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Astron. Astrophys. 328, 167-174 (1997)

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No stellar age gradient inside supergiant shell LMC 4 *

Jochen M. Braun 1, Dominik J. Bomans 2, 1, ** , Jean-Marie Will 1, *** and Klaas S. de Boer 1

1 Sternwarte der Universität Bonn, Auf dem Hügel 71, D-53121 Bonn, Germany
2 University of Illinois at Urbana-Champaign, Department of Astronomy, 1002 West Green Street, Urbana, IL 61801, USA

Received 2 May 1997 / Accepted 21 July 1997


The youngest stellar populations of a 'J'-shaped region inside the supergiant shell (SGS) LMC 4 have been analysed with CCD photometry in B, V passbands. This region consists of 2 coherent strips, one from the east to the west reaching about [FORMULA] pc across the OB superassociation LH [FORMULA] and another extending about [FORMULA] pc from south to north.

The standard photometric methods yield 25 colour-magnitude diagrams (CMDs) which were used for age determination of the youngest star population by isochrone fitting. The resultant ages lie in the range from [FORMULA] Myr to [FORMULA] Myr without correlation with the distance to the LMC 4 centre. We therefore conclude that there must have been one triggering event for star formation inside this great LMC SGS with a diameter of [FORMULA] kpc.

We construct the luminosity function and the mass function of five regions consisting of 5 fields to ensure that projection effects don't mask the results. The slopes lie in the expected range ([FORMULA] and [FORMULA] respectively). The greatest values of the slope occur in the north, which is caused by the absence of a young, number-dominating star population.

We have calculated the rate with which supernovae (SNe) have exploded in LMC 4, based on the finding that all stars are essentially coeval. A total of 5-7 [FORMULA] supernovae has dumped the energy of [FORMULA] erg over the past 10 Myr into LMC 4, in fact enough to tear the original star-forming cloud apart in the time span between 5 and 8 Myr after the starformation burst. We conclude that LMC 4 can have been formed without a contribution from stochastic self-propagating star formation (SSPSF), although the ring of young associations and H II regions around the edge have been triggered by the events inside LMC 4.

Key words: stars: early-type – Hertzsprung-Russell (HR) diagram – stars: luminosity function, mass function – ISM: bubbles – ISM: individual objects: LMC 4 – Magellanic Clouds

* Based on observations collected at the European Southern Observatory (ESO), La Silla, Chile.
** Feodor Lynen-Fellow of the Alexander von Humboldt-Foundation
*** Present address: Hewlett-Packard GmbH, Herrenberger Str. 130, D-71034 Böblingen

Send offprint requests to: J.M. Braun ('jbraun@astro.uni-bonn.de')

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© European Southern Observatory (ESO) 1997

Online publication: March 24, 1998