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tokens: of ε Cet are mostly not able to be individually separated, and the use of assumptions are required to untangle them (Docobo Andrade 2013 ). The angular separation of the components was 0.1 arcsec in 2015 (Mason et al. 2001 ). We obtained sixteen polarized spectra for ε Cet over a 6.0 h interval on 2016 September 21, corresponding to 2.5 per cent of the estimated rotational period of 10.2 d. The mean LSD profile (Fig. B4 ) combined 6693 lines, and a magnetic detection was obtained from the mean LSD Stokes V profile. We are unable to determine whether the magnetic detection was on the F5V or F6V components because the two stars could not be separated spectroscopically. We estimated B l at +0.6 ± 0.1 G. Our radial velocity determination +15.81 ± 0.26 km s −1 (Table 5 ) is similar to the value of +15.49 ± 0.19 km s −1 in Anderson Francis ( 2012 ), and our S-index 0.186 ± 0.003 (Table 5 ) was less than 0.219 in Pace ( 2013 ). A4 α Com α Com (HIP 64241) is a triple star consisting of a double-lined spectroscopic binary (Duquennoy, Mayor Halbwachs 1991 ) of F5V and F6V components (Edwards 1976 ; Soubiran et al. 2018 ), and a V magnitude 10.2 component with an angular separation of 85 arcsec in 2014 based on data from the continuously updated Washington Double Star Catalogue (WDS) (Mason et al. 2001 ). The system was first observed by Struve ( 1875 ) who reported that occultations were observed (Muterspaugh et al. 2015 ). Roman ( 1950 ) describes α Com as a close visual binary, with equal F5 components, and showing weak lines. Hartkopf et al. ( 1989 ) describes α Com as a ‘lovely edge-on system’ with an orbital inclination close to 90 deg, and suggested a partial eclipse was possibly missed in early 1990. The eclipsing binary has the third longest period known ( P = 25.85 yr) (Lipunov et al. 2016 ), with only eight eclipsing stars having periods longer than 10 yr. We obtained twenty-seven polarized spectra for α Com over a 3.8 h interval on 2017 February 16, corresponding to 5.3 per cent of the estimated rotational period of 3.0 d. The mean LSD profile (Fig. B5 ) combined 7628 lines, and a magnetic detection is visible in the Stokes V profile. We are unable to determine whether the magnetic detection was on the F5V or F6V components because the two stars could not be separated spectroscopically. We estimated B l at +3.1 ± 0.3 G. Our radial velocity determination −18.02 ± 0.27 km s −1 (Table 5 ) is larger the value of −16.05 ± 0.21 km s −1 in Anderson Francis ( 2012 ), and our S-index 0.272 ± 0.008 (Table 5 ) is smaller than the 0.308 in Pace ( 2013 ). A5 ω Dra ω Dra (HIP 86201) is a triple star system consisting of double-lined spectroscopic binary (Abt Levy 1976 ; Konacki et al. 2010 ), and a V magnitude 13.2 common proper motion companion with an angular separation of 70 arcsec (Abt Levy 1976 ; Fekel, Tomkin Williamson 2009 ). The mases of the primary component are 1.46 M ⊙ and secondary 1.18 M ⊙ (Konacki et al. 2010 ), which corresponds to