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SUMMARY:3D models for the multiphase wind of M82 - Yuxuan Yuan (University
  of Cambridge)
DTSTART:20230301T131500Z
DTEND:20230301T134000Z
UID:TALK197863@talks.cam.ac.uk
CONTACT:Hannah Uebler
DESCRIPTION:Galactic winds are a crucial player in galaxy formation and ev
 olution\, but observations of them have proven extraordinarily difficult t
 o interpret\, leaving large uncertainties even in basic quantities such as
  mass outflow rates. Here we present an analysis of the wind of the nearby
  dwarf starburst galaxy M82 using a semi-analytic model that is able to ta
 ke advantage of the full three-dimensional information present in position
 –position–velocity data cubes measured in the H I 21cm line\, the CO J
  = 2->1 line\, and the Halpha line. Our best-fitting model produces positi
 on-dependent spectra in good agreement with the observations\, and shows t
 hat the total wind mass flux in the atomic and molecular phases is about 1
 0 Msun yr-1 (corresponding to a mass loading factor of about 2-3)\, with l
 ess than a factor of 2 uncertainty\; the mass flux in the warm ionized pha
 se is more poorly constrained\, and may be comparable to or smaller than t
 his. At least over the few kpc off the plane for which we trace the outflo
 w\, it appears to be a wind escaping the galaxy\, rather than a fountain t
 hat falls back. Our fits require that clouds of cool gas entrained into th
 e wind expand only modestly\, suggesting they are confined by magnetic fie
 lds\, radiative cooling\, or a combination of both. Finally\, we demonstra
 te that attempts to model the wind using simplifying assumptions such as i
 nstantaneous acceleration and a constant terminal wind speed can yield sig
 nificantly erroneous results.\n
LOCATION:The Hoyle Lecture Theatre + Zoom 
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