How do Galaxies Get Their Gas?

  • Neal Katz
  • Dusan Keres
  • Romeel Davé
  • David H. Weinberg
Part of the Astrophysics and Space Science Library book series (ASSL, volume 281)


Not the way one might have thought. In hydrodynamic simulations of galaxy formation, some gas follows the traditionally envisioned route, shock heating to the halo virial temperature before cooling to the much lower temperature of the neutral ISM. But most gas enters galaxies without ever heating close to the virial temperature, gaining thermal energy from weak shocks and adiabatic compression, and radiating it just as quickly. This “cold mode” accretion is channeled along filaments, while the conventional, “hot mode” accretion is quasi-spherical. Cold mode accretion dominates high redshift growth by a substantial factor, while at z < 1 the overall accretion rate declines and hot mode accretion has greater relative importance. The decline of the cosmic star formation rate at low z is driven largely by geometry, as the typical cross section of filaments begins to exceed that of the galaxies at their intersections.


Smooth Particle Hydrodynamic Smooth Particle Hydrodynamic Galaxy Formation Dark Matter Halo Smooth Particle Hydrodynamic Simulation 
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 Science+Business Media Dordrecht 2003

Authors and Affiliations

  • Neal Katz
    • 1
  • Dusan Keres
    • 1
  • Romeel Davé
    • 2
  • David H. Weinberg
    • 3
  1. 1.Department of AstronomyUniversity of MassachusettsAmherstUSA
  2. 2.Steward ObservatoryUniversity of ArizonaTucsonUSA
  3. 3.Department of AstronomyOhio State UniversityColumbusUSA

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