The Radial Distribution of the Two Stellar Populations in NGC 1851

Details The Radial Distribution of the Two Stellar Populations in NGC 1851 The Radial Distribution of the Two Stellar Populations in NGC 1851

2009-06-09

arxiv.org/abs/0906.1779v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

11 pages, 10 figures, accepted for pubblication in A&A

Scientific paper

We have analyzed ACS/WFC and WFPC2 images from HST, as well as ground-based data to study the radial distribution of the double sub-giant branch (SGB) recently discovered in the Galactic globular cluster NGC 1851. We found that the SGB split can be followed all the way from the cluster center out to at least 8\arcmin from the center. Beyond this distance out to the tidal radius at $\sim 11.7$ arcmin, there are simply too few SGB stars to dentify the sequences. The number ratio of the bright SGB to the faint SGB stars shows no significant radial trend. Furthermore, we have found that the ratio of blue horizontal-branch (HB) stars plus RR Lyrae to the red HB stars also remains constant from the cluster center to the outer envelope.

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