PSR J1926-0652: A Pulsar with Interesting Emission Properties Discovered at FAST

We describe PSR J1926-0652, a pulsar recently discovered with the Five-hundred-meter Aperture Spherical radio Telescope (FAST). Using sensitive single-pulse detections from FAST and long-term timing observations from the Parkes 64-m radio telescope, we probed phenomena on both long and short time scales. The FAST observations covered a wide frequency range from 270 to 800 MHz, enabling individual pulses to be studied in detail. The pulsar exhibits at least four profile components, short-term nulling lasting from 4 to 450 pulses, complex subpulse drifting behaviours and intermittency on scales of tens of minutes. While the average band spacing P3 is relatively constant across different bursts and components, significant variations in the separation of adjacent bands are seen, especially near the beginning and end of a burst. Band shapes and slopes are quite variable, especially for the trailing components and for the shorter bursts. We show that for each burst the last detectable pulse prior to emission ceasing has different properties compared to other pulses. These complexities pose challenges for the classic carousel-type models.


Introduction
This work made use of the data from the FAST telescope (Five-hundredmeter Aperture Spherical radio Telescope). FAST is a Chinese national mega-science facility built and operated by the National Astronomical Observatories, Chinese Academy of Sciences. Located in southern China, it is the world's largest single-dish radio telescope. Between 2017 August and 2018 February, FAST carried out drift-scan observations using an ultra-wide-bandwidth receiver (UWB) to search for radio pulsars. Before the removal of this UWB in 2018 May (it was installed primarily for commissioning projects), 60 pulsar candidates had been obtained, with 44 of these already confirmed either by further FAST observations or using the Parkes 64 m or Effelsberg 100 m radio telescopes. The survey strategy and the full collection of new discoveries will be published elsewhere, with a brief summary currently available on the Commensal Radio Astronomy FAST survey website 11 and in Qian et al. (2019).
In this paper, we report the discovery of PSRJ1926−0652, which has an ∼1.6 s pulse period. The pulsar was discovered using a single-pulse search pipeline (Zhu et al. 2014) that was applied to observations taken in 2017 August. The pulsar was independently confirmed using the Parkes radio telescope in 2017 October. We have continued observations with both FAST and Parkes and, as described in this paper, show that PSRJ1926 −0652 exhibits a wide-range of emission phenomena.
Most pulsars have been discovered through the detection of their regular pulsed signal. However, soon after the discovery of pulsars it was found that the pulsed emission is seldom completely stable. For example, individual pulses may be significantly stronger than their mean. This led to the development of searches for pulsars through the detection of individual bursts (e.g., McLaughlin et al. 2006) and to the single-pulse search pipelines as used for our discovery.
With sufficiently sensitive telescopes, many pulsars can be shown to have mean pulse profiles formed from subpulses that drift in pulse phase in successive pulses. This phenomenon is known as subpulse drifting and was first reported by Drake & Craft (1968). The subpulse drifting phenomena is often described with a "carousel model" in which a ring of source regions systematically rotates about the magnetic axis (Ruderman & Sutherland 1975). We now know that at least one-third of pulsars exhibit subpulse drifting (Weltevrede et al. 2006a). Various algorithms have been developed to quantify the subpulse drifting. For instance, Edwards & Stappers (2003) show how a two-dimensional fluctuation spectrum (2DFS) can be used to determine the period of the subpulses in both pulse phase (known as P 2 ) and as pulse number (P 3 , measured in time). They noted that observational results indicated that P 2 does not change as a function of observing epoch and P 3 does not change with pulse longitude. The drift rate or slope of a subpulse band, is conventionally defined as Δf=P 2 /P 3 .
Several pulsars that exhibit complex patterns in their drifting subbands are now known. For instance, Qiao et al. (2004) describe a complex model for the "bi-drifting" phenomenon seen in PSRJ0815+09. The observing-frequency-dependence of subpulse drifting has also been studied. For example, Taylor et al. (1975) and Wolszczan et al. (1981) showed that, for PSR B0031−07 and PSR B0809+74, P 2 varied with frequency approximately as ν −0.25 , similar to the dependence expected for radius-to-frequency mapping in polar-cap models of the pulsar emission (Cordes 1978).
The pulsed emission from some pulsars has also been observed to switch off suddenly. This phenomena, known as "nulling" was first reported by Backer (1970). Nulling is relatively common, particularly in long period pulsars (Rankin 1986). For instance, 43 out of 72 well-observed pulsars were found by Biggs (1992) to exhibit evidence for nulling. The duration of null events varies widely. In some cases, one or a few pulses may be missing, whereas in other cases the emission may be undetectable for hours, days, or in extreme cases, months and years. The "null fraction" (NF), the fraction of time that the pulsar is in a null state, can range from close to zero (e.g., PSR B1737+13; Biggs 1992) to more than 90% (Wang et al. 2007). Pulsars that switch off for very long periods (on scales of hours to years) are often termed "intermittent pulsars." Kramer et al. (2006) studied one such pulsar, PSRB1931+24, and showed that the pulsar's slow-down rate is reduced when the pulsar is in its null state. This was explained as a change in magnetospheric currents. Some pulsars are also known to switch between multiple discrete profile states. This is known as "mode changing." Wang et al. (2007) and Lyne et al. (2010) suggested that mode changing and nulling are related phenomena and differ only in the magnitude of the changes in the magnetospheric current flows. A few papers have described studies that explore how the nulling and drifting phenomena may be linked. For instance, Gajjar et al. (2017) studied PSRsJ1741−0840 and J1840 −0840. They reported that for PSRJ1840−0840 the pulsar tended (but not always) to start nulling after the end of a driftband. When PSRJ1840−0840 then switched back on, it typically started at the beginning of a new driftband in both of its profile components.
Long-term monitoring of a pulsar provides information on the spin-down of the pulsar and long timescale intermittent behavior. Such monitoring also provides high signal-to-noise ratio (S/N), polarization-calibrated, average pulse profiles that can be used to determine the emission geometry of the system. The single pulse observations provide information on the nulling and drifting phenomena. Together, these results (for instance, as in Rankin & Wright 2008) can be used to search for the elusive physical model that will link these emission phenomena.
The pulsar that we describe in this paper, PSRJ1926−0652, has multiple pulse profile components and exhibits both subpulse drifting and nulling on various timescales. The paper is organized as follows. In Section 2, we describe our observations of PSRJ1926−0652. In Section 3, we present our analysis of the individual pulses. In Section 4, we describe the long-term behavior and the timing solution, and analyze the polarization and flux-density properties of the average pulse profile. We discuss our results in Section 5 and conclude the paper in Section 6.

Observations
We have carried out observations of PSRJ1926−0652 with both the FAST and Parkes radio telescopes. FAST, which is still being commissioned, has a large collecting area allowing us to observe single pulses from PSRJ1926−0652. The Parkes telescope is not sensitive enough to detect single pulses from this pulsar, but can be accurately calibrated and has been used to measure the polarization properties of the pulsar, as well as to carry out long-term monitoring.

Observation of Single Pulses
We observed PSRJ1926−0652 for ∼50 minutes using FAST on 2017 November 28th (corresponding to a MJD 58085) using a wide-bandwidth receiver covering from 270 MHz to 1.6 GHz. For most of the early FAST commissioning data, including the observation presented here, only one of the two linear polarization signal paths was reliable and the pulsar was only detectable in the low-frequency band. 12 We therefore only make use of the low frequency (270-800 MHz) band with the single available polarization channel. The lack of complete polarization information limits the scope of our single-pulse analysis. We have therefore focused our analysis on the detectable variations in flux density and in pulse phase. During the observation we recorded a total of 1921 single pulses with a time resolution of 100 μs. We subsequently extracted individual pulses 13 with 512 phase bins per pulse period using the DSPSR program (van Straten & Bailes 2011).

Monitoring Observations
The Parkes telescope continues to be used for regular timing observations of PSRJ1926−0652 in the 20 cm (1400 MHz) observing band with the central beam of the 13-beam receiver (Staveley-Smith et al. 1996). We have obtained 35 observations of this pulsar between 2017 October 8 (MJD 58034) and 2018 September 26 (MJD 58387). Integration times are typically 1 hr and the observations are divided into 30 s time segments (known as "subintegrations"). The bandwidth used was 256 MHz, which was divided into 1024 frequency channels and 1024 phase bins were formed across the profile using the Parkes Digital Filterbank Mark 4. In order to obtain highquality flux density and polarization calibration solutions, each observation was preceded by observation of a switched calibration noise source.
We processed the data using the PSRCHIVE software suite (Hotan et al. 2004). Aliased signals and narrowband radio frequency interference (RFI) were removed by giving zero 12 It is currently unclear whether this was because the pointing position was inaccurate or whether the telescope efficiency was low in the higher band during these observations. 13 Note that this requires the use of the -K option. weight to channels within 5% of the band edge and those with a level substantially above a median-smoothed bandpass. PSRJ1926−0652 was clearly detected in 29 observations and was undetected on the other six occasions. Since there is no perceptible worsening of RFI conditions in those six epochs, the nondetection is probably due to nulling. The length of observing time for the six nondetections were 11.5 minutes, 9 minutes, 17.5 minutes, 64 minutes, 55.5 minutes, and 72 minutes. To convert the measured intensity from the Parkes telescope observations to absolute flux density, we made use of observations of the radio galaxy 3C 218 (Hydra A; Baasr et al. 1977, see also Xie et al. 2019) that are taken every few weeks to support the Parkes Pulsar Timing Array project (Manchester et al. 2013). This allowed us to determine the effective flux density of the calibration noise source and consequently an absolute flux scale.
These long-term observations allowed us to model the rotation of the pulsar (see Section 4.1) to produce a high S/N average pulse profile enabling determination of the polarization properties and the flux density of the pulsar (Section 4.2) and determine the long-term on-off timescale for the pulse emission (Section 4.3).
The raw and processed data sets described in this paper are available online. See Appendix A for details.

The Single-pulse Emission
A "pulse stack" is an array of consecutive pulses with pulse phase on the x axis and increasing pulse number on the y axis. The upper panel in Figure 1 shows the entire pulse stack obtained using the FAST single-pulse data set across the frequency band from 270 to 800 MHz with the single available polarization channel. 14 The average profile is shown in the lower panel. This profile and pulse stack has been obtained after summing in frequency over the entire band (from 270 to 800 MHz).
We have labeled the regions in which the emission is "on" in the pulse stack as Bursts 1 to 6. We show these on-states in more detail in the six panels of Figure 2. The average pulse profile from each of these bursts is shown in the lower section of each panel overlaid on the mean pulse profile for the whole observation. Various emission phenomena are seen in these panels including multiple profile components, subpulse drifting, and nulling.
The average pulse profile consists of two main components (labeled as C1 and C4 in the lower panel of Figure 1). An inspection of Figure 2 shows at least two extra components. A weak component to the right of C1 is seen in several bursts (we label this component C2) and similarly, a weak component to the left of C4 leads to the "bump" in the average profile that we have labeled C3. See Appendix B.1 for details. Between these components there is a bridge region of emission.
Over the wide observed FAST band (270 to 800 MHz) we expect to see pulse shape evolution relating to intrinsic profile changes, emission arising from different positions in the magnetosphere and interstellar-medium effects. Figure 3 shows mean pulse profiles for three subbands across this observed bandwidth. It is clear that, as the observing frequency increases, the component separation decreases-pulse widths at 50% of the peak amplitude for the low and high frequency bands are given in Table 1. The reduction in profile width as a function of frequency is well-known in the general pulsar population and is usually attributed to radius-to-frequency mapping (Cordes 1978).
As Figures 1 and 2 show, the observed burst durations cover a wide range. It could be argued that Burst 5 is in fact two bursts, 5a and 5b, separated by a null of four pulse periods. Given this, the burst durations range from 17 pulse periods for Burst 5a to 300 pulse periods for Burst 3. 15 The null durations are also highly variable and range from four to more than 450 pulse periods. The pulsar is in a null state about 75% of the time, but this NF is quite uncertain because of the limited number of bursts observed.
One striking property of the emission is that during the longest burst event, Burst 3, the leading components drift later in phase, with the separation of C1/C2 from C3/C4 decreasing through the burst. This is most easily seen in Figure 1. Similar behavior may be occurring in other bursts, but this is not certain. It appears that the phase of components C1/C2 resets to the same starting value for each burst. Longer data sets are needed to confirm this property and to investigate it in more detail. Figure 2 shows that the slopes of drift bands vary substantially from band to band within a burst, between bursts, and for the two main components, C1 and C4. To make this quantitative, we have fitted a single Gaussian to the intensity of each subpulse group representing a given drift band in each pulse. We then do a weighted fit of a straight line to the centroid phase of the fitted Gaussians for a given drift band to measure the drift rate or band slope Δf=P 2 /P 3 , and its uncertainty. Note that, with this definition, Δfis zero for a vertical band in a stack plot. Histograms of the band slopes for components C1 and C4 for Burst 3 and for all other bursts combined are given in Figure 4. The fitted centroid points and linear fits to these points are shown in Figure 5 for Burst 3.
These histograms confirm that observed band slopes or subpulse drift rates are quite variable, especially for the shorter bursts, and are systematically different for components C1 and C4. Positive drift rates are seen only in the short bursts, specifically Bursts 4, 5a, and 6.
To further investigate the characteristics of the drifting subpulses in PSR J1926−0652, we undertook a Fourier analysis of the longest burst, Burst 3, which also has the most regular drifting. The frequency (or equivalently P 3 modulation period), phase, and amplitude of a cosine function were fitted to the pulse intensities across the burst for each pulse phase bin. Pulse 770, near the center of the burst and at the boundary of the two panels in Figure 5, was adopted as the reference time, t 0 , for the cosine fit. Figure 6 shows the variations of P 3 across the leading and trailing components. The weighted mean values of P 3 (averaged between the vertical dashed lines in Figure 6) are (17.35±0.04)P and (17.31±0.03) P for the leading and trailing components, respectively. The difference between these values is of marginal significance, so we adopt a mean P 3 of (17.33±0.03)P for the whole profile.
Using this mean P 3 value, we fit for the cosine phase at t 0 across the leading and trailing components. For the drift band closest to the reference time t 0 , the time of the cosine maximum for a given pulse phase bin is given by: f 0 is phase of the modulation at t 0 , and t 0 and t max are expressed in units of pulse period. 16 Figure 5 shows the locus of the peak of the cosine function as a function of pulse phase for both the leading and trailing components. The locus of the modulation peak was then replicated for all drift bands in the burst using the same mean value of P 3 for both the leading and trailing components. The rate of Fourier phase drift is fairly stable through the main C1 and C4 components, about −1°.35/P and −1°.95/P, respectively. Given the mean P 3 value, these slopes correspond to P 2 =−23°and −34°respectively, with an uncertainty of about 1°. However, the drift rate is quite nonlinear across each component, appearing to flatten toward the component edges. Furthermore, the modulation phases of the inner Components 2 and 3 do not lie on the extrapolation of the phase variations in the main components. The modulation phases of the main components also differ, with Component 4 reaching its maximum  Profile parameters: Mean flux density at 1400 MHz (mJy) 0.9(2) 50% pulse width at 1400 MHz (°) 45.0(4) 50% pulse width at 700 MHz b (°) 48.6(7) 50% pulse width at 350 MHz b (°) 56.1 (7) Polarization parameters at 1400 MHz: Long-term emission-state parameters: Longest "on" duration (min.) 20 Mean "on" duration (min.) 5.9 Standard Deviation "on" duration (min.) 3.6 Longest "off" duration (min.) Notes. Uncertainties in parentheses refer to the last quoted digit. All the parameters, apart from those indicated, were obtained from the Parkes Observations. a Derived from the Yao et al. (2017) model. b Derived from the FAST observation. 16 Note that for a band drifting toward earlier pulse phases (as in this case) the Fourier (P 3 ) phase at t 0 is an increasing function of pulse phase. The minus sign in Equation (1) then implies that the slope of the drift bands and hence P 2 are negative for this pulsar. This Fourier phase convention is opposite to that adopted by Weltevrede (2016) although the convention on the sign of P 2 is the same.
amplitude about 90°in modulation phase (i.e., 0.25P 3 ) later than Component 1. This means that for most pulses there is emission in one or both components although there are pulses with no significant emission. These are not "nulls" in the usual sense, but just a consequence of the periodic modulations in the various components.
It is clear that the band slopes derived from the Fourier analysis are very different from those derived from the direct Gaussian fitting to the band profiles and illustrated in Figures 4 and 5. Since P 3 is relatively stable, this implies a similarly different distribution of the derived P 2 values. These results will be discussed further in Section 5. Estimates of P 2 and P 3 can also be obtained by computing fluctuation spectra. A description of such an analysis is provided in Appendix B.2, showing a consistent result.
Inspection of Figure 2 indicates that the trailing pulse components (C3 and C4) are always detectable in the last pulse before a null event, whereas the leading pulse components generally are not. In Figure 7 we plot the mean profile of the last active pulse (LAP) of each burst (taking Bursts 5a and 5b separately) and the mean pulse profile over all bursts. The LAP average profile is clearly dominated by the trailing components, although there is occasional emission for components 1 and 2, for example, in Burst 3. Within the uncertainties, the LAP emission for C3 and C4 has the same shape as the mean profile over all burst emission and a similar amplitude. To quantify the significance of the shape change we have carried out 500,000 trials in which we have summed seven randomly selected pulses (from the "on" or burst states) to form an integrated profile. The strength of the leading components relative to the trailing components was determined for each trial by calculating the area beneath the components using PSRSALSA (Weltevrede 2016). Out of the 500,000 trials, only one had a more extreme ratio than is observed in Figure 7 (0.154), thereby confirming that the weakness of the leading components in the LAP prior to a null is not a chance result. 17 The first detectable pulse of each burst is not systematically different from an average pulse, with two bursts starting with the leading component (e.g., Bursts 5a and 5b), one with the trailing component (Burst 4) and two with both components starting at the same time (Bursts 3 and 6).

Timing Solution
Timing residuals were formed using the long-term Parkes monitoring observations. We used the TEMPO2 (Hobbs et al. 2006) software package using the DE421 solar system ephemeris and the TT(TAI) time standard to obtain a phaseconnected timing solution extending over 353 days. The timing residuals are shown in Figure 8. The nulling timescale is too short to search for changes in the spin-down rate during such events and the pulse arrival times are modeled well using a very simple parameterization of the pulsar. The timing solution is presented in Table 1. We also present parameters derived from the timing parameters, including the DM-based distance estimate from the Yao et al. (2017) model for the Galactic free-electron distribution, the pulsar's characteristic age where P is the pulse period andṖ is its first time derivative) and a representative surface-dipole magnetic field strength ( =´Ḃ PP 3.2 10 s 19 Gauss) in the table. The mean flux density at 1400MHz, 0.9±0.2mJy, was calculated by using the PSRCHIVE routine PSRFLUX to give the flux density of each of the Parkes observations and then computing the mean and rms deviation of these values. The pulse widths are at 50% of the peak amplitude and were computed from the mean profiles for the Parkes and FAST observations.
We cross-correlated the pulse profile for each observation with our analytic template and inspected, by eye, the deviation from the scaled template and the observed profiles. We found no evidence for pulse shape changes and therefore have no evidence that this pulsar exhibits discrete pulse-shape states.

Polarization Properties and Flux Density
To probe the polarimetric properties of the pulsar and to measure the average on-state flux density in the 20 cm observing band from the Parkes observations, we selected subintegrations for observations in which emission was detected. Observations were aligned using the timing solution given in Table 1, and then summed to produce a calibrated profile of the pulsar in the 20 cm observing band using the PSRCHIVE software suite (Hotan et al. 2004). This summed profile was plotted using the PSRSALSA software package (Weltevrede 2016) and is shown in the left panel of Figure 9. We determined the rotation measure (RM) of the pulsar (RM = −55±3 rad m −2 ) using the RMFIT package.
The average profile is moderately linearly polarized (dashed curve in the upper left panel of Figure 9) with a fractional linear polarization of 30%±1%. As is commonly observed in "classic" double profiles (e.g., Lyne & Manchester 1988), the degree of linear polarization is low at the profile edges and high in the bridge region. There is little evidence for significant circular polarization (dotted curve in the top panel of the left plot of Figure 9). The position angle (PA) curve of the linear polarization is shown in the bottom panel of the left plot of Figure 9. Its shape can be fitted using the rotating vector model (RVM; Radhakrishnan & Cooke 1969). The fit is remarkably good, but the parameters are not well constrained. 18 In the right-hand panel of Figure 9 we show the reduced χ 2 values of the fit as a function of α and β. The magnetic inclination angle, Figure 4. Histograms of the observed subpulse drift rates or band slopes for all observed drift bands, separately for components C1 and C4. The bin width is the same for all histograms (0°. 2/P) and has been chosen to approximate the typical uncertainty in the measured band slopes. The vertical dashed lines mark zero drift rate.
α, is practically unconstrained and, from the RVM fit alone, we can only conclude that β<13°. We describe more constraints on these parameters in the discussion section.

Long-term, On-off Timescale
The Parkes observations, typically ∼1 hr in duration (but sometimes as long as ∼7 hr), show that the time period during which the emission remains on or off lasts for tens of minutes. Parameterizing the exact on-off timescale is nontrivial as the emission state may have only switched once during a given   observation (and so we have no prior information on how long it was on or off before or after the observation). Also some of the observations were affected by RFI, which was often so strong that we were unable to determine whether the emission switched states during the RFI. Our subintegration time is 30 s for the Parkes observations and so we assume that the emission remains on (or off) when RFI is affecting our data for less than four subintegrations (2 minutes). Similarly, calibration observations (lasting a couple of minutes) were carried out regularly through long observations of the pulsar and we assumed that the pulsar remained in a single state throughout those calibration observations. With these assumptions the maximum on-state duration is ∼20 minutes. The maximum off-state duration is ∼93 minutes. The distribution of on and off state durations are quantified statistically in Figure 10 and Table 1. 19

The Discovery of PSRJ1926-0652
PSRJ1926−0652 is a relatively bright pulsar and can be detected with the Parkes telescope within a few minutes. We therefore wished to understand why this pulsar had not been discovered by previous surveys. We checked the Parkes data archive (Hobbs et al. 2011) and downloaded previous search mode observations (that were not embargoed) that were observed at positions within 10 arcmin of the known pulsar position. We identified two observations, 20 each of 4.3 min duration, and searched for the pulsar usingPRESTO 21 (Ransom 2001). We did not detect the pulsar, but this is not surprising as we know PSRJ1926−0652 has a nulling fraction of ∼75% and an average off-state duration of 20 minutes. The "intermittency" (i.e., the on/off timescale) in the pulse emission timescales is similar to that seen in other pulsars such as PSRJ1717−4054 (Kerr et al. 2014;Young et al. 2015). Clearly it is likely that there are many such pulsars remaining to be discovered by repeated observations of the same sky position.

The Emission and Viewing Geometry
The pulse profile has two primary components (C1 and C4), two inner components (C2 and C3) and bridge emission. Various generic models for pulse profile shapes have been suggested including a core and one or more cones, randomly distributed patches or patchy cones (see, e.g., Karastergiou & Johnston 2007 for a review and an empirical model). Our work does not explicitly confirm, nor rule out, any particular model, but we note that the profile component separations decrease as expected for higher-frequency emission occurring lower in the pulsar magnetosphere. As shown in Section 4.2 the PA of the linear polarization is also remarkably well fitted by an RVM. However, the magnetic inclination angle, α, is unconstrained.
Following the description in Rookyard et al. (2015), further constraints on the viewing geometry can be obtained by making various assumptions. The relatively large width of the profile (taken to be 60°±5°based on the Parkes data) implies either that α is small, or that the emission comes from high up in the magnetosphere. This height can be constrained because the RVM inflection point occurs very close to the midpoint of the profile. Rookyard et al. (2015) considered how the inflection point can be delayed relative to the position of the fiducial plane. The upper limit of this delay for our data is only ∼15°, which implies an emission height lower than 5000 km. In Figure 9 we have identified values of α and β that can produce a pulse of the measured width. These are shown in the green areas and suggest that the magnetic axis is relatively aligned with the pulsar's rotation axis with α<55°.

The Subpulse Drifting and Nulling Phenomena
As Figures 1 and 2 clearly show, PSR J1926−0652 exhibits drifting subpulses. However, their properties are complex. The drifting is more regular in the longer bursts and, specifically for the longest Bursts 1 and 3, is more regular in the leading component C1, compared to the trailing component C4. Figure 5 shows that the modulation phases for the interior components C2 and C3 do not lie on the extrapolation of the band slopes for C1 and C4 respectively. The modulation phases shown in Figure 5 appear to smoothly join the inner C2, C3 components to the outer C1, C4 components, but this may be an artifact of the smoothing in time over the burst inherent in the Fourier analysis. There is no significant P 3 modulation for the bridge region between components C2 and C3.
As mentioned in Section 3, the band slopes obtained from the Gaussian fits to subpulse profiles and the Fourier analysis are systematically different, especially for the trailing component C4. This is most clearly illustrated in the longest burst, Burst 3 ( Figure 5). The Fourier band slopes tend to be flatter (larger absolute values) and, similarly, the derived P 2 values have larger absolute values. The reasons for this are not entirely obvious. The Fourier method averages over the whole burst, while the Gaussian fits are independent for each drift band. There are significant variations in band spacing (P 3 ) from band to band, especially at the beginning and end of the burst, where the actual drift band times differ substantially from the Fourier phase predictions assuming a constant P 3 . Additional band structures not described by the Fourier model exist, most notably the additional bands seen in C1 at pulse number 676 and in C4 at pulse number 661.
On the other hand, there is a degree of subjectivity involved in choosing the subpulse structures to fit with the Gaussian analysis. For example, it could be argued that there are independent double bands for C1 around pulse numbers 704 and 738. For C4, the drift structure is not so clear and the Fourier phases are evidently dominated by a few relatively flat bands, for example, around pulse numbers 655, 792, and 809. Both methods have their strengths but, unless the drift-band structure is very regular, they can give quite different results.
The carousel model, originally proposed by Ruderman & Sutherland (1975), is widely used to interpret drifting subpulses. In this model, emission is produced from a series of "sparks" that circulate at a fixed period around the magnetic axis. As these sparks rotate past the observer's line of sight, they give rise to the characteristic drifting subpulses seen in many pulsars.
PSR J1926−0652 has four profile components, each of which has distinct subpulse behavior. Four components would naturally arise if there is emission from a second, inner carousel of sparks. Within the uncertainties, all components share the same periodicity (P 3 ≈ 17.3P), suggesting that any such nested carousels are phase-locked in the sense that they have the same rotation period and the same number of sparks. Nested phase-locked carousels have been proposed previously, for example, to explain the drifting subpulses of PSRB0818 −41 (Bhattacharya et al. 2009).
However, for PSR J1926−0652 there are a number of features that do not fit naturally into such a carousel model. For example, there are significant variations in band spacing (P 3 ) between different drift bands for a given component. Also,  there are clear extra drift bands that are not part of the regular P 3 modulation.
Other models for drifting subpulses also exist. For instance, Gogoberidze et al. (2005) suggest the possibility that the drifting subpulses result from the modulation of radio emission by magnetospheric oscillations. Such resonances that beat with the rotation of the pulsar may provide more natural explanations than carousel models for apparently complex phenomena such as harmonically related drift rates as seen in, e.g., PSRsB0031−07 and B2016+28 (Taylor et al. 1975), variable and even reversing drift rates as seen in PSRB0826−34 (Gupta et al. 2004) or opposite drift directions in different pulse components such as those observed in PSRs J0815+0939 (Champion et al. 2005) and B1839−04 (Weltevrede 2016).
As described in Section 3, the first pulses observed after a nulling event are comparable to a typical on-state pulse. However, we have shown that the LAP prior to a nulling event are significantly different in that the leading component is significantly weaker than the trailing pulse components (Figure 7). The leading component could be weaker before a null as it fades away, but we see no evidence of such fading in our observation. In contrast we see relatively strong emission in this component at the end of Burst 3. A second possibility is that the nulling events occur when the leading component is at (or near) its weakest point in the modulation cycle. This is similar to that observed by Gajjar et al. (2017) for PSRJ1840 −0840, which consistently enters the null state at the end of a drift-band in one of its profile components. For PSRJ1926 −0652 we cannot make such a definitive statement as we do see clear emission in the leading component in the LAP for Burst 3. However, we will show below that the drift-rate seems to change near the end of this burst.
Our results add to the menagerie of interesting phenomena relating to nulling and subpulse drifting and show that there does not seem to be a single, simple connection between nulling and drifting. For instance, Deich et al. (1986) found, in PSRB1944+17, that null events were preceded by a decay in pulse intensity of around 50% over about three pulse periods. They also showed that, like PSRJ1926−0652, the LAP were quantitatively different in shape and more variable than other pulses. Similarly individual pulses from PSRJ1727−2739 show a decay in intensity before a null event (Wen et al. 2016). This pulsar also has two primary components and, like PSRJ1926−0652, the intensity of the leading component is weaker than the trailing component prior to a null event. In contrast to the pulsar described in this paper, the pulses immediately after a null event in PSRJ1727−2739 were also significantly different from typical pulses.
There is currently no single physical model that can explain all of these phenomena. Further observations that hopefully would capture even longer burst events will be needed to obtain a deeper understanding of this unusual pulsar and drifting and nulling in general.

Conclusions
We report here a pulsar discovery, namely PSRJ1926 −0652, from the FAST radio telescope. Largely through FAST single pulse studies, aided by follow-up timing observations made by the Parkes telescope, PSRJ1926−0652 is found to exhibit a plethora of emission phenomena, including nulling and subpulse drifting. Our main findings include the following: FAST continues to discover pulsars , including bright ones that were probably missed by previous searches because of their nulling properties. We thus expect this work to be just the first of many in reporting new noteworthy pulsars. For PSRJ1926−0652, we have only scratched the surface in terms of analyzing its emission mechanism. We have further observations planned with FAST to obtain more single pulse data sets and Parkes for continued timing and monitoring, particularly with the new ultra-wideband receiver. We will be able to calibrate future FAST data sets and therefore will be able to obtain high S/N single pulses that provide a more detailed insight into the single pulse emission mechanism.
Having a decl. close to zero, this pulsar can be observed by almost all of the major radio telescopes. PSRJ1926−0652 holds the potential to help provide a coherent picture for explaining complex nulling and subpulse drifting, that do not fit easily into the simple carousel model.

MPG-CAS Joint Project "Low-Frequency Gravitational Wave
Astronomy and Gravitational Physics in Space".
The Parkes radio telescope is part of the Australia Telescope National Facility, which is funded by the Australian Government for operation as a National Facility managed by CSIRO. Pulsar research at Jodrell Bank Centre for Astrophysics and Jodrell Bank Observatory is supported by a consolidated grant from the UK Science and Technology Facilities Council (STFC).

Appendix A Data Access
The raw data from the FAST telescope used in the singlepulse study in this paper are owned by the National Astronomical Observatories, Chinese Academy of Sciences, and are available from the corresponding author upon reasonable request. The observations from the Parkes telescopes have been obtained using project codes PX500 and PX501. Conditional on data embargoes, these data are available on CSIRO's data archive 22 (Hobbs et al. 2011). We note that observations of the pulsar currently in the archive were recorded under the source name PSRJ1926−0649 (instead of the correct name of PSR J1926−0652). The raw PX500 data have an 18 month embargo period, whereas the PX501 data have a 10-yr embargo period.
We have produced a publicly downloadable data collection available from the CSIRO's data archive containing our processed data files. This data collection contains (1) FAST single-pulse data for PSRJ1926−0652 in four different frequency bands and (2) Parkes timing data at 20 cm, including pulse arrival times, the arrival time file, the timing model file, the timing template file, and the calibrated and summed profiles. This data collection is available from CSIRO Data Access Portal (Zhang et al. 2018).

Appendix B Analysis Using PSRSALSA
The software tools used to conduct the P 3 −fold and fluctuation spectra analysis here are part of the PSRSALSA package (Weltevrede 2016), and are freely available online. 23 The single pulse data was folded at the identified period P 3 =17.33P, which was given in Section 3, using PSRSALSA for Burst 3 (the longest observed burst sequence). This folding results in a high S/N representation of the average driftband, and permits more detailed studies of weak features in the drifting behavior.
The P 3 -fold ( Figure 11) shows that the leading component has an associated average driftband that is relatively steep, while the trailing component shows a much shallower gradient. This is consistent with the measured P 2 value of the trailing component being larger. In addition, the figure reveals that there are two additional weak profile components with distinct drifting subpulse properties. The first of these two minor components (C2 as we described in the Section 3) can be associated with a small "tail" appearing around 170°p ulse longitude and pulse number ∼18. The second minor component (C3 as we described in the Section 3) around 195°pulse longitude appears in the P 3 -fold at pulse number ∼23.

B.2. Fluctuation Spectra Analysis
The longitude-resolved fluctuation spectrum (LRFS) presents the spectral power of fluctuations as a function of rotational phase. The power in the LRFS can be used to quantify the longitude-resolved modulation index, which is shown, for Burst 3, as the points with error bars in the top left panel of Figure 12, together with the pulse profile. More examples of such statistical analyses can be found in, e.g., Edwards & Stappers (2003) and Weltevrede et al. (2006aWeltevrede et al. ( , 2006b. The vertical frequency axis of both the LRFS and 2DFS corresponds to P/P 3 , where P denotes the rotational period of the pulsar. The LRFS shows a clear spectral feature at P/P 3 ;0.058 cycles per period (cpp) for both components. This spectral feature corresponds to the pattern repetition period of the drifting subpulses P 3 ;17P that can also be identified by eye in the pulse stack. In addition to this well-defined spectral feature, there are two weaker peaks for the leading component at ;0.067 cpp corresponding to P 3 ;15 P and at ;0.043 cpp corresponding to P 3 ;23 P (see in the top part of panel (b)) and one weaker peak for the trailing component at ;0.068 cpp corresponding to P 3 ;15 P (see in the bottom part of panel b). These results indicate variations in the P 3 parameter for Burst 3. The horizontal axis of the 2DFS denotes the pattern repetition frequency along the pulse longitude axis, expressed as P/P 2 . Following the description in Weltevrede et al. (2006b), we have measured the P 2 and P 3 for the well-defined spectral feature for the two components. This gives --+  P 29 2 2 3 deg and P 3 ;17±0.5 P for the leading component and --+  P 42 2 10 5 deg and P 3 ;17±0.5 P for the trailing component. We note that the quoted errors do not capture the fact that there is a high variability in the drift band shapes, and only a relatively small number of drift bands are observed. These results are consistent, but less accurate with our Fourier analysis result (17.35±0.04 P and 17.31±0.03 P for the leading and trailing components respectively), which was given in Section 3.