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tokens: dipolar signal exists for HD 41641, as the model fits extremely poorly, fitting extremely few of the features visible in the LSD profiles. To ensure that the fitting process had converged properly, it was repeated several times with various first guess parameters, while also rejecting the region of the main spot within the profile when fitting the Stokes I spectra prior to modelling. The results of the modelling are listed as follows. We determined two combinations of inclination and obliquity angles, which effectively corresponds to i = 70° ± 5° and β = 30° ± 5°, and i = 30° ± 5° and β = 70° ± 5°, both with χ 2 = 1.875. The model also suggests a phase shift Δψ = 0.0738 ± 0.005 and, assuming it is a dipole, a maximum polar field strength of B pol = 1880 ± 10 G. The best-fitting model is visible in Fig. 6 . We stress that the dipolar fit to the data is very poor and the above values must therefore be considered with great care and are provided here only to give an idea of the amplitude of the magnetic field signature. This model again shows that a dipolar fit is not appropriate for this star. Figure 6. Results of dipolar modelling performed on the 16 best profiles. Profiles are ordered in phase, increasing vertically first then horizontally. Model fit is displayed as red overlay. Comparing the results determined here for i , β, and B pol with those calculated in Section 3.2 , it is clear there is quite an offset, though this is expected as a result of the poor-fitting dipolar modelling. We do however see a match between the calculated values of β = 79° ± 11° and i = 22° ± 11° and the model with values of β = 70° ± 5° and i = 30° ± 5°. Finally, the error bar of the calculated B pol looks far more reasonable than the range of possible values determined by the dipolar modelling in Section 3.2 , but considering the bad fit we obtain, this error bar is not realistic. 4 CONCLUSIONS We carried out a spectropolarimetric study of the δ Sct star HD 41641, complementing the findings of E16 . We utilized data taken with the NARVAL echelle spectropolarimeter from 2015 October 21 to 2016 December 2. The spectra were used to determine the existence and possible origin of the magnetic field of HD 41641, as well as confirm some of the stellar parameters as determined by E16 . First of all, we confirm that HD 41641 is indeed magnetic, making it the fourth magnetic δ Sct star discovered to date. Through our subsequent analysis, we determined that a different rotation frequency than the one suggested by E16 fit the data more accurately. Switching from a frequency of 0.17756 to 0.3560 d −1 revealed a periodic variation in the magnetic field measurements and in the LSD Stokes I profiles. As a result, some of the other stellar parameters calculated by E16 , such as the inclination i , were no longer suitable and required recalculation. The new value for i was determined to be i = 22° ± 11° and the magnetic obliquity angle β, assuming a dipolar field, was found to be