Table 4.
Flux ratios, SFRs, dust properties, and dust-corrected SFRs for the emission-line regions in DELS J0411–0907 (upper rows) and VDES J0020–3653 (lower rows).
 |
 |
 |
SFR | E(B − V) | AHα | SFRdust corr | ||
|---|---|---|---|---|---|---|---|---|
| (M⊙ yr−1) | (mag) | (mag) | (M⊙ yr−1) | |||||
| DELS J0411–0907 | ||||||||
| N&B quasar subtraction | ||||||||
| Region 1, GN | 2.4±0.2 | 4.5±0.2 | < 0.1 | 27±1 | ||||
| Region 2, GN | 2.1±0.6 | 4.0±0.9 | < 0.5 | < 33±7 | ||||
| Region 2, GB | – | > 2.1 | – | |||||
| Region 3, GN | – | > 6.3 | – | |||||
| Region 3, GB | – | > 2.4 | – | |||||
| BLR quasar subtraction | ||||||||
| Region 1, GN | 2.8±0.2 | 5.0±0.2 | < 0.1 | 29±1 | ||||
| Region 2, GN | 7.1±1.8 | 7.0±1.7 | < 0.2 | < 91±7 | ||||
| Region 2, GB | – | > 7.6 | – | |||||
| Region 3, GN | – | > 6.3 | – | |||||
| Region 3, GB | – | > 2.7 | – | |||||
| VDES J0020–3653 | ||||||||
| N&B quasar subtraction | ||||||||
| Region 1, GN | 3.8±0.5 | 7.7±0.9 | < 0.2 | 24±2 | 0.2±0.1 | 0.8±0.4 | 51 |
|
| Region 2, GN | 7.5±3.9 | 6.2±3.1 | < 0.3 | < 54±9 | ||||
| Region 2, GB | − | > 1.1 | – | |||||
| Region 3, GN | 4.8±0.9 | 3.9±0.7 | < 0.2 | 18±2 | 0.4 ±0.2 | 1.5 |
70 |
|
| Region 4, GN | 4.0±0.5 | 4.4±0.5 | < 0.2 | 17±1 | 0.3 ±0.1 | 1.0 |
42 |
|
| BLR quasar subtraction | ||||||||
| Region 1, GN | 2.9±0.3 | 6.0±0.5 | < 0.2 | 26±2 | 0.0±0.1 | 0.0±0.3 | 27 |
|
| Region 2, GN | 3.9±0.9 | 3.0±0.6 | < 0.3 | < 55±6 | ||||
| Region 2, GB | < 0.9 | 2.7±0.5 | – | |||||
| Region 3, GN | 4.6±0.8 | 3.7±0.6 | < 0.2 | 18±2 | 0.4 ±0.1 | 1.3 |
60 |
|
| Region 4, GN | 4.0±0.5 | 4.4±0.5 | < 0.2 | 17±1 | 0.3 ±0.1 | 1.0 |
42 |
|
Notes. The upper section lists the derived values from the N&B quasar subtraction, and the lower section lists the values from the BLR quasar subtraction. Line ratios are quoted as values if both lines are detected, limits if one line is detected, and not quoted if neither are detected. We note that we constrained F[O III]λ5007/F[O III]λ4959 = 3 in all regions. The uncertainties on SFR consider only the flux measurement uncertainty, and no systematic uncertainty introduced by the conversion Eq. (7). We quote the Region 2 SFR values as upper limits as the AGN photoionisation will contribute, however these are calculated from a measured Hα flux, not a Hα limit, hence the quoted uncertainties on those values.
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