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VERSION:2.0
PRODID:-//linuxsoftware.nz//NONSGML Joyous v1.4//EN
BEGIN:VEVENT
SUMMARY:MUSE-Faint: Dissecting the faintest galaxies with MUSE
DTSTART:20231214T143000Z
DTEND:20231214T160000Z
DTSTAMP:20260928T062335Z
UID:36f076b6-d110-4236-b44a-85ff328007de
SEQUENCE:1
CREATED:20231211T160614Z
DESCRIPTION:ABSTRACT: Ultra-faint dwarfs are the lowest mass and most dark
 -matter dominated systems known. The shallow potential wells make them sus
 ceptible to feedback from star formation and their low baryonic content al
 lows us to use their stars as test-particles in the dark matter potential.
  Here I will give an overview of the MUSE-Faint survey\, a MUSE GTO survey
  of 10 ultra-faint dwarfs. After introducing the survey\, I will outline h
 ow the high density of stellar spectra obtainable with MUSE can be used to
  constrain the dark matter content and density profiles of the galaxies an
 d discuss how the data can be used to constrain dark matter models and the
  details of galaxy formation models in the very most star poor dark matter
  halos known.  
LAST-MODIFIED:20231211T160614Z
LOCATION:Sala de Seminários do DF\,  Pavilhão de Física\, 2º piso
URL:http://df.vps.tecnico.ulisboa.pt/pt/eventos/muse-faint-dissecting-the-
 faintest-galaxies-with-muse/
X-ALT-DESC;FMTTYPE=text/html:<p data-block-key="z9ys6">ABSTRACT:</p><p dat
 a-block-key="a4n15"> Ultra-faint dwarfs are the lowest mass and most dark-
 matter dominated systems known. The shallow potential wells make them susc
 eptible to feedback from star formation and their low baryonic content all
 ows us to use their stars as test-particles in the dark matter potential. 
 </p><p data-block-key="5ft30"></p><p data-block-key="62bn5">Here I will gi
 ve an overview of the MUSE-Faint survey\, a MUSE GTO survey of 10 ultra-fa
 int dwarfs. After introducing the survey\, I will outline how the high den
 sity of stellar spectra obtainable with MUSE can be used to constrain the 
 dark matter content and density profiles of the galaxies and discuss how t
 he data can be used to constrain dark matter models and the details of gal
 axy formation models in the very most star poor dark matter halos known.  
 </p>
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