Table 1.
Models considered when studying properties of cLRDs.
| Property | |||
|---|---|---|---|
| Column density | max: integrates the column | outmax80: when radiation | |
| density from the position of | pressure on dusty gas | ||
| the MBH to the host galaxy | dominates excludes from the | ||
| virial radius | integration the inner 80 pc | ||
| around the MBH | |||
| MBHs | distr: MBH masses are extracted | distr overm: MBH masses | distr sEdd: Eddington ratios |
| from the MBH-Mstar | are extracted from the MBH- | are extracted in log space | |
| relation from G20 while Eddington | Mstar relation from P24 while | from a normal distribution | |
| ratios are extracted in log | Eddington ratios are extracted | centered in log(0.5) with | |
| space from a normal distribution | in log space from a normal | standard deviation 0.5 dex | |
| centered in log(0.25) with standard | distribution centered in with | ||
| deviation 0.5 dex | log(0.25) standard deviation 0.5 dex | ||
| dust | MW-like: a mass fraction | SMC-like: 100% silicates | |
| of 54% in silicates and 46% | with MRN size distribution | ||
| in carbonaceous grains with | |||
| MRN size distribution cut | |||
| out at 0.25 μm) | |||
Notes. “max” integrates the column density from the position of the MBH to the host galaxy virial radius; “outmax80” integrates the column density from outside an 80-pc sphere around the MBH to the host galaxy virial radius to mimic the effect of radiation pressure on dust.
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