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PRODID:-//Heidelberg University//HePhySTO//EN
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DTEND:20261015T101500Z
UID:6f66c7a89ef7aee8c8cfb2b4063cc818@physik.uni-heidelberg.de
DTSTAMP:20261007T213312Z
LOCATION:ARI\, Moenchhofstrasse 12-14\, Seminarraum 1.OG
DESCRIPTION:Globular clusters (GCs) are old\, densely-packed groups of thou
 sands to millions of stars and have\nlong been hypothesized to be the build
 ing blocks of the Milky Way’s stellar halo due to their high star formation
  efficiency. Excitingly\, early results from JWST suggest that clustered st
 ar formation may also be dominant in other galaxies at high redshifts. Alth
 ough the Milky Way is a perfect laboratory in which to study GCs due to our
  ability to resolve individual stars\, the clusters we observe today are li
 kely to be only the most massive survivors of what was once a much larger p
 opulation of Galactic GCs. In this talk\, I will summarize how we can trace
  the contribution of the Milky’s Way’s disrupted GCs to the Galaxy by ident
 ifying their most unusual stars\, those with such high nitrogen-to-oxygen r
 atios ([N/O]) that they can reliably be identified as having originated in 
 a GC even long after escaping. I will then summarize our recent work to ide
 ntify which of these anomalous GC-origin stars in the field may have been b
 orn in surviving Milky Way GCs by associating stars\nand clusters via their
  integrals of motion. Although in bulk it appears that the high-[N/O] stars
  originated in inner Galaxy GCs\, specific star-to-cluster tagging is compl
 icated by the fact that integrals of motion are likely not conserved due to
  the effects of dynamical friction and the Galactic bar. These results have
  interesting implications for the feasibility of chemodynamical studies of 
 the Milky Way halo.\n\nImported from https://www.physik.uni-heidelberg.de/h
 ephysto/ (no warranty for accuracy).
URL;VALUE=URI:https://www.physik.uni-heidelberg.de/hephysto/index.php?s=tal
 k&id=13005
SUMMARY:ARI Institute Colloquium: Sarah Kane - A graveyard of disrupted glo
 bular clusters in the Milky Way’s stellar halo
DTSTART:20261015T091500Z
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