• Fabio Governato
  • Beth Willman
  • Lucio Mayer
Part of the Astrophysics and Space Science Proceedings book series (ASSSP)


We have used fully cosmological, high resolution N-body + SPH simulations to followthe formation of disk galaxies with a rotational velocity between 140 and 280 km/s in a ΛCDM universe. The simulations include gas cooling, star formation (SF), the effects of a uniform UV background and a physically motivated description of feedback from supernovae(SN). The host dark matter (DM) halos have a spin and last major merger redshift typical of galaxy sized halos as measured in recent large scale N–Body simulations. Galaxies formed rotationally supported disks with realistic exponential scale lengths and fall on the I-band and baryonic Tully-Fisher relations. The combination of UV background and SN feedback drastically reduced the number of visible satellites orbiting inside a Milky Way sizedhalo, bringing it fair agreement with observations. Feedback delays SF in small galaxies and more massive ones contain older stellar populations. The current star formation ratesas a function of galaxy stellar mass are in good agreement with those measured by the SDSS.


Star Formation Star Formation Rate Disk Galaxy Stellar Disk Galaxy Formation 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.


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Copyright information

© Springer 2007

Authors and Affiliations

  • Fabio Governato
    • 1
    • 2
  • Beth Willman
    • 3
  • Lucio Mayer
    • 4
  1. 1.INAF-BreraMilanoItaly
  2. 2.University of WashingtonSeattleUSA
  3. 3.NYUGotham CityUSA
  4. 4.Institute fur AstronomieETH ZurichSwitzerland

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