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VERSION:2.0
CALSCALE:GREGORIAN
PRODID:UW-Madison-Physics-Events
BEGIN:VEVENT
SEQUENCE:0
UID:UW-Physics-Event-2842
DTSTART:20121029T170000Z
DTEND:20121029T180000Z
DTSTAMP:20260420T034757Z
LAST-MODIFIED:20121022T165528Z
LOCATION:4421 Sterling Hall
SUMMARY:Star Formation in N-Body Dwarf Galaxy Simulations\, Special Lu
 nch Astronomy Talk\, Ferah Munshi\, University of Washington
DESCRIPTION:In this talk\, we examine the total stellar-to-halo mass r
 atio as a function of halo mass for a new sample of simulated field ga
 laxies using fully cosmological\, I>CDM\, high resolution SPH + N-Body
  simulations carried to the present time. These simulations include ex
 plicit H2 and metal cooling\, star formation (SF) and supernovae (SN) 
 driven gas outflows. We find extremely good agreement between the simu
 lations and predictions from the statistical Halo Occupation Distribut
 ion model presented in Moster et al. (2012). This is due to a combinat
 ion of systematic factors: a) gas outflows that reduce the overall SF 
 efficiency b) estimating the stellar masses of simulated galaxies usin
 g artificial observations and photometric techniques similar to those 
 used in observations. Our analysis provides an excellent match to prev
 ious observational estimates and suggests that stellar mass estimates 
 based on photometric magnitudes underestimate the contribution of old 
 stellar populations to the total stellar mass\, leading to stellar mas
 s errors of up to 50% for individual galaxies. These results highlight
  the importance of using proper techniques to compare simulations with
  observations and reduce the perceived tension between the star format
 ion efficiency in galaxy formation models and in real galaxies.
URL:https://www.physics.wisc.edu/events/?id=2842
END:VEVENT
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