Table C.1.
Comparison of total counts (fractions) of excitation types.
| WHAN diagnostic | mIRdds | |
|---|---|---|
| diagram | mIRdds | (W3−W4 = 1.6×(W2−W3)−2.6, |
| (1) | (this work) | W2−W3 > 1.5) |
| HRS (285 objects) | ||
| sAGN 24 (0.08) | Sy2 29 (0.10) | Sy2 10 (0.04) |
| wAGN 63 (0.22) | LINER 60 (0.21) | LINER 62 (0.22) |
| H II 170 (0.60) | SFG 115 (0.40) | SFG 177 (0.62) |
| RET 28 (0.10) | Retired 81 (0.28) | Retired 36 (0.13) |
| RPS sample (67 objects) | ||
| sAGN 1 (0.01) | Sy2 8 (0.12) | Sy2 4 (0.06) |
| wAGN 8 (0.12) | LINER 13 (0.19) | LINER 12 (0.18) |
| H II 55 (0.82) | SFG 37 (0.55) | SFG 50 (0.75) |
| RET 3 (0.04) | Retired 9 (0.13) | Retired 1 (0.01) |
Notes. The total counts (fractions) of excitation types are derived from the WHAN diagnostic diagram (1) and from the mid-infrared diagnostics (mIRdds using mid-colour indices) throughout this work (first and second columns, respectively). The third column lists adjusted mIRdd counts (fractions) designed to more closely match the WHAN classifications. These adjustments involve modifying the intercept in the (2) AGN/SFG separation criterion (from −3.2 to −2.6), and adopting the star-forming threshold of (3) (W2−W3 > 1.5) instead of that from (4).
Reference. (1) Gavazzi et al. (2018); (2) Coziol et al. (2015); (3) Cluver et al. (2014); (4) Herpich et al. (2016).
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