Table 1.
Distance Network datasets.
| Measure | Reference | Notes |
|---|---|---|
| Milky Way (MW) | Riess et al. (2018, 2021, 2022a) | (a) |
| LMC | Pietrzyński et al. (2019) | μ0 = 18.477±0.024; converted from distance in kpc |
| SMC | Graczyk et al. (2020) | μ0 = 18.977 ± 0.032; converted from distance in kpc |
| NGC 4258 Masers | Reid et al. (2019) | μ0 = 29.397 ± 0.032 |
| Primary distance indicators | ||
| HST Cepheids | Riess et al. (2022b) | SN hosts, separate measures, N4258, MW, LMC (R22a fits 9,10,11) |
| Riess et al. (2022a) | MW cluster Cepheid photometry | |
| Riess et al. (2019) | LMC | |
| Yuan et al. (2022) | NGC 4258 | |
| Breuval et al. (2024) | SMC | |
| JWST Cepheids | Riess et al. (2024, 2025) | |
| JWST TRGB | Anand et al. (2024a) | |
| Li et al. (2024a, 2025a) | ||
| JWST TRGB | Hoyt et al. (2025) | |
| JWST TRGB | Anand et al. (2024b, 2025) | |
| HST TRGB | Anand et al. (2024a) | |
| HST TRGB | Freedman et al. (2025) | |
| HST TRGB | de Jaeger et al. (2022) | and contained references |
| JAGB | Li et al. (2025b) | |
| JAGB | Freedman et al. (2025) | |
| Miras | Huang et al. (2024) | Modified in correspondence with C. Huang to N4258-only values |
| Secondary distance indicators | ||
| SNIa Pantheon+ | Brout et al. (2022a) | https://github.com/PantheonPlusSH0ES/DataRelease |
| SNIa SNooPy (post v2.7) | Burns, priv. comm. | Refitting the official data from Uddin et al. (2024) |
| SNIa SNooPy (pre v2.7) | Uddin et al. (2024) | https://github.com/syeduddin/h0csp/tree/main/data/working |
| SNIa BayesSN | Dhawan et al. (2023) | also Hayes priv. comm. for additional fits |
| SNIa Salt3 | Kenworthy et al. (2021) | |
| SNIa IR | Galbany et al. (2023) | J, H bands separately |
| SNII (SCM) | de Jaeger et al. (2020b) | de Jaeger, priv. comm. |
| TF | Boubel et al. (2024b) | Cosmicflows-4 catalog; data curated by the authors |
| Other | ||
| SNII EPM | Vogl et al. (2025), | Removed galaxies M61 and NGC6946, for which peculiar |
| Csörnyei et al. (2023b) | velocities could not be meaningfully established | |
| Megamasers | Pesce et al. (2020b, Tab. 1) | We also adopt our own peculiar velocity treatments |
| Coma FP | Said et al. (2025) | (See also Appendix B.3.8) |
| SBF | Jensen et al. (2025) | Ancillary info from priv. comm. with J. B. Jensen |
Notes. For all references, the listed uncertainties have been decomposed into those coming from the anchor (which the Distance Network treats separately) and those coming from the actual measurement of the distance indicator (separated between the components within and without the anchor).
For the measurement of calibrators within the Milky Way galaxy, its extent is quite relevant. Therefore we adopted the individual measurements standardized to a 1 kpc reference distance.
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