2018/05/31 by Shihong Liao, Liang Gao · 39 citations
Environmental Science · Physics and Astronomy · #Accretion (finance) #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Baryon #Dark matter #Dark matter halo #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy formation and evolution #Halo #Physics #Plant Water Relations and Carbon Dynamics #Protein filament #Redshift #Star formation #astro-ph.GA
paper · pdf · doi:10.1093/mnras/stz441
published in Monthly Notices of the Royal Astronomical Society 485(1), 464-473 (Oxford University Press) · 10 pages, 8 figures, version accepted by MNRAS
openalex created_date 2018/06/01 · arxiv created 2019/02/14 · openalex publication_date 2019/02/14 · arxiv updated 2019/02/25 · openalex updated_date 2026/08/05
We use a high-resolution zoom-in hydrodynamical simulation to investigate the impact of filaments on galaxy formation in their residing dark matter haloes. A method based on the density field and the Hoshen–Kopelman algorithm is developed to identify filaments. We show that cold and dense gas pre-processed by dark matter filaments can be further accreted into residing individual low-mass haloes in directions along the filaments. Consequently, comparing with field haloes, gas accretion is very anisotropic for filament haloes. About 30 per cent of the accreted gas of a residing filament halo was pre-processed by filaments, leading to two different thermal histories for the gas in filament haloes. Filament haloes have higher baryon and stellar fractions when compared with their field counterparts. Without including stellar feedback, our results suggest that filaments assist gas cooling and enhance star formation in their residing dark matter haloes at high redshifts (i.e. |z| = 4.0 and 2.5).