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The Infrared Luminosity Function in the 30 Dor Cluster

Published online by Cambridge University Press:  03 August 2017

Hans Zinnecker ,
Morten Andersen ,
Bernhard Brandl ,
Wolfgang Brandner ,
Deidre Hunter ,
Richard Larson ,
Mark McCaughrean ,
Georges Meylan  and
Andrea Moneti
Hans Zinnecker
Affiliation:
Astrophysikalisches Institut Potsdam, Germany
Morten Andersen
Affiliation:
Astrophysikalisches Institut Potsdam, Germany
Bernhard Brandl
Affiliation:
Cornell University, Ithaca, USA
Wolfgang Brandner
Affiliation:
ESO Garching, Germany
Deidre Hunter
Affiliation:
Lowell Observatory, Flagstaff, USA
Richard Larson
Affiliation:
Yale Astronomy Department, New Haven, USA
Mark McCaughrean
Affiliation:
Astrophysikalisches Institut Potsdam, Germany
Georges Meylan
Affiliation:
STScI, Baltimore, USA
Andrea Moneti
Affiliation:
Institut d'Astrophysique, Paris, France

Abstract

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We present the first infrared luminosity function in the 30 Doradus star cluster obtained with the HST NIC1 camera (0.043″ pixel−1) in the F160W (H-band) filter. Despite diffraction limited resolution (0.15″), crowding and blending is so severe that the cluster centre R136 cannot be studied. Instead a neighbouring NIC1 field (about 15″ away from the centre), for which an empirical PSF could be obtained, was analysed. We obtained photometry for some 750 stars in the range H = 14 to 22 mag. The luminosity function continues rising up to H = 2.1 mag (1 M⊙ at an age of 2 Myr) after which incompleteness corrections become dramatic (exceeding 50%). Contrary to recent optical studies based on a V vs. V—I diagram (Sirianni et al. 2000), we do not infer a flattening or turnover of the implied IMF slope near 2 M⊙.

Type
Part 4. Star Cluster Formation and Evolution: Theory and Observation
Information
Symposium - International Astronomical Union , Volume 207: Extragalactic Star Clusters , 2002 , pp. 531 - 538
Copyright
Copyright © Astronomical Society of the Pacific 2002 

References

Brandl, B. et al. 1996, ApJ, 466, 254 Google Scholar
Brandner, W. et al. 2001, AJ, 122, 858 Google Scholar
D'Antona, F., & Mazzitelli, I. 1994, ApJS, 90, 467 Google Scholar
Hunter, D. A. et al. 1995, ApJ, 448, 179 Google Scholar
Hunter, D. A. et al. 1996, ApJ, 459, L27 Google Scholar
Kennicutt, R. C., & Chu, Y.-H. 1994, in Violent Star Formation, ed. Tenorio-Tagle, G. (Cambridge: Cambridge Univ. Press), 1 Google Scholar
Massey, P., & Hunter, D. A. 1998, ApJ, 493, 180 Google Scholar
Melnick, J. 1985, A&A, 153, 235 Google Scholar
Pehlemann, E., Hofmann, K.-H., & Weigelt, G. 1992, A&A, 256, 701 Google Scholar
Selman, F. et al. 1999, A&A, 347, 532 Google Scholar
Sirianni, M. et al. 2000, ApJ, 533, 203 CrossRefGoogle Scholar
Weigelt, G., & Baier, G. 1985, A&A, 150, L18 Google Scholar
Zinnecker, H. et al. 1999, in IAU-Symp. 190, New Views of the Magellanic Clouds, ed. Chu, Y.-H., Suntzeff, N., Hesser, J., & Bohlender, D. (San Francisco: ASP), 222 Google Scholar