Journal
ASTROPHYSICAL JOURNAL
Volume 769, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/769/1/74
Keywords
galaxies: evolution; galaxies: formation; galaxies: halos; galaxies: kinematics and dynamics; intergalactic medium; methods: numerical
Categories
Funding
- NASA [NNX09AG01G]
- National Aeronautics and Space Administration
- Grainger Foundation
- Swiss National Science Foundation (SNF)
- NASA ATP
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1009999] Funding Source: National Science Foundation
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1153335] Funding Source: National Science Foundation
- NASA [NNX09AG01G, 118606] Funding Source: Federal RePORTER
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We use high-resolution cosmological hydrodynamic simulations to study the angular momentum acquisition of gaseous halos around Milky-Way-sized galaxies. We find that cold mode accreted gas enters a galaxy halo with similar to 70% more specific angular momentum than dark matter averaged over cosmic time ( though with a very large dispersion). In fact, we find that all matter has a higher spin parameter when measured at accretion than when averaged over the entire halo lifetime, and is well characterized by. lambda similar to 0.1, at accretion. Combined with the fact that cold flow gas spends a relatively short time (1-2 dynamical times) in the halo before sinking to the center, this naturally explains why cold flow halo gas has a specific angular momentum much higher than that of the halo and often forms cold flow disks. We demonstrate that the higher angular momentum of cold flow gas is related to the fact that it tends to be accreted along filaments.
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