Gaseous Haloes: Linking Galaxies to the IGM

Filippo Fraternali; James Binney; Tom Oosterloo; Renzo Sancisi

doi:10.1086/508797 10.1016/j.newar.2006.10.009

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arXiv · astro-ph/0701402

Gaseous Haloes: Linking Galaxies to the IGM

Filippo Fraternali·James Binney·Tom Oosterloo·Renzo Sancisi

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Abstract

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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Filippo Fraternali, James Binney, Tom Oosterloo, Renzo Sancisi. 2007-01-15. Gaseous Haloes: Linking Galaxies to the IGM. https://doi.org/10.1086/508797%2010.1016%2Fj.newar.2006.10.009

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