Table 4.
Summary of TDCOSMO studies.
| Paper | Lens modelling | Dynamical modelling | Kinematic data uncertainty | H0 uncertainty | |||
|---|---|---|---|---|---|---|---|
| PL | C | λint | aperture(s) | 2D map | in flat ΛCDM | ||
| TDCOSMO I | ✓ | ✓ | sph. Jeans | 1, ∼4–10% | – | 4–9% per lens | |
| TDCOSMO IV | ✓ | ✓ | sph. Jeans | 1, ∼4–10% | – | 8% (sample of 7 lenses) | |
| TDCOSMO V | ✓ | ✓ | sph. Jeans | 1–10, 3–5% | — | 4–9% (sample of 7 lenses) | |
| TDCOSMO X | ✓ | ✓ | ✓ | JAM | – | 2.5% (stat.) + 2% (sys.) | 4% for RXJ1131−1231 |
| (This work) | |||||||
Notes. In the lens modelling, the primary lens mass distribution is parameterised by either a power-law (PL) or a composite (C) mass model, consisting of baryons and dark matter; some lens models also allow for an internal MST parameter λint. Dynamical modelling is based on spherical Jeans modelling or Jeans Anisotropic MGE (JAM; Cappellari 2008). Uncertainties for the kinematic data are per aperture or per 2D kinematic bin for the TDCOSMO lenses, or in the case of TDCOSMO V, the precision is on the overall uncertainty on the mean of the stellar velocity dispersion across the target.
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