A Chemical Composition Survey of the Iron-complex Globular Cluster NGC 6273 (M19)
AuthorJohnson, C. I.
Rich, R. Michael
Bailey, III, John I.
Clarkson, William I.
Olszewski, Edward W.
Walker, Matthew G.
AffiliationUniv Arizona, Steward Observ
general - globular clusters
individual ( NGC 6273, M19) - stars
abundances Supporting material
MetadataShow full item record
PublisherIOP PUBLISHING LTD
CitationA Chemical Composition Survey of the Iron-complex Globular Cluster NGC 6273 (M19) 2017, 836 (2):168 The Astrophysical Journal
JournalThe Astrophysical Journal
Rights© 2017. The American Astronomical Society. All rights reserved.
Collection InformationThis 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 email@example.com.
AbstractRecent observations have shown that a growing number of the most massive Galactic globular clusters contain multiple populations of stars with different [Fe/H] and neutron-capture element abundances. NGC 6273 has only recently been recognized as a member of this "iron-complex" cluster class, and we provide here a chemical and kinematic analysis of > 300 red giant branch and asymptotic giant branch member stars using high-resolution spectra obtained with the Magellan-M2FS and VLT-FLAMES instruments. Multiple lines of evidence indicate that NGC 6273 possesses an intrinsic metallicity spread that ranges from about [Fe/H] = -2 to -1 dex, and may include at least three populations with different [Fe/H] values. The three populations identified here contain separate first (Na/Al-poor) and second (Na/Al-rich) generation stars, but a Mg-Al anti-correlation may only be present in stars with [Fe/H] greater than or similar to -1.65. The strong correlation between [La/Eu] and [Fe/H] suggests that the sprocess must have dominated the heavy element enrichment at higher metallicities. A small group of stars with low [alpha/Fe] is identified and may have been accreted from a former surrounding field star population. The cluster's large abundance variations are coupled with a complex, extended, and multimodal blue horizontal branch (HB). The HB morphology and chemical abundances suggest that NGC 6273 may have an origin that is similar to omega Cen and M54.
VersionFinal published version
SponsorsNational Aeronautics and Space Administration; National Science Foundation; Clay Fellowship; National Science Foundation [AST-0923160, AST-1313045, AST-1412999, AST-1413755, AST-1313006]; NASA through Space Telescope Science Institute [GO-14197]