Table 1.
Photometric distance uncertainties and percentage of spectroscopic galaxies in each sample.
| Name | Distance uncertainties | Spectroscopic distances |
|---|---|---|
| σ0 | – | 100% |
| σ1 | 𝒩(0 Mpc, (1 Mpc)2) | 0% |
| σ2 | 𝒩(0 Mpc, (2 Mpc)2) | 0% |
| σ3 | 𝒩(0 Mpc, (3 Mpc)2) | 0% |
| σ5 | 𝒩(0 Mpc, (5 Mpc)2) | 0% |
| σ7 | 𝒩(0 Mpc, (7 Mpc)2) | 0% |
| σ10 | 𝒩(0 Mpc, (10 Mpc)2) | 0% |
| σ5s50 | 𝒩(0 Mpc, (5 Mpc)2) | 50% |
| σ5s40 | 𝒩(0 Mpc, (5 Mpc)2) | 40% |
| σ5s30 | 𝒩(0 Mpc, (5 Mpc)2) | 30% |
| σ5s20 | 𝒩(0 Mpc, (5 Mpc)2) | 20% |
| σ5s10 | 𝒩(0 Mpc, (5 Mpc)2) | 10% |
| σ10s50 | 𝒩(0 Mpc, (10 Mpc)2) | 50% |
| σ10s40 | 𝒩(0 Mpc, (10 Mpc)2) | 40% |
| σ10s30 | 𝒩(0 Mpc, (10 Mpc)2) | 30% |
| σ10s20 | 𝒩(0 Mpc, (10 Mpc)2) | 20% |
| σ10s10 | 𝒩(0 Mpc, (10 Mpc)2) | 10% |
| s50 | – | 50% |
| s40 | – | 40% |
| s30 | – | 30% |
Notes. The distance uncertainties column shows the Gaussian distribution used to generate uncertainties for distances of photometric galaxies. The last column shows the percentage of the brightest galaxies with spectroscopic distances, i.e., exact distances. Samples that do not have galaxies with photometric distances are indicated with an en dash (–) in the second column.
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