Table 4
Derived properties of the WR population and WR number ratios.
| Galaxy | Region | Hβ (clump) | c (Hβ) | Blue WR bump | Red WR bump | EW (Hβ ) | τ | η 0 | N 0 | NWR/N0 |
|
|
| ID | (× 10-14 cgs) | EW (Å) | EW (Å) | (Å) | (Myr) | log (cgs) | log (cgs) | |||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) | (13) |
|
|
||||||||||||
| IC 0225 | R1 | 3.23 ± 0.07 | 0.06 | 1.4 ± 0.8 | − | 31  |
5.5 ± 0.3 | 0.30 ±0.05 | 551  |
0.14  |
51.56 | 51.31 ± 0.16 |
| NGC 3353 | R1 | 81.51 ± 0.54 | 0.19 | 3.8 ± 0.4 | 0.9 ± 0.2 | 90  |
4.5 ± 0.3 | 0.25  |
4919  |
0.17  |
52.52 | 52.32 ± 0.11 |
| NGC 3381 | R1 | 6.61 ± 0.12 | 0.15 | 4.5 ± 0.8 | − | 45  |
4.3 ± 0.2 | 0.35  |
<172 | >1.75 | 51.92 | >51.89 |
| NGC 3773 | R1 | 22.07 ± 0.31 | 0.07 | 3.5 ± 1.1 | 4.5 ± 1.6 | 46  |
5.2 ± 0.2 | 0.25 ±0.05 | <1139 | >0.19 | 51.95 | >51.91 |
| NGC 4630 | R1 | 11.01 ± 0.14 | 0.28 | 3.0 ± 0.7 | − | 49  |
4.3 ± 0.5 | 0.35  |
252  |
0.24  |
51.38 | 51.19 ± 0.04 |
| NGC 5954 | R2 | 12.03 ± 0.20 | 0.42 | 0.9 ± 0.2 | − | 41  |
5.5 ± 0.3 | 0.30 ±0.05 | 5123  |
0.04  |
52.32 | 51.77 ± 0.06 |
| UGC 6320 | R1 | 13.90 ± 0.12 | 0.13 | 4.5 ± 0.6 | 1.1 ± 0.2 | 74  |
4.8 ± 0.2 | 0.22 ±0.05 | 744  |
0.31  |
51.88 | 51.78 ± 0.08 |
| R2 | 6.64 ± 0.07 | 0.09 | 1.9 ± 0.5 | − | 79  |
4.8 ± 0.2 | 0.22  |
1124  |
0.04 |
51.56 | 51.04 ± 0.05 | |
Notes. Column (1): name of the galaxy. Column (2): region identification number. Column (3): the extinction corrected Hβ line intensity of the corresponding Hα clump. Column (4): extinction coefficient. Column (5): equivalent width of the He iiλ4686 line measured in the WR region, corrected by the continuum emission of non-ionizing populations. Column (6): same as (5) but for the broad C ivλ5808 line. Column (7): equivalent width of Hβ measured in the Hα clump and corrected by the continuum emission of non-ionizing populations. Column (8): derived age of the ionizing population using the EWs reported in (7) and the POPSTAR models. Column (9): adopted η0 parameter. Column (10): derived number O stars. Column (11): number ratio of WR stars with respect to the total numbers of O stars. Column (12): total Lyman continuum flux, as derived with the Hα luminosity (the random uncertainty is in all cases below 2%). Column (13): estimated Lyman continuum flux emerging from WR stars.
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