Poster details
Bridging spectroscopic observations of galaxy clusters and filaments to simulations
Abstract
We undergo preparatory work for the WEAVE Wide Field Cluster Survey (WWFCS) – an upcoming survey
providing thousands of galaxy spectra for each of ~ 20 galaxy clusters. Each cluster’s observation will be
entirely covered out to 5R200. This provides a unique insight into the infall region surrounding clusters,
allowing us to study the effect of pre-processing of galaxies as they enter a cluster’s potential well. We
use The ThreeHundred project, a hydrodynamical re-simulation of 324 massive clusters in a 1Gpc/h
cubed box. Using a halo finder (AHF), we obtain the halo distribution surrounding each individual
cluster. Mock observations are generated using the halo positions from TheThreeHundred and the
positions of the WEAVE pointings to determine where fibres should be placed on the fields. We compare
the mass distribution of WEAVE clusters to TheThreeHundred clusters to create a mass matched sample.
Once we obtain spectra from WEAVE, we aim to extract cosmic filaments using the filament extractor,
DisPerSE, at the boundaries of clusters and to quantify how matter is fed through these high-density
channels. This enables us to better understand the mass assembly of the universe as matter is accreted
from the cosmic web and investigate how galaxy properties (such as SFR, colour, AGN feedback), change
as a function of distance from the filaments. Using the spectra from WEAVE, we also wish to quantify
where and how changes in morphology and star formation occur and their related timescales. Further to
this, we will look to determine what fraction of galaxies fall into clusters through filaments and how this
varies with the cluster’s dynamical state.
providing thousands of galaxy spectra for each of ~ 20 galaxy clusters. Each cluster’s observation will be
entirely covered out to 5R200. This provides a unique insight into the infall region surrounding clusters,
allowing us to study the effect of pre-processing of galaxies as they enter a cluster’s potential well. We
use The ThreeHundred project, a hydrodynamical re-simulation of 324 massive clusters in a 1Gpc/h
cubed box. Using a halo finder (AHF), we obtain the halo distribution surrounding each individual
cluster. Mock observations are generated using the halo positions from TheThreeHundred and the
positions of the WEAVE pointings to determine where fibres should be placed on the fields. We compare
the mass distribution of WEAVE clusters to TheThreeHundred clusters to create a mass matched sample.
Once we obtain spectra from WEAVE, we aim to extract cosmic filaments using the filament extractor,
DisPerSE, at the boundaries of clusters and to quantify how matter is fed through these high-density
channels. This enables us to better understand the mass assembly of the universe as matter is accreted
from the cosmic web and investigate how galaxy properties (such as SFR, colour, AGN feedback), change
as a function of distance from the filaments. Using the spectra from WEAVE, we also wish to quantify
where and how changes in morphology and star formation occur and their related timescales. Further to
this, we will look to determine what fraction of galaxies fall into clusters through filaments and how this
varies with the cluster’s dynamical state.