Table 1.
Results of comparing the [O III] emission-line profiles for AGN that we classify as radio compact versus radio extended for various subsets of the sample.
| z | L1.4 GHz | L[O III] | NComp. | NExt. | p-value | p-value | Compact | Extended | Compact more |
|---|---|---|---|---|---|---|---|---|---|
| (log[W Hz−1]) | (log[erg s−1]) | FWHMAvg | FWHMB | %> 1000 km s−1 | %> 1000 km s−1 | extreme outflows? | |||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) |
| 0.02–0.2 | All | All | 1620 | 1302 | 3.9 × 10−14(< 6.6 × 10−9) | 2.7 × 10−12 (< 1.7 × 10−6) | 11 (< 13) | 5.7 (< 8.5) | Y |
| 0.1–0.2 | All | All | 813 | 584 | 2.6 × 10−8 (< 4.1 × 10−4) | 6.4 × 10−5 (< 1.6 × 10−2) | 15 (< 19) | 9.1 (< 13) | Y |
| 0.02–0.2 | 21.5–22.5 | All | 433 | 460 | 2.2 × 10−2 (< 4.1 × 10−1) | 3.2 × 10−3 (< 4.3 × 10−1) | 4.0 (< 7.4) | 2.2 (< 5.9) | ? |
| 0.02–0.2 | 22.5–23.5 | All | 958 | 723 | 8.4 × 10−6 (< 3.5 × 10−3) | 3.8 × 10−6 (< 9.1 × 10−3) | 11 (< 14) | 7.9 (< 11) | Y |
| 0.02–0.2 | 23.5–24.5 | All | 180 | 60 | 4.4 × 10−4 (< 3.0 × 10−2) | 4.4 × 10−3 (< 5.9 × 10−2) | 25 (< 28) | 6.7 (< 14) | Y |
| 0.02–0.2 | All | 39.5–40.5 | 274 | 258 | 6.1 × 10−4 (< 2.0 × 10−1) | 3.4 × 10−1 (< 1.0 × 10−0) | 1.1 (< 4.9) | 0.0 (< 5.4) | ? |
| 0.02–0.2 | All | 40.5–41.5 | 869 | 741 | 4.4 × 10−5 (< 3.0 × 10−2) | 9.6 × 10−6 (< 3.8 × 10−2) | 7.8 (< 11) | 5.1 (< 8.6) | ? |
| 0.02–0.2 | All | 41.5–42.5 | 440 | 264 | 5.2 × 10−6 (< 7.4 × 10−4) | 6.1 × 10−5 (< 1.3 × 10−2) | 22 (< 25) | 13 (< 16) | Y |
Notes. Column definitions are as follows: Columns (1)–(3): ranges of redshift, radio luminosity and [O III] luminosity used in each subset; Cols. (4) and (5): number of AGN in the subset with compact and extended radio emission, respectively; Cols. (6) and (7): p-values from two-sided KS-tests for comparing the distributions of FWHMAvg and FWHMB (see Sect. 4.2), respectively, for the compact versus extended radio sources (p-values < 5 × 10−2 means statistically different distributions); Cols. (8) and (9): the percentage of compact and extended radio sources, respectively, with a broad [O III] emission-line component FWHMB > 1000 km s−1 (see Sect. 4.1) (for Cols. (6)–(9) we list the 99.7th percentile of the corresponding values from a 104 run Monte Carlo simulation in brackets where we randomly perturbed all relevant values by their uncertainties; see Sect. 4.2); Col. (10): based on the 99.7th percentiles: “Y” if it is verified that compact radio sources have a higher prevalence of FWHMB > 1000 km s−1 components, otherwise “?”.
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