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tokens: from this indicator (Kewley Ellison 2008 ). At the time that Tüllmann et al. derived their metallicities, the tools for assessing which branch to adopt for this double-valued indicator were less robust. Extraplanar H ii regions in the two massive spirals NGC 3628 and NGC 4522 show modest or no abundance offsets relative to their disks. Our results for these galaxies are consistent with the conclusions reached by Stein et al. ( 2017 ). In particular, the nebula at z ≈ 1.4 from the midplane of NGC 4522 is projected onto extraplanar H i identified as matter being stripped from the disk via the ram pressure interaction with the intracluster medium of the Virgo cluster in the maps of Kenney et al. ( 2004 ). Stein et al. ( 2017 ) noted that the extraplanar H ii regions in NGC 3628 are projected onto an H i filament seen in the maps of Wilding et al. ( 1993 ) that has been identified as a tidal feature due to the interaction of this galaxy with its neighbor NGC 3627. Thus, the extraplanar H ii regions may plausibly arise in gas stripped from both of the galaxies, and they represent fundamentally different phenomena than the extraplanar H ii regions in NGC 55 and NGC 4013. The spiral galaxy NGC 4522 resides in the Virgo cluster; direct imaging shows spectacular evidence for ram-pressure-stripping of gas from the disk (Abramson Kenney 2014 ). The extraplanar H ii region measured in this galaxy is associated with this material that seems to clearly have an origin in the disk of that galaxy (Stein et al. 2017 ). We derive a joint abundance offset between the two disk H ii regions observed and the single extraplanar H ii region of = −0.03 ± 0.07 (68% confidence), consistent with no offset. This is as expected for material recently stripped from the disk. In the case of NGC 3628 (part of the Leo Triplet of galaxies), two extraplanar H ii regions are seen at z ≈ 3 kpc in close proximity to one another. Stein et al. note that these H ii regions are likely associated with a filament of H i at similar velocities that likely represents tidal material due to an interaction of NGC 3628 with its neighbor NGC 3627 (Wilding et al. 1993 ). There are hints that the filament may have arisen in the outer parts of NGC 3628 (Stein et al. 2017 ), but they seem inconclusive. Compared with the single disk H ii region measured in that galaxy, we find offsets of = −0.17 ± 0.10 and −0.05 ± 0.11 (68% confidence). If one assumes a single abundance offset is appropriate, the joint distribution implies = −0.12 ± 0.07. There is a hint that the abundances of these H ii regions may have a slightly lower abundance than the disk, but the hint is not robust at the 95% level. While the extraplanar regions tracing stripped material have abundances consistent with the disks of those galaxies, the extraplanar nebulae in the dwarf galaxy NGC 55 have higher abundances than the disk. The extraplanar H ii regions in NGC 55 seem to be connected with supershells produced by vigorous star