 | An example solution (MJD 56244) used to calibrate the data. Panel (a) shows the degree of cross-coupling between receivers, (b) shows the ellipticity of the receivers (the two colors show the two polarizations; $\theta_{1}$ is assumed to be zero so black is not shown in the above panel.), (c) shows the differential phase, (d) shows the differential gain, and (e) shows the absolute gain of the receiver (specified in units of the square root of the reference flux density). (See \citealt{solution} for more details of this procedure). |
 | Magnetic field values derived from pulsar rotation measures superposed on an Aitoff plot of the Galaxy. The color bar at the bottom shows the value of $\langle B_{\parallel} \rangle$ in unit of $\mu$G. Results from this work are combined with those of \citet{Gentile2018} to get a complete picture of the values around the sky. Note: the plot of \citet{Gentile2018} is incorrect in terms of the sign of the Galactic longitude of the pulsars (which is corrected here). |
 | Pulse profile for pulsars J0340+4130 and J0613--0200. The black line is the total intensity, red is the circular polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Pulse profile for pulsars J0340+4130 and J0613--0200. The black line is the total intensity, red is the circular polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Pulse profile for pulsars J0340+4130 and J0613--0200. The black line is the total intensity, red is the circular polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Pulse profile for pulsars J0340+4130 and J0613--0200. The black line is the total intensity, red is the circular polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | The pulse profile for pulsars J0636+5128 and J0645+5158. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | The pulse profile for pulsars J0636+5128 and J0645+5158. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | The pulse profile for pulsars J0636+5128 and J0645+5158. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | The pulse profile for pulsars J0636+5128 and J0645+5158. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J0740+6620 and J0931--1902. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J0740+6620 and J0931--1902. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J0740+6620 and J0931--1902. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J0740+6620 and J0931--1902. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1012+5307 and J1024--0719 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent in J1024--0719. The polarization position angle is shown in the top panel. The microcomponent plots for J1024--0719 have been plotted with fewer bins to increase the signal-to-noise. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1012+5307 and J1024--0719 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent in J1024--0719. The polarization position angle is shown in the top panel. The microcomponent plots for J1024--0719 have been plotted with fewer bins to increase the signal-to-noise. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1012+5307 and J1024--0719 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent in J1024--0719. The polarization position angle is shown in the top panel. The microcomponent plots for J1024--0719 have been plotted with fewer bins to increase the signal-to-noise. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1012+5307 and J1024--0719 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent in J1024--0719. The polarization position angle is shown in the top panel. The microcomponent plots for J1024--0719 have been plotted with fewer bins to increase the signal-to-noise. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1012+5307 and J1024--0719 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent in J1024--0719. The polarization position angle is shown in the top panel. The microcomponent plots for J1024--0719 have been plotted with fewer bins to increase the signal-to-noise. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1012+5307 and J1024--0719 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent in J1024--0719. The polarization position angle is shown in the top panel. The microcomponent plots for J1024--0719 have been plotted with fewer bins to increase the signal-to-noise. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1125+7819 and J1455--3330 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent of J1455--3330. The microcomponent plots for J1455--3330 have been plotted with fewer bins increase the signal-to-noise. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1125+7819 and J1455--3330 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent of J1455--3330. The microcomponent plots for J1455--3330 have been plotted with fewer bins increase the signal-to-noise. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1125+7819 and J1455--3330 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent of J1455--3330. The microcomponent plots for J1455--3330 have been plotted with fewer bins increase the signal-to-noise. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1125+7819 and J1455--3330 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent of J1455--3330. The microcomponent plots for J1455--3330 have been plotted with fewer bins increase the signal-to-noise. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1125+7819 and J1455--3330 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent of J1455--3330. The microcomponent plots for J1455--3330 have been plotted with fewer bins increase the signal-to-noise. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1125+7819 and J1455--3330 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent of J1455--3330. The microcomponent plots for J1455--3330 have been plotted with fewer bins increase the signal-to-noise. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1600--3053 and J1614--3053 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent of J1600--3053. The microcomponent plots for J1455--3330 have been plotted with fewer bins increase the signal-to-noise. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1600--3053 and J1614--3053 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent of J1600--3053. The microcomponent plots for J1455--3330 have been plotted with fewer bins increase the signal-to-noise. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1600--3053 and J1614--3053 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent of J1600--3053. The microcomponent plots for J1455--3330 have been plotted with fewer bins increase the signal-to-noise. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1600--3053 and J1614--3053 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent of J1600--3053. The microcomponent plots for J1455--3330 have been plotted with fewer bins increase the signal-to-noise. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1600--3053 and J1614--3053 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent of J1600--3053. The microcomponent plots for J1455--3330 have been plotted with fewer bins increase the signal-to-noise. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1600--3053 and J1614--3053 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent of J1600--3053. The microcomponent plots for J1455--3330 have been plotted with fewer bins increase the signal-to-noise. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1643--1224 and J1713+0747 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent in each J1713+0747 profile. The microcomponent plot for J1713--0747 have been plotted with fewer bins to increase the signal-to-noise. The polarization position angle is shown in the top panel. Note: there is no detection of the microcomponent of J1713+0747 at 820\,MHz, the plot is just shown for comparison. |
 | Pulse profiles for pulsars J1643--1224 and J1713+0747 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent in each J1713+0747 profile. The microcomponent plot for J1713--0747 have been plotted with fewer bins to increase the signal-to-noise. The polarization position angle is shown in the top panel. Note: there is no detection of the microcomponent of J1713+0747 at 820\,MHz, the plot is just shown for comparison. |
 | Pulse profiles for pulsars J1643--1224 and J1713+0747 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent in each J1713+0747 profile. The microcomponent plot for J1713--0747 have been plotted with fewer bins to increase the signal-to-noise. The polarization position angle is shown in the top panel. Note: there is no detection of the microcomponent of J1713+0747 at 820\,MHz, the plot is just shown for comparison. |
 | Pulse profiles for pulsars J1643--1224 and J1713+0747 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent in each J1713+0747 profile. The microcomponent plot for J1713--0747 have been plotted with fewer bins to increase the signal-to-noise. The polarization position angle is shown in the top panel. Note: there is no detection of the microcomponent of J1713+0747 at 820\,MHz, the plot is just shown for comparison. |
 | Pulse profiles for pulsars J1643--1224 and J1713+0747 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent in each J1713+0747 profile. The microcomponent plot for J1713--0747 have been plotted with fewer bins to increase the signal-to-noise. The polarization position angle is shown in the top panel. Note: there is no detection of the microcomponent of J1713+0747 at 820\,MHz, the plot is just shown for comparison. |
 | Pulse profiles for pulsars J1643--1224 and J1713+0747 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent in each J1713+0747 profile. The microcomponent plot for J1713--0747 have been plotted with fewer bins to increase the signal-to-noise. The polarization position angle is shown in the top panel. Note: there is no detection of the microcomponent of J1713+0747 at 820\,MHz, the plot is just shown for comparison. |
 | Pulse profiles for pulsars J1744--1134 and J1747--4036. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1744--1134 and J1747--4036. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1744--1134 and J1747--4036. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1744--1134 and J1747--4036. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1832--0836 and J1909--3744 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent in each J1909--3744 profile. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1832--0836 and J1909--3744 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent in each J1909--3744 profile. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1832--0836 and J1909--3744 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent in each J1909--3744 profile. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1832--0836 and J1909--3744 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent in each J1909--3744 profile. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1832--0836 and J1909--3744 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent in each J1909--3744 profile. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J1832--0836 and J1909--3744 including microcomponents. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The black arrow points to the location of the microcomponent in each J1909--3744 profile. The polarization position angle is shown in the top panel. |
 | Pulse profile for pulsars J1918--0642 and B1937+21 including microcomponents. The black arrow points to the location of the microcomponent in each B1937+21 profile. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Pulse profile for pulsars J1918--0642 and B1937+21 including microcomponents. The black arrow points to the location of the microcomponent in each B1937+21 profile. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Pulse profile for pulsars J1918--0642 and B1937+21 including microcomponents. The black arrow points to the location of the microcomponent in each B1937+21 profile. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Pulse profile for pulsars J1918--0642 and B1937+21 including microcomponents. The black arrow points to the location of the microcomponent in each B1937+21 profile. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Pulse profile for pulsars J1918--0642 and B1937+21 including microcomponents. The black arrow points to the location of the microcomponent in each B1937+21 profile. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Pulse profile for pulsars J1918--0642 and B1937+21 including microcomponents. The black arrow points to the location of the microcomponent in each B1937+21 profile. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J2010--1323 and J2145--0750 including microcomponents. The black arrow points to the location of the microcomponent in each J2145--0750 profile. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J2010--1323 and J2145--0750 including microcomponents. The black arrow points to the location of the microcomponent in each J2145--0750 profile. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J2010--1323 and J2145--0750 including microcomponents. The black arrow points to the location of the microcomponent in each J2145--0750 profile. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J2010--1323 and J2145--0750 including microcomponents. The black arrow points to the location of the microcomponent in each J2145--0750 profile. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J2010--1323 and J2145--0750 including microcomponents. The black arrow points to the location of the microcomponent in each J2145--0750 profile. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J2010--1323 and J2145--0750 including microcomponents. The black arrow points to the location of the microcomponent in each J2145--0750 profile. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J2302+4442. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Pulse profiles for pulsars J2302+4442. The black line is the total intensity, red is the linear polarization, and blue is the circular polarization. The polarization position angle is shown in the top panel. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J0340+4130 and J0613--0200. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value are those reported by TEMPO, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J0340+4130 and J0613--0200. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value are those reported by TEMPO, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J0340+4130 and J0613--0200. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value are those reported by TEMPO, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J0340+4130 and J0613--0200. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value are those reported by TEMPO, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field variations over time for pulsars J0645+5158 and J1012+5307. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field variations over time for pulsars J0645+5158 and J1012+5307. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field variations over time for pulsars J0645+5158 and J1012+5307. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field variations over time for pulsars J0645+5158 and J1012+5307. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J1024--0719 and J1455--3330. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J1024--0719 and J1455--3330. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J1024--0719 and J1455--3330. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J1024--0719 and J1455--3330. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J1600--3053 and J1614--2230. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. Note: the plots for J1614--2203 contain two outliers at epochs of small ecliptic angle (less than 3 degrees) (MJDs 55892 and 55893, as discussed in Section \ref{5.1.3}). These points are excluded from the fitting and the mean RM and B calculation but included in the plot to show the spike in RM, DM, and B-field when the pulsar is close to the Sun. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J1600--3053 and J1614--2230. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. Note: the plots for J1614--2203 contain two outliers at epochs of small ecliptic angle (less than 3 degrees) (MJDs 55892 and 55893, as discussed in Section \ref{5.1.3}). These points are excluded from the fitting and the mean RM and B calculation but included in the plot to show the spike in RM, DM, and B-field when the pulsar is close to the Sun. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J1600--3053 and J1614--2230. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. Note: the plots for J1614--2203 contain two outliers at epochs of small ecliptic angle (less than 3 degrees) (MJDs 55892 and 55893, as discussed in Section \ref{5.1.3}). These points are excluded from the fitting and the mean RM and B calculation but included in the plot to show the spike in RM, DM, and B-field when the pulsar is close to the Sun. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J1600--3053 and J1614--2230. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. Note: the plots for J1614--2203 contain two outliers at epochs of small ecliptic angle (less than 3 degrees) (MJDs 55892 and 55893, as discussed in Section \ref{5.1.3}). These points are excluded from the fitting and the mean RM and B calculation but included in the plot to show the spike in RM, DM, and B-field when the pulsar is close to the Sun. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J1643--1224 and J1713+0747. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J1643--1224 and J1713+0747. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J1643--1224 and J1713+0747. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J1643--1224 and J1713+0747. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J1744--1134 and J1747--4036. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J1744--1134 and J1747--4036. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J1744--1134 and J1747--4036. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J1744--1134 and J1747--4036. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J1909--3744 and J1918--0642. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J1909--3744 and J1918--0642. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J1909--3744 and J1918--0642. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J1909--3744 and J1918--0642. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars B1937+21 and J2010$-$1323. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars B1937+21 and J2010$-$1323. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars B1937+21 and J2010$-$1323. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars B1937+21 and J2010$-$1323. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J2145--0750 and J2302+4442. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J2145--0750 and J2302+4442. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J2145--0750 and J2302+4442. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |
 | Ionosphere-corrected rotation measure, dispersion measure, and magnetic field changes over time for pulsars J2145--0750 and J2302+4442. The error bars on the RM are a combination of fitting for Faraday rotation and from the ionospheric correction, errors on the DM come from those on the DMX value, and errors on the magnetic field are a combination of the two. The trendline shown is that with the lowest reduced $\chi^2_{r}$ value of all of the trends. No trend is shown if the lowest $\chi^2_{r}$ value for the fits was that of a horizontal line with a slope of zero. |