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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}
| GPM - compiled catalogue of absolute proper motions of stars in selected areas of sky with galaxies.
Not Available
| Diffuse Stellar Light at 100 Kiloparsec Scales in M87
In a new survey of nearby galaxies from stacked photographic images,seemingly regular galaxies of several types show amorphous, oftenasymmetrical features at very faint levels (28 mag arcsec-2). In M87, adiffuse fan of stellar material extends along the projected southeast(major) axis out to about 100 kpc. We suggest that accretion of a smallspheroidal galaxy into a larger potential is the most likely explanationfor the diffuse structure. The orbit is required to pass close to thecenter of the potential in order to produce a fan that is nearly alignedwith the major axis and has a large opening angle, as seen in M87. Oursimulations include a rigid primary potential with characteristicssimilar to those derived for M87 and a populated secondary potential. Weinvestigate the structure of the dark matter at large galactic radii byrepresenting M87 with different potentials. The morphologies of thedebris of intruder spheres and disks of different masses and orbitalparameters limit the possible accretion scenarios. The total luminosityof the fan and the kinematics of debris in the center of the primarypotential are analyzed and compared with substructure in M87. The shortlifetimes (tfan <~ 5 x 108 yr) of the simulated diffuse fans and lackof observed shells indicates either that we are seeing M87 at a "specialtime" during its evolution or that infall from small intruder galaxiesis common. Our simulations indicate that several accretion events couldbe hidden in galaxies. For many orbits, intruder material is quicklyspread out to very low light levels. Observations of the high specificfrequency of globular clusters in M87 provide evidence that the galaxymay experience frequent accretions of this type.
| An infrared-optical study of IRAS point sources in the Virgo region
Optical identifications for 199 of the 206 IRAS point sources in a 113sq deg area centered on the Virgo cluster are made using four deepIIIa-J plates obtained with the 1.2-m UK Schmidt Telescope. Only 4percent of the E and S0 galaxies brigher than B = 16 are detected, ascompared with 44 percent of the Sc galaxies. Infrared properties of theVirgo cluster are found to be similar to those of field galaxies atsimilar redshifts. Such IRAS galaxies are typical spirals with B of lessthan about 14, infrared to optical luminosity ratios of about 1, andinfrared luminosities of about 10 to the 9th solar luminosities,properties which are independent of neutral hydrogen content for theVirgo cluster galaxies. Data suggest that the optically faint galaxieshave L(IR) of greater than 10 to the 12th solar luminosities.
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| Takýmyýldýz: | Basakci |
| Sað Açýklýk: | 12h28m34.42s |
| Yükselim: | +12°07'02.8" |
| Görünürdeki Parlaklýk: | 7.986 |
| Uzaklýk: | 215.517 parsek |
| özdevim Sað Açýklýk: | 17.2 |
| özdevim Yükselim: | -21.2 |
| B-T magnitude: | 9.301 |
| V-T magnitude: | 8.095 |
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