods of establishing absoluteproper motion for the globular cluster M15. The orbital parameters ofM15 have been derived. As a by-product of our work, we obtained foreight stars of the HIPPARCOS input catalog absolute proper motions,which may be used for the calibration of the HIPPARCOS proper motionsystem.
| An astrometric catalogue of stars in the region of M15
We present positions and proper motions with respect to the PPMcatalogue of 863 stars in a field of 8 deg x 6 deg centered on theglobular cluster M15. The catalogue is based on measurements of 136plates from the Carte du Ciel telescope of Bordeaux, the CERGA Schmidttelescope, and the double refractor of Bonn. The modal accuracy of theproper motions is +/- 0 arcsec 15/100 a.
| Polarimetric investigation of dark patches of globular clusters
A polarimetric investigation has been conducted of dark patches innorthern globular clusters, using polarimetry to disentangle readingsfrom dust within the cluster from those in its foreground. Themeasurements obtained are in good agreement with those of previousstudies. Observations of M 15 yield confirmation of enhancedpolarization in the direction of an 'historical' dark patch likelycaused by the fluctuation of interstellar polarization. Calculationsindicate that the size of the dark patches and the wavelength variationof the apparent extinction are generally consistent with that expectedfor holes in the star distribution.
| Der kugelfoermige Sternhaufen Messier 15
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Member of following groups:
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Observation and Astrometry data
| Constellation: | Pégase |
| Right ascension: | 21h29m11.90s |
| Declination: | +11°57'10.5" |
| Apparent magnitude: | 7.332 |
| Distance: | 220.264 parsecs |
| Proper motion RA: | 57.2 |
| Proper motion Dec: | -59.2 |
| B-T magnitude: | 8.984 |
| V-T magnitude: | 7.469 |
Catalogs and designations:
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