Table 5.
Average offsets and standard deviation obtained for each galaxy subsample of size N where the chemical abundances could be compared (ΔO/H) between the various optical-based determinations and the HCM-IR estimates.
| ΔO/H | HCm | DM | PG16-R | PG-16-S | ||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| Input lines in HCM-IR | Mean | σ | N | Mean | σ | N | Mean | σ | N | Mean | σ | N |
| All lines | +0.02 | 0.10 | 5 | +0.02 | – | 2 | +0.05 | 0.14 | 4 | +0.09 | 0.11 | 5 |
| [Ne II]12.8, [Ne III]15.6, [S III]18.7, 33.5, [S IV]10.5, [O III]52, 88, [N II]122, [N III]57 | +0.06 | 0.14 | 6 | +0.01 | 0.10 | 6 | +0.07 | 0.13 | 5 | +0.10 | 0.10 | 6 |
| [O III]52, 88, [N II]122, [N III]57 | −0.07 | 0.19 | 12 | +0.05 | 0.17 | 7 | +0.11 | 0.13 | 7 | +0.12 | 0.09 | 12 |
| H I, [S III]18.7, 33.5, [S IV]10.5, [Ne II]12.8, [Ne III]15.6 | +0.02 | 0.15 | 21 | +0.08 | 0.14 | 11 | 0.00 | 0.17 | 18 | 0.00 | 0.17 | 20 |
| [S III]18.7, 33.5, [S IV]10.5, [Ne II]12.8, [Ne III]15.6 | +0.02 | 0.21 | 32 | +0.03 | 0.24 | 22 | −0.02 | 0.21 | 26 | −0.03 | 0.23 | 30 |
| [S III]18.7, 33.5, [S IV]10.5 | +0.09 | 0.24 | 37 | +0.11 | 0.27 | 27 | −0.02 | 0.21 | 30 | −0.03 | 0.22 | 34 |
| [Ne II]12.8, [Ne III]15.6 | −0.17 | 0.18 | 43 | −0.18 | 0.25 | 22 | −0.04 | 0.23 | 31 | −0.04 | 0.23 | 40 |
| [N II]122, [N III]57 | −0.17 | 0.12 | 12 | −40.14 | – | 2 | +0.11 | 0.13 | 7 | +0.12 | 0.09 | 12 |
Notes. The optical methods used are HCM from Pérez-Montero (2014), the direct method (DM) values provided by Madden et al. (2013), and the strong-line calibrations from Pilyugin & Grebel (2016), namely the R and S calibrations. The differences reported for the DM are estimated using only the sample of dwarf galaxies, where DM abundances are available (Madden et al. 2013).
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