# The Thousand-Pulsar-Array programme on MeerKAT XIV: On the high linearly
polarized pulsar signals

Simon Johnston1, Dipanjan Mitra2,3, Michael J. Keith4, Lucy S. Oswald5,6, Aris
Karastergiou5
1Australia Telescope National Facility, CSIRO Space and Astronomy, PO Box 76,
Epping NSW 1710, Australia
$2$National Centre for Radio Astrophysics, Tata Institute for Fundamental
Research, Post Bag 3, Ganeshkhind, Pune 411007, India
$3$Janusz Gil Institute of Astronomy, University of Zielona Góra, ul. Szafrana
2, 65-516 Zielona Góra, Poland
4Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy,
University of Manchester, Manchester M13 9PL, UK
5Department of Astrophysics, University of Oxford, Denys Wilkinson Building,
Keble Road, Oxford OX1 3RH, UK
6Magdalen College, University of Oxford, Oxford OX1 4AU, UK
<EMAIL_ADDRESS>
(Accepted XXX. Received YYY; in original form ZZZ)

###### Abstract

The S-shaped swing of the linear polarization position angle (PPA) observed in
many pulsars can be interpreted by the rotating vector model (RVM). However,
efforts to fit the RVM for a large sample of pulsars observed with the MeerKAT
telescope as a part of the Thousand-Pulsar-Array (TPA) programme, only
succeeded for about half the cases. High time-resolution studies suggest that
the failed cases arise due to the presence of orthogonal polarization modes,
or highly disordered distribution of PPA points. One such example is PSR
J1645–0317. Recently it has been shown that the RVM can be recovered in this
pulsar by using only time samples which are greater than 80% linearly
polarized. In this work we test this novel approach on the brightest 249
pulsars from the TPA sample, of which 177 yield sufficient highly polarized
samples to be amenable to our method. Remarkably, only 9 of these pulsars (5%)
now fail to fit the RVM as opposed to 59% from the original analysis. This
result favours the paradigm that the underlying mechanism is coherent
curvature radiation.

###### keywords:

pulsars:general – radiation mechanisms: non-thermal

††pubyear: 2024††pagerange: The Thousand-Pulsar-Array programme on MeerKAT
XIV: On the high linearly polarized pulsar signals–A

##  1 Introduction

Radhakrishnan & Cooke (1969) first observed the characteristic S-shaped swing
of the linear polarization position angle (PPA) across the pulse profile in
the Vela pulsar and proposed the rotating vector model (RVM) to explain the
observations. In the RVM the PPA swing results due to an emission mechanism
where the linearly polarized emission traces the variation in the dipolar
magnetic field line planes. As the star rotates, the observer cuts different
dipolar magnetic field lines, which then produces the characteristic S-shaped
swing. Radhakrishnan (1969) suggested that the underlying emission mechanism
was vacuum curvature radiation, with emission originating close to the
magnetic pole of the neutron star and the electric field vectors lying in the
dipolar magnetic field line plane. In subsequent studies however it was found
that the electric field emerging from the Vela pulsar lies perpendicular to
the dipolar magnetic field planes (Helfand et al., 2001; Lai et al., 2001),
and hence the vacuum curvature radiation model for the Vela pulsar had to be
abandoned.

In due course as more pulsars were discovered, polarization studies have been
reported for a large sample of pulsars (see e.g. Manchester 1971; Gould & Lyne
1998; Weisberg et al. 1999; Johnston et al. 2008; Han et al. 2009; Johnston &
Kerr 2018; Rankin et al. 2023; Wang et al. 2023; Posselt et al. 2023). The
majority of these studies are so-called average profile studies, where the
Stokes parameters are averaged for a few hundred to a few thousand pulses.
These studies often reveal that the smooth PPA traverse is interrupted by
jumps of 90° due to the presence of orthogonal polarization modes (OPM;
Manchester 1975; Backer et al. 1976). The PPA behaviour of the larger sample
of pulsars showed that the RVM is a reasonable model for the normal pulsar
population i.e. pulsars with periods longer than $\sim$ 0.05 second, and in
this work we focus on this population. While the RVM is a good fit to many
normal pulsars, there are equally a large number of pulsars where the RVM
fails. The most comprehensive study in this regard is by Johnston et al.
(2023) (hereafter J23), where they tested the validity of the RVM against the
average PPA behaviour for 850 pulsars, and found that the RVM could only be
fitted to just over half of the sample, even when the orthogonal jumps are
accounted for.

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---|---
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Figure 1: Results for four pulsars with non-RVM PPA tracks after integrating
all the single pulses. Each pulsar’s data is represented by four panels. The
top left panel shows in cyan the position angle of the linear polarization in
the integrated profile superposed on a heat-map of all the individual position
angle points. The bottom left panel show the integrated profile (black), the
linear polarization (red) and the circular polarization (blue). The right hand
panels depict the same scheme but only for those samples which are more than
80% polarized.

Instead of integrating over many rotations of the pulsar, examination of the
polarization on a continuous train of time-samples (typically of duration 1 ms
or less) often provides a better understanding of the PPA behaviour. Gil &
Lyne (1995) showed that in a pulsar with a complex non-RVM like PPA traverse,
the time-sampled PPA distribution clearly showed two parallel orthogonal RVM
tracks. However the many PPA values which did not conform to the RVM were then
speculated to be due to mode mixing and propagation effects. This aspect of
OPM averaging has also been seen in other studies of bright pulsars (e.g.
Rankin & Rathnasree 1995; Ramachandran et al. 2004; Mitra et al. 2016a). A
handful of these time-sampled polarization emission surveys have been carried
out for normal pulsars (Manchester et al. 1975; Stinebring et al. 1984; Mitra
& Rankin 2011; Mitra et al. 2016b; Olszanski et al. 2019), where often RVM-
like OPM tracks are seen in many pulsars across different frequencies. These
OPM tracks are usually thought to be associated with the natural modes i.e.
the extraordinary (X) and ordinary (O) propagation modes of pair plasma
embedded in the strong magnetic field (Cocke & Pacholczyk, 1976; Melrose &
Stoneham, 1977) .

There exists another category of pulsars which are significant in number,
where the time-sampled PPA appear to show no organized pattern and the
corresponding average PPA has a complex non-RVM like behaviour. Recently Mitra
et al. (2023a) (MMB23 hereafter) claimed that the high linearly polarized time
samples must correspond to purely linearly polarized X and O mode of the
strongly magnetized pair plasma, and if the underlying emission mechanism is
excited due to coherent curvature radiation (CCR hereafter), then these time
samples across the pulse should reproduce the RVM. This line of reasoning is
similar to an earlier study by Mitra et al. (2009) and Melikidze et al. (2014)
where they demonstrated that the PPA corresponding to the high linearly
polarized subpulses in several pulsars follow the average RVM like PPA
traverse. MMB23 applied the high linearly polarized time sample criterion to
PSR J1645$-$0317, which has a disordered single pulse PPA distribution and
complex non-RVM average PPA traverse. Remarkably they found that the high
linearly polarized samples followed the PPA track which can be fitted with the
RVM accurately. In this case only one PPA track was clearly visible, and a
hint of presence of high linearly polarized orthogonal PPAs for a small range
of pulse longitude was seen. MMB23 surmised that the low linearly polarized
samples dominate the disordered non-RVM PPAs, presumably due to mixing of the
modes and propagation effects.

The high linearly polarized sample criteria can hence be employed to a larger
dataset to check two predictions of MMB23: firstly in pulsars with disordered
PPA the high linearly polarized samples should follow the RVM and secondly
there must be several cases where these samples follow the two tracks of X and
O mode. The sample set used by J23 is particularly suitable for this exercise,
since for many pulsars high quality, high time-resolution data have also been
recorded. In this paper we report an analysis of high linearly polarized
samples from the TPA observations. In section 2 we define the sample
selection, section 3 we describe the analysis technique and present the
results and in section 4 we state our conclusions.

##  2 Sample selection

The Thousand Pulsar Array Program (TPA) on MeerKAT has observed in excess of
1200 pulsars (Johnston et al., 2020). The integration time on each of the
pulsars was generally sufficient to produce at least 1000 single pulses (Song
et al., 2021). Details of the TPA observing, processing, calibration and
analysis can be found in Serylak et al. (2021), Posselt et al. (2021) and Song
et al. (2023). In brief the observing band runs from 896 to 1671 MHz
subdivided into 1 MHz channels. Typically 1024 phase bins per pulsar period
are formed and the data are both flux and polarization calibrated.

In this paper we used high time-resolution data for 1202 pulsars. From the J23
paper, these pulars are classified as follows: 411 follow the RVM, 342 are
non-RVM, 70 are ‘flat’ i.e no significant PPA changes across the pulse profile
but still can be fitted with RVM, 20 are interpulses and for 359 no RVM fit
was attempted. In J23, the signal-to-noise ratio (s/n) of the linear
polarization in the integrated profile was critical, here however, we require
good s/n for each single pulse and we need sufficient single pulses to build
up the statistics. We therefore restricted the sample to (a) pulsars with more
than 500 pulses and (b) at least 60% of the single pulses had to have s/n more
than 5-$\sigma$ in Stokes $I$. This resulted in a sample of 249 pulsars.

|
---|---
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Figure 2: Results for four pulsars showing RVM tracks with orthogonal jumps.
Each pulsar’s data is represented by four panels. The top left panel shows in
cyan the position angle of the linear polarization in the integrated profile
superposed on a heat-map of all the individual position angle points. The
bottom left panel show the integrated profile (black), the linear polarization
(red) and the circular polarization (blue). The right hand panels depict the
same scheme but only for those samples which are more than 80% polarized.

##  3 Results and Analysis

###  3.1 Forming the highly polarized profiles

The analysis proceeded as follows. First we summed together all the data
modulo the pulsar spin period to produce the average pulse profile and set the
on-pulse window. At the same time, for each phase bin within the pulse window
we computed the PPA provided the linear polarization was more than
3.5-$\sigma$ above the noise. Then we made a second pass through the high
time-resolution data, this time only recording samples which are greater than
80% linearly polarized. We kept track of the number of occurrences of such
samples as a function of pulse longitude. As before, we computed the PPA for
each of these samples. Finally, we produce an integrated profile from these
high polarized samples and an integrated PPA swing. We stress that we deal
with individual time samples, we do not consider single pulses as a whole nor
any specific sub-structure within the single pulse profile.

In Figure 1 we show the output from four pulsars, all of which were classified
as non-RVM in J23. The most noticeable aspect here is that on application of
the high polarized time sample criterion, the disordered PPA distribution
(seen in the left top heat map) vanishes, and a more ordered narrowly confined
PPA distribution is observed (seen in the right top heat map). Consequently
the distortions in the average PPA tracks (cyan points in the left top panel)
smooth out, and more RVM-like tracks appear (cyan points in the right top
panel). The effect is striking in PSR J0837$-$4135, where the classical RVM-
like PPA becomes apparent. In PSR J0908–1739, the OPM in the leading part of
the profile gets clearly resolved. In PSR J1224–6407, while most of the
disordered PPA distribution vanishes leaving behind a narrowly defined PPA
track, one can still see some excess spread of PPA towards the center of the
profile which results in a small kinky feature in average PPA. In PSR
J1430–6623 the several PPA patches almost disappear in the high polarized case
and only a single RVM like PPA track is seen.

In Figure 2 we show four examples of pulsars that were classified as RVM in
J23. After applying the high polarized criteria the average PPA traverse for
these pulsars still follows the RVM. The high polarized PPA distributions show
assorted properties: in PSRs J0729–1836 and J1703–1846 the two parallel OPM
tracks are seen in both the full and high polarized case; in PSR J1312–5516
two tracks are seen in the full data while only one track is visible in high
polarized case; in PSR J1605–5257 the multiple OPM jumps in the full data are
reproduced in the high polarized data.

It should be noted that, for low $\dot{E}$ pulsars, only a few percent of the
samples go into making the profiles shown in Figures 1 and 2. This would imply
that part of the depolarization is due to the spread of the PPA, but most of
the depolarization must already occur internally in the magnetosphere, before
the emission detaches.

Table 1: Results for the 249 pulsars analysed here. The first column is the classifcation given by the RVM fitter (see J23 for details). The second and third column denote how many pulsars fall into each class according to J23 and from the present work. Class | J23 | current work
---|---|---
RVM | 90 | 146
Flat | 11 | 9
non-RVM | 146 | 22
No Pol | 2 | 72

###  3.2 RVM fitting

The same RVM fitter that was used in J23 was now used to fit the high linearly
polarized average PPA tracks for all 249 pulsars with the results given in
Table 1. None of the pulsars previously classified as RVM became non-RVM after
selecting the high polarized samples. In 72 of the 249 pulsars, there were not
sufficient PPA points for the fitter to proceed (i.e. there were not
sufficient highly polarized samples). Of the 177 remaining pulsars we found
that only 22, i.e. 12%, failed to give good fits with $\chi^{2}$ values less
than 3 and hence were classified as non-RVM. This is a significant improvement
over the results of J23, where RVM failed to fit to the average PPA for 59% of
the pulsars under consideration here.

We carefully scrutinized the 22 cases which the fitter classified as ‘non-
RVM’. These cases may be influenced by our analysis method, where due to
practical considerations for retaining sufficient time samples we have defined
the high linearly polarized sample to be above 80%, whereas MMB23 suggest that
the RVM will be reproduced only by 100% linearly polarized samples. The lower
fractional polarization can be a result of mixing of the X and O modes, and it
is possible that this leads to deviation from the RVM. We tested this by re-
analysing the data for these 22 pulsars when setting the threshold to 90%
linear rather than 80%. This indeed reduces the number of non-RVM cases to 9.
We surmise that more sensitive observations and a larger number of pulsar
rotations would be beneficial to sort out the remaining cases.

In Figure 3 we show the cumulative $\dot{E}$ distributions for the entire TPA
sample of 1202 pulsars, the 249 pulsars considered here and the 72 pulsars
without any highly polarized samples. Two points can be gleaned. First the 249
pulsars are somewhat lower in $\dot{E}$ than the entire sample; this implies
that single pulses from lower $\dot{E}$ pulsars are brighter than those from
high $\dot{E}$ pulsars (possibly due to the fact that their distances are
smaller). Secondly the pulsars without highly polarized data points are
significantly lower in $\dot{E}$ than the sample as a whole. However, we
caution that with only $\sim$1000 single pulses per pulsar that some of the
seemingly unpolarized cases may be resolved with a much larger number of
pulses. This will not be true in all cases, for example the very bright PSR
J1534–5334 shows no samples with linear polarization greater than 50%.

###  3.3 Circular Polarization and OPM jumps

In the profiles made from the highly linearly polarized samples there often
remains a significant degree of circular polarization, for example PSR
J1224–6407 in Figure 1 and PSRs J0729–1836 and J1312–5516 in Figure 2. One
possibility is that the modes are elliptically polarized. For PSR J1312–5516
in particular the standard integrated profile with its two competing modes
shows almost no circular whereas in the highly polarized profile a single mode
dominates with positive circular polarization.

In the highly polarized profiles we find that OPM tracks are present in 35% of
cases, a number not too dissimilar to that found by J23 in a much larger
sample of integrated pulse profiles. For the pulsars which do show evidence of
OPM jumps in J23, 50% of them retain the OPM jumps in the highly polarized
profiles. It therefore seems clear that sometimes the X mode provides the
highly polarized samples, sometimes in the O mode and sometimes a mixture of
the two as a function of pulse longitude. In regions of pulse longitude where
there are mode mixtures, we find that the average PPA tends to follow one of
the modes, and the OPM jumps in the average PPA can be clearly distinguished.
The RVM fitter is designed to detect OPM jumps of 90°, and hence fitting RVM
to the average PPA performs well. For a given pulsar there is no immediate way
to tell which of O or X is the dominant mode. Thus, any theoretical emission
model should take this into account.

---
Figure 3: Cumulative distributions of the log of the spin-down energy,
$\dot{E}$, for the 1202 pulsars from the TPA (black), the 249 pulsars used in
this sample (blue) and the 69 pulsars with no highly polarized samples (red).
---
Figure 4: Percentage linear polarization as a function of $\dot{E}$. The blue
points show the linear polarization of the integrated profile, the green
points show the mean linear polarization of the individual samples..

###  3.4 Tabular description of results

In Table 2 we present the results for the 249 pulsars analysed here using the
selection criteria outlined in Section 2. The first two columns report the
pulsar’s Jname and the log of the spin-down energy ($\dot{E}$). Columns 3 and
4 given the number of single pulses recorded ($N_{p}$) and the percentage of
those above 5-$\sigma$ ($N_{f}$). Columns 5 and 6 give the percentage of
linear ($\%L_{t}$) and circular ($\%V_{t}$) polarization in the integrated
profile. Note that these values may differ slightly from those given in
Posselt et al. (2023) as the observations used here are not necessarily the
same as used in their paper. Columns 7 and 8 give the mean percentage of all
the samples in linear ($\%L_{s}$) and circular ($\%V_{s}$) polarization
provided that the total intensity of the sample is greater than 3.5-$\sigma$.
The last two columns give the class from the RVM fitting according to J23 and
after formation of the high linear profile. We denote with a dagger symbol
those pulsars which remain non-RVM even after the application of a higher
linear threshold as outlined in Section 3.2.

Figure 4 shows the percentage linear polarization of the integrated profile
(blue points) and the average of the individual samples (green points). First
it should be noted the relative paucity of points above an $\dot{E}$ of
$10^{34}$ ergs-1. This is because these pulsars are generally too weak to
satisfy our single pulse thresholds. However, the blue points show the trend
pointed out by Weltevrede & Johnston (2008), Posselt et al. (2023) and others
in that pulsars with high $\dot{E}$ are highly polarized whereas pulsars at
low $\dot{E}$ much less so. In the single samples we see, as expected, that
the fractional linear polarization increases. The trend still remains;
relatively few pulsars at low $\dot{E}$ have a fractional polarization greater
than 50%. This implies that the majority of samples must have fractional
linear polarization less than 25% and that the modes have already mixed on
this short time-scale.

##  4 Conclusions

MMB23 suggest that if the underlying emission mechanism is CCR, then high
linearly polarized samples in pulsars should have orthogonal PPA tracks that
follow the RVM. We tested this hypothesis on the sample set of TPA pulsars. We
found that in pulsars with a disordered PPA distribution, the RVM can be
recovered in the vast majority of cases. Further, we clearly see examples of
high linearly polarized OPM tracks which can be interpreted as the X and O
modes of the strongly magnetized pair plasma. The escape of the X and O modes
requires the plasma flow to be inhomogeneous and Mitra et al. (2023b) alluded
to the fact that the observed change in degree of linear polarization with
pulsar spindown energy may be related to the change in the degree of
inhomogeneity in the plasma.

Mitra et al. (2023b) suggested that as the linearly polarized modes propagate
through the magnetospheric plasma, the modes can get partially converted into
circular polarization due to propagation effects, and thus the observed
signals are generally elliptically polarized. The non-RVM PPAs can be
interpreted as incoherent averaging of the X and O mode from a large number of
sources. A different idea was put forward by Oswald et al. (2023b). In their
picture, both coherent and incoherent mixing of the modes take place, the
coherent mixing produces the circular polarization and also distorts the PPA.
This model provides a good fit to the broad-band data presented in Oswald et
al. (2023a).

CCR can be excited in a pulsar plasma by a stable charge bunch streaming at
relativistic speeds along the curved magnetic field. Theoretically, formation
of relativistic charge solitons is thought to be an excellent candidate for
the formation of such charge bunches (Melikidze & Pataraia 1980; Asseo &
Melikidze 1998; Melikidze et al. 2000; Lakoba et al. 2018; Rahaman et al.
2020; Manthei et al. 2021; Rahaman et al. 2022b). The theory of charge
solitons has been developed in the one dimensional approximation, and further
improvement in the theory in needed to verify the stability of the solitons in
a more realistic situation of two or three dimension. Further the physical
process of the escape of X and O mode in pulsar plasma and the origin of
circular polarization still needs to be understood (e.g. Melikidze et al.
2014; Rahaman et al. 2022a; Mitra et al. 2023b). The observational evidence
for CCR presented in this work strongly motivates theoretical research in
these directions.

## Acknowledgements

DM acknowledges CSIRO for supporting a visiting position, the Department of
Atomic Energy, Government of India, under project No. 12-R&D-TFR-5.02-0700 and
grant 2020/37/B/ST9/02215 from the National Science Centre, Poland. LSO
acknowledges the support of Magdalen College, Oxford. We thank M Rahaman for
useful comments. The MeerKAT telescope is operated by the South African Radio
Astronomy Observatory (SARAO), which is a facility of the National Research
Foundation, an agency of the Department of Science and Innovation. SARAO
acknowledges the ongoing advice and calibration of GPS systems by the National
Metrology Institute of South Africa (NMISA) and the time space reference
systems department department of the Paris Observatory. PTUSE was developed
with support from the Australian SKA Office and Swinburne University of
Technology. This work made use of the OzSTAR national HPC facility at
Swinburne University of Technology. MeerTime data is housed on the OzSTAR
supercomputer. The OzSTAR program receives funding in part from the Astronomy
National Collaborative Research Infrastructure Strategy (NCRIS) allocation
provided by the Australian Government.

## Data Availability

Data are available on reasonable request.

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##  Appendix A Table of Results

Table 2 lists the 249 pulsars used in this analysis. For a description of the
table see Section 3.4.

Table 2: Results for 249 pulsars. The first two columns report the pulsar’s Jname and the log of the spin–down energy ($\dot{E}$). Columns 3 and 4 given the number of single pulses recorded ($N_{p}$) and the percentage of those above 5–$\sigma$ ($N_{f}$). Columns 5 and 6 give the percentage of linear ($\%L_{t}$) and circular ($\%V_{t}$) polarization in the integrated profile. Columns 7 and 8 give the mean percentage of all the samples in linear ($\%L_{s}$) and circular ($\%V_{s}$) polarization. The last two columns give the Class from the RVM fitting according to Johnston et al. (2023) and after formation of the high linear profile. The dagger symbol denotes pulsars which remain non–RVM even after application of a higher linear threshold. JNAME | log($\dot{E}$) | $N_{p}$ | $N_{f}$ | $\%L_{t}$ | $\%V_{t}$ | $\%L_{s}$ | $\%V_{s}$ | Old Class | New Class
---|---|---|---|---|---|---|---|---|---
J0034–0721 | 31.3 | 1042 | 54.5 | 15.9 | 4.4 | 37.4 | 4.0 | non–RVM | RVM
J0108–1431 | 30.8 | 1042 | 55.6 | 80.6 | 12.1 | 69.5 | 7.4 | flat | flat
J0134–2937 | 33.1 | 1110 | 88.1 | 51.4 | –20.3 | 47.9 | –13.7 | RVM | RVM
J0151–0635 | 30.7 | 1039 | 97.6 | 38.9 | 0.2 | 41.0 | –1.0 | RVM | RVM
J0152–1637 | 31.9 | 1047 | 86.4 | 15.7 | –1.4 | 25.8 | –1.6 | non–RVM | No poln
J0255–5304 | 31.1 | 1226 | 81.9 | 9.2 | –5.0 | 31.3 | –4.5 | non–RVM | non–RVM
J0302+2252 | 30.3 | 1030 | 57.2 | 25.4 | –0.2 | 40.9 | –0.1 | non–RVM | non–RVM
J0304+1932 | 31.3 | 1032 | 89.2 | 36.8 | 12.5 | 45.0 | 12.6 | RVM | RVM
J0401–7608 | 32.6 | 1078 | 98.1 | 28.8 | –2.3 | 34.8 | –2.4 | non–RVM | RVM
J0448–2749 | 31.8 | 1048 | 58.1 | 23.1 | –15.3 | 36.1 | –17.3 | flat | flat
J0452–1759 | 33.1 | 1042 | 100.0 | 18.3 | –0.0 | 33.7 | 0.5 | RVM | RVM
J0517+2212 | 31.6 | 1036 | 83.0 | 21.1 | 6.1 | 30.2 | 6.7 | non–RVM | RVM
J0525+1115 | 31.8 | 1048 | 95.1 | 13.8 | 9.1 | 24.5 | 9.2 | non–RVM | No poln
J0536–7543 | 31.1 | 1041 | 92.6 | 51.5 | –11.6 | 55.3 | –10.9 | RVM | RVM
J0543+2329 | 34.6 | 1033 | 97.8 | 53.3 | –11.1 | 61.7 | –12.2 | RVM | RVM
J0601–0527 | 32.9 | 1063 | 96.9 | 32.1 | 1.5 | 38.4 | –0.5 | non–RVM | RVM
J0614+2229 | 34.8 | 1032 | 100.0 | 76.9 | 16.2 | 80.5 | 15.9 | RVM | RVM
J0624–0424 | 31.5 | 1056 | 97.5 | 28.8 | 6.3 | 41.5 | 6.1 | non–RVM | non–RVM
J0629+2415 | 32.9 | 1030 | 100.0 | 23.5 | 11.1 | 31.7 | 11.7 | non–RVM | RVM
J0630–2834 | 32.2 | 1043 | 100.0 | 52.1 | –5.1 | 55.1 | –4.9 | RVM | RVM
J0646+0905 | 31.6 | 1046 | 87.4 | 37.5 | –3.8 | 40.7 | –3.8 | RVM | RVM
J0659+1414 | 34.6 | 1047 | 63.4 | 85.8 | –14.0 | 88.4 | –14.4 | RVM | RVM
J0719–2545 | 32.5 | 1043 | 48.1 | 21.6 | 8.3 | 28.7 | 8.3 | non–RVM | RVM
J0729–1836 | 33.7 | 1042 | 80.7 | 27.2 | –8.3 | 40.1 | –8.2 | RVM | RVM
J0738–4042 | 33.0 | 1095 | 100.0 | 27.1 | –6.2 | 43.7 | –6.0 | non–RVM | RVM
J0742–2822 | 35.1 | 2969 | 100.0 | 90.4 | –4.8 | 93.0 | –4.9 | RVM | RVM
J0758–1528 | 32.3 | 1044 | 79.3 | 18.8 | –1.1 | 32.0 | –0.8 | non–RVM | RVM
J0809–4753 | 32.9 | 1044 | 99.8 | 27.4 | –0.9 | 31.2 | –0.8 | non–RVM | RVM
J0818–3232 | 30.5 | 1029 | 79.6 | 20.2 | –3.8 | 33.1 | –2.9 | non–RVM | No poln
J0820–1350 | 31.6 | 1056 | 98.0 | 14.6 | –9.7 | 27.4 | –10.3 | non–RVM | RVM
J0820–4114 | 30.7 | 1048 | 93.9 | 30.6 | 3.3 | 31.4 | 2.2 | No poln | RVM
J0823+0159 | 30.8 | 1076 | 99.3 | 10.9 | –2.3 | 31.4 | –1.8 | non–RVM | RVM
J0835–4510 | 36.8 | 3433 | 100.0 | 88.0 | –9.0 | 88.9 | –9.3 | RVM | RVM
J0837+0610 | 32.1 | 1037 | 92.4 | 8.6 | –4.4 | 28.5 | –4.2 | non–RVM | No poln
J0837–4135 | 32.5 | 1041 | 99.5 | 15.8 | 12.4 | 30.1 | 12.5 | non–RVM | RVM
J0840–5332 | 32.2 | 1035 | 97.0 | 17.6 | 14.1 | 27.0 | 14.5 | non–RVM | RVM
J0846–3533 | 31.7 | 1033 | 99.9 | 40.3 | –10.4 | 42.0 | –10.8 | non–RVM | RVM
J0855–3331 | 32.1 | 1030 | 64.2 | 15.5 | 2.2 | 28.3 | 2.4 | non–RVM | No poln
J0856–6137 | 31.9 | 1033 | 86.6 | 3.7 | 5.0 | 10.9 | 4.8 | RVM | No poln
J0902–6325 | 31.2 | 1033 | 97.6 | 33.9 | 6.9 | 38.5 | 8.9 | non–RVM | RVM
J0904–7459 | 32.0 | 1040 | 86.0 | 32.6 | 2.1 | 33.6 | 1.5 | RVM | RVM
J0905–4536 | 30.8 | 1030 | 89.3 | 41.4 | 2.5 | 45.5 | 1.4 | RVM | RVM
J0905–5127 | 34.4 | 1064 | 2.4 | 100.2 | 8.2 | 84.2 | 9.4 | RVM | RVM
J0907–5157 | 33.6 | 1073 | 100.0 | 37.1 | 3.1 | 44.0 | 2.3 | RVM | RVM
J0908–1739 | 32.6 | 1050 | 61.9 | 13.8 | 1.9 | 30.2 | 2.9 | non–RVM | RVM
J0908–4913 | 35.7 | 1045 | 100.0 | 98.1 | 1.1 | 96.1 | 1.0 | RVM | RVM
J0909–7212 | 30.7 | 1035 | 70.8 | 32.4 | 9.2 | 38.7 | 8.0 | RVM | RVM
J0922+0638 | 33.8 | 2090 | 100.0 | 55.2 | 8.6 | 58.5 | 8.5 | RVM | RVM
J0924–5302 | 33.5 | 1032 | 92.8 | 8.5 | –5.9 | 13.3 | –6.3 | non–RVM | No poln
J0924–5814 | 32.7 | 1044 | 99.9 | 53.9 | –3.9 | 56.1 | –4.2 | RVM | RVM
J0934–5249 | 31.8 | 1031 | 98.5 | 19.4 | –12.8 | 35.0 | –12.4 | non–RVM | RVM
J0942–5552 | 33.5 | 1040 | 98.1 | 38.9 | –2.6 | 48.1 | 0.8 | non–RVM | RVM
J0944–1354 | 31.0 | 1041 | 98.7 | 20.1 | 16.0 | 29.4 | 15.4 | non–RVM | No poln
J0953+0755 | 32.7 | 803 | 99.8 | 14.0 | –5.6 | 37.0 | –6.5 | non–RVM | RVM
Table 2: Results for 249 pulsars (continued) JNAME | log($\dot{E}$) | $N_{p}$ | $N_{f}$ | $\%L_{t}$ | $\%V_{t}$ | $\%L_{s}$ | $\%V_{s}$ | Old Class | New Class
---|---|---|---|---|---|---|---|---|---
J0959–4809 | 31.0 | 1049 | 95.3 | 43.9 | –7.8 | 39.6 | –10.6 | RVM | RVM
J1001–5507 | 32.8 | 1030 | 100.0 | 6.7 | –0.6 | 15.4 | –0.9 | non–RVM | No poln
J1001–5559 | 30.9 | 1031 | 88.8 | 23.2 | 10.2 | 30.5 | 13.1 | non–RVM | No poln
J1001–5939 | 30.7 | 517 | 43.3 | 35.3 | 1.2 | 39.1 | 0.8 | RVM | No poln
J1016–5345 | 32.2 | 1033 | 51.8 | 20.4 | 3.7 | 30.1 | 3.8 | RVM | RVM
J1017–5621 | 33.0 | 1046 | 73.3 | 18.4 | –17.1 | 48.1 | –17.4 | non–RVM | non–RVM$\dagger$
J1018–1642 | 31.1 | 1029 | 61.7 | 16.7 | 20.3 | 34.9 | 24.0 | non–RVM | non–RVM
J1034–3224 | 30.8 | 1035 | 100.0 | 8.2 | 5.8 | 13.2 | 4.5 | non–RVM | No poln
J1041–1942 | 31.1 | 1055 | 98.3 | 33.4 | 7.6 | 43.0 | 8.8 | RVM | RVM
J1042–5521 | 32.2 | 1032 | 86.1 | 11.9 | 3.9 | 20.1 | –6.3 | RVM | No poln
J1048–5832 | 36.3 | 7270 | 85.3 | 72.2 | 4.5 | 74.0 | 4.8 | RVM | RVM
J1049–5833 | 31.2 | 1035 | 48.9 | 25.6 | –7.6 | 38.6 | –7.7 | RVM | No poln
J1056–6258 | 33.3 | 1049 | 100.0 | 44.4 | –2.4 | 51.7 | –2.5 | flat | flat
J1057–5226 | 34.5 | 1022 | 100.0 | 69.1 | 0.1 | 75.5 | –0.2 | non–RVM | non–RVM$\dagger$
J1059–5742 | 32.0 | 1054 | 96.3 | 10.0 | –0.4 | 22.6 | 0.1 | non–RVM | No poln
J1110–5637 | 32.7 | 1041 | 95.8 | 28.7 | –8.0 | 36.7 | –8.9 | RVM | RVM
J1112–6613 | 32.9 | 1033 | 99.9 | 17.6 | 7.2 | 18.5 | 8.0 | non–RVM | RVM
J1112–6926 | 32.3 | 1036 | 63.0 | 11.0 | 3.1 | 21.3 | 2.9 | non–RVM | No poln
J1114–6100 | 33.4 | 1036 | 83.9 | 18.9 | –0.8 | 27.3 | –1.5 | RVM | RVM
J1116–4122 | 32.6 | 1037 | 82.7 | 10.0 | –0.8 | 28.8 | –1.4 | RVM | No poln
J1121–5444 | 32.9 | 1033 | 99.3 | 26.7 | –7.3 | 27.7 | –7.7 | non–RVM | RVM
J1123–4844 | 32.3 | 1057 | 96.7 | 31.7 | 27.0 | 34.0 | 26.3 | non–RVM | RVM
J1133–6250 | 31.2 | 1033 | 92.2 | 13.9 | 2.5 | 23.3 | 1.6 | non–RVM | No poln
J1136+1551 | 31.9 | 1031 | 85.0 | 18.5 | –8.1 | 34.6 | –8.4 | non–RVM | RVM
J1136–5525 | 33.8 | 1047 | 98.6 | 9.3 | –2.2 | 25.0 | –1.9 | non–RVM | RVM
J1137–6700 | 31.2 | 1096 | 93.6 | 14.6 | –1.9 | 23.3 | –0.9 | flat | No poln
J1141–6545 | 33.4 | 5200 | 85.4 | 13.6 | 5.7 | 19.7 | 4.5 | RVM | RVM
J1146–6030 | 33.5 | 1067 | 97.5 | 26.9 | 3.3 | 41.2 | 4.2 | RVM | RVM
J1157–6224 | 33.4 | 1052 | 97.6 | 32.6 | 10.8 | 38.1 | 8.9 | non–RVM | non–RVM
J1202–5820 | 33.0 | 1031 | 98.7 | 28.0 | 7.8 | 45.2 | 7.0 | non–RVM | RVM
J1224–6407 | 34.3 | 1071 | 100.0 | 35.4 | 22.5 | 50.5 | 22.9 | non–RVM | RVM
J1232–4742 | 28.9 | 962 | 82.1 | 33.2 | –2.9 | 38.1 | –4.1 | flat | flat
J1237–6725 | 31.0 | 1030 | 58.5 | 2.5 | 1.2 | 9.4 | 1.0 | non–RVM | No poln
J1239+2453 | 31.1 | 1029 | 94.8 | 42.1 | 0.4 | 47.9 | 0.2 | non–RVM | RVM
J1243–6423 | 33.5 | 1058 | 99.6 | 24.6 | –3.5 | 31.4 | –2.8 | non–RVM | non–RVM
J1246+2253 | 31.5 | 1032 | 50.9 | 8.8 | –2.1 | 29.3 | –3.4 | non–RVM | No poln
J1253–5820 | 33.7 | 1068 | 98.8 | 63.2 | 6.8 | 73.1 | 7.0 | RVM | RVM
J1257–1027 | 31.8 | 1072 | 97.2 | 33.4 | –4.8 | 37.5 | –3.5 | non–RVM | non–RVM
J1305–6455 | 32.9 | 1036 | 98.8 | 35.2 | 10.4 | 31.0 | 13.1 | non–RVM | non–RVM
J1306–6617 | 33.3 | 1037 | 95.6 | 17.3 | 7.5 | 24.9 | 7.6 | non–RVM | No poln
J1312–5516 | 32.6 | 709 | 94.6 | 21.9 | 0.1 | 39.2 | –0.5 | RVM | RVM
J1320–5359 | 34.2 | 1043 | 86.9 | 26.0 | –8.9 | 31.9 | –7.2 | RVM | RVM
J1326–5859 | 33.1 | 1048 | 96.5 | 37.5 | 8.6 | 39.0 | 8.7 | non–RVM | RVM
J1326–6408 | 32.4 | 1034 | 85.6 | 24.5 | 2.5 | 25.1 | 1.9 | non–RVM | No poln
J1326–6700 | 33.1 | 1037 | 99.8 | 36.8 | –5.8 | 52.6 | –6.1 | RVM | RVM
J1327–6222 | 33.7 | 1043 | 100.0 | 6.4 | 5.0 | 16.5 | 4.0 | non–RVM | RVM
J1327–6301 | 33.9 | 1075 | 96.4 | 29.7 | 0.2 | 31.7 | 2.0 | RVM | RVM
J1328–4357 | 32.9 | 1038 | 89.1 | 32.5 | 6.4 | 42.2 | 6.9 | RVM | RVM
J1328–4921 | 30.9 | 527 | 85.2 | 17.6 | 6.7 | 24.2 | 3.1 | non–RVM | No poln
J1338–6204 | 32.5 | 1034 | 99.8 | 21.4 | 13.3 | 24.9 | 14.2 | non–RVM | RVM
J1355–5153 | 32.6 | 933 | 86.2 | 2.4 | –2.1 | 7.0 | –2.9 | non–RVM | No poln
J1401–6357 | 33.0 | 1035 | 97.6 | 26.7 | –0.9 | 40.2 | 0.1 | RVM | RVM
J1414–6802 | 30.4 | 538 | 68.8 | 34.0 | 11.3 | 42.7 | 11.7 | RVM | RVM
J1420–5416 | 31.0 | 1025 | 52.2 | 11.5 | –13.9 | 18.8 | –14.4 | non–RVM | No poln
J1424–5822 | 33.5 | 1028 | 49.1 | 21.8 | 3.2 | 18.7 | 4.1 | flat | No poln
Table 2: Results for 249 pulsars (continued) JNAME | log($\dot{E}$) | $N_{p}$ | $N_{f}$ | $\%L_{t}$ | $\%V_{t}$ | $\%L_{s}$ | $\%V_{s}$ | Old Class | New Class
---|---|---|---|---|---|---|---|---|---
J1428–5530 | 32.6 | 1037 | 72.1 | 30.9 | 0.7 | 42.4 | 0.8 | RVM | RVM
J1430–6623 | 32.4 | 1040 | 100.0 | 15.2 | 2.1 | 29.1 | 1.6 | non–RVM | RVM
J1440–6344 | 32.7 | 1032 | 85.8 | 21.3 | 3.2 | 27.5 | 5.0 | non–RVM | No poln
J1453–6413 | 34.3 | 1087 | 92.7 | 31.4 | 4.4 | 35.6 | 4.9 | non–RVM | RVM
J1456–6843 | 32.3 | 1075 | 99.8 | 9.8 | 1.5 | 38.7 | –1.0 | non–RVM | non–RVM
J1507–4352 | 33.4 | 1043 | 91.7 | 27.9 | –6.2 | 34.5 | –6.5 | RVM | RVM
J1507–6640 | 33.0 | 1042 | 50.8 | 8.9 | 7.4 | 21.1 | 6.4 | non–RVM | No poln
J1514–4834 | 32.6 | 1043 | 48.5 | 7.5 | –3.4 | 19.8 | –1.8 | non–RVM | No poln
J1522–5829 | 33.1 | 1046 | 98.1 | 28.7 | 1.4 | 32.5 | 1.5 | non–RVM | RVM
J1527–3931 | 31.7 | 743 | 50.3 | 16.3 | 12.7 | 23.7 | 11.5 | RVM | No poln
J1527–5552 | 32.6 | 1030 | 55.2 | 18.4 | 13.9 | 20.6 | 13.4 | non–RVM | No poln
J1534–5334 | 31.3 | 1032 | 100.0 | 4.2 | 0.9 | 10.8 | 0.0 | non–RVM | No poln
J1535–4114 | 33.3 | 1043 | 62.1 | 51.8 | –11.2 | 22.6 | –62.6 | RVM | RVM
J1536–3602 | 31.1 | 1032 | 61.4 | 25.8 | –7.6 | 37.5 | –9.3 | non–RVM | RVM
J1539–5626 | 34.1 | 1078 | 89.4 | 32.7 | 1.6 | 27.9 | –0.9 | non–RVM | RVM
J1539–6322 | 30.3 | 1104 | 91.1 | 48.8 | 5.4 | 49.2 | 5.9 | RVM | RVM
J1543+0929 | 31.6 | 1028 | 98.9 | 26.5 | –4.9 | 30.2 | –9.4 | non–RVM | RVM
J1544–5308 | 32.6 | 1087 | 99.8 | 17.8 | –4.1 | 25.4 | –5.5 | non–RVM | RVM
J1555–2341 | 32.3 | 1046 | 83.9 | 19.3 | 2.0 | 35.2 | 2.3 | RVM | RVM
J1555–3134 | 31.3 | 1045 | 99.8 | 16.0 | 2.9 | 26.9 | 2.7 | non–RVM | No poln
J1557–4258 | 32.6 | 1038 | 85.7 | 32.2 | –13.8 | 39.1 | –15.3 | non–RVM | non–RVM
J1559–4438 | 33.4 | 1066 | 100.0 | 41.0 | –10.3 | 42.0 | –10.0 | RVM | RVM
J1602–5100 | 33.6 | 1030 | 94.3 | 20.6 | 6.0 | 28.6 | –4.4 | non–RVM | RVM
J1603–2531 | 33.4 | 2131 | 94.3 | 27.7 | 0.6 | 44.5 | –0.4 | flat | flat
J1603–2712 | 32.4 | 1030 | 64.8 | 33.1 | 1.2 | 40.0 | 1.7 | non–RVM | non–RVM
J1604–4909 | 33.0 | 1043 | 99.9 | 9.8 | 0.8 | 17.1 | 1.1 | non–RVM | No poln
J1604–7203 | 31.9 | 1764 | 93.0 | 20.2 | 5.5 | 23.6 | 4.9 | non–RVM | No poln
J1605–5257 | 31.5 | 1037 | 99.8 | 37.0 | 5.1 | 45.0 | 4.9 | RVM | RVM
J1607–0032 | 32.2 | 1031 | 95.3 | 7.2 | 1.6 | 29.9 | –0.2 | non–RVM | No poln
J1622–4332 | 31.9 | 1039 | 58.5 | 16.8 | 12.4 | 25.2 | 8.8 | non–RVM | No poln
J1623–0908 | 31.7 | 1030 | 52.3 | 2.0 | 2.8 | 7.8 | 1.9 | non–RVM | No poln
J1625–4048 | 30.1 | 523 | 44.0 | 19.7 | 1.6 | 22.3 | 2.0 | non–RVM | No poln
J1635–5954 | 32.6 | 1030 | 97.9 | 36.8 | 8.1 | 34.9 | 8.8 | non–RVM | RVM
J1645–0317 | 33.1 | 1062 | 100.0 | 12.8 | –1.2 | 24.2 | –0.7 | non–RVM | RVM
J1646–6831 | 31.1 | 1031 | 70.2 | 40.6 | 6.8 | 46.8 | 6.2 | non–RVM | non–RVM$\dagger$
J1650–1654 | 31.4 | 1029 | 66.0 | 19.7 | 7.2 | 36.6 | 4.8 | non–RVM | No poln
J1651–4246 | 32.5 | 2143 | 96.1 | 39.6 | –15.4 | 43.5 | –13.7 | non–RVM | RVM
J1651–5222 | 32.4 | 1054 | 99.2 | 19.9 | –5.6 | 34.9 | –5.3 | non–RVM | RVM
J1700–3312 | 31.9 | 1037 | 76.0 | 38.4 | –15.2 | 44.0 | –14.8 | RVM | RVM
J1703–1846 | 32.1 | 1057 | 67.8 | 34.5 | 3.9 | 48.0 | 4.2 | RVM | RVM
J1703–3241 | 31.2 | 1040 | 99.7 | 46.2 | –0.5 | 52.5 | –0.6 | RVM | RVM
J1705–1906 | 33.8 | 868 | 100.0 | 53.2 | –17.5 | 58.1 | –17.6 | non–RVM | non–RVM$\dagger$
J1705–3423 | 33.4 | 1098 | 97.4 | 13.7 | 1.9 | 19.4 | 2.3 | non–RVM | RVM
J1709–1640 | 32.9 | 1033 | 96.0 | 10.5 | 2.0 | 31.9 | 2.4 | RVM | RVM
J1709–4429 | 36.5 | 2204 | 93.0 | 97.5 | –21.3 | 86.9 | –21.3 | flat | flat
J1711–5350 | 32.9 | 669 | 60.5 | 11.9 | –2.3 | 22.5 | –0.5 | non–RVM | RVM
J1720–1633 | 31.8 | 1033 | 76.8 | 17.3 | 3.5 | 24.1 | 2.1 | RVM | RVM
J1720–2933 | 32.1 | 1048 | 69.8 | 15.6 | 5.7 | 29.8 | 5.2 | RVM | No poln
J1722–3207 | 32.4 | 1068 | 100.0 | 23.9 | 1.1 | 26.6 | 0.7 | RVM | RVM
J1722–3712 | 34.5 | 1100 | 34.5 | 54.8 | 12.4 | 41.3 | 12.2 | RVM | RVM
J1731–4744 | 34.0 | 1049 | 100.0 | 18.0 | 4.0 | 37.8 | 3.7 | non–RVM | non–RVM$\dagger$
J1735–0724 | 32.8 | 1072 | 91.0 | 28.5 | 0.9 | 33.9 | 1.9 | non–RVM | RVM
J1738–3211 | 31.8 | 1054 | 52.4 | 17.9 | –5.0 | 44.0 | –5.5 | non–RVM | non–RVM$\dagger$
J1740+1000 | 35.4 | 1311 | 77.0 | 99.7 | –3.1 | 84.6 | –2.2 | RVM | RVM
J1740+1311 | 32.0 | 1039 | 98.9 | 44.5 | 4.1 | 49.7 | 4.0 | RVM | RVM
Table 2: Results for 249 pulsars (continued) JNAME | log($\dot{E}$) | $N_{p}$ | $N_{f}$ | $\%L_{t}$ | $\%V_{t}$ | $\%L_{s}$ | $\%V_{s}$ | Old Class | New Class
---|---|---|---|---|---|---|---|---|---
J1740–3015 | 34.9 | 1032 | 99.7 | 85.3 | –34.0 | 85.3 | –34.9 | RVM | RVM
J1741–0840 | 31.0 | 1037 | 71.8 | 37.4 | –4.4 | 44.0 | –4.1 | RVM | RVM
J1741–3927 | 32.7 | 1055 | 100.0 | 25.2 | 4.5 | 29.9 | 4.7 | non–RVM | RVM
J1742–4616 | 31.3 | 1035 | 38.5 | 36.9 | –8.9 | 39.6 | –8.9 | flat | No poln
J1743–3150 | 32.5 | 1035 | 89.1 | 23.4 | –3.7 | 27.8 | –3.0 | RVM | RVM
J1744–1610 | 31.2 | 569 | 62.4 | 21.0 | –2.6 | 27.2 | –2.4 | non–RVM | No poln
J1745–3040 | 33.9 | 1060 | 78.5 | 49.5 | –2.7 | 53.6 | –3.5 | non–RVM | non–RVM
J1748–1300 | 32.9 | 1041 | 93.8 | 26.9 | 3.5 | 30.3 | 4.5 | RVM | RVM
J1750–3157 | 31.0 | 1043 | 59.4 | 11.1 | –2.7 | 17.3 | –3.3 | non–RVM | No poln
J1751–4657 | 32.1 | 1050 | 97.0 | 17.9 | 9.1 | 30.5 | 8.7 | non–RVM | RVM
J1752–2806 | 33.3 | 1050 | 99.9 | 11.1 | 2.8 | 36.6 | 4.6 | non–RVM | non–RVM$\dagger$
J1759–3107 | 32.1 | 1032 | 45.8 | 24.2 | 1.0 | 33.2 | –3.6 | RVM | RVM
J1801–2920 | 32.0 | 1029 | 78.3 | 44.7 | –6.9 | 48.5 | –6.6 | RVM | RVM
J1806–1154 | 32.6 | 1030 | 94.3 | 35.6 | –0.3 | 35.8 | –0.8 | RVM | RVM
J1807–0847 | 32.4 | 1123 | 99.9 | 24.6 | 5.6 | 31.3 | 6.0 | non–RVM | RVM
J1808–0813 | 31.9 | 1034 | 80.2 | 23.1 | 6.8 | 31.4 | 7.0 | RVM | RVM
J1810–5338 | 32.9 | 2300 | 99.9 | 43.5 | –0.3 | 42.0 | –1.4 | RVM | RVM
J1817–3618 | 33.1 | 1063 | 68.8 | 19.4 | –12.4 | 32.5 | –13.2 | RVM | RVM
J1817–3837 | 32.6 | 1068 | 96.8 | 14.9 | 0.7 | 31.8 | 1.1 | non–RVM | RVM
J1819+1305 | 31.1 | 1034 | 60.2 | 21.2 | –1.9 | 28.1 | –2.8 | RVM | RVM
J1820–0427 | 33.1 | 1138 | 94.1 | 22.9 | –6.2 | 30.2 | –6.1 | non–RVM | RVM
J1823+0550 | 31.3 | 1032 | 100.0 | 22.4 | 3.9 | 31.5 | 3.8 | non–RVM | RVM
J1823–3106 | 33.7 | 1201 | 91.6 | 44.4 | –4.9 | 47.0 | –4.6 | RVM | RVM
J1824–1945 | 34.5 | 1112 | 97.7 | 18.9 | –2.3 | 20.9 | –2.6 | non–RVM | RVM
J1825–0935 | 33.7 | 1031 | 99.9 | 34.5 | 4.4 | 38.2 | 3.7 | non–RVM | non–RVM$\dagger$
J1826–1131 | 31.3 | 1032 | 87.0 | 0.8 | –6.3 | 9.1 | –4.2 | non–RVM | No poln
J1829–1751 | 33.9 | 685 | 100.0 | 35.5 | –9.3 | 39.7 | –9.6 | non–RVM | flat
J1832–0827 | 34.0 | 1052 | 81.3 | 14.8 | –2.3 | 24.1 | –0.9 | non–RVM | No poln
J1834–0426 | 32.1 | 1071 | 100.0 | 28.2 | –1.8 | 23.9 | –2.3 | No poln | RVM
J1836–1008 | 33.4 | 1041 | 100.0 | 14.7 | 5.2 | 18.3 | 5.2 | non–RVM | No poln
J1837–0653 | 30.6 | 1029 | 54.4 | 20.2 | –4.2 | 28.3 | –7.5 | non–RVM | No poln
J1839–1238 | 31.4 | 1034 | 66.7 | 21.1 | 7.2 | 23.8 | 6.9 | RVM | No poln
J1840–0809 | 32.0 | 1030 | 86.3 | 32.6 | –10.7 | 36.1 | –9.7 | RVM | RVM
J1840–0815 | 31.9 | 1029 | 78.0 | 7.3 | –0.9 | 15.8 | –0.1 | non–RVM | No poln
J1842–0359 | 30.5 | 1035 | 98.9 | 52.1 | 3.7 | 51.2 | 3.3 | RVM | RVM
J1843–0000 | 32.7 | 1028 | 100.0 | 15.5 | –0.6 | 35.8 | –0.8 | RVM | RVM
J1844+1454 | 33.1 | 1030 | 96.0 | 36.1 | 0.5 | 36.7 | 0.5 | non–RVM | RVM
J1847–0402 | 34.0 | 1054 | 99.7 | 17.1 | 2.2 | 24.3 | 2.3 | non–RVM | RVM
J1848–0123 | 32.9 | 1047 | 100.0 | 4.8 | 0.9 | 7.8 | 1.0 | non–RVM | No poln
J1848–1150 | 31.4 | 518 | 39.8 | 16.1 | 7.9 | 29.0 | 7.2 | non–RVM | No poln
J1849–0636 | 32.8 | 1032 | 52.3 | 8.7 | 2.6 | 15.9 | 2.7 | non–RVM | No poln
J1852–0635 | 33.6 | 1048 | 96.8 | 66.7 | –1.4 | 72.2 | –1.4 | RVM | RVM
J1854–1421 | 32.0 | 575 | 88.5 | 22.0 | 0.1 | 33.2 | 0.9 | RVM | RVM
J1900–2600 | 31.5 | 1062 | 95.7 | 35.6 | –0.1 | 43.9 | 0.1 | non–RVM | RVM
J1900–7951 | 31.5 | 515 | 67.6 | 29.0 | –1.6 | 34.8 | –2.6 | non–RVM | RVM
J1901+0331 | 33.0 | 1034 | 100.0 | 38.8 | 4.6 | 41.5 | 4.8 | non–RVM | RVM
J1901–0906 | 31.0 | 1034 | 96.0 | 30.0 | 0.3 | 41.4 | –1.7 | non–RVM | RVM
J1902+0556 | 33.1 | 1031 | 80.1 | 21.4 | –4.9 | 26.3 | –3.5 | non–RVM | No poln
J1902+0615 | 33.0 | 1035 | 63.9 | 11.8 | 4.5 | 16.9 | 4.0 | RVM | No poln
J1903+0135 | 32.6 | 1033 | 99.7 | 14.5 | 9.3 | 27.0 | 9.3 | non–RVM | RVM
J1903–0632 | 33.2 | 1388 | 48.7 | 22.4 | 3.8 | 26.6 | 4.7 | RVM | RVM
J1909+0007 | 32.3 | 1277 | 71.6 | 2.2 | 2.4 | 6.2 | 3.9 | non–RVM | No poln
J1909+1102 | 33.7 | 1053 | 62.1 | 30.4 | –14.7 | 35.7 | –18.5 | non–RVM | RVM
J1910+0358 | 31.1 | 1033 | 94.5 | 26.3 | –11.6 | 36.8 | –11.4 | non–RVM | RVM
J1912+2104 | 31.6 | 1029 | 74.6 | 39.8 | –11.3 | 38.7 | –8.5 | RVM | RVM
Table 2: Results for 249 pulsars (continued) JNAME | log($\dot{E}$) | $N_{p}$ | $N_{f}$ | $\%L_{t}$ | $\%V_{t}$ | $\%L_{s}$ | $\%V_{s}$ | Old Class | New Class
---|---|---|---|---|---|---|---|---|---
J1913–0440 | 32.5 | 1053 | 100.0 | 14.8 | –1.1 | 21.4 | –1.1 | non–RVM | RVM
J1914+0219 | 32.6 | 1046 | 80.0 | 43.1 | –3.1 | 44.5 | 0.1 | RVM | RVM
J1915+0738 | 31.6 | 1033 | 39.8 | 37.1 | –18.7 | 40.7 | –17.5 | RVM | No poln
J1917+1353 | 34.6 | 1058 | 99.9 | 48.5 | –8.6 | 48.4 | –8.3 | RVM | RVM
J1919+0021 | 32.2 | 1037 | 73.3 | 16.4 | 5.5 | 25.1 | 5.9 | non–RVM | No poln
J1919+0134 | 30.7 | 1033 | 92.9 | 28.1 | –9.4 | 40.2 | –9.6 | non–RVM | RVM
J1921+1948 | 31.8 | 1034 | 85.5 | 13.6 | –2.7 | 17.0 | –6.7 | non–RVM | No poln
J1921+2153 | 31.3 | 1030 | 100.0 | 10.2 | 1.6 | 24.4 | 1.7 | non–RVM | RVM
J1926+0431 | 31.9 | 558 | 69.2 | 12.5 | 1.1 | 36.1 | 0.9 | non–RVM | RVM
J1932+1059 | 33.6 | 1033 | 100.0 | 75.6 | –2.7 | 81.5 | –3.3 | RVM | RVM
J1935+1616 | 33.7 | 1033 | 100.0 | 22.4 | –0.8 | 27.2 | –0.0 | non–RVM | RVM
J1941–2602 | 32.8 | 1067 | 78.2 | 50.6 | –12.4 | 71.4 | –13.3 | non–RVM | RVM
J1943–1237 | 31.9 | 1046 | 63.5 | 12.3 | –2.4 | 26.1 | –2.1 | RVM | No poln
J1945–0040 | 31.3 | 1147 | 86.1 | 15.9 | 7.0 | 22.3 | 7.9 | non–RVM | No poln
J1946+1805 | 31.0 | 1042 | 40.1 | 37.4 | –6.6 | 43.9 | –6.9 | flat | flat
J1946–2913 | 31.8 | 1035 | 73.7 | 5.8 | 3.5 | 12.6 | 2.8 | non–RVM | No poln
J2006–0807 | 31.0 | 1051 | 53.3 | 47.6 | 2.9 | 49.0 | 2.8 | non–RVM | non–RVM$\dagger$
J2037+1942 | 31.0 | 520 | 58.6 | 18.3 | –1.3 | 25.5 | –1.6 | non–RVM | No poln
J2046+1540 | 30.7 | 1035 | 63.8 | 19.8 | 1.9 | 29.5 | –4.7 | non–RVM | No poln
J2046–0421 | 31.2 | 1036 | 99.7 | 7.2 | –12.8 | 28.0 | –11.0 | non–RVM | No poln
J2048–1616 | 31.8 | 1036 | 89.5 | 41.0 | 3.9 | 47.8 | 4.2 | RVM | RVM
J2053–7200 | 32.3 | 1040 | 98.8 | 29.1 | –6.1 | 36.0 | –3.7 | non–RVM | RVM
J2136–1606 | 29.5 | 1044 | 45.7 | 7.6 | 8.9 | 13.2 | 10.8 | non–RVM | No poln
J2139+2242 | 31.6 | 1030 | 99.5 | 35.6 | –0.9 | 41.9 | –0.3 | RVM | RVM
J2144–3933 | 28.5 | 519 | 99.0 | 27.4 | 4.0 | 27.8 | 2.7 | non–RVM | No poln
J2215+1538 | 33.3 | 1077 | 99.6 | 34.9 | –0.5 | 46.3 | –0.2 | RVM | RVM
J2253+1516 | 30.7 | 1063 | 42.6 | 17.1 | –4.7 | 31.6 | –3.5 | non–RVM | No poln
J2307+2225 | 30.3 | 1029 | 83.4 | 22.0 | 3.5 | 29.9 | 1.6 | flat | flat
J2330–2005 | 31.6 | 1036 | 83.1 | 17.1 | –8.3 | 28.4 | –7.7 | non–RVM | non–RVM
J2346–0609 | 31.5 | 1033 | 70.6 | 46.5 | 11.4 | 49.6 | 10.5 | RVM | RVM