Hostname: page-component-7c8c6479df-ph5wq Total loading time: 0 Render date: 2024-03-29T12:31:13.195Z Has data issue: false hasContentIssue false

The Infrared Luminosity Function in the 30 Dor Cluster

Published online by Cambridge University Press:  03 August 2017

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

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.

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
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