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tokens: trials. There are nine pulsars in our sample that have had RMs measured for the first time. These are listed in Table 3 . PSR J1643−4505, once the high RM is taken into account, joins the ranks of pulsars with high and very high linear polarization fraction. In contrast, the linear polarization fraction for the high pulsar PSR J1055−6028 remains low even after the RM correction. We note the extremely high value of RM uncovered for PSR J1114−6100, described in more detail in the subsection below. We have found a substantial number of pulsars for which our value of RM is more than 10 rad m −2 away from the published values as given in v1.63 of the ATNF pulsar catalogue (Manchester et al. 2005 ). 1 These pulsars are listed in Table 4 . The published value of PSR J1413−6141 was seriously in error, applying the correct value reveals that this pulsar has only a moderate linear polarization fraction. For PSR J0857−4424, the published value from 20 yr ago of −75 rad m −2 is erroneous; we measure +162 rad m −2 , a difference of more than 200 units. Table 3. Pulsars without previous RM measurements. The uncertainty is given in brackets and refers to the last digit. Table 4. Pulsars with derived RMs that differ by more than 10 rad m −2 from the published values, RM cat . The uncertainties, σ and σ cat , are also listed. Note . References: (1) Crawford, Manchester Kaspi ( 2001 ), (2) Hamilton Lyne ( 1987 ), (3) Han et al. ( 2006 ), (4) Han et al. ( 2018 ), (5) Han, Manchester Qiao ( 1999 ), (6) Johnston Weisberg ( 2006 ), (7) Johnston et al. ( 2007 ), (8) Noutsos et al. ( 2008 ), (9) O’Brien et al. ( 2008 ), (10) Rand Lyne ( 1994 ), (11) Taylor, Manchester Lyne ( 1993 ), (12) Weltevrede Johnston ( 2008 ). We observe that there are sometimes significant differences between the RMs returned by the two methods as can be seen in Fig. 7 . Karastergiou ( 2009 ) pointed out that the effects of interstellar scattering can lead to erroneous measurements of RM, and that the method of Noutsos et al. ( 2008 ) was best to use in the case of scattered profiles. In addition, Ilie et al. ( 2019 ) showed the presence of (apparent) RM variations across the pulse profile that meant that different RMs can be obtained depending on the method used. The most extreme example of this is PSR J1600−5044 for which we obtain an RM of 90 and 135 rad m −2 using the two methods. At low frequencies, the pulsar is heavily scattered, at high frequencies the position angle of the linear polarization has a very steep swing across the pulse profile. This is the scenario pointed out by Karastergiou ( 2009 ) as being the most detrimental to measuring correct values of RM. 6.1 PSR J1114−6100 We measured a value of −6729 ± 2 rad m −2 for the RM of PSR J1114−6100. This is the fourth highest value of |RM| for any known pulsar, beaten only by the Galactic centre magnetar PSR J1745−2900 (Shannon Johnston 2013 ), and two other pulsars near the Galactic centre, PSRs J1746−2849 and J1746−2856