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Exploring the Chemical Composition and Double Horizontal Branch of the Bulge Globular Cluster NGC 6569
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Johnson_2018_AJ_155_71.pdf
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Final Published Version
Author
Johnson, C. I.Rich, R. Michael
Caldwell, Nelson
Mateo, Mario
Bailey, John I.
Olszewski, Edward W.
Walker, Matthew G.
Affiliation
Univ Arizona, Steward ObservIssue Date
2018-01-18
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IOP PUBLISHING LTDCitation
Exploring the Chemical Composition and Double Horizontal Branch of the Bulge Globular Cluster NGC 6569 2018, 155 (2):71 The Astronomical JournalJournal
The Astronomical JournalRights
© 2018. The American Astronomical Society. All rights reserved.Collection Information
This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.Abstract
Photometric and spectroscopic analyses have shown that the Galactic bulge cluster Terzan 5 hosts several populations with different metallicities and ages that manifest as a double red horizontal branch (HB). A recent investigation of the massive bulge cluster NGC 6569 revealed a similar, though less extended, HB luminosity split, but little is known about the cluster's detailed chemical composition. Therefore, we have used high- resolution spectra from the Magellan-M2FS and VLT-FLAMES spectrographs to investigate the chemical compositions and radial velocity distributions of red giant branch and HB stars in NGC 6569. We found the cluster to have a mean heliocentric radial velocity of -48.8 km s(-1) (sigma = 5.3 km s(-1); 148 stars) and <[Fe/H]> = -0.87 dex (19 stars), but the cluster's 0.05 dex [Fe/H] dispersion precludes a significant metallicity spread. NGC 6569 exhibits light- and heavy-element distributions that are common among old bulge/inner Galaxy globular clusters, including clear (anti) correlations between [O/Fe], [Na/Fe], and [Al/Fe]. The light-element data suggest that NGC 6569 may be composed of at least two distinct populations, and the cluster's low <[La/Eu]> = -0.11 dex indicates significant pollution with r- process material. We confirm that both HBs contain cluster members, but metallicity and lightelement variations are largely ruled out as sources for the luminosity difference. However, He mass fraction differences as small as Delta Y similar to 0.02 cannot be ruled out and may be sufficient to reproduce the double HB.ISSN
1538-3881Version
Final published versionSponsors
National Aeronautics and Space Administration; National Science Foundation; Clay Fellowship; National Science Foundation [AST-0923160, AST-1312997, AST-1313045, AST-1412999, AST-1413755]; M2FSAdditional Links
http://stacks.iop.org/1538-3881/155/i=2/a=71?key=crossref.f916c8f8e4e1a6763ee991d4e6917dafae974a485f413a2113503eed53cd6c53
10.3847/1538-3881/aaa294