New CCD spectrophotometry and circular spectropolarimetry data are presented for white dwarfs PG 1658+441 and PG 0136+251. The data confirm a magnetic field of mean surface strength Bs = 2.3 +/-0.2 MG for the former star but provide only marginal evidence for a much weaker longitudinal component of Be = -75 +/-35 kG (1 sigma) for the latter object. By adopting straightforward approximations for the magnetic object, the lines are successfully fitted with synthetic spectra from stellar atmosphere models, allowing the T(eff) and surface gravity of each star to be determined. It is found that the enhanced Balmer lines of both stars can be attributed to unusually large surface gravities and therefore high mass (greater than 1.2 solar mass). The implications of the results are discussed.
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Schmidt et al. (1992) studied this question.