Table 1.
Satellite slopes (α values) for the different LX thresholds and modeling assumptions in our simulation framework.
| α values (z = 0) |
||||
|---|---|---|---|---|
| log LX limit [erg s−1] | 41 | 42 | 43 | 44 |
| Model 1; ERDF 1 | 0.92 ± 0.01 | 0.92 ± 0.02 | 0.91 ± 0.05 | 0.94 ± 0.19 |
| Model 1; ERDF 2 | 0.83 ± 0.02 | 0.82 ± 0.05 | 0.82 ± 0.10 | 0.88 ± 0.35 |
| Model 2; ERDF 1 | 0.89 ± 0.02 | 0.87 ± 0.02 | 0.81 ± 0.05 | 0.80 ± 0.16 |
| Model 2; ERDF 2 | 0.79 ± 0.02 | 0.77 ± 0.03 | 0.77 ± 0.08 | 0.87 ± 0.17 |
| Model 1; ERDF 1; κ(λEdd) | 0.90 ± 0.01 | 0.90 ± 0.02 | 0.87 ± 0.05 | 1.00 ± 0.27 |
| Model 2; ERDF 1; κ(λEdd) | 0.87 ± 0.01 | 0.86 ± 0.02 | 0.81 ± 0.04 | 0.85 ± 0.16 |
Notes. In addition to the two MBH − MVir models (Model 1 and Model 2), we tested two different Eddington ratio distribution functions; one universal distribution (ERDF 1; Ananna et al. 2022) and one whose normalization is mass-dependent (ERDF 2). Lastly, while a constant X-ray bolometric correction was assumed by default, we also calculated α for each model assuming an Eddington-ratio-dependent BC (κ(λEdd); Vasudevan & Fabian 2007).
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