The mass–richness normalization from this work and from previous works that estimated the same using different techniques: a slightly older version of EVL (F16), weak lensing (McClintock et al. 2019), CMB lensing (Baxter et al. 2018), and from a combined cosmological analysis of different probes, including cluster-scale haloes (To et al. 2021). The estimates for McClintock et al. (2019) and To et al. (2021) are quoted away their respective pivot points, and thus their errors include additional uncertainties coming from the redshift and richness evolution. The uncertainties at their pivot scales are |$5.1$| and |$4.6\,\,\mathrm{ per}\,\mathrm{ cent}$|, respectively.
| Source . | Technique . | 〈log10M200c|λ = 30, z = 0.2〉 . | Error . |
|---|---|---|---|
| This work, All sims | Ensemble velocity likelihood (EVL) | 14.28 ± 0.037 | |$8.7\,\mathrm{ per}\,\mathrm{ cent}$| |
| This work, Sims w/o BM | EVL | 14.30 ± 0.031 | |$7.4\,\mathrm{ per}\,\mathrm{ cent}$| |
| Farahi et al. (2016) | Older EVL | 14.19 ± 0.096 | |$22\,\mathrm{ per}\,\mathrm{ cent}$| |
| McClintock et al. (2019) | Background galaxy weak lensing | 14.22 ± 0.035 | |$8.1\,\mathrm{ per}\,\mathrm{ cent}$| |
| To et al. (2021) | Galaxy/DM clustering + cluster abundance | 14.30 ± 0.079 | |$18\,\mathrm{ per}\,\mathrm{ cent}$| |
| Baxter et al. (2018) | CMB lensing | 14.19 ± 0.074 | |$17\,\mathrm{ per}\,\mathrm{ cent}$| |
| Source . | Technique . | 〈log10M200c|λ = 30, z = 0.2〉 . | Error . |
|---|---|---|---|
| This work, All sims | Ensemble velocity likelihood (EVL) | 14.28 ± 0.037 | |$8.7\,\mathrm{ per}\,\mathrm{ cent}$| |
| This work, Sims w/o BM | EVL | 14.30 ± 0.031 | |$7.4\,\mathrm{ per}\,\mathrm{ cent}$| |
| Farahi et al. (2016) | Older EVL | 14.19 ± 0.096 | |$22\,\mathrm{ per}\,\mathrm{ cent}$| |
| McClintock et al. (2019) | Background galaxy weak lensing | 14.22 ± 0.035 | |$8.1\,\mathrm{ per}\,\mathrm{ cent}$| |
| To et al. (2021) | Galaxy/DM clustering + cluster abundance | 14.30 ± 0.079 | |$18\,\mathrm{ per}\,\mathrm{ cent}$| |
| Baxter et al. (2018) | CMB lensing | 14.19 ± 0.074 | |$17\,\mathrm{ per}\,\mathrm{ cent}$| |
The mass–richness normalization from this work and from previous works that estimated the same using different techniques: a slightly older version of EVL (F16), weak lensing (McClintock et al. 2019), CMB lensing (Baxter et al. 2018), and from a combined cosmological analysis of different probes, including cluster-scale haloes (To et al. 2021). The estimates for McClintock et al. (2019) and To et al. (2021) are quoted away their respective pivot points, and thus their errors include additional uncertainties coming from the redshift and richness evolution. The uncertainties at their pivot scales are |$5.1$| and |$4.6\,\,\mathrm{ per}\,\mathrm{ cent}$|, respectively.
| Source . | Technique . | 〈log10M200c|λ = 30, z = 0.2〉 . | Error . |
|---|---|---|---|
| This work, All sims | Ensemble velocity likelihood (EVL) | 14.28 ± 0.037 | |$8.7\,\mathrm{ per}\,\mathrm{ cent}$| |
| This work, Sims w/o BM | EVL | 14.30 ± 0.031 | |$7.4\,\mathrm{ per}\,\mathrm{ cent}$| |
| Farahi et al. (2016) | Older EVL | 14.19 ± 0.096 | |$22\,\mathrm{ per}\,\mathrm{ cent}$| |
| McClintock et al. (2019) | Background galaxy weak lensing | 14.22 ± 0.035 | |$8.1\,\mathrm{ per}\,\mathrm{ cent}$| |
| To et al. (2021) | Galaxy/DM clustering + cluster abundance | 14.30 ± 0.079 | |$18\,\mathrm{ per}\,\mathrm{ cent}$| |
| Baxter et al. (2018) | CMB lensing | 14.19 ± 0.074 | |$17\,\mathrm{ per}\,\mathrm{ cent}$| |
| Source . | Technique . | 〈log10M200c|λ = 30, z = 0.2〉 . | Error . |
|---|---|---|---|
| This work, All sims | Ensemble velocity likelihood (EVL) | 14.28 ± 0.037 | |$8.7\,\mathrm{ per}\,\mathrm{ cent}$| |
| This work, Sims w/o BM | EVL | 14.30 ± 0.031 | |$7.4\,\mathrm{ per}\,\mathrm{ cent}$| |
| Farahi et al. (2016) | Older EVL | 14.19 ± 0.096 | |$22\,\mathrm{ per}\,\mathrm{ cent}$| |
| McClintock et al. (2019) | Background galaxy weak lensing | 14.22 ± 0.035 | |$8.1\,\mathrm{ per}\,\mathrm{ cent}$| |
| To et al. (2021) | Galaxy/DM clustering + cluster abundance | 14.30 ± 0.079 | |$18\,\mathrm{ per}\,\mathrm{ cent}$| |
| Baxter et al. (2018) | CMB lensing | 14.19 ± 0.074 | |$17\,\mathrm{ per}\,\mathrm{ cent}$| |
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