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VERSION:2.0
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SUMMARY:The Milky Way mass function as a probe of dark matter models
DTSTART:20220512T143000Z
DTEND:20220512T160000Z
DTSTAMP:20260812T092324Z
UID:8f27fc8a-8a5b-44b6-a23d-9360d90f4956
SEQUENCE:1
CREATED:20220506T170139Z
DESCRIPTION: ABSTRACT: Predictions for the properties of the Milky Way (MW
 ) satellite galaxies are crucial tests for competing dark matter models. D
 eviations from the cold and collisionless picture of dark matter\, such as
  free-streaming\, dark acoustic oscillations\, and self-interactions betwe
 en dark matter particles\, modify predictions for the number of MW satelli
 te galaxies and/or for their densities. Calculating accurate predictions i
 s complicated by the large array of factors relevant to satellite formatio
 n and processing\, including the stochasticity of MW halo formation\, the 
 difficulties in modelling satellite stripping with limited resolution\, an
 d for contraction of the host halo through cooling baryons\, to name but a
  few. In this talk I will use the COCO N-body simulations of MWanalogue sy
 stems to make estimates for the MW satellite population properties in thre
 e models: cold dark matter (CDM)\, a warm dark matter model (WDM) with a t
 hermal relic mass of 3.3keV\, and a self-interacting dark matter model (SI
 DM) that enables gravothermal collapse. I will use these models to predict
  the range of viable subhalo hosts for ~33 observed MW satellites\, and th
 en discuss how future observations will enable us to ascertain which model
  best describes the properties of dark matter.  
LAST-MODIFIED:20220506T170139Z
LOCATION:Sala de Reuniões (2-8.3) Pavilhão de Física
URL:http://df.vps.tecnico.ulisboa.pt/pt/eventos/the-milky-way-mass-functio
 n-as-a-probe-of-dark-matter-models/
X-ALT-DESC;FMTTYPE=text/html:<p data-block-key="bhcuh"> ABSTRACT: Predicti
 ons for the properties of the Milky Way (MW) satellite galaxies are crucia
 l tests for competing dark matter models. Deviations from the cold and col
 lisionless picture of dark matter\, such as free-streaming\, dark acoustic
  oscillations\, and self-interactions between dark matter particles\, modi
 fy predictions for the number of MW satellite galaxies and/or for their de
 nsities. Calculating accurate predictions is complicated by the large arra
 y of factors relevant to satellite formation and processing\, including th
 e stochasticity of MW halo formation\, the difficulties in modelling satel
 lite stripping with limited resolution\, and for contraction of the host h
 alo through cooling baryons\, to name but a few. In this talk I will use t
 he COCO N-body simulations of MWanalogue systems to make estimates for the
  MW satellite population properties in three models: cold dark matter (CDM
 )\, a warm dark matter model (WDM) with a thermal relic mass of 3.3keV\, a
 nd a self-interacting dark matter model (SIDM) that enables gravothermal c
 ollapse. I will use these models to predict the range of viable subhalo ho
 sts for ~33 observed MW satellites\, and then discuss how future observati
 ons will enable us to ascertain which model best describes the properties 
 of dark matter.  </p>
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