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Second Parameter Effects in and between M3 and Palomar 3

Published online by Cambridge University Press:  03 August 2017

M. Catelan ,
R. T. Rood  and
F. R. Ferraro
M. Catelan
Affiliation:
University of Virginia, Department of Astronomy, P.O. Box 3818, Charlottesville, VA 22903-0818, USA
R. T. Rood
Affiliation:
University of Virginia, Department of Astronomy, P.O. Box 3818, Charlottesville, VA 22903-0818, USA
F. R. Ferraro
Affiliation:
Osservatorio Astronomico di Bologna, via Ranzani 1, I-40126 Bologna, Italy

Abstract

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We study the globular clusters M3 and Palomar 3 as a “second parameter (2ndP) pair,” showing that: i) M3 has a surprisingly strong internal 2ndP; ii) The dispersion in mass on the Pal 3 horizontal branch (HB) is intrinsically very small, leading to the most apparent differences in HB morphology between M3 and Pal 3; iii) Ignoring the difference in HB mass dispersion between M3 and Pal 3, their relative HB types can be accounted for by a fairly small difference in age, of order 0.5–1 Gyr.

Type
Part 1. The Star Clusters of Local Group Galaxies
Information
Symposium - International Astronomical Union , Volume 207: Extragalactic Star Clusters , 2002 , pp. 113 - 115
Copyright
Copyright © Astronomical Society of the Pacific 2002 

References

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