Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 454, Issue 3, Pages 3341-3350Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stv2260
Keywords
hydrodynamics; large-scale structure of Universe
Categories
Funding
- Department of Energy [DESC0011114]
- William S. Dietrich II Presidential PhD Fellowship
- DOE-ASC
- NASA
- NSF
- NASA ROSES [12-EUCLID12-0004]
- NSF [AST-1313169]
- DOE
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1517593] Funding Source: National Science Foundation
- Direct For Mathematical & Physical Scien
- Division Of Mathematical Sciences [1513412] Funding Source: National Science Foundation
Ask authors/readers for more resources
In this paper, we study the filamentary structures and the galaxy alignment along filaments at redshift z = 0.06 in the MassiveBlack-II simulation, a state-of-the-art, high-resolution hydrodynamical cosmological simulation which includes stellar and AGN feedback in a volume of (100 Mpc h(-1))(3). The filaments are constructed using the subspace constrained mean shift (SCMS; Ozertem & Erdogmus; Chen et al.). First, we show that reconstructed filaments using galaxies and reconstructed filaments using dark matter particles are similar to each other; over 50 per cent of the points on the galaxy filaments have a corresponding point on the dark matter filaments within distance 0.13 Mpc h(-1) (and vice versa) and this distance is even smaller at high-density regions. Second, we observe the alignment of the major principal axis of a galaxy with respect to the orientation of its nearest filament and detect a 2.5 Mpc h(-1) critical radius for filament's influence on the alignment when the subhalo mass of this galaxy is between 10(9) M-circle dot h(-1) and 10(12) M-circle dot h(-1). Moreover, we find the alignment signal to increase significantly with the subhalo mass. Third, when a galaxy is close to filaments (less than 0.25 Mpc h(-1)), the galaxy alignment towards the nearest galaxy group is positively correlated with the galaxy subhalo mass. Finally, we find that galaxies close to filaments or groups tend to be rounder than those away from filaments or groups.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available