We obtained new optical spectra of 13 H ii regions in WLM with EFOSC2 ; oxygen abundances are derived for nine H ii regions .
The temperature-sensitive [ O iii ] \lambda 4363 emission line was measured in two bright H ii regions HM 7 and HM 9 .
The direct oxygen abundances for HM 7 and HM 9 are 12 + log ( O/H ) = 7.72 \pm 0.04 and 7.91 \pm 0.04 , respectively .
We adopt a mean oxygen abundance of 12 + log ( O/H ) = 7.83 \pm 0.06 .
This corresponds to [ O/H ] = -0.83 dex , or 15 % of the solar value .
In H ii regions where [ O iii ] \lambda 4363 was not measured , oxygen abundances derived with bright-line methods are in general agreement with direct values of the oxygen abundance to an accuracy of about 0.2 dex .
In general , the present measurements show that the H ii region oxygen abundances agree with previous values in the literature .
The nebular oxygen abundances are marginally consistent with the mean stellar magnesium abundance ( [ Mg/H ] = -0.62 ) .
However , there is still a 0.62 dex discrepancy in oxygen abundance between the nebular result and the A-type supergiant star WLM 15 ( [ O/H ] = -0.21 ) .
Non-zero reddening values derived from Balmer line ratios were found in H ii regions near a second H i peak .
There may be a connection between the location of the second H i peak , regions of higher extinction , and the position of WLM 15 on the eastern side of the galaxy .