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|Title:||The Hubble Space Telescope UV Legacy Survey of Galactic Globular Clusters. I. Overview of the Project and Detection of Multiple Stellar Populations||Authors:||Piotto, G.
Milone, A. P.
King, I. R.
Marino, A. F.
Brown, T. M.
Cool, A. M.
Ferraro, F. R.
van der Marel, R. P.
|Issue Date:||2015||Journal:||THE ASTRONOMICAL JOURNAL||Number:||149||Issue:||3||First Page:||91||Abstract:||In this paper we describe a new UV-initiative Hubble Space Telescope project (GO-13297) that will complement the existing F606W and F814W database of the Advanced Camera for Surveys Globular Cluster (GC) Treasury by imaging most of its clusters through UV/blue WFC3/UVIS filters F275W, F336W, and F438W. This “magic trio” of filters has shown an uncanny ability to disentangle and characterize multiple population (MP) patterns in GCs in a way that is exquisitely sensitive to C, N, and O abundance variations. Combination of these passbands with those in the optical also gives the best leverage for measuring helium enrichment. The dozen clusters that had previously been observed in these bands exhibit a bewildering variety of MP patterns, and the new survey will map the full variance of the phenomenon. The ubiquity of multiple stellar generations in GCs has made the formation of these cornerstone objects more intriguing than ever; GC formation and the origin of their MPs have now become one and the same problem. In this paper we will describe the database and our data reduction strategy, as well as the uses we intend to make of the final photometry, astrometry, and PMs. We will also present preliminary color-magnitude diagrams from the data so far collected. These diagrams also draw on data from GO-12605 and GO-12311, which served as a pilot project for the present GO-13297. <P />Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555.||Acknowledgments:||A.A., S.C., S.H., M.M., and G.P. recognize partial support by the IAC (grant P301031) and the Ministry of Competitiveness and Innovation of Spain (grant AYA2010-16717). J.A., A.C., I.R.K., A.S., and E.V. acknowledge support from STScI grant GO-13297. A.P.M. acknowledges support by the Australian Research Council through Discovery Project grant DP120100475. M.Z. acknowledges support by Proyecto Fondecyt Regular 1110393, by the BASAL Center for Astrophysics and Associated Technologies PFB-06, and by Project IC120009 “Millennium Institute of Astrophysics (MAS)” of Iniciativa Científica Milenio by the Chilean Ministry of Economy, Development and Tourism. F.R.F., B.L. and E.D. acknowledge the support from the Cosmic-Lab project (web site: http://www.cosmic-lab.eu ) funded by the European Research Council, under contract ERC-2010-AdG-267675.||URI:||http://hdl.handle.net/20.500.12386/23806||URL:||https://iopscience.iop.org/article/10.1088/0004-6256/149/3/91||ISSN:||0004-6256||DOI:||10.1088/0004-6256/149/3/91||Bibcode ADS:||2015AJ....149...91P||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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