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SUMMARY:Mapping the deforming dark matter haloes of the Milky Way and the 
 LMC with stellar streams
DTSTART;VALUE=DATE-TIME:20230320T104500Z
DTEND;VALUE=DATE-TIME:20230320T110000Z
DTSTAMP;VALUE=DATE-TIME:20241114T092409Z
UID:indico-contribution-210@meetings.aip.de
DESCRIPTION:Speakers: Sophia Lilleengen (University of Surrey)\nThe ongoin
 g merger of the Milky Way and the Large Magellanic Cloud (LMC) is deformin
 g the dark matter haloes of both galaxies\, effectively making these galax
 ies a local dark matter collider. Within this collider\, stellar streams a
 ct as useful detectors as they are very sensitive to the gravitational pot
 ential\, and span large parts of the Milky Way halo. \nThe Orphan-Chenab (
 OC) stream is particularly insightful as it spans the inner and outer Milk
 y Way\, and it passes close to the LMC (within 10kpc). In this talk\, I wi
 ll present the first models of the OC stream in the time-dependent halos o
 f the Milky Way and the LMC that are described by basis function expansion
 s of N-body simulations of the Milky Way-LMC passage. I will show how thes
 e deformations have an observable signature on the OC stream. In particula
 r\, we find that the Milky Way’s dipole has the most significant effect.
  \nWe do not currently have the tools to fit these deformations and ignori
 ng them may result in biases. To test this\, we fit mock streams evolved i
 n these deforming potentials with current state-of-the-art stream models. 
 Even though the MW is spherical in these mocks\, we infer extremely large 
 flattenings of the DM halos with q=0.6 and q=1.5. This shows that current 
 measurements of the MW DM halo shape are likely biased and motivates the n
 eed for computationally efficient tools to describe these deformations. Th
 is work is an important first step in measuring the Milky Way’s mass pro
 file over time.\n\nhttps://iaus379.aip.de/event/20/contributions/210/
LOCATION:Haus H\, Telegrafenberg
URL:https://iaus379.aip.de/event/20/contributions/210/
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