Forecasting the success of the WEAVE Wide-Field Cluster Survey on the extraction of the cosmic web filaments around galaxy clusters
| Autor: | Daniel J Cornwell, Ulrike Kuchner, Alfonso Aragón-Salamanca, Meghan E Gray, Frazer R Pearce, J Alfonso L Aguerri, Weiguang Cui, J Méndez-Abreu, Luis Peralta de Arriba, Scott C Trager |
|---|---|
| Přispěvatelé: | Astronomy |
| Rok vydání: | 2022 |
| Předmět: |
galaxies: haloes
Cosmology and Nongalactic Astrophysics (astro-ph.CO) galaxies: clusters: general Space and Planetary Science Astrophysics of Galaxies (astro-ph.GA) FOS: Physical sciences Astronomy and Astrophysics large-scale structure of Universe methods: data analysis Astrophysics - Astrophysics of Galaxies techniques: spectroscopic methods: numerical Astrophysics - Cosmology and Nongalactic Astrophysics |
| Zdroj: | Monthly Notices of the Royal Astronomical Society, 517, 1678-1694. Oxford University Press |
| ISSN: | 1365-2966 0035-8711 |
| Popis: | Next-generation wide-field spectroscopic surveys will observe the infall regions around large numbers of galaxy clusters with high sampling rates for the first time. Here we assess the feasibility of extracting the large-scale cosmic web around clusters using forthcoming observations, given realistic observational constraints. We use a sample of 324 hydrodynamic zoom-in simulations of massive galaxy clusters from TheThreeHundred project to create a mock-observational catalogue spanning $5R_{200}$ around 160 analogue clusters. These analogues are matched in mass to the 16 clusters targetted by the forthcoming WEAVE Wide-Field Cluster Survey (WWFCS). We consider the effects of the fibre allocation algorithm on our sampling completeness and find that we successfully allocate targets to 81.7 $\% \pm$ 1.3 of the members in the cluster outskirts. We next test the robustness of the filament extraction algorithm by using a metric, $D_{\text{skel}}$, which quantifies the distance to the filament spine. We find that the median positional offset between reference and recovered filament networks is $D_{\text{skel}} = 0.13 \pm 0.02$ Mpc, much smaller than the typical filament radius of $\sim$ 1 Mpc. Cluster connectivity of the recovered network is not substantially affected. Our findings give confidence that the WWFCS will be able to reliably trace cosmic web filaments in the vicinity around massive clusters, forming the basis of environmental studies into the effects of pre-processing on galaxy evolution. 18 pages, 14 figures. Accepted by MNRAS for publication |
| Databáze: | OpenAIRE |
| Externí odkaz: |
|