Hostname: page-component-586b7cd67f-tf8b9 Total loading time: 0 Render date: 2024-11-25T10:32:28.380Z Has data issue: false hasContentIssue false
  • English
  • Français

Formation History of Binary Clusters in the Large Magellanic Cloud

Published online by Cambridge University Press:  30 October 2019

Rhorom Priyatikanto Open the ORCID record for Rhorom Priyatikanto [Opens in a new window] ,
Mochamad Ikbal Arifyanto ,
Rendy Darma ,
Aprilia  and
Muhamad Irfan Hakim
Rhorom Priyatikanto
Affiliation:
Space Science Center, National Institute of Aeronautics and Space (LAPAN), Indonesia email: [email protected]
Mochamad Ikbal Arifyanto
Affiliation:
Astronomy Research Division, Faculty of Mathematics and Natural Sciences, Institut Teknologi Bandung, Indonesia
Rendy Darma
Affiliation:
Astronomy Research Division, Faculty of Mathematics and Natural Sciences, Institut Teknologi Bandung, Indonesia
Aprilia
Affiliation:
Astronomy Research Division, Faculty of Mathematics and Natural Sciences, Institut Teknologi Bandung, Indonesia
Muhamad Irfan Hakim
Affiliation:
Astronomy Research Division, Faculty of Mathematics and Natural Sciences, Institut Teknologi Bandung, Indonesia
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Global history of star or cluster formation in the Large Magellanic Cloud (LMC) has been the center of interest in several studies as it is thought to be influenced by tidal interaction with the Small Magellanic Cloud and even the Milky Way. This study focus on the formation history of the LMC in relation with the context of binary star clusters population, the apparent binary fraction (e.g., percentage of cluster pairs) in different epoch were calculated and analyzed. From the established distributions, it can be deduced that the binary clusters tend to be young (∽ 100 Myr) while their locations coincide with the locations of star forming complexes. There is an indication that the binary fraction increases as the rise of star formation rate in the last millions years. In the LMC, the increase of binary fraction at age ∽ 100 Myr can be associated to the last episode of close encounter with the Small Magellanic Cloud at ∽ 150 Myr ago. This observational evidence supports the theory of binary cluster formation through the fission of molecular cloud where the encounter between galaxies enhanced the clouds velocity dispersion which in turn increased the probability of cloud-cloud collisions that produce binary clusters.

Keywords

galaxies: star clustersstatisticsevolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S344: Dwarf Galaxies: From the Deep Universe to the Present , August 2018 , pp. 118 - 121
Copyright
© International Astronomical Union 2019 

References

Baumgardt, H., Parmentier, G., Anders, P. & Grebel, E. 2013, MNRAS, 430, 676 CrossRefGoogle Scholar
Bekki, K., Beasley, M. A., Forbes, D. A. & Couch, W. J. 2004, ApJ, 602, 730 CrossRefGoogle Scholar
Bekki, K. & Chiba, M. 2007, PASA, 24, 21 CrossRefGoogle Scholar
Bhatia, R. K. & Hadzidimitriou, D. 1988, MNRAS, 230, 215 CrossRefGoogle Scholar
Bressan, A., Marigo, P., Girardi, L., Salasnich, B., Dal Cero, C., Rubele, S. & Nanni, A. 2012, MNRAS, 427, 127 CrossRefGoogle Scholar
Fujii, M. S., Saitoh, T. R. & Portegiez Zwart, S. F. 2012, ApJ, 753, 85 CrossRefGoogle Scholar
Fujimoto, M. & Kumai, Y. 1997, AJ, 113, 249 CrossRefGoogle Scholar
Harris, J. & Zaritsky, D. 2009, AJ, 138, 1243 CrossRefGoogle Scholar
Priyatikanto, R., Kouwenhoven, M. B. N., Arifyanto, M. I., Wulandari, H. R. T. & Siregar, S. 2016, MNRAS, 457, 1339 CrossRefGoogle Scholar
Udalski, A., Kubiak, M. & Szymański, M. 1997, Acta Astron., 47, 319 Google Scholar
Zaritsky, D., Harris, J., Thompson, I. B. & Grebel, E. K. 2004, AJ, 128, 1606 CrossRefGoogle Scholar