Star counts in the cluster NGC 2070

Details Star counts in the cluster NGC 2070 Star counts in the cluster NGC 2070

Nov 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997arep...41..746s&link_type=abstract

Astronomy Reports, Volume 41, Issue 6, November 1997, pp.746-752

Astronomy and Astrophysics

Astronomy

2

Scientific paper

Star counts are used to investigate the structure of the cluster NGC 2070 in the Large Magellanic Cloud. The analysis is based on published ground-based and Hubble Space Telescope data. The effect of variable extinction in the cluster region on the star counts is studied. The projected surface density profiles in different directions from the cluster center are significantly different from each other. These profiles reflect inhomogeneities in the halo region in the form of steps and secondary maxima, suggesting that the cluster is far from a steady state. The cluster halo is asymmetric; the size of the cluster increases when the limiting magnitude is increased. This is probably due to the fact that NGC 2070 is the core of a stellar association. Using stars to a limiting magnitude of M_B = _1.9^m, the estimated radius of the cluster is >2', the number of member stars is >1250, and the mass is >2.2 x 10^4 M_solar.

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