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For refcode 1989AJ.....98..590K:
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1989AJ.....98..590K ELLIPTICITIES AT R_h_ OF LMC STAR CLUSTERS E. KONTIZAS National Observatory of Athens, Astronomical Institute, P.0. Box 20048, Athens 118 10, Greece M. KONTIZAS University of Athens, Department of Physics, Laboratory of Astrophysics, Panepistimiopolis, Zografos 15783, Greece G. SEDMAK Universita di Trieste, Dipartimento di Astronomia, Via Tiepolo 11, 34131-Trieste, Italy and Osservatorio Astronomico di Trieste, Via Tiepolo 11, 34131-Trieste, Italy R. SMAREGLIA Osservatorio Astronomico di Trieste, Via Tiepolo 11, 34131-Trieste, Italy Received 28 December 1988; revised 18 April 1989 ABSTRACT The projected ellipticities of 53 populous LMC star clusters have been derived by means of PDS 1O1OA scans and a computer interactive method of reduction implemented by the authors on an Apollo 570 workstation. Film copies of a pair of J and U plates taken with the 1.2 m U.K. Schmidt Telescope in Australia were used. The ellipticities derived here agree with those found by previous investigators, when comparisons were possible at the same radius. Ellipticity variations within individual globular clusters are seen to be a common phenomenon, so the ellipticities e_h_ (at a distance corresponding to the half-mass radius R_h_ from the center) were adopted to represent the cluster's flatness. Using these values for the LMC clusters, it is found that LMC clusters are more elliptical than those of our galaxy. Although the young LMC globular clusters show a tendency to be more elliptical than the old ones, there is no strong evidence for a significant difference among them. Finally, e_h_ was found to increase with the total mass of the clusters, possibly indicating that high-mass clusters having higher angular momentum, or having more difficulty in shedding angular momentum than do low mass clusters, remain longer in their initial flattened shape.
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