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<p align="justify">The star cluster is a group of stars, that are bound by their gravitational forces to each other. All the stars in the star cluster move together in a direction with the parallel path. The star trajectory in the cluster appears to center or radiate to or from a poi...
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| Format: | Final Project |
| Language: | Indonesia |
| Online Access: | https://digilib.itb.ac.id/gdl/view/31790 |
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| Institution: | Institut Teknologi Bandung |
| Language: | Indonesia |
| Summary: | <p align="justify">The star cluster is a group of stars, that are bound by their gravitational forces to each other. All the stars in the star cluster move together in a direction with the parallel path. The star trajectory in the cluster appears to center or radiate to or from a point. Star clusters are divided into two types: open clusters and globular clusters. Both of these groups can be distingushed from the number of star members, location, and distribution of the cluster. The determination of membership in open clusters will be more difficult than detemination membership of the globular clusters. This is due to the location of open clusters which located on the galactic disk. From that location, when observing open clusters, it will be observed foreground and background stars. So determining the membership of open clusters becomes important for knowing the actual members of the cluster. Determination of membership in cluster could be done by calculating the probability of a star becoming a cluster member. The method of determining cluster membership is differentiated into parametric and nonparametric. The parametric method uses the Gaussian function to fit the distribution of proper motion in cluster, while the nonparametric method will determine the distribution function of the cluster empirically. The parametric method based on Markov Chain Monte Carlo (MCMC) Metropolis Hastings Algorithm is used in this research to obtain the probability of open cluster membership. There are seven open clusters that their memberships are determined: NGC 2244, NGC 2360, NGC 2396, NGC 2682, NGC 2972, Haffner 8, and Ruprecht 18. To determine membership based on quality of fit, which is the value of the parameter D that close to 0. The smaller the value of D, the higher quality of fitting between data and model. This method can be used to determination of another open cluster membership.<p align="justify"> <br />
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