2008/11/19 by Andrew J. Davis, Priyamvada Natarajan
Physics and Astronomy · #Angular momentum #Astronomy #Astrophysics #Classical mechanics #Cold dark matter #Cosmology and Gravitation Theories #Dark matter #Galaxies: Formation, Evolution, Phenomena #Galaxy #Physics #Redshift #Spin (aerodynamics) #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2008.14267.x
6 pages, 3 figures. Accepted MNRAS
arxiv created 2008/11/19 · openalex publication_date 2009/02/07 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
In this paper, we study the angular momentum properties of simulated dark matter haloes at high redshifts that likely host the first stars in the Universe. Calculating the spin distributions of these 106– 107 M⊙ haloes in redshift slices from z= 15 to 6, we find that they are well fit by a lognormal distribution as is found for lower redshift and more massive haloes in earlier work. We find that both the mean value of the spin and dispersion are largely unchanged with redshift for all haloes. Our key result is that subsamples of low- and high-spin, 106 and 107 M⊙, haloes show difference in clustering strength. In both mass bins, higher spin haloes are more strongly clustered in concordance with a tidal torquing picture for the growth of angular momentum in dark matter haloes in the cold dark matter paradigm.