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Astron. Astrophys. 336, 503-517 (1998)

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7. Conclusions

From the previous investigation we can summarize as follows:

  1. The clusters SL 666 and NGC 2098 are two populous young clusters among those found frequent in the LMC. SL 666 is observed in excellent conditions and the data given for this object allowed better interpretation. The stellar component for both clusters consists of early type stars with the brightest ones centrally concentrated.

    The age of NGC 2098 is [FORMULA]yr, whereas for SL 666 is [FORMULA]yr.

  2. The number counts show that the radial density distribution of stars in both clusters exhibit a trend in their slopes with evidence of mass segregation, in the sense that the heavier stars are centrally concentrated.

  3. The LFs show a similar trend with the slopes increasing radially from the centre of the clusters. Therefore mass segregation is observed and it is investigated whether this is a star formation and/or dynamical phenomenon.

  4. The dynamical parameters of SL 666 found from star count give (from single mass models) a total mass of [FORMULA] and a lowest limit for the relaxation time [FORMULA] yr. SL 666 shows evidence of mass segregation due to the star formation process. The disruption time of the cluster and its radial profile implies that the cluster is bound and the star formation is slow.

  5. NGC 2098 is also a candidate, but we need to extrapolate [FORMULA] mag the results, and it is less certain until we have better photometry to clear up this ambiguity.

  6. The central densities of both clusters give evidence of a bound system since their disruption times are at least 10 times their present age.

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© European Southern Observatory (ESO) 1998

Online publication: July 20, 1998