Abstract Details
| Name: Prasanta Kumar Nayak Affiliation: Indian Institute of Astrophysics Conference ID: ASI2016_702 Title : STUDY OF STAR CLUSTERS IN THE LARGE MAGELLANIC CLOUDS USING OGLE III SURVEY DATA Authors and Co-Authors : A. Subramaniam (Indian Institute of Astrophysics, Bangalore), S. Choudhury (Indian Institute of Science), G. Indu (Indian Institute of Astrophysics, Bangalore), Ram Sagar (Indian Institute of Astrophysics, Bangalore) Abstract Type : Poster Abstract Category : Stars, The Milky Way Galaxy and its neighbours Abstract : The Large Magellanic Cloud (LMC) is a neighbouring galaxy (d $\sim 50$ kpc) to the Milky Way. It hosts a large number star clusters which are ideal tools to study stellar evolution, star formation history, cluster formation and dissolution processes in the galaxy. The most recent catalogue of star clusters in the LMC is by Bica et al. (2008), in which they have listed the preliminary information (coordinates and sizes) for ~ 3000 clusters. Only $\sim$ 30 \% of these catalogued clusters have information about their parameters like reddening and age (Pietrzynsky and Udalski 2000, Glatt et al. 2010, Popescu et al. 2012). A large fraction of star clusters are thus either not well-studied or are unstudied due to shallow photometric depth. A more precise determination of cluster parameters of larger sample is required to understand the star and cluster formation history of the LMC. In an effort to fill this gap, we have used one of the recent, and relatively high spatial resolution and deep optical photometric survey, the Optical Gravitational Lensing Experiment (OGLE) III survey for the LMC. We identified and estimated the ages and reddenings of over 1000 star clusters in LMC, which includes $\sim$ 600 clusters whose ages and reddenings are estimated for the first time. In our study the ages of the clusters are found to be in the range, log(t)= 6.80 - 9.4 (6.6 Myr - 2.3 Gyr), with an uncertainty of ± 0.20, better than previous age estimations. The colour excess in (V - I) lie between 0.013 to 0.57. We shall present and discuss these preliminary results. |