Table E.2
Comparison of the phenomenological and self-consistent model.
| Phenomenological model | Self-consistent model | |||||
|
|
||||||
| Source | θ | a | β | θ | a | β |
| (°) | (°) | |||||
|
|
||||||
| IC4329A | 28 |
≥ 0 | ≤ 1.3 | 34 |
≥ 0 |
|
| MCG-5-23-16 | 21 |
≥ 0 | ≤ 1.6 |
|
≥ 0 |
|
| ESO511-G030 | 18 ± 7 | ≥ 0 | ≤ 1.1 |
|
≥ 0 |
|
| MCG-6-30-15 | 40 |
0.86 |
4.1 ± 0.2 | 39 ± 5 | ≥ 0.8 | 3.4 |
| NGC4051 | 22 ± 6 | ≥ 0.46 | 2.9 |
18 |
≥ 0.3 | 2.5 |
| NGC3516 | 27 |
≥ 0.48 | 2.8 |
|
≥ 0.3 | 2.7 ± 0.4 |
| NGC3783 | ≤ 8 | ≥ 0.16 | 2.7 |
27 |
≥ 0.2 | 3.1 |
| NGC3227 | 23 ± 4 | ≥ 0 | 1.9 |
26 ± 9 | ≥ 0 | 2.3 |
| MRK509 | 53 ± 1 |
|
≥ 3.8 | ≥ 45 | ≥ 0.4 | 2.8 |
| MRK766 | 20 |
≥ 0.47 | 2.7 |
28 ± 8 | ≥ 0.3 | 2.6 |
| ARK120 | ≥ 59 | ≥ 0 | 2.2 |
48 ± 12 | ≥ 0.1 | 2.7 |
Notes. This table shows a comparison of the best-fitting relativistic parameters (only disc parameters are shown) obtained by applying the phenomenological model discussed throughout the paper (whose full results are given in Table 2) and the more self-consistent one discussed in Appendix E. Here, only sources for which a detection of a relativistic line component is claimed in the paper are shown.
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