The role of cold flows in the assembly of galaxy disks

292Citations
Citations of this article
68Readers
Mendeley users who have this article in their library.

Abstract

We use high-resolution cosmological hydrodynamical simulations to demonstrate that cold flow gas accretion, particularly along filaments, modifies the standard picture of gas accretion and cooling onto galaxy disks. In the standard picture, all gas is initially heated to the virial temperature of the galaxy as it enters the virial radius. Low-mass galaxies are instead dominated by accretion of gas that stays well below the virial temperature, and even when a hot halo is able to develop in more massive galaxies there exist dense filaments that penetrate inside of the virial radius and deliver cold gas to the central galaxy. For galaxies up to L*, this cold accretion gas is responsible for the star formation (SF) in the disk at all times to the present. Even for galaxies at higher masses, cold flows dominate the growth of the disk at early times. Within this modified picture, galaxies are able to accrete a large mass of cold gas, with lower initial gas temperatures leading to shorter cooling times to reach the disk. Although SF in the disk is mitigated by supernovae feedback, the short cooling times allow for the growth of stellar disks at higher redshifts than predicted by the standard model. © 2009 The American Astronomical Society.

Cite

CITATION STYLE

APA

Brooks, A. M., Governato, F., Quinn, T., Brook, C. B., & Wadsley, J. (2009). The role of cold flows in the assembly of galaxy disks. Astrophysical Journal, 694(1), 396–410. https://doi.org/10.1088/0004-637X/694/1/396

Register to see more suggestions

Mendeley helps you to discover research relevant for your work.

Already have an account?

Save time finding and organizing research with Mendeley

Sign up for free