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SEQUENCE:0
UID:UW-Physics-Event-9220
DTSTART:20250512T180000Z
DTEND:20250512T200000Z
DTSTAMP:20260413T135048Z
LAST-MODIFIED:20250430T203349Z
LOCATION:B343 Sterling or https://uwmadison.zoom.us/j/6552547315
SUMMARY:The Magellanic System: The Clouds and their circumgalactic med
 ium within a cosmological context\, Preliminary Exam\, Robin Chisholm\
 , Physics PhD student
DESCRIPTION:Despite tremendous strides in our understanding of the Mag
 ellanic Clouds -the closest and most massive dwarf galaxies to the Mil
 ky Way (MW)- many questions\, especially regarding their circumgalacti
 c medium (CGM)\, remain open. We characterize the warm CGM of an isola
 ted dwarf galaxy pair with properties similar to the Magellanic Clouds
  prior to their infall into a MW-mass halo\, in the HESTIA cosmologica
 l simulations. The massive dwarf hosts a warm coronal gas envelope wit
 h a temperature of T ~ 3 x 10^5 K\, consistent with expectations for v
 irialized CGM in dwarf halos. Tidal interactions produce a neutral gas
  stream that extends over ~ 150 kpc\, with an HI mass of ~ 10^8 M⊙\,
  similar to the Magellanic Stream. Furthermore\, in the Hestia simulat
 ion suite\, we find that coronal gas is ubiquitous in all halos with M
  > 10^11 M⊙\, implying that massive dwarfs generically develop exten
 ded gaseous envelopes prior to accretion. This result has significant 
 implications for the survival of neutral tidal structures\, and sugges
 ts that current and future high-ion UV absorption-line observations ar
 e indicative of warm coronae surrounding LMC-mass dwarfs\, independent
  of their environment. We conclude by discussing future plans to furth
 er our understanding of the Magellanic System by running a suite of is
 olated simulations to constrain the Small Magellanic Cloud's orbital h
 istories.
URL:https://www.physics.wisc.edu/events/?id=9220
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