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Star Formation in the LMC: Comparative CCD Observations of Young Stellar Populations in two Giant Molecular Clouds

Published online by Cambridge University Press:  13 April 2010

Jan Ruppert  and
Hans Zinnecker
Jan Ruppert
Affiliation:
European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile email: jruppert@eso.org
Hans Zinnecker
Affiliation:
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany email: hzinnecker@aip.de
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Abstract

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This work deals with a CCD imaging study at optical and near-infrared wavelength of two giant molecular clouds (plus a control field) in the southern region of the Large Magellanic Cloud, one of which shows multiple signs of star formation, whereas the other does not. The observational data from VLT FORS2 (R-band) and NTT SOFI (Ks-band) have been analyzed to derive luminosity functions and color-magnitude diagrams. The young stellar content of these two giant molecular clouds is compared and confirmed to be different, in the sense that the apparently “starless” cloud has so far formed only low-luminosity, low-mass stars (fainter than mKs = 16.5 mag, not seen by 2MASS), while the other cloud has formed both faint low-mass and luminous high-mass stars. The surface density excess of low-luminosity stars (~ 2 per square arcmin) in the “starless” cloud with respect to the control field is about 20% whereas the excess is about a factor of 3 in the known star-forming cloud. The difference may be explained theoretically by the gravo-turbulent evolution of giant molecular clouds, one being younger and less centrally concentrated than the other.

Keywords

stars: formationluminosity functionISM: cloudsevolutionHII regionsgalaxies: stellar contentinfrared: stars
Type
Poster Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S262: Stellar Populations – Planning for the Next Decade , August 2009 , pp. 424 - 425
Copyright
Copyright © International Astronomical Union 2010

References

Blitz, L. et al. 2007, in: Reipurth, B., Jewitt, D., Keil, K. (eds.), Protostars and Planets V (Tucson: University of Arizona Press), 951, 81–96Google Scholar
Fukui, Y. et al. 2001, PASJ, 53, L41–L44CrossRefGoogle Scholar
Fukui, Y. 2005, in: Cesaroni, R., Felli, M., Churchwell, E., Walmsley, M. (eds.), IAU Symposium Proceedings (Cambridge: Cambridge University Press), 227, 328–336Google Scholar
Mizuno, N. et al. 2001 PASJ, 53, 971–984Google Scholar
MacLow, M.-M. & Klessen, R. S. 2004, RvMP, 76, 125–194Google Scholar
Megeath, S. T. et al. 2009, AJ, 137, 4072–4082CrossRefGoogle Scholar
Ruppert, J. & Zinnecker, H. 2009, AN, 330, 773–783Google Scholar