The age spread and initial mass function of NGC 3293 - Implications for the formation of clusters

Details The age spread and initial mass function of NGC 3293 - Implications for the formation of clusters The age spread and initial mass function of NGC 3293 - Implications for the formation of clusters

Nov 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982aj.....87.1478h&link_type=abstract

Astronomical Journal, vol. 87, Nov. 1982, p. 1478-1490.

Astronomy and Astrophysics

Astronomy

73

Galactic Clusters, Stellar Evolution, Stellar Mass, Stellar Spectrophotometry, Ubv Spectra, Astronomical Photography, Color-Magnitude Diagram, Hertzsprung-Russell Diagram, Main Sequence Stars, O Stars, Star Clusters, Stellar Luminosity, Time Dependence

Scientific paper

UBV photographic photometry observations of 350 stars in the field of the young cluster NGC 3293 are presented and applied to the study of cluster formation. A contraction of age of at least 25 + or - 10 million years is implied by the faint population of the main sequence of the cluster. As this is greater than its nuclear age of 6 + or - 2 million years, several implications are presented: an age spread of at least 20 + or - 10 million years, and the possibility that lower-mass stars formed first. The luminosity function is derived to be approximately +5. Data are used to derive an initial mass function (IMF), showing that the cluster contains an excess of high-mass stars as compared with the IMF of field stars. Finally, the age spread, color-magnitude diagram, and IMF of NGC 3293 are most likely typical of galactic clusters, which suggests that: clusters with O-star members are more than 10 or 20 million years old, star formation in clusters is a gradual process, and during the cluster formation period the IMF varies with time.

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