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BEGIN:VEVENT
DTSTART;TZID=Atlantic/Canary:20210427T120000
DTEND;TZID=Atlantic/Canary:20210427T130000
UID:iactalks-1451
X-WR-CALNAME: IAC Talks: Open Astronomy Seminars
X-ORIGINAL-URL: /iactalks/Talks/view/1451
CREATED:2021-04-27T12:00:00+01:00
X-WR-CALDESC: IAC Talks upcomming talks
SUMMARY:Where feedback fails: clues from the dynamics of massive galaxies?
DESCRIPTION:Where feedback fails: clues from the dynamics of massive galaxi
 es?\nDr. Lorenzo Posti\n\n \nIt is widely understood that galaxies us
 e, throughout the  Hubble time, only a small fraction of the baryons assoc
 iated to their  dark matter halos to form stars. Such low baryon-to-stars 
 conversion  efficiencies are expected in galaxy formation scenarios where 
 stellar  & AGN feedback play a key role in regulating star formation i
 n  galaxies, respectively at the low- and high-mass end.\nIn  this talk I 
 will show how we can constrain this scenario using galaxy  dynamics. Both 
 robust determinations of disc dynamical scaling relations  (e.g. Tully-Fis
 her, mass-size) and accurate measurements of dark matter  halo masses from
  HI rotation curves of spirals and from the kinematics  of globular cluste
 rs around ellipticals, provide compelling evidence  that the population of
  massive spirals has systematically larger  baryon-to-stars conversion eff
 iciencies than ellipticals. In fact, we  see that the baryon-to-stars conv
 ersion efficiency monotonically  increases with mass for late-type galaxie
 s, while it shows a clear turn  over at about L* only for early-type galax
 ies. Thus, while massive early  types are compatible with standard stellar
 -to-halo mass relations based  on abundance matching, massive late types a
 re systematically discrepant  from it.\nI will discuss the possible reperc
 ussions  that these results have, highlighting in particular what they imp
 ly in  terms of AGN feedback and merging in galaxies of different types.  
 Finally I will show that current state-of-the-art cosmological  hydrodynam
 ical simulations (EAGLE, TNG) still struggle to reproduce what  we observe
  for the most massive discs.
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