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Mass segregation in the young open cluster NGC 2547
We present a study of mass segregation of the young (20-35 Myrisochronal age) open cluster NGC 2547. We find good evidence that masssegregation exists in NGC 2547 down to 3 Msolar, and weakevidence for mass segregation down to 1 Msolar. Theoreticalmodels of an initially unsegregated model of NGC 2547 using the NBODY2code show weaker mass segregation, implying that at least some of theobserved mass segregation has a primordial origin. We also report thediscovery of three possible escaped cluster members, which share theproper motion and colours of the cluster, but lie nearly a degree fromthe cluster centre.
| Absolute proper motions of open clusters. I. Observational data
Mean proper motions and parallaxes of 205 open clusters were determinedfrom their member stars found in the Hipparcos Catalogue. 360 clusterswere searched for possible members, excluding nearby clusters withdistances D < 200 pc. Members were selected using ground basedinformation (photometry, radial velocity, proper motion, distance fromthe cluster centre) and information provided by Hipparcos (propermotion, parallax). Altogether 630 certain and 100 possible members werefound. A comparison of the Hipparcos parallaxes with photometricdistances of open clusters shows good agreement. The Hipparcos dataconfirm or reject the membership of several Cepheids in the studiedclusters. Tables 1 and 2 are only available in electronic form at theCDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Open clusters with Hipparcos. I. Mean astrometric parameters
New memberships, mean parallaxes and proper motions of all 9 openclusters closer than 300 pc (except the Hyades) and 9rich clusters between 300 and 500 pc have been computed using Hipparcosdata. Precisions, ranging from 0.2 to 0.5 mas for parallaxes and 0.1 to0.5 mas/yr for proper motions, are of great interest for calibratingphotometric parallaxes as well as for kinematical studies. Carefulinvestigations of possible biases have been performed and no evidence ofsignificant systematic errors on the mean cluster parallaxes has beenfound. The distances and proper motions of 32 more distant clusters,which may be used statistically, are also indicated. Based onobservations made with the ESA Hipparcos astrometry satellite
| The VELA star cloud. III - The B8 to A0 stars and interstellar reddening
The present discussion of intermediate band and H-beta observations of360 HD stars B8-A0 in Vela, and all of the CPD stars in a small adjacentregion, notes that the interstellar absorption in both cases can beunderstood as a combination of three absorbing clouds of 1 kpc-A(V) =1.5, 0.5, and 0.17. The major difference in the two environments is thepresence of numerous T Tauri stars in Taurus. Several clusters in theVela region are discussed.
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| Takýmyýldýz: | Yelken |
| Sað Açýklýk: | 08h14m42.44s |
| Yükselim: | -49°58'59.6" |
| Görünürdeki Parlaklýk: | 8.846 |
| Uzaklýk: | 543.478 parsek |
| özdevim Sað Açýklýk: | -9.5 |
| özdevim Yükselim: | 2.4 |
| B-T magnitude: | 8.874 |
| V-T magnitude: | 8.849 |
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