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Recent spectropolarimetric studies of 7 SPB and $\beta$ Cep stars havesuggested that photospheric magnetic fields are more common in B-type pulsatorsthan in the general population of B stars, suggesting a significant connectionbetween magnetic and pulsational phenomena. We present an analysis of new andpreviously published spectropolarimetric observations of these stars. NewStokes $V$ observations obtained with the high-resolution ESPaDOnS and Narvalinstruments confirm the presence of a magnetic field in one of the stars($\epsilon$ Lup), but find no evidence of magnetism in 5 others. A re-analysisof the published longitudinal field measurements obtained with thelow-resolution FORS1/2 spectropolarimeters finds that the measurements of allstars show more scatter from zero than can be attributed to Gaussian noise,suggesting the presence of a signal and/or systematic under-estimation of errorbars. Re-reduction and re-measurement of the FORS1/2 spectra from the ESOarchive demonstrates that small changes in reduction procedure lead tosubstantial changes in the inferred longitudinal field, and substantiallyreduces the number of field detections at the 3$\sigma$ level. Furthermore, wefind that the published periods are not unique solutions to the time series ofeither the original or the revised FORS1/2 data. We conclude that the reportedfield detections, proposed periods and field geometry models for $\alpha$ Pyx,15 CMa, 33 Eri and V1449 Aql are artefacts of the data analysis and reductionprocedures, and that magnetic fields at the reported strength are no morecommon in SPB/$\beta$ Cep stars than in the general population of B stars.

astrophysical journal/the astrophysical journal

Critical evaluation of magnetic field detections reported for pulsating  B-type stars in the light of ESPaDOnS, Narval and reanalyzed FORS1/2  observations