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SUMMARY:Modeling Dark Matter Halo Spin using Observations and Simulations:
  application to UGC 5288
DTSTART;VALUE=DATE-TIME:20230322T150300Z
DTEND;VALUE=DATE-TIME:20230322T150500Z
DTSTAMP;VALUE=DATE-TIME:20240704T115746Z
UID:indico-contribution-278@meetings.aip.de
DESCRIPTION:Speakers: Ansar Sioree (Indian Institute of Astrophysics\, Ben
 galuru)\nDark matter halo properties are well studied in cosmological simu
 lations but are very challenging to estimate from observations. The dark m
 atter halo density profile of galaxies from observations has been modeled 
 previously using multiple probes that trace the dark matter potential\, ho
 wever\, the angular momentum distribution of the dark matter halos is stil
 l a subject of debate. In this study\, we demonstrate a method for estimat
 ing the halo spin and halo concentration of a low luminosity\, gas-rich dw
 arf galaxy by forward modeling disk properties derived from observations o
 f the stellar and gas surface densities\, the disk scale length\, the neut
 ral hydrogen rotation curve\, the bar length\, and bar ellipticity. Our me
 thod is a combination of semi-analytical techniques and N-body/SPH simulat
 ions. Here\, we apply our method to the low surface brightness (LSB) dwarf
  galaxy UGC 5288\, and model its dark matter halo with both a cuspy Hernqu
 ist profile and a flat-core pseudo-isothermal profile. We find that the be
 st match with observations is a pseudo-isothermal halo model with core rad
 ius r$_{c}$ = 0.23 kpc and a high halo spin $\\lambda$ = 0.08 at the viria
 l radius. These findings are consistent with previous rotation curve estim
 ates of the halo density profile of UGC 5288\, as well as the theoreticall
 y predicted high spins of dwarf LSB galaxies. We finally compare our resul
 ts with the halo spin distribution of barred galaxies in one of the high r
 esolution cosmological magneto-hydrodynamical simulations TNG-50. We find 
 that our model predicts halo spin distribution of UGC5288 up to a ballpark
  value\, although\, there remain significant uncertainties due to the form
 ation history of the dark matter halos from the TNG50 simulations. We also
  find that the inner halo spin in barred galaxies is different from that o
 f unbarred ones\, and the halo spin shows weak correlations with bar prope
 rties.\n\nhttps://meetings.aip.de/event/20/contributions/278/
LOCATION:Haus H\, Telegrafenberg
URL:https://meetings.aip.de/event/20/contributions/278/
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