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tokens: were measured with an accuracy of (Table 4 ). Moreover, we were unable to measure [O iii ]λ4959 and [O iii ]λ5007 lines for these objects. These two regions were also excluded from further analysis. 3.2 Oxygen and nitrogen abundances We are unable to use the direct T e -method to estimate the oxygen and nitrogen abundances, since auroral lines in spectra of H ii regions from our sample, such as [O iii ]λ4363 or [N ii ]λ5755, are too faint to be detected. Thus, we need to use empirical calibrations. Such methods are well developed (Kobulnicky Kewley 2004 ; Pettini Pagel 2004 ; Pilyugin Thuan 2005 ; Bresolin 2007 ; Pilyugin et al. 2010 ; Pilyugin Mattsson 2011 ; Marino et al. 2013 ; Pilyugin Grebel 2016 ). The most modern two-dimensional R and S-calibrations (Pilyugin Grebel 2016 ) are the simplest and the most popular now. The R-calibration, based on the [O ii ] and [N ii ] strong emission lines, is more resistant to the presence of diffuse ionized gas (see e.g. Sanders et al. 2017 ; Kumari et al. 2019 ; Poetrodjojo et al. 2019 ), but it is sensitive to extinction errors. The S-method, based on the [N ii ] and [S ii ] lines, does not depend strongly on extinction, but it cannot be used for the nitrogen abundance estimates (Pilyugin Grebel 2016 ). Among the other methods we distinguish the NS-calibration (Pilyugin Mattsson 2011 ), which is based on the [O iii ], [N ii ], and [S ii ] emission-line intensities (see discussion in Gusev et al. 2012 , 2014 ). All the empirical calibrations are constructed under some assumptions. One of them is that the H ii regions are in the low-density regime (Pilyugin Mattsson 2011 ; Pilyugin Grebel 2016 ), which is typical for the majority of extragalactic H ii regions (Zaritsky et al. 1994 ; Bresolin et al. 2005 ; Gutiérrez Beckman 2010 ). The dependence n e versus [S ii ]λ6717/[S ii ]λ6731 degenerates at low n e (Proxauf et al. 2014 ), thus we give upper limits of n e in Table 3 for most H ii regions. Large upper limits of n e for H ii region nos. 12, 15, and 16 in NGC 3963 are rather a result of large line flux errors. However, one H ii region of our sample, no. 6 in NGC 3963, is an apparently high-density object (see Table 3 ). The empirical calibrations are not applicable to such regions. As a result, this region was eliminated from further consideration. We calculated the oxygen and nitrogen abundances in H ii regions using three different calibrations discussed above. Data of emission lines fluxes from Table 4 were used. For several regions, where the [O iii ]λ4959 or [N ii ]λ6548 lines fluxes have not been measured, we adopt I ([O iii ]λ4959+[O iii ]λ5007) = 1.33 I ([O iii ]λ5007) and I ([N ii ]λ6548+[N ii ]λ6584) = 1.33 I ([N ii ]λ6584) according to results of Storey Zeippen ( 2000 ). The resultant oxygen abundances from the R, NS, and S-calibrations abundances, and nitrogen abundances from the R and NS-calibrations, and NS-calibration electron temperatures are given in Table 5 . Table 5. Oxygen and