The ACS Survey of Galactic Globular Clusters. I. Overview and Clusters without PreviousHubble Space TelescopePhotometry

2006/12/20 by Ata Sarajedini, L. Bedin, Luigi R. Bedin +26 · 518 citations
Physics and Astronomy · #Advanced Camera for Surveys #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Elliptical galaxy #Galaxy #Galaxy cluster #Galaxy groups and clusters #Gamma-ray bursts and supernovae #Globular cluster #Hubble sequence #Hubble space telescope #Open cluster #Photometry (optics) #Physics #Star cluster #Stars #Stellar, planetary, and galactic studies #astro-ph

paper · pdf · doi:10.1086/511979

published in The Astronomical Journal 133(4), 1658-1672 (Institute of Physics) · 22 pages, 29 figures, accepted for publication in The Astronomical Journal, April 2007. High resolution version available at http://www.astro.ufl.edu/~ata/GC_Treasury/Web_Page/publications.html

arxiv created 2006/12/20 · openalex publication_date 2007/03/12 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05

Abstract

We present the first results of a large Advanced Camera for Surveys (ACS) survey of Galactic globular clusters. This Hubble Space Telescope ( HST ) Treasury project is designed to obtain photometry with S/N (signal-to-noise ratio) ≳10 for main-sequence stars with masses ≳0.2 M ⊙ in a sample of globulars using the ACS Wide Field Channel. Here we focus on clusters without previous HST imaging data. These include NGC 5466, NGC 6779, NGC 5053, NGC 6144, Palomar 2, E3, Lyngå 7, Palomar 1, and NGC 6366. Our color-magnitude diagrams (CMDs) extend reliably from the horizontal branch to as much as 7 mag fainter than the main-sequence turnoff and represent the deepest CMDs published to date for these clusters. Using fiducial sequences for three standard clusters (M92, NGC 6752, and 47 Tuc) with well-known metallicities and distances, we perform main-sequence fitting on the target clusters in order to obtain estimates of their distances and reddenings. These comparisons, along with fitting the cluster main sequences to theoretical isochrones, yield ages for the target clusters. We find that the majority of the clusters have ages that are consistent with the standard clusters at their metallicities. The exceptions are E3, which appears ∼2 Gyr younger than 47 Tuc, and Pal 1, which could be as much as 8 Gyr younger than 47 Tuc.

Citations

• UBVRI passbands

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