Second Parameter Effects in and between M3 and Palomar 3

Details Second Parameter Effects in and between M3 and Palomar 3 Second Parameter Effects in and between M3 and Palomar 3

2001-05-21

arxiv.org/abs/astro-ph/0105350v1

Astronomy and Astrophysics

Astrophysics

Three pages, three figures. To appear in: "Extragalactic Star Clusters", IAU Symp. Ser. Vol. 207, ed. E. K. Grebel, D. Geisler

Scientific paper

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.

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