Gaseous Haloes: Linking Galaxies to the IGM

Details Gaseous Haloes: Linking Galaxies to the IGM Gaseous Haloes: Linking Galaxies to the IGM

2007-01-15

arxiv.org/abs/astro-ph/0701402v1

Astrophys.J.653:1517-1530,2006; New Astron.Rev.51:95-98,2007

Astronomy and Astrophysics

Astrophysics

5 pages, 3 figures, to appear in New Astronomy Review, Vol. 51; proceedings of "The Fate of Gas in Galaxies", Dwingeloo, July

Scientific paper

10.1086/508797 10.1016/j.newar.2

In recent years evidence has accumulated that nearby spiral galaxies are surrounded by massive haloes of neutral and ionised gas. These gaseous haloes rotate more slowly than the disks and show inflow motions. They are clearly analogous to the High Velocity Clouds of the Milky Way. We show that these haloes cannot be produced by a galactic fountain process (supernova outflows from the disk) where the fountain gas conserves its angular momentum. Making this gas interact with a pre-existing hot corona does not solve the problem. These results point at the need for a substantial accretion of low angular momentum material from the IGM.

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