Hostname: page-component-78c5997874-8bhkd Total loading time: 0 Render date: 2024-11-20T04:26:38.933Z Has data issue: false hasContentIssue false
  • English
  • Français

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

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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

Borissova, J., Spassova, N., Catelan, M., & Ivanov, V. D. 1998, in ASP Conf. Ser. Vol. 135, A Half-Century of Stellar Pulsation Interpretations, ed. Bradley, P. A. & Guzik, J. A. (San Francisco: ASP), 188 Google Scholar
Catelan, M. 2000, ApJ, 531, 826 Google Scholar
Stetson, P. B., et al. 1999, AJ, 117, 247 Google Scholar
VandenBerg, D. A. 2000, ApJS, 129, 315 Google Scholar