Table 1.
Connectivity in the literature.
| Cosmological | Box | mDM | Cosmic web | Persistence | Calibration |
|---|---|---|---|---|---|
| simulations | [Mpc/h] | [109 M⊙] | tracers | σ | method |
| Poisson DM-only (This work) | 205 | 8 | DM/halos | 7/1 | CPmax-halos |
| Monge-Ampère DM-only (This work) | 205 | 8 | DM/halos | 9.5 / 7 | CPmax-halos |
| DM-only (Aragón-Calvo et al. 2010) | 150 | 2 | DM | – | – |
| HzAGN 2D (Darragh Ford et al. 2019) | 100 | 0.08 | 2D galaxies | 1.5 | HzAGN 3D |
| ITNG-300 (Gouin et al. 2021) | 205 | 0.06 | halos | 3 | CPmax-halos |
| The300 (Santoni et al. 2023) | 1000 | 1.8 | gas | 0.21 | – |
| HzAGN 3D (Kraljic et al. 2020)* | 100 | 0.08 | 3D galaxies | 3 | – |
| MTNG (Galárraga-Espinosa et al. 2024)* | 7500 | 11 | 3D galaxies | 2 | CPmax-halos |
| Observations | Redshift | Persistence | Calibration | Number of clusters | Sky area |
| σ | method | or groups | deg2 | ||
| COSMOS2015 (Darragh Ford et al. 2019) | 0.5–1.2 | 1.5 | HzAGN 2D | 900 | 1.38 |
| CFHTLS (Sarron et al. 2019) | 0.15–0.7 | 2 | 2D CFHTLS | – | 154 |
| Coma (Malavasi et al. 2020) | local | 5 | – | 1 | – |
| Abell 2142 (Einasto et al. 2020) | local | – | – | 1 | – |
| SDSS DR10 (Einasto et al. 2021) | 0.009–0.2 | – | – | 4 | 112 |
Notes. From left to right, the columns give the data type, the size of the box, the resolution and the cosmic web tracers for simulations, the redshift of observed data, the persistence threshold to detect filaments, and the calibration method to set this free parameter of the DisPerSE code. If the persistence is not specified, it means that the skeleton has not been extracted with the DisPerSE code. One of the calibration methods consists of comparing the positions of peaks (CPmax) to those of the most massive halos such as galaxy groups and clusters (> 1013 M⊙) (see Sect. 2.4). For the cosmological simulations, all the cosmic web tracers are 3D quantities except for the HzAGN simulation. For the COSMOS and CFHTLS data, the calibration method involves optimally recovering the filaments in the 2D light-cone catalogues created from 3D cosmological simulations.1 It corresponds to an absolute persistence cut because DisPerSE is not applied to discrete particles but on a 3D grid for the gas. *These data are not taken into account in our study (for the reasons, see Sect. 2.5).
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