A method of open cluster membership determination

516 8 2149 1 5895 document 2149 A&A_Vasil_Kukhianidze_2006_Cluster_Method.pdf application/pdf 9486baae84254dd0689d9959205af334 MD5 209765 2014-01-24 10:40:50 http://eprints.iliauni.edu.ge/516/1/A%26A_Vasil_Kukhianidze_2006_Cluster_Method.pdf 516 1 1 application/pdf text en public

A&A_Vasil_Kukhianidze_2006_Cluster_Method.pdf

2150 2 5903 document 2150 lightbox.jpg image/png f35b3a3d4312f9550f438d5e7d282727 MD5 52790 2014-01-24 10:50:54 http://eprints.iliauni.edu.ge/516/2/lightbox.jpg 516 2 2 image/png other Thumbnails conversion from text to thumbnail_lightbox ge public

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http://eprints.org/relation/isVersionOf http://eprints.iliauni.edu.ge/id/document/2149 http://eprints.org/relation/isVolatileVersionOf http://eprints.iliauni.edu.ge/id/document/2149 http://eprints.org/relation/issmallThumbnailVersionOf http://eprints.iliauni.edu.ge/id/document/2149 archive 134 disk0/00/00/05/16 2014-01-25 08:11:55 2015-03-27 10:03:07 2014-01-25 08:11:55 article show Javakhishvili G. Kukhianidze V. vasil.kukhianidze@iliauni.edu.ge Todua M. A method of open cluster membership determination pub QB public galaxies: stars clusters, methods: analytical A new method for the determination of open cluster membership based on a cumulative effect is proposed. In the field of a plate the relative x and y coordinate positions of each star with respect to all the other stars are added. The procedure is carried out for two epochs t1 and t2 separately, then one sum is subtracted from another. For a field star the differences in its relative coordinate positions of two epochs will be accumulated. For a cluster star, on the contrary, the changes in relative positions of cluster members at t1 and t2 will be very small. On the histogram of sums the cluster stars will gather to the left of the diagram, while the field stars will form a tail to the right. The procedure allows us to efficiently discriminate one group from another. The greater the distance between t1 and t2 and the more cluster stars present, the greater is the effect. The accumulation method does not require reference stars, determination of centroids and modelling the distribution of field stars, necessary in traditional methods. By the proposed method 240 open clusters have been processed, including stars up to m<13. The membership probabilities have been calculated and compared to those obtained by the most commonly used Vasilevskis-Sanders method. The similarity of the results acquired the two different approaches is satisfactory for the majority of clusters. 2006-03-01 published Astronomy and Astrophysics 447 3 EDP Sciences 915-919 10.1051/0004-6361:20040297 TRUE