Table 3.
Parameter space ranges and marginalized posterior estimates of the free parameters used in our model, for both the red and blue sample.
| Parameter | Priors | Red | Blue |
|---|---|---|---|
| fc | [0, 1] |
 |
– |
| log(M0/[h−2 M⊙]) | [7, 13] |
 |
 |
| log(M1/[h−2 M⊙]) | [9, 14] |
 |
 |
| γ1 | 𝒩(3, 3) |
 |
 |
| γ2 | [0, 10] |
 |
 |
| σc | [0.05, 2.5] |
 |
 |
| b | [0.2, 5] |
 |
 |
| fs | [0, 1] |
 |
– |
| αs | 𝒩(−1.1, 0.9) |
 |
 |
| b1 | 𝒩(0.0, 1.5) |
 |
 |
| b2 | 𝒩(1.5, 1.5) |
 |
 |
Notes. M0 is the normalization of the stellar-to-halo mass relation (SHMR); M1 is the characteristic mass scale of the same SHMR; fc is the normalization of the concentration-mass relation; σc is the scatter between the stellar and halo mass; γ1 and γ2 are the low and high-mass slopes of the SHMR; fs is the normalization of the concentration-mass relation for satellite galaxies; and αs, b0, and b1 govern the behavior of the satellite galaxies. As the parameters fc and fs of the blue sample are not constrained and they recover the prior ranges, we do not provide their values. As discussed in the text, the parameters that describe the CSMF are biased as a result of the cut in apparent magnitude that defines the KiDS-Bright sample.
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