2D gas and SZ maps recover 3D cosmic web filaments around simulated clusters with median distances of 0.22-0.24 h^{-1} Mpc, and filaments contribute ~80% to the outskirts' integrated Compton-Y.
Title resolution pending
4 Pith papers cite this work. Polarity classification is still indexing.
4
Pith papers citing it
citation-role summary
method 2
citation-polarity summary
verdicts
UNVERDICTED 4roles
method 2polarities
use method 2representative citing papers
Late-type galaxies dominate shape-shape alignments in the filaments of the Perseus-Pisces supercluster while early-types cluster near dense centers, indicating distinct tidal mechanisms out to 1 Mpc/h.
Simulations of Euclid Deep Fields show that cosmic web structures can be reconstructed from H-alpha galaxies with biases from redshift distortions and selection effects that can be partially mitigated, allowing recovery of stellar mass gradients toward filaments.
IllustrisTNG simulations link filament density to galaxy morphology trends across redshifts and predict that Roman's planned HLWAS survey needs greater depth to accurately map the z=1 cosmic web.
citing papers explorer
-
The Three Hundred project: cosmic web identification from 2D gas and Compton-$y$ maps of galaxy clusters outskirts
2D gas and SZ maps recover 3D cosmic web filaments around simulated clusters with median distances of 0.22-0.24 h^{-1} Mpc, and filaments contribute ~80% to the outskirts' integrated Compton-Y.
-
Dissecting the Perseus-Pisces supercluster observed with CFHT-MegaCam: Exploring late-type galaxy shape alignments within the local cosmic web
Late-type galaxies dominate shape-shape alignments in the filaments of the Perseus-Pisces supercluster while early-types cluster near dense centers, indicating distinct tidal mechanisms out to 1 Mpc/h.
-
Euclid preparation. 3D reconstruction of the cosmic web with simulated Euclid Deep spectroscopic samples
Simulations of Euclid Deep Fields show that cosmic web structures can be reconstructed from H-alpha galaxies with biases from redshift distortions and selection effects that can be partially mitigated, allowing recovery of stellar mass gradients toward filaments.
-
Impact of Cosmic Filaments on Galaxy Morphological Evolution and Predictions of Early Cosmic Web Structure for Roman
IllustrisTNG simulations link filament density to galaxy morphology trends across redshifts and predict that Roman's planned HLWAS survey needs greater depth to accurately map the z=1 cosmic web.