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The properties of molecular clouds across the Magellanic System

Published online by Cambridge University Press:  01 July 2008

Norikazu Mizuno
Norikazu Mizuno*
Affiliation:
Department of Astrophysics, Nagoya University, Furocho Chikusa-ku, Nagoya 464-8602, Japan email: [email protected]
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Abstract

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Most stars form in Giant Molecular Clouds (GMCs) and regulate the evolution of galaxies in various respects. The formed stars affect the surrounding materials strongly via their UV photons, stellar winds, and supernova explosions, which lead to trigger the formation of next-generations of stars in the GMCs. It is therefore crucial to reveal the distribution and properties of GMCs in a galaxy. The Magellanic System is a unique target to make such detailed comprehensive study of GMCs. This is because it is nearby and the LMC is nearly face-on, making it feasible to unambiguously identify associated young objects within GMCs. Recent millimeter and sub-millimeter observations in the Magellanic System have started to reveal the distribution and properties of the individual GMCs in detail and their relation to star formation activities. From the NANTEN CO surveys, three types of GMCs can be classified in terms of star formation activities; Type I is starless, Type II is with H ii regions only, and Type III is associated with active star formation indicated by huge H ii regions and young star clusters. The further observations to obtain detailed structure of the GMCs by Mopra and SEST and to search for the dense cores by ASTE and NANTEN2 in higher tansition lines of CO have been carried out with an angular resolution of about 5 to 10 pc. These observations revealed that the differences of the physical properties represent an evolutionary sequence of GMCs in terms of density increase leading to star formation. Type I and II GMCs are at the early phase of star formation where density does not yet become high enough to show active star formation, and Type III GMCs represent the later phase where the average density is increased and the GMCs are forming massive stars.

Keywords

stars: formationISM: cloudsMagellanic Cloudsradio lines: ISMsubmillimeter
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S256: The Magellanic System: Stars, Gas, and Galaxies , July 2008 , pp. 203 - 214
Copyright
Copyright © International Astronomical Union 2009

References

Bica, E., Clariá, J. J., Dottori, H., Santos, J. F. C. Jr., & Piatti, A. E. 1996, ApJS, 102, 57CrossRefGoogle Scholar
Blitz, L., Fukui, Y., Kawamura, A., Leroy, A., Mizuno, N., & Rosolowsky, E. 2007, in Reipurth, B., Jewitt, D., & Keil, K. (eds.), Protostars and Planets V (Tucson: University of Arizona Press), p. 951Google Scholar
Bolatto, A. D., Simon, J. D., Stanimirović, S., et al. 2007, ApJ, 655, 212CrossRefGoogle Scholar
Bolatto, A. D., Leroy, A. K., Rosolowsky, E., Walter, F., & Blitz, L. 2008, ApJ, 686, 948CrossRefGoogle Scholar
Bot, C., Boulanger, F., Rubio, M., & Rantakyro, F. 2007, A&A, 471, 103Google Scholar
Brüns, C., Kerp, J., Staveley-Smith, L., et al. 2005, A&A, 432, 45Google Scholar
Cohen, R. S., Dame, T. M., Garay, G., Montani, J., Rubio, M., & Thaddeus, P. 1988, ApJ, 331, L95CrossRefGoogle Scholar
de Boer, K. S., Braun, J. M., Vallenari, A., & Mebold, U. 1998, A&A, 329, 49Google Scholar
Fukui, Y., Mizuno, N., Yamaguchi, R., et al. 1999, PASJ, 51, 745CrossRefGoogle Scholar
Fukui, Y., Mizuno, N., Yamaguchi, R., Mizuno, A., & Onishi, T. 2001, PASJ, 53, L41CrossRefGoogle Scholar
Fukui, Y. 2007, in Elmegreen, B. G. & Palouš, J. (eds.), Triggered Star Formation in a Turbulent ISM, IAU Conf. Proc. (Cambridge: CUP), p. 31Google Scholar
Fukui, Y., Kawamura, A., Minamidani, T., et al. 2008, ApJS, 178, 56Google Scholar
Fujimoto, M. & Noguchi, M. 1990, PASJ, 42, 505Google Scholar
Kawamura, A., Minamidani, T., Mizuno, Y., Onishi, T., Mizuno, N., Mizuno, A., & Fukui, Y. 2007, in Elmegreen, B. G. & Palouš, J. (eds.), Triggered Star Formation in a Turbulent ISM, IAU Conf. Proc. (Cambridge: CUP), p. 101Google Scholar
Kawamura, A., Minamidani, T., Mizuno, Y., Onishi, T., Mizuno, N., Mizuno, A., & Fukui, Y. 2008, ApJS, submittedGoogle Scholar
Kim, S., Staveley-Smith, L., Dopita, M. A., Freeman, K. C., Sault, R. J., Kesteven, M. J., & McConnell, D. 1998, ApJ, 503, 674CrossRefGoogle Scholar
Kim, S., Dopita, M. A., Staveley-Smith, L., & Bessell, M. S. 1999, AJ, 118, 2797CrossRefGoogle Scholar
Kim, S., Staveley-Smith, L., Dopita, M. A., Sault, R. J., Freeman, K. C., Lee, Y., & Chu, Y.-H. 2003, ApJS, 148, 473Google Scholar
Kutner, M. L., Rubio, M., Booth, R. S., et al. 1997, A&AS, 122, 255Google Scholar
Leroy, A., Bolatto, A. D., Stanimirović, S., Mizuno, N., Israel, F., & Bot, C. 2007, ApJ, 658, 1027CrossRefGoogle Scholar
Minamidani, T., Mizuno, N., Mizuno, Y., et al. 2008, ApJS, 175, 485CrossRefGoogle Scholar
Mizuno, N., Yamaguchi, R., Mizuno, A., et al. 2001a, PASJ, 53, 971CrossRefGoogle Scholar
Mizuno, N., Rubio, M., Mizuno, A., Yamaguchi, R., Onishi, T., & Fukui, Y. 2001b, PASJ, 53, L45CrossRefGoogle Scholar
Mizuno, N., Muller, E., Maeda, H., Kawamura, A., Minamidani, T., Onishi, T., Mizuno, A., & Fukui, Y. 2006, ApJ, 643, L107CrossRefGoogle Scholar
Muller, E., Staveley-Smith, L., & Zealey, W. J. 2003, MNRAS, 338, 609CrossRefGoogle Scholar
Nakagawa, M., Onishi, T., Mizuno, A., & Fukui, Y. 2005, PASJ, 57, 917CrossRefGoogle Scholar
Ott, J., Wong, T., Pineda, J., et al. 2008, PASA, 25, 129CrossRefGoogle Scholar
Pineda, J. L., Mizuno, N., Stutzki, J., et al. 2008, A&A, 482, 197Google Scholar
Rosolowsky, E. & Leroy, A. 2006, PASP, 118, 590Google Scholar
Rubio, M., Lequeux, J., & Boulanger, F. 1993, A&A, 271, 9Google Scholar
Rubio, M., Boulanger, F., Rantakyro, F., & Contursi, A 2004, A&A, 425, L1Google Scholar
Stanimirović, S., Staveley-Smith, L., Dickey, J. M., Sault, R. J., & Snowden, S. L. 1999, MNRAS, 302, 417CrossRefGoogle Scholar
Whitney, B. A., Sewilo, M., Indebetouw, R., et al. 2008, AJ, 553, 185Google Scholar
Yamaguchi, R., Mizuno, N., Onishi, T., Mizuno, A., & Fukui, Y. 2001a, ApJ, 553, L185CrossRefGoogle Scholar
Yamaguchi, R., Mizuno, N., Onishi, T., Mizuno, A., & Fukui, Y. 2001b, PASJ 53, 959CrossRefGoogle Scholar
Yamaguchi, R., Mizuno, N., Mizuno, A., et al. 2001c, PASJ 53, 985Google Scholar