Volume 402, Number 2, May I 2003
|Page(s)||549 - 564|
|Section||Galactic structure, stellar clusters, and populations|
|Published online||14 April 2003|
Facultad de Ciencias Astronómicas y Geofísicas de la UNLP, IALP-CONICET, Paseo del Bosque s/n, 1900 La Plata, Argentina
2 Dipartimento di Astronomia, Università di Padova, Vicolo Osservatorio 2, 35122 Padova, Italy
Corresponding author: G. Baume, email@example.com
Accepted: 17 January 2003
Deep and extensive CCD photometric observations at were carried out in the area of the open cluster NGC 3293. The new data set allows to see the entire cluster sequence down to , revealing that stars with are evolving off the main sequence; stars with are located on the main sequence and stars with are placed above it. According to our analysis, the cluster distance is ± ( ± 0.2) and its nuclear age is 8 ± 1 Myr. NGC 3293 contains an important fraction of pre–main sequence (PMS) stars distributed along a parallel band to the ZAMS with masses from 1 to and a mean contraction age of 10 Myr. This last value does not differ too much from the nuclear age estimate. If we take into account the many factors that may affect the PMS star positions on the colour–magnitude diagram, both ages can be perfectly reconciled. The star formation rate, on the other hand, suggests that NGC 3293 stars formed surely in one single event, therefore favouring a coeval process of star formation. Using the data, we detected nineteen stars with signs of emission in the region of NGC 3293, another indication that the star formation process is still active in the region. The computed initial mass function for the cluster has a slope of , a bit flatter than the typical slope for field stars and similar to the values found for other young open clusters.
Key words: Galaxy: open clusters and associations: individual: NGC 3293 / stars: imaging / stars: luminosity function, mass function
Based on observations collected at UTSO, ESO (Dutch 0.9 m telescope) and CASLEO. The CCD and data acquisition system at CASLEO has been partly financed by R.M. Rich through U.S. NSF Grant AST-90-15827.
© ESO, 2003
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