<figure><img src="image_10.png" /></figure>

**Figure 9.** Pulse profiles for the MSP PSR J0030+0451. Weighted LAT pulse profiles in different energy bands are shown in black. The pulse profiles above 10 GeV are in light gray, more apparent for other pulsars shown in Appendix B. The radio pulse profile for this pulsar at 1.4 GHz is shown in red, and a fit of the integrated gamma-ray pulse profile over 0.1 GeV is displayed in magenta when the *H*-test test significance exceeds 100. Horizontal blue lines correspond to the expected background levels in the gamma-ray pulse profiles, plus or minus one standard deviation. The quantities at the top left correspond to the weighted *H*-test TS for the LAT pulse profile shown in the top panel, and the total integration time. At top right are listed: the pulsar name, its rotational period and Galactic latitude, and the "PSR" and "CHAR" codes defined in the captions for Tables 2 and 3 (top row), the radio observatory used to acquire the radio profile (if available), and the corresponding radio frequency (second row). For pulsars with radio profiles, a marker at the top right indicates the phase alignment uncertainty stemming from the DM. See Section 5 for more details about light-curve construction and the fitting procedure.

(The complete figure set (294 images) is available.)
<figure><img src="image_11.png" /></figure>

**Figure 9.** Pulse profiles for the MSP PSR J0030+0451. Weighted LAT pulse profiles in different energy bands are shown in black. The pulse profiles above 10 GeV are in light gray, more apparent for other pulsars shown in Appendix B. The radio pulse profile for this pulsar at 1.4 GHz is shown in red, and a fit of the integrated gamma-ray pulse profile over 0.1 GeV is displayed in magenta when the *H*-test test significance exceeds 100. Horizontal blue lines correspond to the expected background levels in the gamma-ray pulse profiles, plus or minus one standard deviation. The quantities at the top left correspond to the weighted *H*-test TS for the LAT pulse profile shown in the top panel, and the total integration time. At top right are listed: the pulsar name, its rotational period and Galactic latitude, and the "PSR" and "CHAR" codes defined in the captions for Tables 2 and 3 (top row), the radio observatory used to acquire the radio profile (if available), and the corresponding radio frequency (second row). For pulsars with radio profiles, a marker at the top right indicates the phase alignment uncertainty stemming from the DM. See Section 5 for more details about light-curve construction and the fitting procedure.

(The complete figure set (294 images) is available.)
Table 8 lists a single MSP with well-measured $\mu$ but $(1 - \xi) < 0$, implying implausible spin-up, $\dot{E}^{\text{int}} < 0$. It is PSR J1024-0719, with a binary companion in an atypical multi-century orbit that leads to mismeasured $\dot{P}^{\text{int}}$ (Bassa et al. 2016b; Guillemot et al. 2016; Kaplan et al. 2016). Six other MSPs have $\dot{E}^{\text{int}} \lesssim 2 \times 10^{33} \text{ erg s}^{-1}$, some with nominally small uncertainties. The lowest is $\dot{E}^{\text{int}} = 9_{-8}^{+21} \times 10^{32} \text{ erg s}^{-1}$ for PSR J1946+3417. Improved precision and a larger sample will clarify the gamma-ray “deathline” for MSPs, below which emission in the LAT range ceases. A useful tool to understand the uncertainty on $\dot{E}^{\text{int}}$ are plots of $\mu$ versus $d$ showing the constraints suggested by the neutron star’s transverse velocity $v_T = \mu d$, minimum $\dot{E}^{\text{int}}$, and so on. A powerful constraint is to require $\dot{E}^{\text{int}} > L_\gamma$ (Section 6.7 addresses luminosity $L_\gamma$). Examples of $\mu$ versus $d$ plots, or similar, are Figure 11 in 2PC (which includes PSR J1024-0719), Figure 1 in Guillemot et al. (2016), and Figure 4 in Clark et al. (2018).

# 5. Light Curves and Profile Characterization

## 5.1. Gamma-Ray and Radio Light Curves

Figure 9 shows an example of gamma-ray light curves in different energy bands for the MSP PSR J0030+0451. All 294 sources are available in the Figure Set. Figure 4 shows further examples, overlaid with radio profiles when available.

After preparation according to Section 2, the photon arrival times were converted to rotational phase using timing models obtained from pulsar timing observations conducted in radio or X-rays, or by direct timing of the LAT photons, as described in Section 3. In a number of cases, the timing models' validity interval only partially overlapped with the time range of the LAT data set. To avoid contaminating off-pulse phase regions by extrapolating inaccurate models, we restricted the LAT data sets to the validity intervals in the cases of (1) timing solutions containing high-order (≥3) frequency derivatives suggestive of strong timing noise; (2) “IFUNC” or “WAVE” terms (also used to mitigate timing noise); or (3) “ORBIFUNC” or high-order (≥2) orbital frequency derivatives for pulsars in binary systems, or black-widow pulsars that are often subject to timing instabilities. For other objects, generally stable MSPs, all LAT photons were used, and we checked that the pulse phases do not drift outside the ephemeris validity intervals (see Figure 4). Additionally, we conservatively excluded 10 days of data before and after pulsar glitch epochs, to avoid contamination of off-pulse phase intervals caused by imperfect glitch modeling. At the top of all of the plots like Figure 9, $t_{\text{int}}$ gives the number of years of LAT data retained.

Pulse profiles as in Figures 4 and 9 were generated by computing histograms of the rotational phases $\phi_j$, weighted by the photon weights $w_j$. The weighted phase histograms repeat over two pulsar rotations to clarify structures near phase 0. The uncertainty for the $i$th histogram bin containing $N_i$ photons was calculated as $\sigma_i^2 = \sum_{j=1}^N w_j^2 + (\max_{j \in \{1, N_i\}} w_j)^2$. The first term is the sample variance, while the second term adds in quadrature the maximum possible variance for a bin with one photon. This is an ad hoc correction for bins with few counts, where by chance the observed sample variance may be far below the typical value: this prescription provides more realistic error bars than those used in 2PC. The number of bins in the weighted histograms was chosen based on the H-test TS above 0.1 GeV: 25 bins for pulsars with $H < 100$, 50 bins

when $100 \le H < 1000$, 100 bins when $1000 \le H < 10,000$, and so on.

Dashed horizontal lines in the figures show the background contribution from neighboring point sources and from diffuse emission. As in 2PC, it was estimated as $b = (\sum_{j=1}^N w_j - \sum_{j=1}^N w_j^2)/N_{\text{bin}}$ where N is the number of sources, excluding the pulsar, and $N_{\text{bin}}$ is the number of histogram bins. The background uncertainty is dominated by systematic errors in the diffuse background normalization, estimated by changing the background normalization by ±6%, also shown as the dashed horizontal lines. A pulsar wind nebula (PWN) may surround the pulsar, but with a power-law spectrum extending to high energies. If omitted from the source model, it appears as an excess above background, especially at higher energies. Section 6.2 lists the pulsars for which we added a PWN component to our source model, in addition to the Crab and Vela. 2PC describes a search for off-pulse emission, which measured off-pulse spectra for pulsars with an excess above the background level.

For gamma-ray pulsars with no radio emission, we rotated the pulse profiles such that the phase of the first emission component (as determined from the light-curve fit above 0.1 GeV, described in the next section) is at phase 0.1 (see the profile for PSR J0007+7307 in Figure 9.2 available online for an example). When radio profiles are available, a radio fiducial phase at infinite frequency was determined (see below) and placed at phase 0. The gamma-ray light curves were rotated accordingly, to preserve the relative radio/gamma-ray phase offset, including DM delays (see Section 4.2). We determined the uncertainty on the radio/gamma-ray phase offset stemming from the DM uncertainty neglecting DM time-derivative terms, and show it in the figures with a horizontal error bar at the top-right. Figure 9.104 for PSR J1311-3430 available online shows a case where a large DM uncertainty leads to a large relative phase uncertainty. For some pulsars, the DM and its uncertainty were not determined during the radio timing analysis; for these objects we used external DM information, generally from the ATNF pulsar catalog or separate analyses. Those cases are highlighted with a marker underneath the phasing error bar, as illustrated in Figure 9.285 available online showing the pulse profile for PSR J2229+6114. In a very few other cases, the radio data analysis did not yield the information necessary to determine the relative radio/gamma-ray phase offset. For these light curves, we indicated the arbitrary relative phase offset with a \* symbol.

Identifying the “fiducial phase” at which the magnetic pole of the neutron star crosses the line of sight is of interest. For some pulsars, this can be inferred from radio polarimetry via the rotating vector model (RVM; Radhakrishnan & Cooke 1969), but we do not consider such models here. As noted in 2PC, for pulsars with a single, symmetric radio peak, the peak maximum can be chosen as an estimator for the fiducial phase. However, many radio profiles in our sample do not consist simply of single, symmetric peaks, so that the choice of the fiducial phase is not always trivial. We adopted the following “Gaussian smoothing” approach, which reduces complex emission structures by replacing them with the best-fitting Gaussian equivalent. Each radio profile was inspected visually, and one peak or peak complex was chosen as the phase reference. This reference peak or set of peaks was then fitted with a single asymmetric Gaussian curve, or with two asymmetric Gaussian curves, depending on the morphology.
Table 8 lists a single MSP with well-measured $\mu$ but $(1 - \xi) < 0$, implying implausible spin-up, $\dot{E}^{\text{int}} < 0$. It is PSR J1024-0719, with a binary companion in an atypical multi-century orbit that leads to mismeasured $\dot{P}^{\text{int}}$ (Bassa et al. 2016b; Guillemot et al. 2016; Kaplan et al. 2016). Six other MSPs have $\dot{E}^{\text{int}} \lesssim 2 \times 10^{33} \text{ erg s}^{-1}$, some with nominally small uncertainties. The lowest is $\dot{E}^{\text{int}} = 9_{-8}^{+21} \times 10^{32} \text{ erg s}^{-1}$ for PSR J1946+3417. Improved precision and a larger sample will clarify the gamma-ray “deathline” for MSPs, below which emission in the LAT range ceases. A useful tool to understand the uncertainty on $\dot{E}^{\text{int}}$ are plots of $\mu$ versus $d$ showing the constraints suggested by the neutron star’s transverse velocity $v_T = \mu d$, minimum $\dot{E}^{\text{int}}$, and so on. A powerful constraint is to require $\dot{E}^{\text{int}} > L_\gamma$ (Section 6.7 addresses luminosity $L_\gamma$). Examples of $\mu$ versus $d$ plots, or similar, are Figure 11 in 2PC (which includes PSR J1024-0719), Figure 1 in Guillemot et al. (2016), and Figure 4 in Clark et al. (2018).

# 5. Light Curves and Profile Characterization

## 5.1. Gamma-Ray and Radio Light Curves

Figure 9 shows an example of gamma-ray light curves in different energy bands for the MSP PSR J0030+0451. All 294 sources are available in the Figure Set. Figure 4 shows further examples, overlaid with radio profiles when available.

After preparation according to Section 2, the photon arrival times were converted to rotational phase using timing models obtained from pulsar timing observations conducted in radio or X-rays, or by direct timing of the LAT photons, as described in Section 3. In a number of cases, the timing models' validity interval only partially overlapped with the time range of the LAT data set. To avoid contaminating off-pulse phase regions by extrapolating inaccurate models, we restricted the LAT data sets to the validity intervals in the cases of (1) timing solutions containing high-order (≥3) frequency derivatives suggestive of strong timing noise; (2) “IFUNC” or “WAVE” terms (also used to mitigate timing noise); or (3) “ORBIFUNC” or high-order (≥2) orbital frequency derivatives for pulsars in binary systems, or black-widow pulsars that are often subject to timing instabilities. For other objects, generally stable MSPs, all LAT photons were used, and we checked that the pulse phases do not drift outside the ephemeris validity intervals (see Figure 4). Additionally, we conservatively excluded 10 days of data before and after pulsar glitch epochs, to avoid contamination of off-pulse phase intervals caused by imperfect glitch modeling. At the top of all of the plots like Figure 9, $t_{\text{int}}$ gives the number of years of LAT data retained.

Pulse profiles as in Figures 4 and 9 were generated by computing histograms of the rotational phases $\phi_j$, weighted by the photon weights $w_j$. The weighted phase histograms repeat over two pulsar rotations to clarify structures near phase 0. The uncertainty for the $i$th histogram bin containing $N_i$ photons was calculated as $\sigma_i^2 = \sum_{j=1}^N w_j^2 + (\max_{j \in \{1, N_i\}} w_j)^2$. The first term is the sample variance, while the second term adds in quadrature the maximum possible variance for a bin with one photon. This is an ad hoc correction for bins with few counts, where by chance the observed sample variance may be far below the typical value: this prescription provides more realistic error bars than those used in 2PC. The number of bins in the weighted histograms was chosen based on the H-test TS above 0.1 GeV: 25 bins for pulsars with $H < 100$, 50 bins

when $100 \le H < 1000$, 100 bins when $1000 \le H < 10,000$, and so on.

Dashed horizontal lines in the figures show the background contribution from neighboring point sources and from diffuse emission. As in 2PC, it was estimated as $b = (\sum_{j=1}^N w_j - \sum_{j=1}^N w_j^2)/N_{\text{bin}}$ where N is the number of sources, excluding the pulsar, and $N_{\text{bin}}$ is the number of histogram bins. The background uncertainty is dominated by systematic errors in the diffuse background normalization, estimated by changing the background normalization by ±6%, also shown as the dashed horizontal lines. A pulsar wind nebula (PWN) may surround the pulsar, but with a power-law spectrum extending to high energies. If omitted from the source model, it appears as an excess above background, especially at higher energies. Section 6.2 lists the pulsars for which we added a PWN component to our source model, in addition to the Crab and Vela. 2PC describes a search for off-pulse emission, which measured off-pulse spectra for pulsars with an excess above the background level.

For gamma-ray pulsars with no radio emission, we rotated the pulse profiles such that the phase of the first emission component (as determined from the light-curve fit above 0.1 GeV, described in the next section) is at phase 0.1 (see the profile for PSR J0007+7307 in Figure 9.2 available online for an example). When radio profiles are available, a radio fiducial phase at infinite frequency was determined (see below) and placed at phase 0. The gamma-ray light curves were rotated accordingly, to preserve the relative radio/gamma-ray phase offset, including DM delays (see Section 4.2). We determined the uncertainty on the radio/gamma-ray phase offset stemming from the DM uncertainty neglecting DM time-derivative terms, and show it in the figures with a horizontal error bar at the top-right. Figure 9.104 for PSR J1311-3430 available online shows a case where a large DM uncertainty leads to a large relative phase uncertainty. For some pulsars, the DM and its uncertainty were not determined during the radio timing analysis; for these objects we used external DM information, generally from the ATNF pulsar catalog or separate analyses. Those cases are highlighted with a marker underneath the phasing error bar, as illustrated in Figure 9.285 available online showing the pulse profile for PSR J2229+6114. In a very few other cases, the radio data analysis did not yield the information necessary to determine the relative radio/gamma-ray phase offset. For these light curves, we indicated the arbitrary relative phase offset with a * symbol.

Identifying the “fiducial phase” at which the magnetic pole of the neutron star crosses the line of sight is of interest. For some pulsars, this can be inferred from radio polarimetry via the rotating vector model (RVM; Radhakrishnan & Cooke 1969), but we do not consider such models here. As noted in 2PC, for pulsars with a single, symmetric radio peak, the peak maximum can be chosen as an estimator for the fiducial phase. However, many radio profiles in our sample do not consist simply of single, symmetric peaks, so that the choice of the fiducial phase is not always trivial. We adopted the following “Gaussian smoothing” approach, which reduces complex emission structures by replacing them with the best-fitting Gaussian equivalent. Each radio profile was inspected visually, and one peak or peak complex was chosen as the phase reference. This reference peak or set of peaks was then fitted with a single asymmetric Gaussian curve, or with two asymmetric Gaussian curves, depending on the morphology.
Single peaks or “patchy” profiles with more than two components were fitted with single asymmetric Gaussian functions. Peaks with two components at their edges were fitted with two asymmetric Gaussians. In the first case, the fiducial phase was simply defined as the best-fit peak phase, and in the second case, the fiducial phase was defined as the average of the two best-fit peak phase values.

While the above procedure for defining the radio fiducial phase works well in most cases, a number of radio profiles in the sample are too complex for the procedure to produce an estimate. We inspected the radio profiles and classified them into four categories:

1. radio profiles for which one can readily define one peak as the main peak, which has a simple, single, or double structure. The procedure for defining the radio fiducial phase should have produced robust results.

2. radio profiles for which one can readily define one peak as the main peak, whose structure is complex (i.e., patchy profiles). The procedure is believed to be robust.

3. one can define a radio peak as the main one, but cannot readily determine whether it is isolated, or part of a broader structure with other peaks. The radio fiducial phase estimate may not be robust for these objects.

4. the profile morphology is too complex for the fiducial phase to be unambiguously chosen, based on the profile alone.

The categories, or “radio classes,” assigned to the different pulsars are listed in Tables 9 and 10. The fiducial phases were finally placed at phase 0 in the radio and gamma-ray pulse profiles, and the gamma-ray phases were rotated accordingly.

### 5.2. Gamma-Ray Light-curve Fitting above 0.1 GeV

Fits of the LAT weighted histograms above 0.1 GeV are displayed in the Figures as magenta lines (see, e.g., Figure 9). We followed a similar approach as in 2PC for fitting the LAT pulse profiles, by representing the gamma-ray light curves as wrapped probability density functions (PDFs) of $\phi \in [0, 1)$, and constructing the PDFs for the individual pulsars as linear combinations of $N_{\text{peaks}}$ unimodal distributions:

$$f(\phi) = \sum_{i=1}^{N_{\text{peaks}}} n_i g_i(\phi) + \left(1 - \sum_{i=1}^{N_{\text{peaks}}} n_i\right). \quad (7)$$

In the above expression, $n_i$ terms represent normalization factors, and the $g_i$ terms represent individually normalized distributions, and the term in parentheses is a uniform distribution representing an unpulsed component. We chose to fit gamma-ray light-curve peaks using asymmetric Gaussian or Lorentzian distributions, wrapped onto a circle:

$$g(\phi) = \sum_{k=-\infty}^{+\infty} g'(\phi + k), \quad (8)$$

with $g'$ defined on the real line, and $k$ being an integer number of rotations. In practice, the sum needed to be truncated, and we summed phases over $[-N_{\text{rot}}, N_{\text{rot}} + 1]$ with $N_{\text{rot}} = 2$. The PDFs were defined as follows:

$$g'(\phi) = \frac{2}{\pi(\sigma_1 + \sigma_2)(1 + z^2)} \times (\text{Asymmetric Lorentzian}), \quad (9)$$

$$g'(\phi) = \sqrt{\frac{2}{\pi} \frac{\exp(-z^2/2)}{\sigma_1 + \sigma_2}} \quad (\text{Asymmetric Gaussian}), \quad (10)$$

with $z$ defined as $(\phi - \phi_0)/\sigma$, with $\phi_0$ the phase location of the peak and $\sigma = \sigma_1$ if $\phi < \phi_0$ and $\sigma = \sigma_2$ otherwise. Best-fit normalization, phase, and width parameters for each component were determined using maximum likelihood. The logarithm of the likelihood is defined as:

$$\log L = \sum_{j=1}^{N} \log [w_j f(\phi_j) + (1 - w_j)]. \quad (11)$$

The fit was carried out using the MultiNest Bayesian inference tool (Feroz et al. 2009). We fitted binned weighted histograms above 0.1 GeV with twice as many bins as displayed in the figures. In some cases, the width parameters converged toward the lower edge of the prior; in these cases, we doubled the number of phase bins for the fit. For each gamma-ray component in the pulse profiles, we tested the different PDFs and chose the one maximizing the log likelihood value. The number of gamma-ray components was determined by adding components at possible peak locations (based on visual inspection) and choosing the model that minimized the Bayesian information criterion (BIC). Pulse profile fits were carried out and plotted in the Figures for the 236 pulsars with H-test values above 100.

In most pulsars with more than two gamma-ray components, one can readily distinguish two “main” gamma-ray peaks at phases $\phi_1$ and $\phi_2$ whose separation is denoted as $\Delta = \phi_2 - \phi_1$. In an archetypal gamma-ray pulse profile such as for the Vela pulsar (PSR J0835-4510), a first main gamma-ray peak lags the radio emission peak by $\delta = \phi_1 - \phi_r \approx 0.1 - 0.2$ (where $\phi_r$ denotes the radio fiducial phase, as discussed previously, if radio emission is also detected), and a second main gamma-ray peak lags the first one by $\lesssim 0.5$ with emission between the peaks. However, in some cases, one cannot straightforwardly determine which of the gamma-ray peaks should be labeled as peak 1 and peak 2. Therefore, for each profile with more than one statistically significant emission component, we chose peak 1 and peak 2 based on similarity with the above-described prototype. Then, for each pulsar, we considered the following criteria:

1. $\delta < 0.5$,

2. $\Delta < 0.5$,

3. $\sigma_2 > \sigma_1$ for the first peak (i.e., is the first peak oriented toward the second one),

4. $\sigma_1 > \sigma_2$ for the second peak (i.e., is the second peak oriented toward the first one),

5. presence of statistically significant emission between the two main peaks,

and inspected those meeting fewer than four of the above criteria (i.e., pulse profiles that do not correspond to the “typical” Vela-like profile). In some of these cases, peak 1 and peak 2 were inverted based on visual inspection, and a number of objects were flagged as “uncertain.”

In addition to those cases where the ordering of the two main gamma-ray peaks is ambiguous, some other pulsars have “complex” pulse profiles in which the choice of the two main peaks is itself ambiguous, for various reasons. In an attempt to list these objects, we searched the best-fit pulse profiles for examples that contain at least one peak not overlapping with the two main peaks chosen from initial visual inspection, and
Single peaks or “patchy” profiles with more than two components were fitted with single asymmetric Gaussian functions. Peaks with two components at their edges were fitted with two asymmetric Gaussians. In the first case, the fiducial phase was simply defined as the best-fit peak phase, and in the second case, the fiducial phase was defined as the average of the two best-fit peak phase values.

While the above procedure for defining the radio fiducial phase works well in most cases, a number of radio profiles in the sample are too complex for the procedure to produce an estimate. We inspected the radio profiles and classified them into four categories:

1. radio profiles for which one can readily define one peak as the main peak, which has a simple, single, or double structure. The procedure for defining the radio fiducial phase should have produced robust results.

2. radio profiles for which one can readily define one peak as the main peak, whose structure is complex (i.e., patchy profiles). The procedure is believed to be robust.

3. one can define a radio peak as the main one, but cannot readily determine whether it is isolated, or part of a broader structure with other peaks. The radio fiducial phase estimate may not be robust for these objects.

4. the profile morphology is too complex for the fiducial phase to be unambiguously chosen, based on the profile alone.

The categories, or “radio classes,” assigned to the different pulsars are listed in Tables 9 and 10. The fiducial phases were finally placed at phase 0 in the radio and gamma-ray pulse profiles, and the gamma-ray phases were rotated accordingly.

### 5.2. Gamma-Ray Light-curve Fitting above 0.1 GeV

Fits of the LAT weighted histograms above 0.1 GeV are displayed in the Figures as magenta lines (see, e.g., Figure 9). We followed a similar approach as in 2PC for fitting the LAT pulse profiles, by representing the gamma-ray light curves as wrapped probability density functions (PDFs) of $\phi \in [0, 1)$, and constructing the PDFs for the individual pulsars as linear combinations of $N_{\text{peaks}}$ unimodal distributions:

$$f(\phi) = \sum_{i=1}^{N_{\text{peaks}}} n_i g_i(\phi) + \left(1 - \sum_{i=1}^{N_{\text{peaks}}} n_i\right). \quad (7)$$

In the above expression, $n_i$ terms represent normalization factors, and the $g_i$ terms represent individually normalized distributions, and the term in parentheses is a uniform distribution representing an unpulsed component. We chose to fit gamma-ray light-curve peaks using asymmetric Gaussian or Lorentzian distributions, wrapped onto a circle:

$$g(\phi) = \sum_{k=-\infty}^{+\infty} g'(\phi + k), \quad (8)$$

with $g'$ defined on the real line, and $k$ being an integer number of rotations. In practice, the sum needed to be truncated, and we summed phases over $[-N_{\text{rot}}, N_{\text{rot}} + 1]$ with $N_{\text{rot}} = 2$. The PDFs were defined as follows:

$$g'(\phi) = \frac{2}{\pi(\sigma_1 + \sigma_2)(1 + z^2)} \times (\text{Asymmetric Lorentzian}), \quad (9)$$

$$g'(\phi) = \sqrt{\frac{2}{\pi} \frac{\exp(-z^2/2)}{\sigma_1 + \sigma_2}} \quad (\text{Asymmetric Gaussian}), \quad (10)$$

with $z$ defined as $(\phi - \phi_0)/\sigma$, with $\phi_0$ the phase location of the peak and $\sigma = \sigma_1$ if $\phi < \phi_0$ and $\sigma = \sigma_2$ otherwise. Best-fit normalization, phase, and width parameters for each component were determined using maximum likelihood. The logarithm of the likelihood is defined as:

$$\log L = \sum_{j=1}^{N} \log [w_j f(\phi_j) + (1 - w_j)]. \quad (11)$$

The fit was carried out using the MultiNest Bayesian inference tool (Feroz et al. 2009). We fitted binned weighted histograms above 0.1 GeV with twice as many bins as displayed in the figures. In some cases, the width parameters converged toward the lower edge of the prior; in these cases, we doubled the number of phase bins for the fit. For each gamma-ray component in the pulse profiles, we tested the different PDFs and chose the one maximizing the log likelihood value. The number of gamma-ray components was determined by adding components at possible peak locations (based on visual inspection) and choosing the model that minimized the Bayesian information criterion (BIC). Pulse profile fits were carried out and plotted in the Figures for the 236 pulsars with H-test values above 100.

In most pulsars with more than two gamma-ray components, one can readily distinguish two “main” gamma-ray peaks at phases $\phi_1$ and $\phi_2$ whose separation is denoted as $\Delta = \phi_2 - \phi_1$. In an archetypal gamma-ray pulse profile such as for the Vela pulsar (PSR J0835-4510), a first main gamma-ray peak lags the radio emission peak by $\delta = \phi_1 - \phi_r \approx 0.1 - 0.2$ (where $\phi_r$ denotes the radio fiducial phase, as discussed previously, if radio emission is also detected), and a second main gamma-ray peak lags the first one by $\lesssim 0.5$ with emission between the peaks. However, in some cases, one cannot straightforwardly determine which of the gamma-ray peaks should be labeled as peak 1 and peak 2. Therefore, for each profile with more than one statistically significant emission component, we chose peak 1 and peak 2 based on similarity with the above-described archetype. Then, for each pulsar, we considered the following criteria:

1. $\delta < 0.5$,

2. $\Delta < 0.5$,

3. $\sigma_2 > \sigma_1$ for the first peak (i.e., is the first peak oriented toward the second one),

4. $\sigma_1 > \sigma_2$ for the second peak (i.e., is the second peak oriented toward the first one),

5. presence of statistically significant emission between the two main peaks,

and inspected those meeting fewer than four of the above criteria (i.e., pulse profiles that do not correspond to the “typical” Vela-like profile). In some of these cases, peak 1 and peak 2 were inverted based on visual inspection, and a number of objects were flagged as “uncertain.”

In addition to those cases where the ordering of the two main gamma-ray peaks is ambiguous, some other pulsars have “complex” pulse profiles in which the choice of the two main peaks is itself ambiguous, for various reasons. In an attempt to list these objects, we searched the best-fit pulse profiles for examples that contain at least one peak not overlapping with the two main peaks chosen from initial visual inspection, and
<table><caption>**Table 9**
Pulse Shape Parameters of Young LAT-detected Pulsars</caption><thead><tr><th>PSR</th><th>Peaks</th><th>Radio/Gamma Phase Lag, δ</th><th>Peak Separation, Δ</th><th>Comment</th><th>Radio Class</th></tr></thead><tbody><tr><td>J0002+6216</td><td>2</td><td>0.162<sup>+0.015</sup><sub>-0.009</sub></td><td>0.433<sup>+0.015</sup><sub>-0.009</sub></td><td></td><td>1</td></tr><tr><td>J0007+7303</td><td>3</td><td>...</td><td>0.2383 ± 0.0014</td><td></td><td>...</td></tr><tr><td>J0106+4855</td><td>2</td><td>0.057 ± 0.008</td><td>0.4869<sup>+0.0010</sup><sub>-0.0012</sub></td><td>u</td><td>1</td></tr><tr><td>J0205+6449</td><td>2</td><td>0.0400 ± 0.0024</td><td>0.5039 ± 0.0019</td><td></td><td>1</td></tr><tr><td>J0248+6021</td><td>1</td><td>0.347 ± 0.005</td><td>...</td><td></td><td>1</td></tr><tr><td>J0357+3205</td><td>2</td><td>...</td><td>0.192 ± 0.005</td><td></td><td>...</td></tr><tr><td>J0359+5414</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J0514-4408</td><td>2</td><td>0.4776 ± 0.0034</td><td>0.52<sup>+0.05</sup><sub>-0.03</sub></td><td>u</td><td>3</td></tr><tr><td>J0534+2200</td><td>2</td><td>0.067 ± 0.004</td><td>0.39889 ± 0.00017</td><td></td><td>2</td></tr><tr><td>J0540-6919</td><td>1</td><td>0.96 ± 0.04</td><td>...</td><td></td><td>1</td></tr><tr><td>J0554+3107</td><td>2</td><td>...</td><td>0.339 ± 0.008</td><td></td><td>...</td></tr><tr><td>J0622+3749</td><td>2</td><td>...</td><td>0.544 ± 0.027</td><td></td><td>...</td></tr><tr><td>J0631+0646</td><td>2</td><td>0.332 ± 0.014</td><td>0.311 ± 0.015</td><td></td><td>1</td></tr><tr><td>J0631+1036</td><td>1</td><td>0.507 ± 0.007</td><td>...</td><td></td><td>2</td></tr><tr><td>J0633+0632</td><td>2</td><td>...</td><td>0.4776 ± 0.0009</td><td></td><td>...</td></tr><tr><td>J0633+1746</td><td>3</td><td>...</td><td>0.50398 ± 0.00015</td><td></td><td>...</td></tr><tr><td>J0659+1414</td><td>1</td><td>0.226 ± 0.004</td><td>...</td><td></td><td>1</td></tr><tr><td>J0729-1448</td><td>1</td><td>0.572 ± 0.015</td><td>...</td><td></td><td>2</td></tr><tr><td>J0734-1559</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J0742-2822</td><td>2</td><td>0.533<sup>+0.012</sup><sub>-0.017</sub></td><td>0.082<sup>+0.012</sup><sub>-0.017</sub></td><td></td><td>2</td></tr><tr><td>J0744-2525</td><td>3</td><td>...</td><td>0.468 ± 0.004</td><td></td><td>...</td></tr><tr><td>J0802-5613</td><td>2</td><td>...</td><td>0.261 ± 0.023</td><td></td><td>...</td></tr><tr><td>J0835-4510</td><td>4</td><td>0.133 ± 0.004</td><td>0.431865 ± 0.000032</td><td></td><td>1</td></tr><tr><td>J0908-4913</td><td>2</td><td>0.0971 ± 0.0034</td><td>0.500 ± 0.004</td><td></td><td>2</td></tr><tr><td>J0940-5428</td><td>1</td><td>0.454 ± 0.010</td><td>...</td><td></td><td>1</td></tr><tr><td>J1016-5857</td><td>3</td><td>0.123<sup>+0.008</sup><sub>-0.013</sub></td><td>0.442<sup>+0.009</sup><sub>-0.013</sub></td><td></td><td>1</td></tr><tr><td>J1019-5749</td><td>1</td><td>0.566 ± 0.010</td><td>...</td><td></td><td>1</td></tr><tr><td>J1023-5746</td><td>3</td><td>...</td><td>0.4692 ± 0.0005</td><td></td><td>...</td></tr><tr><td>J1028-5819</td><td>2</td><td>0.1935 ± 0.0010</td><td>0.4727 ± 0.0004</td><td></td><td>1</td></tr><tr><td>J1044-5737</td><td>3</td><td>...</td><td>0.3604 ± 0.0018</td><td></td><td>...</td></tr><tr><td>J1048-5832</td><td>3</td><td>0.1468 ± 0.0012</td><td>0.4221 ± 0.0009</td><td></td><td>2</td></tr><tr><td>J1055-6028</td><td>1</td><td>0.530<sup>+0.011</sup><sub>-0.019</sub></td><td>...</td><td></td><td>1</td></tr><tr><td>J1057-5226</td><td>4</td><td>0.7441 ± 0.0017</td><td>0.3000 ± 0.0010</td><td>c</td><td>4</td></tr><tr><td>J1057-5851</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1105-6037</td><td>2</td><td>...</td><td>0.348 ± 0.014</td><td></td><td>...</td></tr><tr><td>J1105-6107</td><td>2</td><td>0.1268<sup>+0.0027</sup><sub>-0.0035</sub></td><td>0.501 ± 0.006</td><td></td><td>1</td></tr><tr><td>J1111-6039</td><td>2</td><td>...</td><td>0.313 ± 0.018</td><td></td><td>...</td></tr><tr><td>J1112-6103</td><td>2</td><td>0.147 ± 0.018</td><td>0.468 ± 0.020</td><td></td><td>1</td></tr><tr><td>J1119-6127</td><td>1</td><td>0.469 ± 0.008</td><td>...</td><td></td><td>1</td></tr><tr><td>J1124-5916</td><td>2</td><td>0.136 ± 0.009</td><td>0.4985 ± 0.0011</td><td></td><td>1</td></tr><tr><td>J1135-6055</td><td>2</td><td>...</td><td>0.173 ± 0.013</td><td></td><td>...</td></tr><tr><td>J1139-6247</td><td>2</td><td>...</td><td>0.151 ± 0.016</td><td></td><td>...</td></tr><tr><td>J1151-6108</td><td>2</td><td>0.081<sup>+0.009</sup><sub>-0.013</sub></td><td>0.429<sup>+0.011</sup><sub>-0.014</sub></td><td></td><td>2</td></tr><tr><td>J1203-6242</td><td>3</td><td>...</td><td>0.468 ± 0.005</td><td></td><td>...</td></tr><tr><td>J1208-6238</td><td>2</td><td>...</td><td>0.468 ± 0.007</td><td></td><td>...</td></tr><tr><td>J1224-6407</td><td>1</td><td>0.215 ± 0.018</td><td>...</td><td></td><td>1</td></tr><tr><td>J1231-5113</td><td>2</td><td>...</td><td>0.431 ± 0.008</td><td></td><td>...</td></tr><tr><td>J1231-6511</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1350-6225</td><td>3</td><td>...</td><td>0.485 ± 0.005</td><td></td><td>...</td></tr><tr><td>J1357-6429</td><td>1</td><td>0.388 ± 0.009</td><td>...</td><td></td><td>1</td></tr><tr><td>J1358-6025</td><td>2</td><td>...</td><td>0.298 ± 0.028</td><td></td><td>...</td></tr><tr><td>J1410-6132</td><td>1</td><td>0.537 ± 0.027</td><td>...</td><td></td><td>1</td></tr><tr><td>J1413-6205</td><td>3</td><td>...</td><td>0.3707 ± 0.0014</td><td></td><td>...</td></tr><tr><td>J1418-6058</td><td>3</td><td>...</td><td>0.4626 ± 0.0016</td><td></td><td>...</td></tr><tr><td>J1420-6048</td><td>2</td><td>0.222<sup>+0.003</sup><sub>-0.004</sub></td><td>0.311 ± 0.005</td><td></td><td>1</td></tr><tr><td>J1422-6138</td><td>2</td><td>...</td><td>0.196 ± 0.012</td><td></td><td>...</td></tr><tr><td>J1429-5911</td><td>3</td><td>...</td><td>0.4738 ± 0.0030</td><td></td><td>...</td></tr><tr><td>J1447-5757</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1459-6053</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1509-5850</td><td>2</td><td>0.156 ± 0.006</td><td>0.258 ± 0.006</td><td></td><td>1</td></tr><tr><td>J1513-5908</td><td>1</td><td>0.321 ± 0.010</td><td>...</td><td></td><td>1</td></tr><tr><td>J1522-5735</td><td>2</td><td>...</td><td>0.465 ± 0.011</td><td></td><td>...</td></tr><tr><td>J1528-5838</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr></tbody></table>
<table><caption>**Table 9**
Pulse Shape Parameters of Young LAT-detected Pulsars</caption><thead><tr><th>PSR</th><th>Peaks</th><th>Radio/Gamma Phase Lag, δ</th><th>Peak Separation, Δ</th><th>Comment</th><th>Radio Class</th></tr></thead><tbody><tr><td>J0002+6216</td><td>2</td><td>0.162<sup>+0.015</sup><sub>-0.009</sub></td><td>0.433<sup>+0.015</sup><sub>-0.009</sub></td><td></td><td>1</td></tr><tr><td>J0007+7303</td><td>3</td><td>...</td><td>0.2383 ± 0.0014</td><td></td><td>...</td></tr><tr><td>J0106+4855</td><td>2</td><td>0.057 ± 0.008</td><td>0.4869<sup>+0.0010</sup><sub>-0.0012</sub></td><td>u</td><td>1</td></tr><tr><td>J0205+6449</td><td>2</td><td>0.0400 ± 0.0024</td><td>0.5039 ± 0.0019</td><td></td><td>1</td></tr><tr><td>J0248+6021</td><td>1</td><td>0.347 ± 0.005</td><td>...</td><td></td><td>1</td></tr><tr><td>J0357+3205</td><td>2</td><td>...</td><td>0.192 ± 0.005</td><td></td><td>...</td></tr><tr><td>J0359+5414</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J0514-4408</td><td>2</td><td>0.4776 ± 0.0034</td><td>0.52<sup>+0.05</sup><sub>-0.03</sub></td><td>u</td><td>3</td></tr><tr><td>J0534+2200</td><td>2</td><td>0.067 ± 0.004</td><td>0.39889 ± 0.00017</td><td></td><td>2</td></tr><tr><td>J0540-6919</td><td>1</td><td>0.96 ± 0.04</td><td>...</td><td></td><td>1</td></tr><tr><td>J0554+3107</td><td>2</td><td>...</td><td>0.339 ± 0.008</td><td></td><td>...</td></tr><tr><td>J0622+3749</td><td>2</td><td>...</td><td>0.544 ± 0.027</td><td></td><td>...</td></tr><tr><td>J0631+0646</td><td>2</td><td>0.332 ± 0.014</td><td>0.311 ± 0.015</td><td></td><td>1</td></tr><tr><td>J0631+1036</td><td>1</td><td>0.507 ± 0.007</td><td>...</td><td></td><td>2</td></tr><tr><td>J0633+0632</td><td>2</td><td>...</td><td>0.4776 ± 0.0009</td><td></td><td>...</td></tr><tr><td>J0633+1746</td><td>3</td><td>...</td><td>0.50398 ± 0.00015</td><td></td><td>...</td></tr><tr><td>J0659+1414</td><td>1</td><td>0.226 ± 0.004</td><td>...</td><td></td><td>1</td></tr><tr><td>J0729-1448</td><td>1</td><td>0.572 ± 0.015</td><td>...</td><td></td><td>2</td></tr><tr><td>J0734-1559</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J0742-2822</td><td>2</td><td>0.533<sup>+0.012</sup><sub>-0.017</sub></td><td>0.082<sup>+0.012</sup><sub>-0.017</sub></td><td></td><td>2</td></tr><tr><td>J0744-2525</td><td>3</td><td>...</td><td>0.468 ± 0.004</td><td></td><td>...</td></tr><tr><td>J0802-5613</td><td>2</td><td>...</td><td>0.261 ± 0.023</td><td></td><td>...</td></tr><tr><td>J0835-4510</td><td>4</td><td>0.133 ± 0.004</td><td>0.431865 ± 0.000032</td><td></td><td>1</td></tr><tr><td>J0908-4913</td><td>2</td><td>0.0971 ± 0.0034</td><td>0.500 ± 0.004</td><td></td><td>2</td></tr><tr><td>J0940-5428</td><td>1</td><td>0.454 ± 0.010</td><td>...</td><td></td><td>1</td></tr><tr><td>J1016-5857</td><td>3</td><td>0.123<sup>+0.008</sup><sub>-0.013</sub></td><td>0.442<sup>+0.009</sup><sub>-0.013</sub></td><td></td><td>1</td></tr><tr><td>J1019-5749</td><td>1</td><td>0.566 ± 0.010</td><td>...</td><td></td><td>1</td></tr><tr><td>J1023-5746</td><td>3</td><td>...</td><td>0.4692 ± 0.0005</td><td></td><td>...</td></tr><tr><td>J1028-5819</td><td>2</td><td>0.1935 ± 0.0010</td><td>0.4727 ± 0.0004</td><td></td><td>1</td></tr><tr><td>J1044-5737</td><td>3</td><td>...</td><td>0.3604 ± 0.0018</td><td></td><td>...</td></tr><tr><td>J1048-5832</td><td>3</td><td>0.1468 ± 0.0012</td><td>0.4221 ± 0.0009</td><td></td><td>2</td></tr><tr><td>J1055-6028</td><td>1</td><td>0.530<sup>+0.011</sup><sub>-0.019</sub></td><td>...</td><td></td><td>1</td></tr><tr><td>J1057-5226</td><td>4</td><td>0.7441 ± 0.0017</td><td>0.3000 ± 0.0010</td><td>c</td><td>4</td></tr><tr><td>J1057-5851</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1105-6037</td><td>2</td><td>...</td><td>0.348 ± 0.014</td><td></td><td>...</td></tr><tr><td>J1105-6107</td><td>2</td><td>0.1268<sup>+0.0027</sup><sub>-0.0035</sub></td><td>0.501 ± 0.006</td><td></td><td>1</td></tr><tr><td>J1111-6039</td><td>2</td><td>...</td><td>0.313 ± 0.018</td><td></td><td>...</td></tr><tr><td>J1112-6103</td><td>2</td><td>0.147 ± 0.018</td><td>0.468 ± 0.020</td><td></td><td>1</td></tr><tr><td>J1119-6127</td><td>1</td><td>0.469 ± 0.008</td><td>...</td><td></td><td>1</td></tr><tr><td>J1124-5916</td><td>2</td><td>0.136 ± 0.009</td><td>0.4985 ± 0.0011</td><td></td><td>1</td></tr><tr><td>J1135-6055</td><td>2</td><td>...</td><td>0.173 ± 0.013</td><td></td><td>...</td></tr><tr><td>J1139-6247</td><td>2</td><td>...</td><td>0.151 ± 0.016</td><td></td><td>...</td></tr><tr><td>J1151-6108</td><td>2</td><td>0.081<sup>+0.009</sup><sub>-0.013</sub></td><td>0.429<sup>+0.011</sup><sub>-0.014</sub></td><td></td><td>2</td></tr><tr><td>J1203-6242</td><td>3</td><td>...</td><td>0.468 ± 0.005</td><td></td><td>...</td></tr><tr><td>J1208-6238</td><td>2</td><td>...</td><td>0.468 ± 0.007</td><td></td><td>...</td></tr><tr><td>J1224-6407</td><td>1</td><td>0.215 ± 0.018</td><td>...</td><td></td><td>1</td></tr><tr><td>J1231-5113</td><td>2</td><td>...</td><td>0.431 ± 0.008</td><td></td><td>...</td></tr><tr><td>J1231-6511</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1350-6225</td><td>3</td><td>...</td><td>0.485 ± 0.005</td><td></td><td>...</td></tr><tr><td>J1357-6429</td><td>1</td><td>0.388 ± 0.009</td><td>...</td><td></td><td>1</td></tr><tr><td>J1358-6025</td><td>2</td><td>...</td><td>0.298 ± 0.028</td><td></td><td>...</td></tr><tr><td>J1410-6132</td><td>1</td><td>0.537 ± 0.027</td><td>...</td><td></td><td>1</td></tr><tr><td>J1413-6205</td><td>3</td><td>...</td><td>0.3707 ± 0.0014</td><td></td><td>...</td></tr><tr><td>J1418-6058</td><td>3</td><td>...</td><td>0.4626 ± 0.0016</td><td></td><td>...</td></tr><tr><td>J1420-6048</td><td>2</td><td>0.222<sup>+0.003</sup><sub>-0.004</sub></td><td>0.311 ± 0.005</td><td></td><td>1</td></tr><tr><td>J1422-6138</td><td>2</td><td>...</td><td>0.196 ± 0.012</td><td></td><td>...</td></tr><tr><td>J1429-5911</td><td>3</td><td>...</td><td>0.4738 ± 0.0030</td><td></td><td>...</td></tr><tr><td>J1447-5757</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1459-6053</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1509-5850</td><td>2</td><td>0.156 ± 0.006</td><td>0.258 ± 0.006</td><td></td><td>1</td></tr><tr><td>J1513-5908</td><td>1</td><td>0.321 ± 0.010</td><td>...</td><td></td><td>1</td></tr><tr><td>J1522-5735</td><td>2</td><td>...</td><td>0.465 ± 0.011</td><td></td><td>...</td></tr><tr><td>J1528-5838</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr></tbody></table>
<table><caption>**Table 9**
(Continued)</caption><thead><tr><th>PSR</th><th>Peaks</th><th>Radio/Gamma Phase Lag, δ</th><th>Peak Separation, Δ</th><th>Comment</th><th>Radio Class</th></tr></thead><tbody><tr><td>J1531-5610</td><td>1</td><td>0.40 ± 0.04</td><td>...</td><td></td><td>1</td></tr><tr><td>J1615-5137</td><td>2</td><td>...</td><td>0.270<sup>+0.014</sup><sub>-0.010</sub></td><td></td><td>...</td></tr><tr><td>J1620-4927</td><td>2</td><td>...</td><td>0.246 ± 0.007</td><td></td><td>...</td></tr><tr><td>J1623-5005</td><td>2</td><td>...</td><td>0.389 ± 0.010</td><td></td><td>...</td></tr><tr><td>J1624-4041</td><td>2</td><td>...</td><td>0.422 ± 0.005</td><td></td><td>...</td></tr><tr><td>J1641-5317</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1646-4346</td><td>1</td><td>0.535 ± 0.014</td><td>...</td><td></td><td>1</td></tr><tr><td>J1648-4611</td><td>2</td><td>0.263 ± 0.010</td><td>0.310 ± 0.011</td><td></td><td>1</td></tr><tr><td>J1650-4601</td><td>2</td><td>...</td><td>0.358 ± 0.011</td><td></td><td>...</td></tr><tr><td>J1702-4128</td><td>1</td><td>0.45<sup>+0.03</sup><sub>-0.05</sub></td><td>...</td><td></td><td>1</td></tr><tr><td>J1705-1906</td><td>1</td><td>0.562<sup>+0.010</sup><sub>-0.007</sub></td><td>...</td><td></td><td>2</td></tr><tr><td>J1709-4429</td><td>3</td><td>0.2364 ± 0.0004</td><td>0.2515 ± 0.0004</td><td></td><td>1</td></tr><tr><td>J1714-3830</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1718-3825</td><td>1</td><td>0.398 ± 0.005</td><td>...</td><td></td><td>2</td></tr><tr><td>J1730-3350</td><td>2</td><td>0.129<sup>+0.003</sup><sub>-0.006</sub></td><td>0.417<sup>+0.005</sup><sub>-0.007</sub></td><td></td><td>1</td></tr><tr><td>J1732-3131</td><td>3</td><td>0.0876 ± 0.0026</td><td>0.4104<sup>+0.0010</sup><sub>-0.0007</sub></td><td></td><td>4</td></tr><tr><td>J1736-3422</td><td>2</td><td>...</td><td>0.437 ± 0.009</td><td></td><td>...</td></tr><tr><td>J1741-2054</td><td>2</td><td>0.035 ± 0.005</td><td>0.240<sup>+0.003</sup><sub>-0.006</sub></td><td></td><td>2</td></tr><tr><td>J1742-3321</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1746-3239</td><td>2</td><td>...</td><td>0.133 ± 0.009</td><td></td><td>...</td></tr><tr><td>J1747-2958</td><td>3</td><td>0.156 ± 0.005</td><td>0.392 ± 0.004</td><td></td><td>1</td></tr><tr><td>J1748-2815</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1801-2451</td><td>2</td><td>0.118 ± 0.007</td><td>0.495 ± 0.007</td><td></td><td>1</td></tr><tr><td>J1803-2149</td><td>3</td><td>...</td><td>0.379 ± 0.005</td><td></td><td>...</td></tr><tr><td>J1809-2332</td><td>3</td><td>...</td><td>0.3465 ± 0.0007</td><td></td><td>...</td></tr><tr><td>J1813-1246</td><td>3</td><td>...</td><td>0.489 ± 0.004</td><td></td><td>...</td></tr><tr><td>J1817-1742</td><td>2</td><td>...</td><td>0.518 ± 0.005</td><td></td><td>...</td></tr><tr><td>J1826-1256</td><td>2</td><td>...</td><td>0.4737 ± 0.0004</td><td></td><td>...</td></tr><tr><td>J1827-1446</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1828-1101</td><td>2</td><td>0.110 ± 0.005</td><td>0.500<sup>+0.008</sup><sub>-0.010</sub></td><td></td><td>1</td></tr><tr><td>J1833-1034</td><td>2</td><td>0.142 ± 0.016</td><td>0.4530 ± 0.0023</td><td></td><td>1</td></tr><tr><td>J1835-1106</td><td>1</td><td>0.55<sup>+0.02</sup><sub>-0.06</sub></td><td>...</td><td></td><td>1</td></tr><tr><td>J1836+5925</td><td>3</td><td>...</td><td>0.5167 ± 0.0016</td><td></td><td>...</td></tr><tr><td>J1837-0604</td><td>2</td><td>0.197 ± 0.009</td><td>0.486 ± 0.021</td><td></td><td>1</td></tr><tr><td>J1838-0537</td><td>2</td><td>...</td><td>0.304 ± 0.009</td><td></td><td>...</td></tr><tr><td>J1844-0346</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1846+0919</td><td>2</td><td>...</td><td>0.227 ± 0.017</td><td></td><td>...</td></tr><tr><td>J1856+0113</td><td>2</td><td>0.106<sup>+0.027</sup><sub>-0.017</sub></td><td>0.469<sup>+0.028</sup><sub>-0.018</sub></td><td></td><td>1</td></tr><tr><td>J1857+0143</td><td>1</td><td>0.43<sup>+0.05</sup><sub>-0.07</sub></td><td>...</td><td></td><td>1</td></tr><tr><td>J1906+0722</td><td>2</td><td>...</td><td>0.222 ± 0.023</td><td></td><td>...</td></tr><tr><td>J1907+0602</td><td>3</td><td>0.282 ± 0.008</td><td>0.3850 ± 0.0013</td><td></td><td>1</td></tr><tr><td>J1913+0904</td><td>2</td><td>0.20<sup>+0.07</sup><sub>-0.03</sub></td><td>0.40<sup>+0.07</sup><sub>-0.03</sub></td><td></td><td>1</td></tr><tr><td>J1932+1916</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1952+3252</td><td>3</td><td>0.1572 ± 0.0007</td><td>0.4752 ± 0.0006</td><td></td><td>1</td></tr><tr><td>J1954+2836</td><td>3</td><td>...</td><td>0.4521 ± 0.0025</td><td></td><td>...</td></tr><tr><td>J1957+5033</td><td>2</td><td>...</td><td>0.178 ± 0.009</td><td></td><td>...</td></tr><tr><td>J1958+2846</td><td>3</td><td>...</td><td>0.4371 ± 0.0016</td><td></td><td>...</td></tr><tr><td>J2006+3102</td><td>1</td><td>0.570 ± 0.007</td><td>...</td><td></td><td>1</td></tr><tr><td>J2017+3625</td><td>2</td><td>...</td><td>0.401<sup>+0.014</sup><sub>-0.010</sub></td><td></td><td>...</td></tr><tr><td>J2021+3651</td><td>3</td><td>0.1369 ± 0.0019</td><td>0.47147 ± 0.00011</td><td></td><td>1</td></tr><tr><td>J2021+4026</td><td>3</td><td>...</td><td>0.553 ± 0.005</td><td>c</td><td>4</td></tr><tr><td>J2022+3842</td><td>1</td><td>0.420<sup>+0.020</sup><sub>-0.025</sub></td><td>...</td><td></td><td>...</td></tr><tr><td>J2028+3332</td><td>3</td><td>...</td><td>0.432 ± 0.005</td><td></td><td>...</td></tr><tr><td>J2030+3641</td><td>2</td><td>0.300 ± 0.007</td><td>0.320 ± 0.008</td><td></td><td>1</td></tr><tr><td>J2030+4415</td><td>3</td><td>...</td><td>0.490 ± 0.004</td><td></td><td>...</td></tr><tr><td>J2032+4127</td><td>2</td><td>0.1626 ± 0.0009</td><td>0.4831 ± 0.0008</td><td>u</td><td>1</td></tr><tr><td>J2043+2740</td><td>2</td><td>0.136<sup>+0.005</sup><sub>-0.008</sub></td><td>0.435<sup>+0.006</sup><sub>-0.008</sub></td><td></td><td>1</td></tr><tr><td>J2055+2539</td><td>2</td><td>...</td><td>0.172<sup>+0.009</sup><sub>-0.016</sub></td><td></td><td>...</td></tr><tr><td>J2111+4606</td><td>3</td><td>...</td><td>0.3459 ± 0.0034</td><td></td><td>...</td></tr><tr><td>J2139+4716</td><td>2</td><td>...</td><td>0.55<sup>+0.06</sup><sub>-0.02</sub></td><td></td><td>...</td></tr><tr><td>J2229+6114</td><td>2</td><td>0.2959<sup>+0.0016</sup><sub>-0.0021</sub></td><td>0.2221<sup>+0.0012</sup><sub>-0.0018</sub></td><td></td><td>1</td></tr><tr><td>J2238+5903</td><td>2</td><td>...</td><td>0.5002 ± 0.0005</td><td></td><td>...</td></tr></tbody></table>
<table><caption>**Table 9**
(Continued)</caption><thead><tr><th>PSR</th><th>Peaks</th><th>Radio/Gamma Phase Lag, δ</th><th>Peak Separation, Δ</th><th>Comment</th><th>Radio Class</th></tr></thead><tbody><tr><td>J1531-5610</td><td>1</td><td>0.40 ± 0.04</td><td>...</td><td></td><td>1</td></tr><tr><td>J1615-5137</td><td>2</td><td>...</td><td>0.270<sup>+0.014</sup><sub>-0.010</sub></td><td></td><td>...</td></tr><tr><td>J1620-4927</td><td>2</td><td>...</td><td>0.246 ± 0.007</td><td></td><td>...</td></tr><tr><td>J1623-5005</td><td>2</td><td>...</td><td>0.389 ± 0.010</td><td></td><td>...</td></tr><tr><td>J1624-4041</td><td>2</td><td>...</td><td>0.422 ± 0.005</td><td></td><td>...</td></tr><tr><td>J1641-5317</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1646-4346</td><td>1</td><td>0.535 ± 0.014</td><td>...</td><td></td><td>1</td></tr><tr><td>J1648-4611</td><td>2</td><td>0.263 ± 0.010</td><td>0.310 ± 0.011</td><td></td><td>1</td></tr><tr><td>J1650-4601</td><td>2</td><td>...</td><td>0.358 ± 0.011</td><td></td><td>...</td></tr><tr><td>J1702-4128</td><td>1</td><td>0.45<sup>+0.03</sup><sub>-0.05</sub></td><td>...</td><td></td><td>1</td></tr><tr><td>J1705-1906</td><td>1</td><td>0.562<sup>+0.010</sup><sub>-0.007</sub></td><td>...</td><td></td><td>2</td></tr><tr><td>J1709-4429</td><td>3</td><td>0.2364 ± 0.0004</td><td>0.2515 ± 0.0004</td><td></td><td>1</td></tr><tr><td>J1714-3830</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1718-3825</td><td>1</td><td>0.398 ± 0.005</td><td>...</td><td></td><td>2</td></tr><tr><td>J1730-3350</td><td>2</td><td>0.129<sup>+0.003</sup><sub>-0.006</sub></td><td>0.417<sup>+0.005</sup><sub>-0.007</sub></td><td></td><td>1</td></tr><tr><td>J1732-3131</td><td>3</td><td>0.0876 ± 0.0026</td><td>0.4104<sup>+0.0010</sup><sub>-0.0007</sub></td><td></td><td>4</td></tr><tr><td>J1736-3422</td><td>2</td><td>...</td><td>0.437 ± 0.009</td><td></td><td>...</td></tr><tr><td>J1741-2054</td><td>2</td><td>0.035 ± 0.005</td><td>0.240<sup>+0.003</sup><sub>-0.006</sub></td><td></td><td>2</td></tr><tr><td>J1742-3321</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1746-3239</td><td>2</td><td>...</td><td>0.133 ± 0.009</td><td></td><td>...</td></tr><tr><td>J1747-2958</td><td>3</td><td>0.156 ± 0.005</td><td>0.392 ± 0.004</td><td></td><td>1</td></tr><tr><td>J1748-2815</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1801-2451</td><td>2</td><td>0.118 ± 0.007</td><td>0.495 ± 0.007</td><td></td><td>1</td></tr><tr><td>J1803-2149</td><td>3</td><td>...</td><td>0.379 ± 0.005</td><td></td><td>...</td></tr><tr><td>J1809-2332</td><td>3</td><td>...</td><td>0.3465 ± 0.0007</td><td></td><td>...</td></tr><tr><td>J1813-1246</td><td>3</td><td>...</td><td>0.489 ± 0.004</td><td></td><td>...</td></tr><tr><td>J1817-1742</td><td>2</td><td>...</td><td>0.518 ± 0.005</td><td></td><td>...</td></tr><tr><td>J1826-1256</td><td>2</td><td>...</td><td>0.4737 ± 0.0004</td><td></td><td>...</td></tr><tr><td>J1827-1446</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1828-1101</td><td>2</td><td>0.110 ± 0.005</td><td>0.500<sup>+0.008</sup><sub>-0.010</sub></td><td></td><td>1</td></tr><tr><td>J1833-1034</td><td>2</td><td>0.142 ± 0.016</td><td>0.4530 ± 0.0023</td><td></td><td>1</td></tr><tr><td>J1835-1106</td><td>1</td><td>0.55<sup>+0.02</sup><sub>-0.06</sub></td><td>...</td><td></td><td>1</td></tr><tr><td>J1836+5925</td><td>3</td><td>...</td><td>0.5167 ± 0.0016</td><td></td><td>...</td></tr><tr><td>J1837-0604</td><td>2</td><td>0.197 ± 0.009</td><td>0.486 ± 0.021</td><td></td><td>1</td></tr><tr><td>J1838-0537</td><td>2</td><td>...</td><td>0.304 ± 0.009</td><td></td><td>...</td></tr><tr><td>J1844-0346</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1846+0919</td><td>2</td><td>...</td><td>0.227 ± 0.017</td><td></td><td>...</td></tr><tr><td>J1856+0113</td><td>2</td><td>0.106<sup>+0.027</sup><sub>-0.017</sub></td><td>0.469<sup>+0.028</sup><sub>-0.018</sub></td><td></td><td>1</td></tr><tr><td>J1857+0143</td><td>1</td><td>0.43<sup>+0.05</sup><sub>-0.07</sub></td><td>...</td><td></td><td>1</td></tr><tr><td>J1906+0722</td><td>2</td><td>...</td><td>0.222 ± 0.023</td><td></td><td>...</td></tr><tr><td>J1907+0602</td><td>3</td><td>0.282 ± 0.008</td><td>0.3850 ± 0.0013</td><td></td><td>1</td></tr><tr><td>J1913+0904</td><td>2</td><td>0.20<sup>+0.07</sup><sub>-0.03</sub></td><td>0.40<sup>+0.07</sup><sub>-0.03</sub></td><td></td><td>1</td></tr><tr><td>J1932+1916</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1952+3252</td><td>3</td><td>0.1572 ± 0.0007</td><td>0.4752 ± 0.0006</td><td></td><td>1</td></tr><tr><td>J1954+2836</td><td>3</td><td>...</td><td>0.4521 ± 0.0025</td><td></td><td>...</td></tr><tr><td>J1957+5033</td><td>2</td><td>...</td><td>0.178 ± 0.009</td><td></td><td>...</td></tr><tr><td>J1958+2846</td><td>3</td><td>...</td><td>0.4371 ± 0.0016</td><td></td><td>...</td></tr><tr><td>J2006+3102</td><td>1</td><td>0.570 ± 0.007</td><td>...</td><td></td><td>1</td></tr><tr><td>J2017+3625</td><td>2</td><td>...</td><td>0.401<sup>+0.014</sup><sub>-0.010</sub></td><td></td><td>...</td></tr><tr><td>J2021+3651</td><td>3</td><td>0.1369 ± 0.0019</td><td>0.47147 ± 0.00011</td><td></td><td>1</td></tr><tr><td>J2021+4026</td><td>3</td><td>...</td><td>0.553 ± 0.005</td><td>c</td><td>...</td></tr><tr><td>J2022+3842</td><td>1</td><td>0.420<sup>+0.020</sup><sub>-0.025</sub></td><td>...</td><td></td><td>4</td></tr><tr><td>J2028+3332</td><td>3</td><td>...</td><td>0.432 ± 0.005</td><td></td><td>...</td></tr><tr><td>J2030+3641</td><td>2</td><td>0.300 ± 0.007</td><td>0.320 ± 0.008</td><td></td><td>1</td></tr><tr><td>J2030+4415</td><td>3</td><td>...</td><td>0.490 ± 0.004</td><td></td><td>...</td></tr><tr><td>J2032+4127</td><td>2</td><td>0.1626 ± 0.0009</td><td>0.4831 ± 0.0008</td><td>u</td><td>1</td></tr><tr><td>J2043+2740</td><td>2</td><td>0.136<sup>+0.005</sup><sub>-0.008</sub></td><td>0.435<sup>+0.006</sup><sub>-0.008</sub></td><td></td><td>1</td></tr><tr><td>J2055+2539</td><td>2</td><td>...</td><td>0.172<sup>+0.009</sup><sub>-0.016</sub></td><td></td><td>...</td></tr><tr><td>J2111+4606</td><td>3</td><td>...</td><td>0.3459 ± 0.0034</td><td></td><td>...</td></tr><tr><td>J2139+4716</td><td>2</td><td>...</td><td>0.55<sup>+0.06</sup><sub>-0.02</sub></td><td></td><td>...</td></tr><tr><td>J2229+6114</td><td>2</td><td>0.2959<sup>+0.0016</sup><sub>-0.0021</sub></td><td>0.2221<sup>+0.0012</sup><sub>-0.0018</sub></td><td></td><td>1</td></tr><tr><td>J2238+5903</td><td>2</td><td>...</td><td>0.5002 ± 0.0005</td><td></td><td>...</td></tr></tbody></table>
<table><caption>**Table 9**
(Continued)</caption><thead><tr><th>PSR</th><th>Peaks</th><th>Radio/Gamma Phase Lag, δ</th><th>Peak Separation, Δ</th><th>Comment</th><th>Radio Class</th></tr></thead><tbody><tr><td>J2240+5832</td><td>2</td><td>0.119<sup>+0.012</sup><sub>-0.009</sub></td><td>0.475<sup>+0.012</sup><sub>-0.009</sub></td><td></td><td>1</td></tr></tbody></table>

**Note.** Column 2 gives the gamma-ray peak multiplicity. Columns 3 and 4 give the radio/gamma phase lag $δ$ and separation $Δ$ between the two main gamma-ray peaks. In Column 5, “u” indicates uncertain ordering of the first and second gamma-ray peaks, and “c” means the profile is complex. For pulsars with radio emission, Column 6 lists flags quantifying the robustness of the fiducial phase definition (see the text for details).

whose maximum amplitude is at least half that of the smaller of the two main peaks. The handful of objects that matched this criterion were flagged as “complex.”

For all of these pulsars for which the choice of peak 1 and peak 2 is not obvious, the values for $δ$ and $Δ$ are also uncertain.

Tables 9 and 10 list the best-fit parameters. Figure 10 shows a plot of the separation of the two main gamma-ray peaks, $Δ$, versus the radio/gamma-ray phase separation, $δ$. Figure 11 shows the $Δ$ values plotted against the spin-down power values, $\dot{E}$. For the pulsars with radio emission and at least two gamma-ray components (and therefore, with both $δ$ and $Δ$ values in Tables 9 and 10 and in Figure 10), and excluding pulsars with profiles considered as complex or with uncertain peak ordering, we find a Spearman rank coefficient of ~-0.30, indicative of a negative correlation between $δ$ and $Δ$ with a probability of chance correlation of ~2 × 10⁻³. The anticorrelation of $δ$ and $Δ$, already noted in, e.g., 2PC, is a well-known prediction of outer magnetospheric pulsar emission models. No strong relation is seen in Figure 11. These results and other trends visible in these figures are further discussed in Section 8.

We compared $δ$ and $Δ$ in Tables 9 and 10 with the 2PC values, for pulsars in both catalogs. Table 11 lists pulsars for which $δ$ and/or $Δ$ differ by more than three times the statistical uncertainty, and with an absolute difference >0.03. For $Δ$, no strong inconsistencies appeared: inverted gamma-ray profile fit components, or differing numbers of components or component phases explain most discrepancies. Similarly, the $δ$ parameters between 2PC and 3PC are qualitatively similar in most cases: differences typically arise from choices of radio pulse reference phase, or choices of the gamma-ray component used to find $δ$. The only pulsars with significantly discrepant radio/gamma-ray alignment properties in 2PC and 3PC are PSRs J2047+1053 and J2215+5135.

We further compared our radio/gamma-ray alignment results to those in the literature but not in 2PC, finding discrepant radio and gamma-ray alignments for PSRs J1341-6220, J1431-4715, J1646-4346, J1731-4744, J1816+4510, J1921+1929, J1935+2025, and J2039-3616. We stress that the $δ$ values listed in Tables 9 and 10, and the relative radio/gamma-ray alignment results in general, should be taken with a grain of salt due to the numerous systematic effects. In the case of PSR J0318+0253, whose $δ$-parameter is not listed in Table 10, varying rotational phase references during the commissioning of the FAST telescope prevent us from determining the alignment properly. Different choices for the radio fiducial phase, different central frequencies or frequency bandwidths used for the radio observations, or ill-determined (or varying) DM values can also lead to inconsistent $δ$ estimates between different analyses, to name but a few examples. Nevertheless, we have established that for almost all pulsars the relative radio and gamma-ray alignments are qualitatively consistent with published results.

### 5.3. Energy-resolved Light-curve Fitting

The best-fit profiles above 0.1 GeV were then used to fit gamma-ray pulse profiles in narrower energy ranges. To this end, we divided the LAT data sets into logarithmically spaced energy intervals, and fitted the pulsar pulse profiles in each energy interval independently. The number of energy intervals per decade was determined by the H-test TS above 0.1 GeV: one per decade for pulsars with H-test TS values between 100 and 1000, two per decade when 1000 ≤ H ≤ 10,000, and so on. Profile fits are again done only if H-test > 100 in an energy band: 167 pulsars have at least two such intervals. Profile parameters were allowed to vary within the same ranges as for the fits over the entire energy range. By default, the number of components for a given pulsar was the same as for the fit over the entire energy range. However, profile fits in the narrow energy ranges often require fewer components than for the entire range. We fitted the profiles with $N_{peaks} > 2$ components in the individual energy ranges with all possible component combinations, and selected the combination favored by the BIC in most energy intervals. For most objects, the number of peaks remained the same; for the others, the third component (typically, bridge emission) was discarded. PSR J0007+7303, shown in Appendix B, is an example. The peak shapes, Gaussian or Lorentzian, are the same in the sub-bands as in the energy-integrated profile.

Figure 12 summarizes the results for one pulsar. The component amplitudes, phases, and widths vary with energy, as sometimes seen in other pulsars: see, for example, the phase-resolved analyses in Abdo et al. (2010f, 2010g, 2010h). In this Figure, results are shown in energy bins in which the pulsar has an H-test TS greater than 300. Peaks with amplitudes smaller than 1/100 of the maximum peak value in that energy bin, with areas smaller than 5 × 10⁻³ of the total area of the reconstructed pulsed emission and with widths larger than 20 times the median value, are not plotted and not included in the fit described in the following paragraph. As for the pulse profiles described in Section 5.1, all summary plots from the energy-resolved light-curve fitting are in Figure Set 12.

We searched for trends in the amplitude ratios between the first and second gamma-ray peaks as a function of energy, for pulsars with at least two identifiable components. Assuming that the first two components have spectra that follow exponentially cutoff power laws, the amplitude ratio can be written as follows:

$$ \log_{10}\left(\frac{\text{Amp}_2}{\text{Amp}_1}\right) = C - (\Gamma_2 - \Gamma_1) \times \log_{10}(E) \\ - (1/E_{c,2} - 1/E_{c,1}) \times E/\ln 10, \quad (12) $$

where C is an energy-independent constant, and $Γ_i$ and $E_{c,i}$, respectively, denote the spectral index and cutoff energy of the
<table><caption>**Table 9**
(Continued)</caption><thead><tr><th>PSR</th><th>Peaks</th><th>Radio/Gamma Phase Lag, δ</th><th>Peak Separation, Δ</th><th>Comment</th><th>Radio Class</th></tr></thead><tbody><tr><td>J2240+5832</td><td>2</td><td>0.119<sup>+0.012</sup><sub>-0.009</sub></td><td>0.475<sup>+0.012</sup><sub>-0.009</sub></td><td></td><td>1</td></tr></tbody></table>

**Note.** Column 2 gives the gamma-ray peak multiplicity. Columns 3 and 4 give the radio/gamma phase lag $δ$ and separation $Δ$ between the two main gamma-ray peaks. In Column 5, “u” indicates uncertain ordering of the first and second gamma-ray peaks, and “c” means the profile is complex. For pulsars with radio emission, Column 6 lists flags quantifying the robustness of the fiducial phase definition (see the text for details).

whose maximum amplitude is at least half that of the smaller of the two main peaks. The handful of objects that matched this criterion were flagged as “complex.”

For all of these pulsars for which the choice of peak 1 and peak 2 is not obvious, the values for $δ$ and $Δ$ are also uncertain.

Tables 9 and 10 list the best-fit parameters. Figure 10 shows a plot of the separation of the two main gamma-ray peaks, $Δ$, versus the radio/gamma-ray phase separation, $δ$. Figure 11 shows the $Δ$ values plotted against the spin-down power values, $\dot{E}$. For the pulsars with radio emission and at least two gamma-ray components (and therefore, with both $δ$ and $Δ$ values in Tables 9 and 10 and in Figure 10), and excluding pulsars with profiles considered as complex or with uncertain peak ordering, we find a Spearman rank coefficient of ~-0.30, indicative of a negative correlation between $δ$ and $Δ$ with a probability of chance correlation of ~2 × 10⁻³. The anticorrelation of $δ$ and $Δ$, already noted in, e.g., 2PC, is a well-known prediction of outer magnetospheric pulsar emission models. No strong relation is seen in Figure 11. These results and other trends visible in these figures are further discussed in Section 8.

We compared $δ$ and $Δ$ in Tables 9 and 10 with the 2PC values, for pulsars in both catalogs. Table 11 lists pulsars for which $δ$ and/or $Δ$ differ by more than three times the statistical uncertainty, and with an absolute difference >0.03. For $Δ$, no strong inconsistencies appeared: inverted gamma-ray profile fit components, or differing numbers of components or component phases explain most discrepancies. Similarly, the $δ$ parameters between 2PC and 3PC are qualitatively similar in most cases: differences typically arise from choices of radio pulse reference phase, or choices of the gamma-ray component used to find $δ$. The only pulsars with significantly discrepant radio/gamma-ray alignment properties in 2PC and 3PC are PSRs J2047+1053 and J2215+5135.

We further compared our radio/gamma-ray alignment results to those in the literature but not in 2PC, finding discrepant radio and gamma-ray alignments for PSRs J1341-6220, J1431-4715, J1646-4346, J1731-4744, J1816+4510, J1921+1929, J1935+2025, and J2039-3616. We stress that the $δ$ values listed in Tables 9 and 10, and the relative radio/gamma-ray alignment results in general, should be taken with a grain of salt due to the numerous systematic effects. In the case of PSR J0318+0253, whose $δ$-parameter is not listed in Table 10, varying rotational phase references during the commissioning of the FAST telescope prevent us from determining the alignment properly. Different choices for the radio fiducial phase, different central frequencies or frequency bandwidths used for the radio observations, or ill-determined (or varying) DM values can also lead to inconsistent $δ$ estimates between different analyses, to name but a few examples. Nevertheless, we have established that for almost all pulsars the relative radio and gamma-ray alignments are qualitatively consistent with published results.

### 5.3. Energy-resolved Light-curve Fitting

The best-fit profiles above 0.1 GeV were then used to fit gamma-ray pulse profiles in narrower energy ranges. To this end, we divided the LAT data sets into logarithmically spaced energy intervals, and fitted the pulsar pulse profiles in each energy interval independently. The number of energy intervals per decade was determined by the *H*-test TS above 0.1 GeV: one per decade for pulsars with *H*-test TS values between 100 and 1000, two per decade when 1000 ≤ *H* ≤ 10,000, and so on. Profile fits are again done only if *H*-test > 100 in an energy band: 167 pulsars have at least two such intervals. Profile parameters were allowed to vary within the same ranges as for the fits over the entire energy range. By default, the number of components for a given pulsar was the same as for the fit over the entire energy range. However, profile fits in the narrow energy ranges often require fewer components than for the entire range. We fitted the profiles with $N_{peaks} > 2$ components in the individual energy ranges with all possible component combinations, and selected the combination favored by the BIC in most energy intervals. For most objects, the number of peaks remained the same; for the others, the third component (typically, bridge emission) was discarded. PSR J0007+7303, shown in Appendix B, is an example. The peak shapes, Gaussian or Lorentzian, are the same in the sub-bands as in the energy-integrated profile.

Figure 12 summarizes the results for one pulsar. The component amplitudes, phases, and widths vary with energy, as sometimes seen in other pulsars: see, for example, the phase-resolved analyses in Abdo et al. (2010f, 2010g, 2010h). In this Figure, results are shown in energy bins in which the pulsar has an *H*-test TS greater than 300. Peaks with amplitudes smaller than 1/100 of the maximum peak value in that energy bin, with areas smaller than 5 × 10⁻³ of the total area of the reconstructed pulsed emission and with widths larger than 20 times the median value, are not plotted and not included in the fit described in the following paragraph. As for the pulse profiles described in Section 5.1, all summary plots from the energy-resolved light-curve fitting are in Figure Set 12.

We searched for trends in the amplitude ratios between the first and second gamma-ray peaks as a function of energy, for pulsars with at least two identifiable components. Assuming that the first two components have spectra that follow exponentially cutoff power laws, the amplitude ratio can be written as follows:

$$ \log_{10}\left(\frac{\text{Amp}_2}{\text{Amp}_1}\right) = C - (\Gamma_2 - \Gamma_1) \times \log_{10}(E) \\ - (1/E_{c,2} - 1/E_{c,1}) \times E/\ln 10, \quad (12) $$

where $C$ is an energy-independent constant, and $\Gamma_i$ and $E_{c,i}$, respectively, denote the spectral index and cutoff energy of the
<table><caption>**Table 10**
Pulse Shape Parameters of LAT-detected MSPs</caption><thead><tr><th>PSR</th><th>Peaks</th><th>Radio/Gamma Phase Lag, δ</th><th>Peak Separation, Δ</th><th>Comment</th><th>Radio Class</th></tr></thead><tbody><tr><td>J0023+0923</td><td>2</td><td>0.321 ± 0.022</td><td>0.280 ± 0.027</td><td></td><td>1</td></tr><tr><td>J0030+0451</td><td>5</td><td>0.1266 ± 0.0014</td><td>0.4485 ± 0.0004</td><td></td><td>2</td></tr><tr><td>J0034-0534</td><td>2</td><td>0.839 ± 0.004</td><td>0.319 ± 0.006</td><td></td><td>1</td></tr><tr><td>J0101-6422</td><td>4</td><td>0.6733 ± 0.0032</td><td>0.4053 ± 0.0031</td><td>c</td><td>1</td></tr><tr><td>J0102+4839</td><td>2</td><td>0.327 ± 0.007</td><td>0.444 ± 0.007</td><td></td><td>1</td></tr><tr><td>J0218+4232</td><td>1</td><td>0.691 ± 0.006</td><td>...</td><td></td><td>1</td></tr><tr><td>J0251+2606</td><td>2</td><td>0.157 ± 0.007</td><td>0.522 ± 0.007</td><td></td><td>1</td></tr><tr><td>J0307+7443</td><td>2</td><td>0.935 ± 0.008</td><td>0.645 ± 0.013</td><td></td><td>1</td></tr><tr><td>J0312-0921</td><td>2</td><td>0.255<sup>+0.010</sup><sub>-0.013</sub></td><td>0.453<sup>+0.008</sup><sub>-0.012</sub></td><td></td><td>1</td></tr><tr><td>J0340+4130</td><td>2</td><td>0.7501 ± 0.0027</td><td>0.239 ± 0.004</td><td></td><td>1</td></tr><tr><td>J0418+6635</td><td>3</td><td>0.737 ± 0.017</td><td>0.391 ± 0.005</td><td></td><td>3</td></tr><tr><td>J0437-4715</td><td>1</td><td>0.4299 ± 0.0023</td><td>...</td><td></td><td>2</td></tr><tr><td>J0533+6759</td><td>2</td><td>0.175 ± 0.005</td><td>0.5270<sup>+0.0018</sup><sub>-0.0028</sub></td><td></td><td>1</td></tr><tr><td>J0605+3757</td><td>2</td><td>0.812 ± 0.027</td><td>0.47<sup>+0.05</sup><sub>-0.04</sub></td><td>u</td><td>2</td></tr><tr><td>J0610-2100</td><td>3</td><td>0.615 ± 0.004</td><td>0.53<sup>+0.04</sup><sub>-0.07</sub></td><td></td><td>1</td></tr><tr><td>J0613-0200</td><td>2</td><td>0.224 ± 0.014</td><td>0.159 ± 0.014</td><td></td><td>2</td></tr><tr><td>J0614-3329</td><td>2</td><td>0.1293 ± 0.0005</td><td>0.5558 ± 0.0004</td><td></td><td>2</td></tr><tr><td>J0621+2514</td><td>2</td><td>0.340 ± 0.030</td><td>0.388 ± 0.032</td><td></td><td>2</td></tr><tr><td>J0737-3039A</td><td>2</td><td>0.137<sup>+0.009</sup><sub>-0.011</sub></td><td>0.506 ± 0.012</td><td>u</td><td>3</td></tr><tr><td>J0740+6620</td><td>2</td><td>0.1964<sup>+0.0028</sup><sub>-0.0020</sub></td><td>0.4622 ± 0.0029</td><td></td><td>3</td></tr><tr><td>J0751+1807</td><td>2</td><td>0.3694 ± 0.0033</td><td>0.272 ± 0.007</td><td></td><td>1</td></tr><tr><td>J0931-1902</td><td>1</td><td>0.040<sup>+0.030</sup><sub>-0.020</sub></td><td>...</td><td></td><td>4</td></tr><tr><td>J0952-0607</td><td>1</td><td>0.053 ± 0.029</td><td>...</td><td></td><td>1</td></tr><tr><td>J0955-6150</td><td>2</td><td>0.883 ± 0.014</td><td>0.479 ± 0.016</td><td></td><td>1</td></tr><tr><td>J1012-4235</td><td>2</td><td>0.290 ± 0.005</td><td>0.496 ± 0.008</td><td></td><td>1</td></tr><tr><td>J1024-0719</td><td>1</td><td>0.561 ± 0.024</td><td>...</td><td></td><td>2</td></tr><tr><td>J1035-6720</td><td>2</td><td>0.307<sup>+0.014</sup><sub>-0.011</sub></td><td>0.528 ± 0.016</td><td></td><td>1</td></tr><tr><td>J1036-8317</td><td>1</td><td>0.273 ± 0.019</td><td>...</td><td></td><td>1</td></tr><tr><td>J1048+2339</td><td>2</td><td>0.1371 ± 0.0032</td><td>0.518<sup>+0.005</sup><sub>-0.011</sub></td><td></td><td>1</td></tr><tr><td>J1124-3653</td><td>3</td><td>0.259 ± 0.010</td><td>0.394 ± 0.005</td><td>c</td><td>1</td></tr><tr><td>J1125-5825</td><td>2</td><td>0.211<sup>+0.021</sup><sub>-0.011</sub></td><td>0.402<sup>+0.020</sup><sub>-0.010</sub></td><td></td><td>2</td></tr><tr><td>J1142+0119</td><td>1</td><td>0.994<sup>+0.003</sup><sub>-0.006</sub></td><td>...</td><td></td><td>1</td></tr><tr><td>J1207-5050</td><td>2</td><td>0.255 ± 0.006</td><td>0.520<sup>+0.006</sup><sub>-0.013</sub></td><td></td><td>1</td></tr><tr><td>J1221-0633</td><td>1</td><td>0.625<sup>+0.015</sup><sub>-0.009</sub></td><td>...</td><td></td><td>3</td></tr><tr><td>J1227-4853</td><td>3</td><td>0.656<sup>+0.013</sup><sub>-0.022</sub></td><td>0.407<sup>+0.015</sup><sub>-0.024</sub></td><td>c</td><td>1</td></tr><tr><td>J1231-1411</td><td>4</td><td>0.2341 ± 0.0011</td><td>0.4056 ± 0.0010</td><td>c</td><td>2</td></tr><tr><td>J1301+0833</td><td>2</td><td>0.104 ± 0.016</td><td>0.393 ± 0.024</td><td></td><td>1</td></tr><tr><td>J1302-3258</td><td>2</td><td>0.147 ± 0.004</td><td>0.394 ± 0.008</td><td></td><td>3</td></tr><tr><td>J1311-3430</td><td>3</td><td>0.906 ± 0.018</td><td>0.3629 ± 0.0017</td><td></td><td>1</td></tr><tr><td>J1312+0051</td><td>2</td><td>0.914 ± 0.019</td><td>0.690 ± 0.020</td><td>u</td><td>3</td></tr><tr><td>J1335-5656</td><td>2</td><td>...</td><td>0.209 ± 0.016</td><td></td><td>...</td></tr><tr><td>J1400-1431</td><td>1</td><td>0.913 ± 0.013</td><td>...</td><td></td><td>1</td></tr><tr><td>J1446-4701</td><td>2</td><td>0.339 ± 0.008</td><td>0.236 ± 0.015</td><td></td><td>1</td></tr><tr><td>J1455-3330</td><td>1</td><td>0.167<sup>+0.021</sup><sub>-0.011</sub></td><td>...</td><td></td><td>2</td></tr><tr><td>J1513-2550</td><td>2</td><td>0.983<sup>+0.005</sup><sub>-0.002</sub></td><td>0.413<sup>+0.005</sup><sub>-0.003</sub></td><td></td><td>3</td></tr><tr><td>J1514-4946</td><td>3</td><td>0.273 ± 0.004</td><td>0.3829<sup>+0.0013</sup><sub>-0.0022</sub></td><td></td><td>1</td></tr><tr><td>J1536-4948</td><td>6</td><td>0.429 ± 0.007</td><td>0.5934 ± 0.0030</td><td>c</td><td>3</td></tr><tr><td>J1543-5149</td><td>1</td><td>0.959 ± 0.015</td><td>...</td><td></td><td>1</td></tr><tr><td>J1552+5437</td><td>2</td><td>0.46<sup>+0.06</sup><sub>-0.03</sub></td><td>0.55<sup>+0.06</sup><sub>-0.04</sub></td><td></td><td>1</td></tr><tr><td>J1555-2908</td><td>2</td><td>0.029 ± 0.004</td><td>0.554 ± 0.007</td><td></td><td>3</td></tr><tr><td>J1600-3053</td><td>2</td><td>0.212 ± 0.007</td><td>0.186 ± 0.015</td><td></td><td>1</td></tr><tr><td>J1614-2230</td><td>3</td><td>0.1716<sup>+0.0017</sup><sub>-0.0013</sub></td><td>0.5312<sup>+0.0017</sup><sub>-0.0014</sub></td><td></td><td>1</td></tr><tr><td>J1625-0021</td><td>2</td><td>0.992 ± 0.005</td><td>0.482<sup>+0.022</sup><sub>-0.012</sub></td><td></td><td>1</td></tr><tr><td>J1628-3205</td><td>2</td><td>0.244 ± 0.016</td><td>0.42<sup>+0.03</sup><sub>-0.07</sub></td><td></td><td>1</td></tr><tr><td>J1630+3734</td><td>2</td><td>0.2544 ± 0.0013</td><td>0.4567 ± 0.0023</td><td></td><td>3</td></tr><tr><td>J1640+2224</td><td>2</td><td>0.332 ± 0.031</td><td>0.185 ± 0.033</td><td></td><td>2</td></tr><tr><td>J1641+8049</td><td>2</td><td>0.108<sup>+0.003</sup><sub>-0.005</sub></td><td>0.392<sup>+0.015</sup><sub>-0.029</sub></td><td></td><td>1</td></tr><tr><td>J1649-3012</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1653-0158</td><td>2</td><td>...</td><td>0.420 ± 0.014</td><td></td><td>...</td></tr><tr><td>J1658-5324</td><td>2</td><td>0.105 ± 0.026</td><td>0.270 ± 0.025</td><td>u</td><td>4</td></tr><tr><td>J1713+0747</td><td>1</td><td>0.318 ± 0.016</td><td>...</td><td></td><td>2</td></tr><tr><td>J1730-2304</td><td>1</td><td>0.300<sup>+0.014</sup><sub>-0.009</sub></td><td>...</td><td></td><td>2</td></tr></tbody></table>
<table><caption>**Table 10**
Pulse Shape Parameters of LAT-detected MSPs</caption><thead><tr><th>PSR</th><th>Peaks</th><th>Radio/Gamma Phase Lag, δ</th><th>Peak Separation, Δ</th><th>Comment</th><th>Radio Class</th></tr></thead><tbody><tr><td>J0023+0923</td><td>2</td><td>0.321 ± 0.022</td><td>0.280 ± 0.027</td><td></td><td>1</td></tr><tr><td>J0030+0451</td><td>5</td><td>0.1266 ± 0.0014</td><td>0.4485 ± 0.0004</td><td></td><td>2</td></tr><tr><td>J0034-0534</td><td>2</td><td>0.839 ± 0.004</td><td>0.319 ± 0.006</td><td></td><td>1</td></tr><tr><td>J0101-6422</td><td>4</td><td>0.6733 ± 0.0032</td><td>0.4053 ± 0.0031</td><td>c</td><td>1</td></tr><tr><td>J0102+4839</td><td>2</td><td>0.327 ± 0.007</td><td>0.444 ± 0.007</td><td></td><td>1</td></tr><tr><td>J0218+4232</td><td>1</td><td>0.691 ± 0.006</td><td>...</td><td></td><td>1</td></tr><tr><td>J0251+2606</td><td>2</td><td>0.157 ± 0.007</td><td>0.522 ± 0.007</td><td></td><td>1</td></tr><tr><td>J0307+7443</td><td>2</td><td>0.935 ± 0.008</td><td>0.645 ± 0.013</td><td></td><td>1</td></tr><tr><td>J0312-0921</td><td>2</td><td>0.255<sup>+0.010</sup><sub>-0.013</sub></td><td>0.453<sup>+0.008</sup><sub>-0.012</sub></td><td></td><td>1</td></tr><tr><td>J0340+4130</td><td>2</td><td>0.7501 ± 0.0027</td><td>0.239 ± 0.004</td><td></td><td>1</td></tr><tr><td>J0418+6635</td><td>3</td><td>0.737 ± 0.017</td><td>0.391 ± 0.005</td><td></td><td>3</td></tr><tr><td>J0437-4715</td><td>1</td><td>0.4299 ± 0.0023</td><td>...</td><td></td><td>2</td></tr><tr><td>J0533+6759</td><td>2</td><td>0.175 ± 0.005</td><td>0.5270<sup>+0.0018</sup><sub>-0.0028</sub></td><td></td><td>1</td></tr><tr><td>J0605+3757</td><td>2</td><td>0.812 ± 0.027</td><td>0.47<sup>+0.05</sup><sub>-0.04</sub></td><td>u</td><td>2</td></tr><tr><td>J0610-2100</td><td>3</td><td>0.615 ± 0.004</td><td>0.53<sup>+0.04</sup><sub>-0.07</sub></td><td></td><td>1</td></tr><tr><td>J0613-0200</td><td>2</td><td>0.224 ± 0.014</td><td>0.159 ± 0.014</td><td></td><td>2</td></tr><tr><td>J0614-3329</td><td>2</td><td>0.1293 ± 0.0005</td><td>0.5558 ± 0.0004</td><td></td><td>2</td></tr><tr><td>J0621+2514</td><td>2</td><td>0.340 ± 0.030</td><td>0.388 ± 0.032</td><td></td><td>2</td></tr><tr><td>J0737-3039A</td><td>2</td><td>0.137<sup>+0.009</sup><sub>-0.011</sub></td><td>0.506 ± 0.012</td><td>u</td><td>3</td></tr><tr><td>J0740+6620</td><td>2</td><td>0.1964<sup>+0.0028</sup><sub>-0.0020</sub></td><td>0.4622 ± 0.0029</td><td></td><td>3</td></tr><tr><td>J0751+1807</td><td>2</td><td>0.3694 ± 0.0033</td><td>0.272 ± 0.007</td><td></td><td>1</td></tr><tr><td>J0931-1902</td><td>1</td><td>0.040<sup>+0.030</sup><sub>-0.020</sub></td><td>...</td><td></td><td>4</td></tr><tr><td>J0952-0607</td><td>1</td><td>0.053 ± 0.029</td><td>...</td><td></td><td>1</td></tr><tr><td>J0955-6150</td><td>2</td><td>0.883 ± 0.014</td><td>0.479 ± 0.016</td><td></td><td>1</td></tr><tr><td>J1012-4235</td><td>2</td><td>0.290 ± 0.005</td><td>0.496 ± 0.008</td><td></td><td>1</td></tr><tr><td>J1024-0719</td><td>1</td><td>0.561 ± 0.024</td><td>...</td><td></td><td>2</td></tr><tr><td>J1035-6720</td><td>2</td><td>0.307<sup>+0.014</sup><sub>-0.011</sub></td><td>0.528 ± 0.016</td><td></td><td>1</td></tr><tr><td>J1036-8317</td><td>1</td><td>0.273 ± 0.019</td><td>...</td><td></td><td>1</td></tr><tr><td>J1048+2339</td><td>2</td><td>0.1371 ± 0.0032</td><td>0.518<sup>+0.005</sup><sub>-0.011</sub></td><td></td><td>1</td></tr><tr><td>J1124-3653</td><td>3</td><td>0.259 ± 0.010</td><td>0.394 ± 0.005</td><td>c</td><td>1</td></tr><tr><td>J1125-5825</td><td>2</td><td>0.211<sup>+0.021</sup><sub>-0.011</sub></td><td>0.402<sup>+0.020</sup><sub>-0.010</sub></td><td></td><td>2</td></tr><tr><td>J1142+0119</td><td>1</td><td>0.994<sup>+0.003</sup><sub>-0.006</sub></td><td>...</td><td></td><td>1</td></tr><tr><td>J1207-5050</td><td>2</td><td>0.255 ± 0.006</td><td>0.520<sup>+0.006</sup><sub>-0.013</sub></td><td></td><td>1</td></tr><tr><td>J1221-0633</td><td>1</td><td>0.625<sup>+0.015</sup><sub>-0.009</sub></td><td>...</td><td></td><td>3</td></tr><tr><td>J1227-4853</td><td>3</td><td>0.656<sup>+0.013</sup><sub>-0.022</sub></td><td>0.407<sup>+0.015</sup><sub>-0.024</sub></td><td>c</td><td>1</td></tr><tr><td>J1231-1411</td><td>4</td><td>0.2341 ± 0.0011</td><td>0.4056 ± 0.0010</td><td>c</td><td>2</td></tr><tr><td>J1301+0833</td><td>2</td><td>0.104 ± 0.016</td><td>0.393 ± 0.024</td><td></td><td>1</td></tr><tr><td>J1302-3258</td><td>2</td><td>0.147 ± 0.004</td><td>0.394 ± 0.008</td><td></td><td>3</td></tr><tr><td>J1311-3430</td><td>3</td><td>0.906 ± 0.018</td><td>0.3629 ± 0.0017</td><td></td><td>1</td></tr><tr><td>J1312+0051</td><td>2</td><td>0.914 ± 0.019</td><td>0.690 ± 0.020</td><td>u</td><td>3</td></tr><tr><td>J1335-5656</td><td>2</td><td>...</td><td>0.209 ± 0.016</td><td></td><td>...</td></tr><tr><td>J1400-1431</td><td>1</td><td>0.913 ± 0.013</td><td>...</td><td></td><td>1</td></tr><tr><td>J1446-4701</td><td>2</td><td>0.339 ± 0.008</td><td>0.236 ± 0.015</td><td></td><td>1</td></tr><tr><td>J1455-3330</td><td>1</td><td>0.167<sup>+0.021</sup><sub>-0.011</sub></td><td>...</td><td></td><td>2</td></tr><tr><td>J1513-2550</td><td>2</td><td>0.983<sup>+0.005</sup><sub>-0.002</sub></td><td>0.413<sup>+0.005</sup><sub>-0.003</sub></td><td></td><td>3</td></tr><tr><td>J1514-4946</td><td>3</td><td>0.273 ± 0.004</td><td>0.3829<sup>+0.0013</sup><sub>-0.0022</sub></td><td></td><td>1</td></tr><tr><td>J1536-4948</td><td>6</td><td>0.429 ± 0.007</td><td>0.5934 ± 0.0030</td><td>c</td><td>3</td></tr><tr><td>J1543-5149</td><td>1</td><td>0.959 ± 0.015</td><td>...</td><td></td><td>1</td></tr><tr><td>J1552+5437</td><td>2</td><td>0.46<sup>+0.06</sup><sub>-0.03</sub></td><td>0.55<sup>+0.06</sup><sub>-0.04</sub></td><td></td><td>1</td></tr><tr><td>J1555-2908</td><td>2</td><td>0.029 ± 0.004</td><td>0.554 ± 0.007</td><td></td><td>3</td></tr><tr><td>J1600-3053</td><td>2</td><td>0.212 ± 0.007</td><td>0.186 ± 0.015</td><td></td><td>1</td></tr><tr><td>J1614-2230</td><td>3</td><td>0.1716<sup>+0.0017</sup><sub>-0.0013</sub></td><td>0.5312<sup>+0.0017</sup><sub>-0.0014</sub></td><td></td><td>1</td></tr><tr><td>J1625-0021</td><td>2</td><td>0.992 ± 0.005</td><td>0.482<sup>+0.022</sup><sub>-0.012</sub></td><td></td><td>1</td></tr><tr><td>J1628-3205</td><td>2</td><td>0.244 ± 0.016</td><td>0.42<sup>+0.03</sup><sub>-0.07</sub></td><td></td><td>1</td></tr><tr><td>J1630+3734</td><td>2</td><td>0.2544 ± 0.0013</td><td>0.4567 ± 0.0023</td><td></td><td>3</td></tr><tr><td>J1640+2224</td><td>2</td><td>0.332 ± 0.031</td><td>0.185 ± 0.033</td><td></td><td>2</td></tr><tr><td>J1641+8049</td><td>2</td><td>0.108<sup>+0.003</sup><sub>-0.005</sub></td><td>0.392<sup>+0.015</sup><sub>-0.029</sub></td><td></td><td>1</td></tr><tr><td>J1649-3012</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1653-0158</td><td>2</td><td>...</td><td>0.420 ± 0.014</td><td></td><td>...</td></tr><tr><td>J1658-5324</td><td>2</td><td>0.105 ± 0.026</td><td>0.270 ± 0.025</td><td>u</td><td>4</td></tr><tr><td>J1713+0747</td><td>1</td><td>0.318 ± 0.016</td><td>...</td><td></td><td>2</td></tr><tr><td>J1730-2304</td><td>1</td><td>0.300<sup>+0.014</sup><sub>-0.009</sub></td><td>...</td><td></td><td>2</td></tr></tbody></table>
<table><caption>**Table 10**
(Continued)</caption><thead><tr><th>PSR</th><th>Peaks</th><th>Radio/Gamma Phase Lag, δ</th><th>Peak Separation, Δ</th><th>Comment</th><th>Radio Class</th></tr></thead><tbody><tr><td>J1732-5049</td><td>1</td><td>0.617<sup>+0.004</sup><sub>-0.006</sub></td><td>...</td><td></td><td>2</td></tr><tr><td>J1741+1351</td><td>2</td><td>0.710<sup>+0.007</sup><sub>-0.003</sub></td><td>0.519<sup>+0.007</sup><sub>-0.003</sub></td><td>u</td><td>1</td></tr><tr><td>J1744-1134</td><td>2</td><td>0.8116 ± 0.0029</td><td>0.727 ± 0.022</td><td>u</td><td>1</td></tr><tr><td>J1744-7619</td><td>2</td><td>...</td><td>0.343 ± 0.008</td><td></td><td>...</td></tr><tr><td>J1745+1017</td><td>1</td><td>0.988<sup>+0.006</sup><sub>-0.003</sub></td><td>...</td><td></td><td>1</td></tr><tr><td>J1747-4036</td><td>1</td><td>0.877 ± 0.013</td><td>...</td><td></td><td>1</td></tr><tr><td>J1805+0615</td><td>2</td><td>0.851<sup>+0.08</sup><sub>-0.04</sub></td><td>0.431<sup>+0.08</sup><sub>-0.04</sub></td><td></td><td>1</td></tr><tr><td>J1810+1744</td><td>2</td><td>0.050 ± 0.013</td><td>0.243 ± 0.015</td><td></td><td>2</td></tr><tr><td>J1811-2405</td><td>2</td><td>0.145<sup>+0.022</sup><sub>-0.012</sub></td><td>0.397<sup>+0.023</sup><sub>-0.014</sub></td><td></td><td>3</td></tr><tr><td>J1816+4510</td><td>3</td><td>0.5300 ± 0.0029</td><td>0.481 ± 0.005</td><td></td><td>1</td></tr><tr><td>J1823-3021A</td><td>2</td><td>0.980 ± 0.004</td><td>0.390 ± 0.005</td><td></td><td>1</td></tr><tr><td>J1824-2452A</td><td>2</td><td>0.669 ± 0.031</td><td>0.530 ± 0.034</td><td></td><td>3</td></tr><tr><td>J1827-0849</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1832-0836</td><td>1</td><td>0.7466<sup>+0.0023</sup><sub>-0.0016</sub></td><td>...</td><td></td><td>4</td></tr><tr><td>J1843-1113</td><td>1</td><td>0.060<sup>+0.013</sup><sub>-0.017</sub></td><td>...</td><td></td><td>1</td></tr><tr><td>J1855-1436</td><td>1</td><td>0.890<sup>+0.013</sup><sub>-0.017</sub></td><td>...</td><td></td><td>1</td></tr><tr><td>J1858-2216</td><td>2</td><td>0.748 ± 0.006</td><td>0.306 ± 0.014</td><td></td><td>3</td></tr><tr><td>J1901-0125</td><td>3</td><td>0.866 ± 0.007</td><td>0.378 ± 0.008</td><td></td><td>1</td></tr><tr><td>J1902-5105</td><td>3</td><td>0.015 ± 0.004</td><td>0.645 ± 0.004</td><td></td><td>1</td></tr><tr><td>J1903-7051</td><td>1</td><td>0.531 ± 0.012</td><td>...</td><td></td><td>1</td></tr><tr><td>J1908+2105</td><td>2</td><td>0.778<sup>+0.008</sup><sub>-0.012</sub></td><td>0.419 ± 0.016</td><td></td><td>1</td></tr><tr><td>J1921+0137</td><td>2</td><td>0.134 ± 0.030</td><td>0.362 ± 0.032</td><td></td><td>1</td></tr><tr><td>J1939+2134</td><td>2</td><td>0.970<sup>+0.005</sup><sub>-0.001</sub></td><td>0.529<sup>+0.009</sup><sub>-0.006</sub></td><td></td><td>2</td></tr><tr><td>J1946-5403</td><td>3</td><td>0.151<sup>+0.05</sup><sub>-0.02</sub></td><td>0.551<sup>+0.05</sup><sub>-0.02</sub></td><td>c</td><td>1</td></tr><tr><td>J1959+2048</td><td>2</td><td>0.9953 ± 0.0014</td><td>0.566 ± 0.007</td><td></td><td>4</td></tr><tr><td>J2006+0148</td><td>2</td><td>0.659<sup>+0.035</sup><sub>-0.021</sub></td><td>0.231<sup>+0.035</sup><sub>-0.021</sub></td><td></td><td>1</td></tr><tr><td>J2017+0603</td><td>2</td><td>0.2244 ± 0.0027</td><td>0.2955 ± 0.0035</td><td></td><td>3</td></tr><tr><td>J2017-1614</td><td>2</td><td>0.183 ± 0.014</td><td>0.459<sup>+0.017</sup><sub>-0.013</sub></td><td></td><td>3</td></tr><tr><td>J2034+3632</td><td>3</td><td>...</td><td>0.225<sup>+0.007</sup><sub>-0.011</sub></td><td></td><td>...</td></tr><tr><td>J2039-3616</td><td>1</td><td>0.274<sup>+0.008</sup><sub>-0.010</sub></td><td>...</td><td></td><td>2</td></tr><tr><td>J2039-5617</td><td>3</td><td>0.107 ± 0.007</td><td>0.296 ± 0.009</td><td></td><td>1</td></tr><tr><td>J2042+0246</td><td>1</td><td>0.766 ± 0.008</td><td>...</td><td>u</td><td>1</td></tr><tr><td>J2043+1711</td><td>3</td><td>0.2503 ± 0.0028</td><td>0.4479 ± 0.0027</td><td></td><td>3</td></tr><tr><td>J2047+1053</td><td>2</td><td>0.219<sup>+0.032</sup><sub>-0.017</sub></td><td>0.330<sup>+0.033</sup><sub>-0.020</sub></td><td></td><td>1</td></tr><tr><td>J2051-0827</td><td>1</td><td>0.381<sup>+0.06</sup><sub>-0.03</sub></td><td>...</td><td></td><td>2</td></tr><tr><td>J2052+1219</td><td>2</td><td>0.675 ± 0.011</td><td>0.381 ± 0.012</td><td></td><td>1</td></tr><tr><td>J2115+5448</td><td>2</td><td>0.146<sup>+0.005</sup><sub>-0.007</sub></td><td>0.386<sup>+0.006</sup><sub>-0.008</sub></td><td></td><td>3</td></tr><tr><td>J2124-3358</td><td>3</td><td>0.8532 ± 0.0026</td><td>0.744 ± 0.009</td><td></td><td>3</td></tr><tr><td>J2129-0429</td><td>3</td><td>0.6694 ± 0.0032</td><td>0.501<sup>+0.003</sup><sub>-0.004</sub></td><td></td><td>3</td></tr><tr><td>J2214+3000</td><td>2</td><td>0.324<sup>+0.007</sup><sub>-0.009</sub></td><td>0.484 ± 0.012</td><td>u</td><td>1</td></tr><tr><td>J2215+5135</td><td>3</td><td>0.573 ± 0.004</td><td>0.447 ± 0.004</td><td></td><td>1</td></tr><tr><td>J2234+0944</td><td>2</td><td>0.680 ± 0.010</td><td>0.187 ± 0.018</td><td></td><td>3</td></tr><tr><td>J2241-5236</td><td>5</td><td>0.1219<sup>+0.0030</sup><sub>-0.0015</sub></td><td>0.317 ± 0.024</td><td>c</td><td>1</td></tr><tr><td>J2256-1024</td><td>2</td><td>0.1510 ± 0.0010</td><td>0.4750<sup>+0.0015</sup><sub>-0.0010</sub></td><td></td><td>2</td></tr><tr><td>J2302+4442</td><td>3</td><td>0.2318 ± 0.0020</td><td>0.3350 ± 0.0021</td><td></td><td>2</td></tr><tr><td>J2310-0555</td><td>2</td><td>0.877<sup>+0.007</sup><sub>-0.012</sub></td><td>0.450<sup>+0.008</sup><sub>-0.013</sub></td><td></td><td>3</td></tr><tr><td>J2339-0533</td><td>3</td><td>0.3036 ± 0.0034</td><td>0.3734 ± 0.0027</td><td></td><td>2</td></tr></tbody></table>

Note. Same as Table 9, for the gamma-ray MSPs.

th component. The top panel of Figure 12 shows the fit using the above expression, and the best-fit parameters.

Figures 13 and 14 show the values of the $\Gamma_2 - \Gamma_1$ and $(1/E_{c,2} - 1/E_{c,1})$ parameters, for pulsars with at least six energy intervals with individual H-test $TS > 300$. Requiring $\ge 6$ data points gives the fit of Equation (12) enough data points and a wide energy range. The minimum detection significance in the energy bins restricts the study to high-quality profile fits. These criteria select 28 pulsars. Figure 12.2 shows that the

measured amplitude ratios between the first and second peaks for PSR J0007+7303 are poorly fit; we hence discarded this pulsar, reducing the sample to 27 objects. The choice of $B_{LC}$ in Figures 13 and 14 is arbitrary; we saw little or no correlation with various abscissa parameters, as discussed further in Section 8. Table 12 summarizes the results for the 27 pulsars. The weighted averages of $\Gamma_2 - \Gamma_1$ and $(1/E_{c,2} - 1/E_{c,1})$ are, respectively, $-0.209(2)$ and $-0.044(1)$ GeV$^{-1}$, clearly incompatible with 0 but dominated by a few measurements with very
<table><caption>**Table 10**
(Continued)</caption><thead><tr><th>PSR</th><th>Peaks</th><th>Radio/Gamma Phase Lag, δ</th><th>Peak Separation, Δ</th><th>Comment</th><th>Radio Class</th></tr></thead><tbody><tr><td>J1732-5049</td><td>1</td><td>0.617<sup>+0.004</sup><sub>-0.006</sub></td><td>...</td><td></td><td>2</td></tr><tr><td>J1741+1351</td><td>2</td><td>0.710<sup>+0.007</sup><sub>-0.003</sub></td><td>0.519<sup>+0.007</sup><sub>-0.003</sub></td><td>u</td><td>1</td></tr><tr><td>J1744-1134</td><td>2</td><td>0.8116 ± 0.0029</td><td>0.727 ± 0.022</td><td>u</td><td>1</td></tr><tr><td>J1744-7619</td><td>2</td><td>...</td><td>0.343 ± 0.008</td><td></td><td>...</td></tr><tr><td>J1745+1017</td><td>1</td><td>0.988<sup>+0.006</sup><sub>-0.003</sub></td><td>...</td><td></td><td>1</td></tr><tr><td>J1747-4036</td><td>1</td><td>0.877 ± 0.013</td><td>...</td><td></td><td>1</td></tr><tr><td>J1805+0615</td><td>2</td><td>0.851<sup>+0.08</sup><sub>-0.04</sub></td><td>0.431<sup>+0.08</sup><sub>-0.04</sub></td><td></td><td>1</td></tr><tr><td>J1810+1744</td><td>2</td><td>0.050 ± 0.013</td><td>0.243 ± 0.015</td><td></td><td>2</td></tr><tr><td>J1811-2405</td><td>2</td><td>0.145<sup>+0.022</sup><sub>-0.012</sub></td><td>0.397<sup>+0.023</sup><sub>-0.014</sub></td><td></td><td>3</td></tr><tr><td>J1816+4510</td><td>3</td><td>0.5300 ± 0.0029</td><td>0.481 ± 0.005</td><td></td><td>1</td></tr><tr><td>J1823-3021A</td><td>2</td><td>0.980 ± 0.004</td><td>0.390 ± 0.005</td><td></td><td>1</td></tr><tr><td>J1824-2452A</td><td>2</td><td>0.669 ± 0.031</td><td>0.530 ± 0.034</td><td></td><td>3</td></tr><tr><td>J1827-0849</td><td>1</td><td>...</td><td>...</td><td></td><td>...</td></tr><tr><td>J1832-0836</td><td>1</td><td>0.7466<sup>+0.0023</sup><sub>-0.0016</sub></td><td>...</td><td></td><td>4</td></tr><tr><td>J1843-1113</td><td>1</td><td>0.060<sup>+0.013</sup><sub>-0.017</sub></td><td>...</td><td></td><td>1</td></tr><tr><td>J1855-1436</td><td>1</td><td>0.890<sup>+0.013</sup><sub>-0.017</sub></td><td>...</td><td></td><td>1</td></tr><tr><td>J1858-2216</td><td>2</td><td>0.748 ± 0.006</td><td>0.306 ± 0.014</td><td></td><td>3</td></tr><tr><td>J1901-0125</td><td>3</td><td>0.866 ± 0.007</td><td>0.378 ± 0.008</td><td></td><td>1</td></tr><tr><td>J1902-5105</td><td>3</td><td>0.015 ± 0.004</td><td>0.645 ± 0.004</td><td></td><td>1</td></tr><tr><td>J1903-7051</td><td>1</td><td>0.531 ± 0.012</td><td>...</td><td></td><td>1</td></tr><tr><td>J1908+2105</td><td>2</td><td>0.778<sup>+0.008</sup><sub>-0.012</sub></td><td>0.419 ± 0.016</td><td></td><td>1</td></tr><tr><td>J1921+0137</td><td>2</td><td>0.134 ± 0.030</td><td>0.362 ± 0.032</td><td></td><td>1</td></tr><tr><td>J1939+2134</td><td>2</td><td>0.970<sup>+0.005</sup><sub>-0.001</sub></td><td>0.529<sup>+0.009</sup><sub>-0.006</sub></td><td></td><td>2</td></tr><tr><td>J1946-5403</td><td>3</td><td>0.15<sup>+0.05</sup><sub>-0.02</sub></td><td>0.551<sup>+0.05</sup><sub>-0.02</sub></td><td>c</td><td>1</td></tr><tr><td>J1959+2048</td><td>2</td><td>0.9953 ± 0.0014</td><td>0.566 ± 0.007</td><td></td><td>4</td></tr><tr><td>J2006+0148</td><td>2</td><td>0.659<sup>+0.035</sup><sub>-0.021</sub></td><td>0.231<sup>+0.035</sup><sub>-0.021</sub></td><td></td><td>1</td></tr><tr><td>J2017+0603</td><td>2</td><td>0.2244 ± 0.0027</td><td>0.2955 ± 0.0035</td><td></td><td>3</td></tr><tr><td>J2017-1614</td><td>2</td><td>0.183 ± 0.014</td><td>0.459<sup>+0.017</sup><sub>-0.013</sub></td><td></td><td>3</td></tr><tr><td>J2034+3632</td><td>3</td><td>...</td><td>0.225<sup>+0.007</sup><sub>-0.011</sub></td><td></td><td>...</td></tr><tr><td>J2039-3616</td><td>1</td><td>0.274<sup>+0.008</sup><sub>-0.010</sub></td><td>...</td><td></td><td>2</td></tr><tr><td>J2039-5617</td><td>3</td><td>0.107 ± 0.007</td><td>0.296 ± 0.009</td><td></td><td>1</td></tr><tr><td>J2042+0246</td><td>1</td><td>0.766 ± 0.008</td><td>...</td><td>u</td><td>1</td></tr><tr><td>J2043+1711</td><td>3</td><td>0.2503 ± 0.0028</td><td>0.4479 ± 0.0027</td><td></td><td>3</td></tr><tr><td>J2047+1053</td><td>2</td><td>0.219<sup>+0.032</sup><sub>-0.017</sub></td><td>0.330<sup>+0.033</sup><sub>-0.020</sub></td><td></td><td>1</td></tr><tr><td>J2051-0827</td><td>1</td><td>0.38<sup>+0.06</sup><sub>-0.03</sub></td><td>...</td><td></td><td>2</td></tr><tr><td>J2052+1219</td><td>2</td><td>0.675 ± 0.011</td><td>0.381 ± 0.012</td><td></td><td>1</td></tr><tr><td>J2115+5448</td><td>2</td><td>0.146<sup>+0.005</sup><sub>-0.007</sub></td><td>0.386<sup>+0.006</sup><sub>-0.008</sub></td><td></td><td>3</td></tr><tr><td>J2124-3358</td><td>3</td><td>0.8532 ± 0.0026</td><td>0.744 ± 0.009</td><td></td><td>3</td></tr><tr><td>J2129-0429</td><td>3</td><td>0.6694 ± 0.0032</td><td>0.501<sup>+0.003</sup><sub>-0.004</sub></td><td></td><td>3</td></tr><tr><td>J2214+3000</td><td>2</td><td>0.324<sup>+0.007</sup><sub>-0.009</sub></td><td>0.484 ± 0.012</td><td>u</td><td>1</td></tr><tr><td>J2215+5135</td><td>3</td><td>0.573 ± 0.004</td><td>0.447 ± 0.004</td><td></td><td>1</td></tr><tr><td>J2234+0944</td><td>2</td><td>0.680 ± 0.010</td><td>0.187 ± 0.018</td><td></td><td>3</td></tr><tr><td>J2241-5236</td><td>5</td><td>0.1219<sup>+0.0030</sup><sub>-0.0015</sub></td><td>0.317 ± 0.024</td><td>c</td><td>1</td></tr><tr><td>J2256-1024</td><td>2</td><td>0.1510 ± 0.0010</td><td>0.4750<sup>+0.0015</sup><sub>-0.0010</sub></td><td></td><td>2</td></tr><tr><td>J2302+4442</td><td>3</td><td>0.2318 ± 0.0020</td><td>0.3350 ± 0.0021</td><td></td><td>2</td></tr><tr><td>J2310-0555</td><td>2</td><td>0.877<sup>+0.007</sup><sub>-0.012</sub></td><td>0.450<sup>+0.008</sup><sub>-0.013</sub></td><td></td><td>3</td></tr><tr><td>J2339-0533</td><td>3</td><td>0.3036 ± 0.0034</td><td>0.3734 ± 0.0027</td><td></td><td>2</td></tr></tbody></table>

Note. Same as Table 9, for the gamma-ray MSPs.

th component. The top panel of Figure 12 shows the fit using the above expression, and the best-fit parameters.

Figures 13 and 14 show the values of the $\Gamma_2 - \Gamma_1$ and $(1/E_{c,2} - 1/E_{c,1})$ parameters, for pulsars with at least six energy intervals with individual H-test $TS > 300$. Requiring $\ge 6$ data points gives the fit of Equation (12) enough data points and a wide energy range. The minimum detection significance in the energy bins restricts the study to high-quality profile fits. These criteria select 28 pulsars. Figure 12.2 shows that the

measured amplitude ratios between the first and second peaks for PSR J0007+7303 are poorly fit; we hence discarded this pulsar, reducing the sample to 27 objects. The choice of $B_{LC}$ in Figures 13 and 14 is arbitrary; we saw little or no correlation with various abscissa parameters, as discussed further in Section 8. Table 12 summarizes the results for the 27 pulsars. The weighted averages of $\Gamma_2 - \Gamma_1$ and $(1/E_{c,2} - 1/E_{c,1})$ are, respectively, $-0.209(2)$ and $-0.044(1)$ GeV$^{-1}$, clearly incompatible with 0 but dominated by a few measurements with very
<figure><img src="image_11.png" /><figcaption>**Figure 10.** Phase separation $\Delta$ between main gamma-ray peaks, vs. phase lag $\delta$ of the first gamma-ray peak relative to the radio emission. Values of $\delta$ between 0.9 and 1 are plotted between -0.1 and 0 in this graph. Values between 0.5 and 0.9 have been “folded” as $\delta' = 1 - \delta$. The markers are the same as in Figure 2. Circled symbols are pulsars for which the ordering of the first and second gamma-ray peaks was considered uncertain. Squares correspond to pulsars with “complex” profiles, in which choosing two main peaks is not straightforward. Opaque symbols are pulsars for which the definition of the radio fiducial point is considered robust, other pulsars are shown as transparent symbols (see the text for details on the definition of radio fiducial points). Pulsars with $\delta$ and no $\Delta$ measurements (i.e., single-peaked gamma-ray pulsars with radio emission) are shown in the gray-shaded region at the bottom, while those with $\Delta$ and no $\delta$ values (i.e., pulsars with at least two gamma-ray components and no radio emission) are plotted in the gray-shaded area at the right. The artificial staggering of the points in these two regions is to improve clarity. At the top and at the right are plotted histograms of the values of $\delta$ and $\Delta$ projected on the axes, for all pulsars shown in the central figure (the “All” panels), and restricting the sample of pulsars to those with $\delta$ and $\Delta$ measurements (the “Both $\delta$ and $\Delta$” panels, i.e., excluding pulsars in the gray-shaded areas).</figcaption></figure>

<figure><img src="image_12.png" /><figcaption>**Figure 11.** Phase separation $\Delta$ between main gamma-ray peaks vs. Shklovskii-corrected spindown power $\dot{E}$. The markers are the same as in Figure 2. See Figure 10 for the definition of the circle and square symbols.</figcaption></figure>
<figure><img src="image_12.png" /><figcaption>**Figure 10.** Phase separation $\Delta$ between main gamma-ray peaks, vs. phase lag $\delta$ of the first gamma-ray peak relative to the radio emission. Values of $\delta$ between 0.9 and 1 are plotted between -0.1 and 0 in this graph. Values between 0.5 and 0.9 have been “folded” as $\delta' = 1 - \delta$. The markers are the same as in Figure 2. Circled symbols are pulsars for which the ordering of the first and second gamma-ray peaks was considered uncertain. Squares correspond to pulsars with “complex” profiles, in which choosing two main peaks is not straightforward. Opaque symbols are pulsars for which the definition of the radio fiducial point is considered robust, other pulsars are shown as transparent symbols (see the text for details on the definition of radio fiducial points). Pulsars with $\delta$ and no $\Delta$ measurements (i.e., single-peaked gamma-ray pulsars with radio emission) are shown in the gray-shaded region at the bottom, while those with $\Delta$ and no $\delta$ values (i.e., pulsars with at least two gamma-ray components and no radio emission) are plotted in the gray-shaded area at the right. The artificial staggering of the points in these two regions is to improve clarity. At the top and at the right are plotted histograms of the values of $\delta$ and $\Delta$ projected on the axes, for all pulsars shown in the central figure (the “All” panels), and restricting the sample of pulsars to those with $\delta$ and $\Delta$ measurements (the “Both $\delta$ and $\Delta$” panels, i.e., excluding pulsars in the gray-shaded areas).</figcaption></figure>

<figure><img src="image_13.png" /><figcaption>**Figure 11.** Phase separation $\Delta$ between main gamma-ray peaks vs. Shklovskii-corrected spindown power $\dot{E}$. The markers are the same as in Figure 2. See Figure 10 for the definition of the circle and square symbols.</figcaption></figure>
<table><caption>**Table 11**

Comparisons of Radio/Gamma Phase Lags $\delta$ and Peak Separations $\Delta$ between 2PC and 3PC, for Pulsars with Apparently Discrepant Results</caption><thead><tr><th>PSR</th><th>2PC Value</th><th>3PC Value</th><th>Comment</th></tr></thead><tbody><tr><td colspan="4" style="text-align:center; font-weight:bold;">Radio/gamma phase lags, δ</td></tr><tr><td>J0030+0451</td><td>0.1600 ± 0.0010</td><td>0.1266 ± 0.0014</td><td>Different choice of radio reference phase</td></tr><tr><td>J0101-6422</td><td>0.145 ± 0.005</td><td>0.6733 ± 0.0032</td><td>Different choice of gamma-ray reference peak</td></tr><tr><td>J0102+4839</td><td>0.259 ± 0.004</td><td>0.327 ± 0.007</td><td>Qualitatively similar results</td></tr><tr><td>J0205+6449</td><td>0.075 ± 0.004</td><td>0.0400 ± 0.0024</td><td>Qualitatively similar results</td></tr><tr><td>J0218+4232</td><td>0.35 ± 0.08</td><td>0.691 ± 0.006</td><td>Different choice of gamma-ray reference peak</td></tr><tr><td>J0534+2200</td><td>0.10900 ± 0.00020</td><td>0.067 ± 0.004</td><td>Different choice of radio reference phase</td></tr><tr><td>J0610-2100</td><td>0.236 ± 0.006</td><td>0.615 ± 0.004</td><td>Different choice of radio reference phase</td></tr><tr><td>J0742-2822</td><td>0.627 ± 0.005</td><td>0.533<sup>+0.012</sup><sub>-0.017</sub></td><td>Different choice of gamma-ray reference peak</td></tr><tr><td>J1019-5749</td><td>0.482 ± 0.010</td><td>0.566 ± 0.010</td><td>Qualitatively similar results</td></tr><tr><td>J1057-5226</td><td>0.3040 ± 0.0029</td><td>0.7441 ± 0.0017</td><td>Different choice of radio reference phase</td></tr><tr><td>J1119-6127</td><td>0.285 ± 0.015</td><td>0.469 ± 0.008</td><td>Different choice of gamma-ray reference peak</td></tr><tr><td>J1125-5825</td><td>0.6450 ± 0.0017</td><td>0.211<sup>+0.021</sup><sub>-0.011</sub></td><td>Different choice of gamma-ray reference peak</td></tr><tr><td>J1410-6132</td><td>0.959 ± 0.023</td><td>0.537 ± 0.027</td><td>Different choice of gamma-ray reference peak</td></tr><tr><td>J1509-5850</td><td>0.271 ± 0.011</td><td>0.156 ± 0.006</td><td>Qualitatively similar results</td></tr><tr><td>J1514-4946</td><td>0.214 ± 0.009</td><td>0.273 ± 0.004</td><td>Different choice of radio reference phase</td></tr><tr><td>J1600-3053</td><td>0.147 ± 0.011</td><td>0.212 ± 0.007</td><td>Qualitatively similar results</td></tr><tr><td>J1658-5324</td><td>0.359 ± 0.014</td><td>0.105 ± 0.026</td><td>Different choice of gamma-ray reference peak</td></tr><tr><td>J1741-2054</td><td>0.074 ± 0.006</td><td>0.035 ± 0.005</td><td>Qualitatively similar results</td></tr><tr><td>J1744-1134</td><td>0.189 ± 0.007</td><td>0.8116 ± 0.0029</td><td>Different choice of radio reference phase</td></tr><tr><td>J1747-4036</td><td>0.031 ± 0.021</td><td>0.877 ± 0.013</td><td>Qualitatively similar results</td></tr><tr><td>J1801-2451</td><td>0.060 ± 0.005</td><td>0.118 ± 0.007</td><td>Qualitatively similar results</td></tr><tr><td>J1810+1744</td><td>0.894 ± 0.018</td><td>0.050 ± 0.013</td><td>Qualitatively similar results</td></tr><tr><td>J1835-1106</td><td>0.139 ± 0.006</td><td>0.55<sup>+0.02</sup><sub>-0.06</sub></td><td>Different choice of gamma-ray reference peak</td></tr><tr><td>J1907+0602</td><td>0.2090 ± 0.0026</td><td>0.282 ± 0.008</td><td>Different choice of radio reference phase</td></tr><tr><td>J2032+4127</td><td>0.0990 ± 0.0007</td><td>0.1626 ± 0.0009</td><td>Qualitatively similar results</td></tr><tr><td>J2047+1053</td><td>0.567 ± 0.010</td><td>0.219<sup>+0.032</sup><sub>-0.017</sub></td><td>Inconsistent results</td></tr><tr><td>J2215+5135</td><td>0.257 ± 0.004</td><td>0.573 ± 0.004</td><td>Inconsistent results</td></tr><tr><td>J2229+6114</td><td>0.187 ± 0.007</td><td>0.2959<sup>+0.0016</sup><sub>-0.0021</sub></td><td>Qualitatively similar results</td></tr><tr><td colspan="4" style="text-align:center; font-weight:bold;">Peak separations, Δ</td></tr><tr><td>J0218+4232</td><td>0.39 ± 0.08</td><td>...</td><td>Only one component in 3PC</td></tr><tr><td>J1119-6127</td><td>0.204 ± 0.020</td><td>...</td><td>Only one component in 3PC</td></tr><tr><td>J1124-3653</td><td>0.21 ± 0.04</td><td>0.394 ± 0.005</td><td>Different component phases</td></tr><tr><td>J1410-6132</td><td>0.46 ± 0.04</td><td>...</td><td>Only one component in 3PC</td></tr><tr><td>J1459-6053</td><td>0.063 ± 0.034</td><td>...</td><td>Only one component in 3PC</td></tr><tr><td>J1747-4036</td><td>0.681 ± 0.033</td><td>...</td><td>Only one component in 3PC</td></tr><tr><td>J1823-3021A</td><td>0.627 ± 0.010</td><td>0.390 ± 0.005</td><td>Components inverted</td></tr><tr><td>J1835-1106</td><td>0.421 ± 0.011</td><td>...</td><td>Only one component in 3PC</td></tr><tr><td>J2021+4026</td><td>0.687 ± 0.009</td><td>0.553 ± 0.005</td><td>Different component phases</td></tr><tr><td>J2032+4127</td><td>0.5160 ± 0.0010</td><td>0.4831 ± 0.0008</td><td>Components inverted</td></tr><tr><td>J2229+6114</td><td>0.299 ± 0.008</td><td>0.2221<sup>+0.0012</sup><sub>-0.0018</sub></td><td>Qualitatively similar results</td></tr><tr><td>J2241-5236</td><td>0.638 ± 0.031</td><td>0.317 ± 0.024</td><td>Different component phases</td></tr></tbody></table>

**Note.** The columns list the pulsar names, 2PC and 3PC values, and a comment on the apparent discrepancy. Pulsars listed here are those for which $\delta$ and/or $\Delta$ differ between 2PC and 3PC by more than three times the statistical uncertainty, but an absolute difference >0.03.

small statistical uncertainties. The respective unweighted averages are -0.14(18) and -0.04(7) GeV⁻¹, where the uncertainties here correspond to the standard deviations on the measured values.

## 6. Phase-averaged Energy Spectra

Two significant improvements enhance our pulsar spectral results relative to 2PC. The first is simply that we have more pulsars, and more photons per pulsar. The second is a change in our expression for the exponentially cutoff power-law spectrum, a characteristic of pulsars in the GeV domain. We replace the classic subexponentially cutoff power-law model (“PLEC”) with the new “PLEC4” expression introduced in

4FGL-DR3. Degeneracies between parameters in PLEC4 are reduced, and the likelihood fits converge better, yielding smaller uncertainties. However, some subtleties of the new expression merit the detailed discussion below.

In this Section we first review the motivations behind the exponentially cutoff power-law spectrum, highlighting the differences between PLEC used in 2PC and PLEC4 used here. We then describe our results, using the 4FGL-DR3 phase-integrated spectral analysis available for 255 pulsars, and explain some refinements of the spectral analyses that help characterize the pulsars’ emission properties, finally yielding 255 pulsars with spectral analyses in this catalog. Tables 13 and 14 list parameter values. Section 6.5 highlights some features of individual pulsar results. Section 6.6 addresses pulsar flux
<table><caption>**Table 11**

Comparisons of Radio/Gamma Phase Lags $\delta$ and Peak Separations $\Delta$ between 2PC and 3PC, for Pulsars with Apparently Discrepant Results</caption><thead><tr><th>PSR</th><th>2PC Value</th><th>3PC Value</th><th>Comment</th></tr></thead><tbody><tr><td colspan="4" style="text-align:center; font-weight:bold;">Radio/gamma phase lags, δ</td></tr><tr><td>J0030+0451</td><td>0.1600 ± 0.0010</td><td>0.1266 ± 0.0014</td><td>Different choice of radio reference phase</td></tr><tr><td>J0101-6422</td><td>0.145 ± 0.005</td><td>0.6733 ± 0.0032</td><td>Different choice of gamma-ray reference peak</td></tr><tr><td>J0102+4839</td><td>0.259 ± 0.004</td><td>0.327 ± 0.007</td><td>Qualitatively similar results</td></tr><tr><td>J0205+6449</td><td>0.075 ± 0.004</td><td>0.0400 ± 0.0024</td><td>Qualitatively similar results</td></tr><tr><td>J0218+4232</td><td>0.35 ± 0.08</td><td>0.691 ± 0.006</td><td>Different choice of gamma-ray reference peak</td></tr><tr><td>J0534+2200</td><td>0.10900 ± 0.00020</td><td>0.067 ± 0.004</td><td>Different choice of radio reference phase</td></tr><tr><td>J0610-2100</td><td>0.236 ± 0.006</td><td>0.615 ± 0.004</td><td>Different choice of radio reference phase</td></tr><tr><td>J0742-2822</td><td>0.627 ± 0.005</td><td>0.533<sup>+0.012</sup><sub>-0.017</sub></td><td>Different choice of gamma-ray reference peak</td></tr><tr><td>J1019-5749</td><td>0.482 ± 0.010</td><td>0.566 ± 0.010</td><td>Qualitatively similar results</td></tr><tr><td>J1057-5226</td><td>0.3040 ± 0.0029</td><td>0.7441 ± 0.0017</td><td>Different choice of radio reference phase</td></tr><tr><td>J1119-6127</td><td>0.285 ± 0.015</td><td>0.469 ± 0.008</td><td>Different choice of gamma-ray reference peak</td></tr><tr><td>J1125-5825</td><td>0.6450 ± 0.0017</td><td>0.211<sup>+0.021</sup><sub>-0.011</sub></td><td>Different choice of gamma-ray reference peak</td></tr><tr><td>J1410-6132</td><td>0.959 ± 0.023</td><td>0.537 ± 0.027</td><td>Different choice of gamma-ray reference peak</td></tr><tr><td>J1509-5850</td><td>0.271 ± 0.011</td><td>0.156 ± 0.006</td><td>Qualitatively similar results</td></tr><tr><td>J1514-4946</td><td>0.214 ± 0.009</td><td>0.273 ± 0.004</td><td>Different choice of radio reference phase</td></tr><tr><td>J1600-3053</td><td>0.147 ± 0.011</td><td>0.212 ± 0.007</td><td>Qualitatively similar results</td></tr><tr><td>J1658-5324</td><td>0.359 ± 0.014</td><td>0.105 ± 0.026</td><td>Different choice of gamma-ray reference peak</td></tr><tr><td>J1741-2054</td><td>0.074 ± 0.006</td><td>0.035 ± 0.005</td><td>Qualitatively similar results</td></tr><tr><td>J1744-1134</td><td>0.189 ± 0.007</td><td>0.8116 ± 0.0029</td><td>Different choice of radio reference phase</td></tr><tr><td>J1747-4036</td><td>0.031 ± 0.021</td><td>0.877 ± 0.013</td><td>Qualitatively similar results</td></tr><tr><td>J1801-2451</td><td>0.060 ± 0.005</td><td>0.118 ± 0.007</td><td>Qualitatively similar results</td></tr><tr><td>J1810+1744</td><td>0.894 ± 0.018</td><td>0.050 ± 0.013</td><td>Qualitatively similar results</td></tr><tr><td>J1835-1106</td><td>0.139 ± 0.006</td><td>0.55<sup>+0.02</sup><sub>-0.06</sub></td><td>Different choice of gamma-ray reference peak</td></tr><tr><td>J1907+0602</td><td>0.2090 ± 0.0026</td><td>0.282 ± 0.008</td><td>Different choice of radio reference phase</td></tr><tr><td>J2032+4127</td><td>0.0990 ± 0.0007</td><td>0.1626 ± 0.0009</td><td>Qualitatively similar results</td></tr><tr><td>J2047+1053</td><td>0.567 ± 0.010</td><td>0.219<sup>+0.032</sup><sub>-0.017</sub></td><td>Inconsistent results</td></tr><tr><td>J2215+5135</td><td>0.257 ± 0.004</td><td>0.573 ± 0.004</td><td>Inconsistent results</td></tr><tr><td>J2229+6114</td><td>0.187 ± 0.007</td><td>0.2959<sup>+0.0016</sup><sub>-0.0021</sub></td><td>Qualitatively similar results</td></tr><tr><td colspan="4" style="text-align:center; font-weight:bold;">Peak separations, Δ</td></tr><tr><td>J0218+4232</td><td>0.39 ± 0.08</td><td>...</td><td>Only one component in 3PC</td></tr><tr><td>J1119-6127</td><td>0.204 ± 0.020</td><td>...</td><td>Only one component in 3PC</td></tr><tr><td>J1124-3653</td><td>0.21 ± 0.04</td><td>0.394 ± 0.005</td><td>Different component phases</td></tr><tr><td>J1410-6132</td><td>0.46 ± 0.04</td><td>...</td><td>Only one component in 3PC</td></tr><tr><td>J1459-6053</td><td>0.063 ± 0.034</td><td>...</td><td>Only one component in 3PC</td></tr><tr><td>J1747-4036</td><td>0.681 ± 0.033</td><td>...</td><td>Only one component in 3PC</td></tr><tr><td>J1823-3021A</td><td>0.627 ± 0.010</td><td>0.390 ± 0.005</td><td>Components inverted</td></tr><tr><td>J1835-1106</td><td>0.421 ± 0.011</td><td>...</td><td>Only one component in 3PC</td></tr><tr><td>J2021+4026</td><td>0.687 ± 0.009</td><td>0.553 ± 0.005</td><td>Different component phases</td></tr><tr><td>J2032+4127</td><td>0.5160 ± 0.0010</td><td>0.4831 ± 0.0008</td><td>Components inverted</td></tr><tr><td>J2229+6114</td><td>0.299 ± 0.008</td><td>0.2221<sup>+0.0012</sup><sub>-0.0018</sub></td><td>Qualitatively similar results</td></tr><tr><td>J2241-5236</td><td>0.638 ± 0.031</td><td>0.317 ± 0.024</td><td>Different component phases</td></tr></tbody></table>

Note. The columns list the pulsar names, 2PC and 3PC values, and a comment on the apparent discrepancy. Pulsars listed here are those for which $\delta$ and/or $\Delta$ differ between 2PC and 3PC by more than three times the statistical uncertainty, but an absolute difference >0.03.

small statistical uncertainties. The respective unweighted averages are -0.14(18) and -0.04(7) GeV⁻¹, where the uncertainties here correspond to the standard deviations on the measured values.

## 6. Phase-averaged Energy Spectra

Two significant improvements enhance our pulsar spectral results relative to 2PC. The first is simply that we have more pulsars, and more photons per pulsar. The second is a change in our expression for the exponentially cutoff power-law spectrum, a characteristic of pulsars in the GeV domain. We replace the classic subexponentially cutoff power-law model (“PLEC”) with the new “PLEC4” expression introduced in

4FGL-DR3. Degeneracies between parameters in PLEC4 are reduced, and the likelihood fits converge better, yielding smaller uncertainties. However, some subtleties of the new expression merit the detailed discussion below.

In this Section we first review the motivations behind the exponentially cutoff power-law spectrum, highlighting the differences between PLEC used in 2PC and PLEC4 used here. We then describe our results, using the 4FGL-DR3 phase-integrated spectral analysis available for 255 pulsars, and explain some refinements of the spectral analyses that help characterize the pulsars’ emission properties, finally yielding 255 pulsars with spectral analyses in this catalog. Tables 13 and 14 list parameter values. Section 6.5 highlights some features of individual pulsar results. Section 6.6 addresses pulsar flux
<figure><img src="image_13.png" /></figure>

**Figure 12.** Summary of the energy-resolved light-curve fitting analysis, for PSR J0205+6449. From top to bottom: ratio of the amplitude of the *i*th pulse profile component to that of the first component as a function of energy; differences between the component phases in the individual energy ranges and those from the global light-curve fit (for energies above 0.1 GeV); component widths as a function of energy. PSR J0205+6449 has two pulse profile components; therefore, each panel has two sets of points, with different colors and symbols. Results are shown in energy bins in which the pulsar is detected with an *H*-test TS greater than 300. Fit results for components with peak values smaller than 1/100 of the maximum peak value in the energy bin are not shown. Likewise, peaks with areas smaller than $5 \times 10^{-3}$ of the area of the total pulsed emission and those with widths larger than 20 times the median value are also not plotted. Horizontal bands in the top and bottom panels indicate the reference results from the global light-curve fit above 0.1 GeV. The middle panel lists the reference results. The dashed curve in the top panel represents a fit of (Amp$_2$/Amp$_1$) vs. energy, with the parameters shown in the bottom-left corner.

(The complete figure set (129 images) is available.)

<figure><img src="image_14.png" /></figure>

**Figure 13.** $\Gamma_2 - \Gamma_1$ from the energy-resolved light-curve fitting, plotted against light cylinder magnetic field, $B_{LC}$. See Section 5.3 for details regarding the measurement of this parameter. See Figure 10 for the definition of the circle and square symbols.
<figure><img src="image_14.png" /></figure>

**Figure 12.** Summary of the energy-resolved light-curve fitting analysis, for PSR J0205+6449. From top to bottom: ratio of the amplitude of the *i*th pulse profile component to that of the first component as a function of energy; differences between the component phases in the individual energy ranges and those from the global light-curve fit (for energies above 0.1 GeV); component widths as a function of energy. PSR J0205+6449 has two pulse profile components; therefore, each panel has two sets of points, with different colors and symbols. Results are shown in energy bins in which the pulsar is detected with an *H*-test TS greater than 300. Fit results for components with peak values smaller than 1/100 of the maximum peak value in the energy bin are not shown. Likewise, peaks with areas smaller than $5 \times 10^{-3}$ of the area of the total pulsed emission and those with widths larger than 20 times the median value are also not plotted. Horizontal bands in the top and bottom panels indicate the reference results from the global light-curve fit above 0.1 GeV. The middle panel lists the reference results. The dashed curve in the top panel represents a fit of (Amp$_2$/Amp$_1$) vs. energy, with the parameters shown in the bottom-left corner.

(The complete figure set (129 images) is available.)

<figure><img src="image_15.png" /></figure>

**Figure 13.** $\Gamma_2 - \Gamma_1$ from the energy-resolved light-curve fitting, plotted against light cylinder magnetic field, $B_{LC}$. See Section 5.3 for details regarding the measurement of this parameter. See Figure 10 for the definition of the circle and square symbols.
<figure><img src="image_15.png" /><figcaption>**Figure 14.** $(1/E_{c,2} - 1/E_{c,1})$ from the energy-resolved light-curve fitting, plotted against light cylinder magnetic field, $B_{LC}$. See Section 5.3 for details regarding the measurement of this parameter. See Figure 10 for the definition of the circle and square symbols.</figcaption></figure>

<table><caption>**Table 12**
Summary of Energy-resolved Fits of the First and Second Gamma-Ray Peak Amplitude Ratios</caption><thead><tr><th>PSR</th><th>Code</th><th>Comment</th><th>Γ<sub>2</sub> - Γ<sub>1</sub></th><th>(1/E<sub>c,2</sub> - 1/E<sub>c,1</sub>) (GeV<sup>-1</sup>)</th></tr></thead><tbody><tr><td>J0205+6449</td><td>rx</td><td></td><td>-0.20 ± 0.06</td><td>-0.12 ± 0.06</td></tr><tr><td>J0534+2200</td><td>rx</td><td></td><td>-0.105 ± 0.006</td><td>-0.072 ± 0.006</td></tr><tr><td>J0614-3329</td><td>mbrx</td><td></td><td>-0.461 ± 0.032</td><td>-0.023 ± 0.011</td></tr><tr><td>J0633+0632</td><td>q</td><td></td><td>0.23 ± 0.05</td><td>-0.098 ± 0.022</td></tr><tr><td>J0633+1746</td><td>xq</td><td></td><td>-0.320 ± 0.005</td><td>-0.1093 ± 0.0034</td></tr><tr><td>J0835-4510</td><td>rx</td><td></td><td>-0.2100 ± 0.0021</td><td>-0.0352 ± 0.0017</td></tr><tr><td>J1023-5746</td><td>q</td><td></td><td>-0.06 ± 0.04</td><td>0.057 ± 0.027</td></tr><tr><td>J1028-5819</td><td>r</td><td></td><td>-0.004 ± 0.024</td><td>-0.010 ± 0.008</td></tr><tr><td>J1044-5737</td><td>q</td><td></td><td>-0.16 ± 0.12</td><td>-0.05 ± 0.06</td></tr><tr><td>J1048-5832</td><td>r</td><td></td><td>-0.14 ± 0.08</td><td>-0.104 ± 0.034</td></tr><tr><td>J1057-5226</td><td>rx</td><td>c</td><td>-0.04 ± 0.11</td><td>-0.12 ± 0.06</td></tr><tr><td>J1124-5916</td><td>rx</td><td></td><td>-0.13 ± 0.07</td><td>-0.08 ± 0.06</td></tr><tr><td>J1231-1411</td><td>mbrx</td><td>c</td><td>-0.39 ± 0.04</td><td>0.024 ± 0.012</td></tr><tr><td>J1413-6205</td><td>q</td><td></td><td>-0.05 ± 0.08</td><td>0.011 ± 0.020</td></tr><tr><td>J1418-6058</td><td>q</td><td></td><td>-0.12 ± 0.06</td><td>-0.00 ± 0.04</td></tr><tr><td>J1709-4429</td><td>rx</td><td></td><td>-0.11 ± 0.08</td><td>-0.06 ± 0.10</td></tr><tr><td>J1732-3131</td><td>r</td><td></td><td>-0.10 ± 0.05</td><td>-0.104 ± 0.015</td></tr><tr><td>J1809-2332</td><td>q</td><td></td><td>-0.194 ± 0.028</td><td>0.018 ± 0.008</td></tr><tr><td>J1826-1256</td><td>xq</td><td></td><td>-0.060 ± 0.025</td><td>0.012 ± 0.011</td></tr><tr><td>J1833-1034</td><td>r</td><td></td><td>-0.02 ± 0.17</td><td>-0.21 ± 0.14</td></tr><tr><td>J1836+5925</td><td>q</td><td></td><td>0.19 ± 0.06</td><td>-0.162 ± 0.028</td></tr><tr><td>J1907+0602</td><td>r</td><td></td><td>-0.23 ± 0.07</td><td>0.111 ± 0.030</td></tr><tr><td>J1952+3252</td><td>rx</td><td></td><td>-0.381 ± 0.033</td><td>0.029 ± 0.018</td></tr><tr><td>J2021+3651</td><td>r</td><td></td><td>0.012 ± 0.016</td><td>-0.047 ± 0.007</td></tr><tr><td>J2032+4127</td><td>br</td><td>u</td><td>-0.58 ± 0.07</td><td>0.029 ± 0.017</td></tr><tr><td>J2229+6114</td><td>rx</td><td></td><td>-0.14 ± 0.04</td><td>-0.014 ± 0.016</td></tr><tr><td>J2238+5903</td><td>q</td><td></td><td>0.06 ± 0.06</td><td>-0.019 ± 0.027</td></tr></tbody></table>

**Note.** In Column 3, “u” indicates that the ordering of the first and second gamma-ray peaks is uncertain, and “c” indicates that the profile is complex. See Section 5.3 for details on the measurement of the parameters listed in Columns 4 and 5.

stability, and in Section 6.7 we combine integrated energy fluxes and distances to obtain gamma-ray luminosities and efficiencies.

## 6.1. Pulsar Spectral Shapes

As we will show, the general GeV pulsar spectrum is peaked around $E_p = 1.5$ GeV (see also Figure B1 in Appendix B). It is natural to relate this to the synchrotron spectrum radiated by an

ultrarelativistic primary particle (Pacholczyk 1970; Dermer & Menon 2009)

$$ \begin{aligned} E^2 dN/dE &\equiv S(E, E_c) \propto E^{4/3} \exp[-E/E_c] \\ &\equiv E^{2-\Gamma_{sr}} \exp[-E/E_c]. \end{aligned} \qquad (13) $$

Here, the asymptotic spectral index is $\Gamma_{sr} = 2/3$, and the cutoff energy $E_c$ depends on the specific radiation mechanism, e.g.,
<figure><img src="image_16.png" /><figcaption>**Figure 14.** $(1/E_{c,2} - 1/E_{c,1})$ from the energy-resolved light-curve fitting, plotted against light cylinder magnetic field, $B_{LC}$. See Section 5.3 for details regarding the measurement of this parameter. See Figure 10 for the definition of the circle and square symbols.</figcaption></figure>

<table><caption>**Table 12**
Summary of Energy-resolved Fits of the First and Second Gamma-Ray Peak Amplitude Ratios</caption><thead><tr><th>PSR</th><th>Code</th><th>Comment</th><th>Γ<sub>2</sub> - Γ<sub>1</sub></th><th>(1/E<sub>c,2</sub> - 1/E<sub>c,1</sub>) (GeV<sup>-1</sup>)</th></tr></thead><tbody><tr><td>J0205+6449</td><td>rx</td><td></td><td>-0.20 ± 0.06</td><td>-0.12 ± 0.06</td></tr><tr><td>J0534+2200</td><td>rx</td><td></td><td>-0.105 ± 0.006</td><td>-0.072 ± 0.006</td></tr><tr><td>J0614-3329</td><td>mbrx</td><td></td><td>-0.461 ± 0.032</td><td>-0.023 ± 0.011</td></tr><tr><td>J0633+0632</td><td>q</td><td></td><td>0.23 ± 0.05</td><td>-0.098 ± 0.022</td></tr><tr><td>J0633+1746</td><td>xq</td><td></td><td>-0.320 ± 0.005</td><td>-0.1093 ± 0.0034</td></tr><tr><td>J0835-4510</td><td>rx</td><td></td><td>-0.2100 ± 0.0021</td><td>-0.0352 ± 0.0017</td></tr><tr><td>J1023-5746</td><td>q</td><td></td><td>-0.06 ± 0.04</td><td>0.057 ± 0.027</td></tr><tr><td>J1028-5819</td><td>r</td><td></td><td>-0.004 ± 0.024</td><td>-0.010 ± 0.008</td></tr><tr><td>J1044-5737</td><td>q</td><td></td><td>-0.16 ± 0.12</td><td>-0.05 ± 0.06</td></tr><tr><td>J1048-5832</td><td>r</td><td></td><td>-0.14 ± 0.08</td><td>-0.104 ± 0.034</td></tr><tr><td>J1057-5226</td><td>rx</td><td>c</td><td>-0.04 ± 0.11</td><td>-0.12 ± 0.06</td></tr><tr><td>J1124-5916</td><td>rx</td><td></td><td>-0.13 ± 0.07</td><td>-0.08 ± 0.06</td></tr><tr><td>J1231-1411</td><td>mbrx</td><td>c</td><td>-0.39 ± 0.04</td><td>0.024 ± 0.012</td></tr><tr><td>J1413-6205</td><td>q</td><td></td><td>-0.05 ± 0.08</td><td>0.011 ± 0.020</td></tr><tr><td>J1418-6058</td><td>q</td><td></td><td>-0.12 ± 0.06</td><td>-0.00 ± 0.04</td></tr><tr><td>J1709-4429</td><td>rx</td><td></td><td>-0.11 ± 0.08</td><td>-0.06 ± 0.10</td></tr><tr><td>J1732-3131</td><td>r</td><td></td><td>-0.10 ± 0.05</td><td>-0.104 ± 0.015</td></tr><tr><td>J1809-2332</td><td>q</td><td></td><td>-0.194 ± 0.028</td><td>0.018 ± 0.008</td></tr><tr><td>J1826-1256</td><td>xq</td><td></td><td>-0.060 ± 0.025</td><td>0.012 ± 0.011</td></tr><tr><td>J1833-1034</td><td>r</td><td></td><td>-0.02 ± 0.17</td><td>-0.21 ± 0.14</td></tr><tr><td>J1836+5925</td><td>q</td><td></td><td>0.19 ± 0.06</td><td>-0.162 ± 0.028</td></tr><tr><td>J1907+0602</td><td>r</td><td></td><td>-0.23 ± 0.07</td><td>0.111 ± 0.030</td></tr><tr><td>J1952+3252</td><td>rx</td><td></td><td>-0.381 ± 0.033</td><td>0.029 ± 0.018</td></tr><tr><td>J2021+3651</td><td>r</td><td></td><td>0.012 ± 0.016</td><td>-0.047 ± 0.007</td></tr><tr><td>J2032+4127</td><td>br</td><td>u</td><td>-0.58 ± 0.07</td><td>0.029 ± 0.017</td></tr><tr><td>J2229+6114</td><td>rx</td><td></td><td>-0.14 ± 0.04</td><td>-0.014 ± 0.016</td></tr><tr><td>J2238+5903</td><td>q</td><td></td><td>0.06 ± 0.06</td><td>-0.019 ± 0.027</td></tr></tbody></table>

**Note.** In Column 3, “u” indicates that the ordering of the first and second gamma-ray peaks is uncertain, and “c” indicates that the profile is complex. See Section 5.3 for details on the measurement of the parameters listed in Columns 4 and 5.

stability, and in Section 6.7 we combine integrated energy fluxes and distances to obtain gamma-ray luminosities and efficiencies.

## 6.1. Pulsar Spectral Shapes

As we will show, the general GeV pulsar spectrum is peaked around $E_p = 1.5$ GeV (see also Figure B1 in Appendix B). It is natural to relate this to the synchrotron spectrum radiated by an

ultrarelativistic primary particle (Pacholczyk 1970; Dermer & Menon 2009)

$$ \begin{aligned} E^2 dN/dE &\equiv S(E, E_c) \propto E^{4/3} \exp[-E/E_c] \\ &\equiv E^{2-\Gamma_{sr}} \exp[-E/E_c]. \end{aligned} \quad (13) $$

Here, the asymptotic spectral index is $\Gamma_{sr} = 2/3$, and the cutoff energy $E_c$ depends on the specific radiation mechanism, e.g.,
<table><caption>**Table 13**

Spectral Fitting Results for Young LAT-detected Pulsars</caption><thead><tr><th>PSR<sup>a</sup></th><th>Energy Flux<br>(erg cm<sup>-2</sup> s<sup>-1</sup>)<br>(×10<sup>-11</sup>)</th><th>Γ<sub>100</sub></th><th>E<sub>p</sub><br>(GeV)</th><th>d<sub>p</sub></th><th>b<sub>free</sub></th><th>Luminosity<br>(10<sup>33</sup> erg s<sup>-1</sup>)</th><th>Efficiency<sup>b</sup><br>(%)</th></tr></thead><tbody><tr><td>J0002+6216</td><td>1.9 ± 0.14</td><td>1.6 ± 0.30</td><td>0.82 ± 0.16</td><td>0.65 ± 0.09</td><td>0.85 ± 0.39</td><td>9.01 ± 0.69 ± 3.2</td><td>5.9 ± 0.4 ± 3</td></tr><tr><td>J0007+7303</td><td>43.0 ± 0.33</td><td>1.2 ± 0.04</td><td>2.44 ± 0.03</td><td>0.36 ± 0.01</td><td>0.56 ± 0.04</td><td>101.23 ± 0.76 ± 39</td><td>22.7 ± 0.2 ± 10</td></tr><tr><td>J0106+4855</td><td>1.9 ± 0.07</td><td>1.2 ± 0.20</td><td>2.37 ± 0.11</td><td>0.67 ± 0.06</td><td>1.05 ± 0.26</td><td>21.57 ± 0.81<sup>+21</sup><sub>-14</sub></td><td>73 ± 3 ± 70</td></tr><tr><td>J0117+5914 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J0139+5814 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J0205+6449</td><td>6.4 ± 0.20</td><td>1.6 ± 0.22</td><td>0.26 ± 0.10</td><td>0.45 ± 0.08</td><td>0.20 ± 0.26</td><td>78.8 ± 2.5 ± 9.5</td><td>0.295 ± 0.009 ± 0.04</td></tr><tr><td>J0248+6021</td><td>2.9 ± 0.21</td><td>1.7 ± 0.26</td><td>0.77 ± 0.10</td><td>1.02 ± 0.12</td><td>1.16 ± 0.38</td><td>14.1 ± 1.0 ± 2.7</td><td>6.6 ± 0.5 ± 1</td></tr><tr><td>J0357+3205</td><td>6.0 ± 0.18</td><td>0.73 ± 0.23</td><td>0.87 ± 0.03</td><td>0.95 ± 0.05</td><td>0.64 ± 0.14</td><td>...</td><td>...</td></tr><tr><td>J0359+5414</td><td>2.0 ± 0.13</td><td>1.0 ± 0.56</td><td>1.31 ± 0.12</td><td>0.86 ± 0.10</td><td>0.59 ± 0.40</td><td>...</td><td>...</td></tr><tr><td>J0514-4408</td><td>0.56 ± 0.04</td><td>...</td><td>0.60 ± 0.06</td><td>1.23 ± 0.19</td><td>...</td><td>0.62 ± 0.05<sup>+0.60</sup><sub>-0.40</sub></td><td>25 ± 2 ± 20</td></tr><tr><td>J0534+2200</td><td>150.0 ± 1.3</td><td>2.0 ± 0.03</td><td>0.04 ± 0.03</td><td>0.23 ± 0.01</td><td>0.61 ± 0.08</td><td>685.1 ± 5.8<sup>+280</sup><sub>-170</sub></td><td>0.157 ± 0.001<sup>+0.06</sup><sub>-0.04</sub></td></tr><tr><td>J0540-6919</td><td>2.7 ± 0.15</td><td>...</td><td>0.02 ± 0.08</td><td>0.26 ± 0.05</td><td>...</td><td>7890 ± 440 ± 350</td><td>5.4 ± 0.3 ± 0.2</td></tr><tr><td>J0554+3107</td><td>1.9 ± 0.09</td><td>0.90 ± 0.43</td><td>1.19 ± 0.07</td><td>1.04 ± 0.11</td><td>0.73 ± 0.31</td><td>...</td><td>...</td></tr><tr><td>J0622+3749</td><td>1.8 ± 0.09</td><td>0.65 ± 0.50</td><td>0.75 ± 0.04</td><td>1.60 ± 0.15</td><td>0.69 ± 0.32</td><td>...</td><td>...</td></tr><tr><td>J0631+0646</td><td>1.6 ± 0.13</td><td>...</td><td>2.65 ± 0.23</td><td>1.05 ± 0.17</td><td>...</td><td>40.3 ± 3.2<sup>+39</sup><sub>-26</sub></td><td>39 ± 3 ± 40</td></tr><tr><td>J0631+1036</td><td>3.0 ± 0.14</td><td>1.6 ± 0.12</td><td>2.00 ± 0.14</td><td>0.60 ± 0.07</td><td>1.55 ± 0.39</td><td>16.06 ± 0.72<sup>+15</sup><sub>-10</sub></td><td>9.4 ± 0.4 ± 9</td></tr><tr><td>J0633+0632</td><td>9.6 ± 0.24</td><td>1.1 ± 0.17</td><td>1.43 ± 0.06</td><td>0.60 ± 0.03</td><td>0.48 ± 0.12</td><td>...</td><td>...</td></tr><tr><td>J0633+1746</td><td>420.0 ± 1.1</td><td>1.1 ± 0.01</td><td>1.63 ± 0.01</td><td>0.66 ± 0.00</td><td>0.70 ± 0.01</td><td>18.23 ± 0.05 ± 9.1</td><td>56.1 ± 0.2 ± 40</td></tr><tr><td>J0659+1414</td><td>2.7 ± 0.09</td><td>1.5 ± 0.27</td><td>0.16 ± 0.03</td><td>0.86 ± 0.09</td><td>0.12 ± 0.29</td><td>0.26 ± 0.01 ± 0.05</td><td>0.69 ± 0.02 ± 0.2</td></tr><tr><td>J0729-1448</td><td>0.6 ± 0.11</td><td>...</td><td>0.07 ± 0.41</td><td>0.43 ± 0.30</td><td>...</td><td>5.16 ± 0.93<sup>+5.0</sup><sub>-3.3</sub></td><td>1.8 ± 0.3 ± 2</td></tr><tr><td>J0729-1836 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J0734-1559</td><td>4.6 ± 0.14</td><td>1.4 ± 0.22</td><td>0.62 ± 0.08</td><td>0.36 ± 0.03</td><td>0.29 ± 0.19</td><td>...</td><td>...</td></tr><tr><td>J0742-2822</td><td>1.5 ± 0.11</td><td>...</td><td>0.95 ± 0.19</td><td>0.55 ± 0.11</td><td>...</td><td>7.28 ± 0.54<sup>+9.1</sup><sub>-4.7</sub></td><td>5.1 ± 0.4<sup>+6</sup><sub>-3</sub></td></tr><tr><td>J0744-2525</td><td>0.46 ± 0.12</td><td>1.6 ± 0.30</td><td>1.45 ± 0.16</td><td>0.64 ± 0.10</td><td>1.23 ± 0.58</td><td>...</td><td>...</td></tr><tr><td>J0802-5613</td><td>0.66 ± 0.06</td><td>...</td><td>1.26 ± 0.12</td><td>1.10 ± 0.20</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J0834-4159 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J0835-4510</td><td>930.0 ± 3.0</td><td>1.4 ± 0.01</td><td>1.27 ± 0.01</td><td>0.52 ± 0.00</td><td>0.49 ± 0.01</td><td>87.18 ± 0.28<sup>+73</sup><sub>-12</sub></td><td>1.289 ± 0.004<sup>+1</sup><sub>-0.2</sub></td></tr><tr><td>J0908-4913</td><td>2.2 ± 0.31</td><td>...</td><td>0.60 ± 0.15</td><td>1.07 ± 0.21</td><td>...</td><td>2.62 ± 0.37<sup>+16</sup><sub>-2.4</sub></td><td>0.53 ± 0.08<sup>+3</sup><sub>-0.5</sub></td></tr><tr><td>J0922+0638 *</td><td>0.22 ± 0.04</td><td>...</td><td>...</td><td>0.12 ± 0.16</td><td>...</td><td>0.31 ± 0.06<sup>+0.12</sup><sub>-0.05</sub></td><td>4.6 ± 0.9<sup>+2</sup><sub>-0.8</sub></td></tr><tr><td>J0940-5428</td><td>1.7 ± 0.15</td><td>...</td><td>1.23 ± 0.18</td><td>0.85 ± 0.15</td><td>...</td><td>0.30 ± 0.03<sup>+0.29</sup><sub>-0.19</sub></td><td>0.015 ± 0.001 ± 0.01</td></tr><tr><td>J1016-5857</td><td>7.0 ± 0.64</td><td>1.5 ± 0.58</td><td>0.89 ± 0.30</td><td>0.63 ± 0.10</td><td>0.58 ± 0.39</td><td>83.8 ± 7.7<sup>+80</sup><sub>-54</sub></td><td>3.3 ± 0.3 ± 3</td></tr><tr><td>J1019-5749</td><td>2.7 ± 0.59</td><td>...</td><td>0.60 ± 0.74</td><td>0.50 ± 0.16</td><td>...</td><td>388 ± 84<sup>+370</sup><sub>-250</sub></td><td>210 ± 50 ± 200</td></tr><tr><td>J1023-5746</td><td>15.0 ± 1.1</td><td>...</td><td>0.62 ± 0.13</td><td>0.67 ± 0.06</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1028-5819</td><td>25.0 ± 0.67</td><td>1.1 ± 0.18</td><td>0.89 ± 0.07</td><td>0.39 ± 0.02</td><td>0.21 ± 0.10</td><td>59.4 ± 1.6<sup>+57</sup><sub>-38</sub></td><td>8.1 ± 0.2 ± 8</td></tr><tr><td>J1044-5737</td><td>11.0 ± 0.35</td><td>1.8 ± 0.11</td><td>0.65 ± 0.08</td><td>0.49 ± 0.03</td><td>0.83 ± 0.18</td><td>...</td><td>...</td></tr><tr><td>J1048-5832</td><td>19.0 ± 0.46</td><td>1.2 ± 0.15</td><td>0.97 ± 0.07</td><td>0.41 ± 0.02</td><td>0.28 ± 0.10</td><td>186.4 ± 4.7<sup>+190</sup><sub>-79</sub></td><td>9.4 ± 0.2<sup>+9</sup><sub>-4</sub></td></tr><tr><td>J1055-6028</td><td>1.9 ± 0.33</td><td>...</td><td>1.22 ± 0.49</td><td>0.69 ± 0.20</td><td>...</td><td>33.6 ± 5.8<sup>+32</sup><sub>-21</sub></td><td>2.9 ± 0.5 ± 3</td></tr><tr><td>J1057-5226</td><td>30.0 ± 0.26</td><td>1.0 ± 0.06</td><td>1.21 ± 0.01</td><td>0.88 ± 0.02</td><td>0.85 ± 0.05</td><td>4.34 ± 0.04<sup>+4.5</sup><sub>-2.9</sub></td><td>14.4 ± 0.1<sup>+20</sup><sub>-10</sub></td></tr><tr><td>J1057-5851</td><td>1.3 ± 0.16</td><td>...</td><td>1.15 ± 0.13</td><td>1.73 ± 0.36</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1105-6037</td><td>3.1 ± 0.35</td><td>...</td><td>1.14 ± 0.27</td><td>0.76 ± 0.13</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1105-6107</td><td>2.3 ± 0.39</td><td>...</td><td>0.52 ± 0.37</td><td>0.69 ± 0.19</td><td>...</td><td>15.6 ± 2.6<sup>+15</sup><sub>-10</sub></td><td>0.6 ± 0.1 ± 0.6</td></tr><tr><td>J1111-6039</td><td>5.9 ± 0.34</td><td>0.84 ± 0.53</td><td>2.68 ± 0.25</td><td>0.58 ± 0.06</td><td>0.30 ± 0.24</td><td>...</td><td>...</td></tr><tr><td>J1112-6103</td><td>2.2 ± 0.42</td><td>...</td><td>0.55 ± 0.54</td><td>0.55 ± 0.18</td><td>...</td><td>53 ± 10<sup>+51</sup><sub>-34</sub></td><td>1.2 ± 0.2 ± 1</td></tr><tr><td>J1119-6127</td><td>4.4 ± 0.32</td><td>-0.64 ± 2.7</td><td>1.08 ± 0.31</td><td>0.72 ± 0.18</td><td>-0.26 ± 0.51</td><td>371 ± 27 ± 35</td><td>16 ± 1 ± 2</td></tr><tr><td>J1124-5916</td><td>6.1 ± 0.20</td><td>1.5 ± 0.22</td><td>0.36 ± 0.09</td><td>0.41 ± 0.04</td><td>0.23 ± 0.20</td><td>168.3 ± 5.6 ± 74</td><td>1.41 ± 0.05 ± 0.4</td></tr><tr><td>J1135-6055</td><td>4.6 ± 0.22</td><td>1.2 ± 0.38</td><td>0.78 ± 0.13</td><td>0.51 ± 0.06</td><td>0.24 ± 0.25</td><td>...</td><td>...</td></tr><tr><td>J1139-6247</td><td>1.9 ± 0.21</td><td>...</td><td>1.92 ± 0.54</td><td>0.39 ± 0.09</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1151-6108</td><td>1.0 ± 0.14</td><td>...</td><td>1.39 ± 0.28</td><td>0.90 ± 0.23</td><td>...</td><td>6.10 ± 0.86<sup>+5.9</sup><sub>-3.9</sub></td><td>1.6 ± 0.2 ± 2</td></tr><tr><td>J1203-6242</td><td>3.7 ± 0.36</td><td>...</td><td>1.10 ± 0.26</td><td>0.58 ± 0.08</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1208-6238</td><td>3.7 ± 0.40</td><td>...</td><td>1.00 ± 0.41</td><td>0.49 ± 0.09</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1224-6407 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1231-5113</td><td>1.1 ± 0.07</td><td>...</td><td>0.60 ± 0.06</td><td>1.10 ± 0.16</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1231-6511</td><td>1.2 ± 0.14</td><td>...</td><td>0.99 ± 0.19</td><td>0.82 ± 0.18</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1253-5820</td><td>0.43 ± 0.10</td><td>...</td><td>0.51 ± 0.16</td><td>1.38 ± 0.57</td><td>...</td><td>1.37 ± 0.33<sup>+1.3</sup><sub>-0.88</sub></td><td>28 ± 7 ± 30</td></tr><tr><td>J1341-6220 *</td><td>2.2 ± 0.52</td><td>...</td><td>...</td><td>0.20 ± 0.13</td><td>...</td><td>424 ± 99<sup>+410</sup><sub>-270</sub></td><td>31 ± 7 ± 30</td></tr><tr><td>J1350-6225</td><td>3.6 ± 0.41</td><td>...</td><td>1.95 ± 0.33</td><td>0.75 ± 0.13</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1357-6429</td><td>2.9 ± 0.24</td><td>...</td><td>0.35 ± 0.12</td><td>0.70 ± 0.12</td><td>...</td><td>33.9 ± 2.8<sup>+33</sup><sub>-22</sub></td><td>1.11 ± 0.09 ± 1</td></tr><tr><td>J1358-6025</td><td>3.2 ± 0.36</td><td>...</td><td>0.72 ± 0.30</td><td>0.52 ± 0.11</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1410-6132</td><td>2.3 ± 0.71</td><td>...</td><td>0.75 ± 0.43</td><td>1.08 ± 0.36</td><td>...</td><td>500 ± 160<sup>+480</sup><sub>-320</sub></td><td>5 ± 2 ± 5</td></tr><tr><td>J1413-6205</td><td>18.0 ± 0.64</td><td>1.0 ± 0.24</td><td>1.57 ± 0.10</td><td>0.50 ± 0.03</td><td>0.34 ± 0.13</td><td>...</td><td>...</td></tr></tbody></table>
<table><caption>**Table 13**

Spectral Fitting Results for Young LAT-detected Pulsars</caption><thead><tr><th>PSR<sup>a</sup></th><th>Energy Flux<br>(erg cm<sup>-2</sup> s<sup>-1</sup>)<br>(×10<sup>-11</sup>)</th><th>Γ<sub>100</sub></th><th>E<sub>p</sub><br>(GeV)</th><th>d<sub>p</sub></th><th>b<sub>free</sub></th><th>Luminosity<br>(10<sup>33</sup> erg s<sup>-1</sup>)</th><th>Efficiency<sup>b</sup><br>(%)</th></tr></thead><tbody><tr><td>J0002+6216</td><td>1.9 ± 0.14</td><td>1.6 ± 0.30</td><td>0.82 ± 0.16</td><td>0.65 ± 0.09</td><td>0.85 ± 0.39</td><td>9.01 ± 0.69 ± 3.2</td><td>5.9 ± 0.4 ± 3</td></tr><tr><td>J0007+7303</td><td>43.0 ± 0.33</td><td>1.2 ± 0.04</td><td>2.44 ± 0.03</td><td>0.36 ± 0.01</td><td>0.56 ± 0.04</td><td>101.23 ± 0.76 ± 39</td><td>22.7 ± 0.2 ± 10</td></tr><tr><td>J0106+4855</td><td>1.9 ± 0.07</td><td>1.2 ± 0.20</td><td>2.37 ± 0.11</td><td>0.67 ± 0.06</td><td>1.05 ± 0.26</td><td>21.57 ± 0.81<sup>+21</sup><sub>-14</sub></td><td>73 ± 3 ± 70</td></tr><tr><td>J0117+5914 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J0139+5814 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J0205+6449</td><td>6.4 ± 0.20</td><td>1.6 ± 0.22</td><td>0.26 ± 0.10</td><td>0.45 ± 0.08</td><td>0.20 ± 0.26</td><td>78.8 ± 2.5 ± 9.5</td><td>0.295 ± 0.009 ± 0.04</td></tr><tr><td>J0248+6021</td><td>2.9 ± 0.21</td><td>1.7 ± 0.26</td><td>0.77 ± 0.10</td><td>1.02 ± 0.12</td><td>1.16 ± 0.38</td><td>14.1 ± 1.0 ± 2.7</td><td>6.6 ± 0.5 ± 1</td></tr><tr><td>J0357+3205</td><td>6.0 ± 0.18</td><td>0.73 ± 0.23</td><td>0.87 ± 0.03</td><td>0.95 ± 0.05</td><td>0.64 ± 0.14</td><td>...</td><td>...</td></tr><tr><td>J0359+5414</td><td>2.0 ± 0.13</td><td>1.0 ± 0.56</td><td>1.31 ± 0.12</td><td>0.86 ± 0.10</td><td>0.59 ± 0.40</td><td>...</td><td>...</td></tr><tr><td>J0514-4408</td><td>0.56 ± 0.04</td><td>...</td><td>0.60 ± 0.06</td><td>1.23 ± 0.19</td><td>...</td><td>0.62 ± 0.05<sup>+0.60</sup><sub>-0.40</sub></td><td>25 ± 2 ± 20</td></tr><tr><td>J0534+2200</td><td>150.0 ± 1.3</td><td>2.0 ± 0.03</td><td>0.04 ± 0.03</td><td>0.23 ± 0.01</td><td>0.61 ± 0.08</td><td>685.1 ± 5.8<sup>+280</sup><sub>-170</sub></td><td>0.157 ± 0.001<sup>+0.06</sup><sub>-0.04</sub></td></tr><tr><td>J0540-6919</td><td>2.7 ± 0.15</td><td>...</td><td>0.02 ± 0.08</td><td>0.26 ± 0.05</td><td>...</td><td>7890 ± 440 ± 350</td><td>5.4 ± 0.3 ± 0.2</td></tr><tr><td>J0554+3107</td><td>1.9 ± 0.09</td><td>0.90 ± 0.43</td><td>1.19 ± 0.07</td><td>1.04 ± 0.11</td><td>0.73 ± 0.31</td><td>...</td><td>...</td></tr><tr><td>J0622+3749</td><td>1.8 ± 0.09</td><td>0.65 ± 0.50</td><td>0.75 ± 0.04</td><td>1.60 ± 0.15</td><td>0.69 ± 0.32</td><td>...</td><td>...</td></tr><tr><td>J0631+0646</td><td>1.6 ± 0.13</td><td>...</td><td>2.65 ± 0.23</td><td>1.05 ± 0.17</td><td>...</td><td>40.3 ± 3.2<sup>+39</sup><sub>-26</sub></td><td>39 ± 3 ± 40</td></tr><tr><td>J0631+1036</td><td>3.0 ± 0.14</td><td>1.6 ± 0.12</td><td>2.00 ± 0.14</td><td>0.60 ± 0.07</td><td>1.55 ± 0.39</td><td>16.06 ± 0.72<sup>+15</sup><sub>-10</sub></td><td>9.4 ± 0.4 ± 9</td></tr><tr><td>J0633+0632</td><td>9.6 ± 0.24</td><td>1.1 ± 0.17</td><td>1.43 ± 0.06</td><td>0.60 ± 0.03</td><td>0.48 ± 0.12</td><td>...</td><td>...</td></tr><tr><td>J0633+1746</td><td>420.0 ± 1.1</td><td>1.1 ± 0.01</td><td>1.63 ± 0.01</td><td>0.66 ± 0.00</td><td>0.70 ± 0.01</td><td>18.23 ± 0.05 ± 9.1</td><td>56.1 ± 0.2 ± 40</td></tr><tr><td>J0659+1414</td><td>2.7 ± 0.09</td><td>1.5 ± 0.27</td><td>0.16 ± 0.03</td><td>0.86 ± 0.09</td><td>0.12 ± 0.29</td><td>0.26 ± 0.01 ± 0.05</td><td>0.69 ± 0.02 ± 0.2</td></tr><tr><td>J0729-1448</td><td>0.6 ± 0.11</td><td>...</td><td>0.07 ± 0.41</td><td>0.43 ± 0.30</td><td>...</td><td>5.16 ± 0.93<sup>+5.0</sup><sub>-3.3</sub></td><td>1.8 ± 0.3 ± 2</td></tr><tr><td>J0729-1836 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J0734-1559</td><td>4.6 ± 0.14</td><td>1.4 ± 0.22</td><td>0.62 ± 0.08</td><td>0.36 ± 0.03</td><td>0.29 ± 0.19</td><td>...</td><td>...</td></tr><tr><td>J0742-2822</td><td>1.5 ± 0.11</td><td>...</td><td>0.95 ± 0.19</td><td>0.55 ± 0.11</td><td>...</td><td>7.28 ± 0.54<sup>+9.1</sup><sub>-4.7</sub></td><td>5.1 ± 0.4<sup>+6</sup><sub>-3</sub></td></tr><tr><td>J0744-2525</td><td>0.46 ± 0.12</td><td>1.6 ± 0.30</td><td>1.45 ± 0.16</td><td>0.64 ± 0.10</td><td>1.23 ± 0.58</td><td>...</td><td>...</td></tr><tr><td>J0802-5613</td><td>0.66 ± 0.06</td><td>...</td><td>1.26 ± 0.12</td><td>1.10 ± 0.20</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J0834-4159 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J0835-4510</td><td>930.0 ± 3.0</td><td>1.4 ± 0.01</td><td>1.27 ± 0.01</td><td>0.52 ± 0.00</td><td>0.49 ± 0.01</td><td>87.18 ± 0.28<sup>+73</sup><sub>-12</sub></td><td>1.289 ± 0.004<sup>+1</sup><sub>-0.2</sub></td></tr><tr><td>J0908-4913</td><td>2.2 ± 0.31</td><td>...</td><td>0.60 ± 0.15</td><td>1.07 ± 0.21</td><td>...</td><td>2.62 ± 0.37<sup>+16</sup><sub>-2.4</sub></td><td>0.53 ± 0.08<sup>+3</sup><sub>-0.5</sub></td></tr><tr><td>J0922+0638 *</td><td>0.22 ± 0.04</td><td>...</td><td>...</td><td>0.12 ± 0.16</td><td>...</td><td>0.31 ± 0.06<sup>+0.12</sup><sub>-0.05</sub></td><td>4.6 ± 0.9<sup>+2</sup><sub>-0.8</sub></td></tr><tr><td>J0940-5428</td><td>1.7 ± 0.15</td><td>...</td><td>1.23 ± 0.18</td><td>0.85 ± 0.15</td><td>...</td><td>0.30 ± 0.03<sup>+0.29</sup><sub>-0.19</sub></td><td>0.015 ± 0.001 ± 0.01</td></tr><tr><td>J1016-5857</td><td>7.0 ± 0.64</td><td>1.5 ± 0.58</td><td>0.89 ± 0.30</td><td>0.63 ± 0.10</td><td>0.58 ± 0.39</td><td>83.8 ± 7.7<sup>+80</sup><sub>-54</sub></td><td>3.3 ± 0.3 ± 3</td></tr><tr><td>J1019-5749</td><td>2.7 ± 0.59</td><td>...</td><td>0.60 ± 0.74</td><td>0.50 ± 0.16</td><td>...</td><td>388 ± 84<sup>+370</sup><sub>-250</sub></td><td>210 ± 50 ± 200</td></tr><tr><td>J1023-5746</td><td>15.0 ± 1.1</td><td>...</td><td>0.62 ± 0.13</td><td>0.67 ± 0.06</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1028-5819</td><td>25.0 ± 0.67</td><td>1.1 ± 0.18</td><td>0.89 ± 0.07</td><td>0.39 ± 0.02</td><td>0.21 ± 0.10</td><td>59.4 ± 1.6<sup>+57</sup><sub>-38</sub></td><td>8.1 ± 0.2 ± 8</td></tr><tr><td>J1044-5737</td><td>11.0 ± 0.35</td><td>1.8 ± 0.11</td><td>0.65 ± 0.08</td><td>0.49 ± 0.03</td><td>0.83 ± 0.18</td><td>...</td><td>...</td></tr><tr><td>J1048-5832</td><td>19.0 ± 0.46</td><td>1.2 ± 0.15</td><td>0.97 ± 0.07</td><td>0.41 ± 0.02</td><td>0.28 ± 0.10</td><td>186.4 ± 4.7<sup>+190</sup><sub>-79</sub></td><td>9.4 ± 0.2<sup>+9</sup><sub>-4</sub></td></tr><tr><td>J1055-6028</td><td>1.9 ± 0.33</td><td>...</td><td>1.22 ± 0.49</td><td>0.69 ± 0.20</td><td>...</td><td>33.6 ± 5.8<sup>+32</sup><sub>-21</sub></td><td>2.9 ± 0.5 ± 3</td></tr><tr><td>J1057-5226</td><td>30.0 ± 0.26</td><td>1.0 ± 0.06</td><td>1.21 ± 0.01</td><td>0.88 ± 0.02</td><td>0.85 ± 0.05</td><td>4.34 ± 0.04<sup>+4.5</sup><sub>-2.9</sub></td><td>14.4 ± 0.1<sup>+20</sup><sub>-10</sub></td></tr><tr><td>J1057-5851</td><td>1.3 ± 0.16</td><td>...</td><td>1.15 ± 0.13</td><td>1.73 ± 0.36</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1105-6037</td><td>3.1 ± 0.35</td><td>...</td><td>1.14 ± 0.27</td><td>0.76 ± 0.13</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1105-6107</td><td>2.3 ± 0.39</td><td>...</td><td>0.52 ± 0.37</td><td>0.69 ± 0.19</td><td>...</td><td>15.6 ± 2.6<sup>+15</sup><sub>-10</sub></td><td>0.6 ± 0.1 ± 0.6</td></tr><tr><td>J1111-6039</td><td>5.9 ± 0.34</td><td>0.84 ± 0.53</td><td>2.68 ± 0.25</td><td>0.58 ± 0.06</td><td>0.30 ± 0.24</td><td>...</td><td>...</td></tr><tr><td>J1112-6103</td><td>2.2 ± 0.42</td><td>...</td><td>0.55 ± 0.54</td><td>0.55 ± 0.18</td><td>...</td><td>53 ± 10<sup>+51</sup><sub>-34</sub></td><td>1.2 ± 0.2 ± 1</td></tr><tr><td>J1119-6127</td><td>4.4 ± 0.32</td><td>-0.64 ± 2.7</td><td>1.08 ± 0.31</td><td>0.72 ± 0.18</td><td>-0.26 ± 0.51</td><td>371 ± 27 ± 35</td><td>16 ± 1 ± 2</td></tr><tr><td>J1124-5916</td><td>6.1 ± 0.20</td><td>1.5 ± 0.22</td><td>0.36 ± 0.09</td><td>0.41 ± 0.04</td><td>0.23 ± 0.20</td><td>168.3 ± 5.6 ± 74</td><td>1.41 ± 0.05 ± 0.4</td></tr><tr><td>J1135-6055</td><td>4.6 ± 0.22</td><td>1.2 ± 0.38</td><td>0.78 ± 0.13</td><td>0.51 ± 0.06</td><td>0.24 ± 0.25</td><td>...</td><td>...</td></tr><tr><td>J1139-6247</td><td>1.9 ± 0.21</td><td>...</td><td>1.92 ± 0.54</td><td>0.39 ± 0.09</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1151-6108</td><td>1.0 ± 0.14</td><td>...</td><td>1.39 ± 0.28</td><td>0.90 ± 0.23</td><td>...</td><td>6.10 ± 0.86<sup>+5.9</sup><sub>-3.9</sub></td><td>1.6 ± 0.2 ± 2</td></tr><tr><td>J1203-6242</td><td>3.7 ± 0.36</td><td>...</td><td>1.10 ± 0.26</td><td>0.58 ± 0.08</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1208-6238</td><td>3.7 ± 0.40</td><td>...</td><td>1.00 ± 0.41</td><td>0.49 ± 0.09</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1224-6407 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1231-5113</td><td>1.1 ± 0.07</td><td>...</td><td>0.60 ± 0.06</td><td>1.10 ± 0.16</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1231-6511</td><td>1.2 ± 0.14</td><td>...</td><td>0.99 ± 0.19</td><td>0.82 ± 0.18</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1253-5820</td><td>0.43 ± 0.10</td><td>...</td><td>0.51 ± 0.16</td><td>1.38 ± 0.57</td><td>...</td><td>1.37 ± 0.33<sup>+1.3</sup><sub>-0.88</sub></td><td>28 ± 7 ± 30</td></tr><tr><td>J1341-6220 *</td><td>2.2 ± 0.52</td><td>...</td><td>...</td><td>0.20 ± 0.13</td><td>...</td><td>424 ± 99<sup>+410</sup><sub>-270</sub></td><td>31 ± 7 ± 30</td></tr><tr><td>J1350-6225</td><td>3.6 ± 0.41</td><td>...</td><td>1.95 ± 0.33</td><td>0.75 ± 0.13</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1357-6429</td><td>2.9 ± 0.24</td><td>...</td><td>0.35 ± 0.12</td><td>0.70 ± 0.12</td><td>...</td><td>33.9 ± 2.8<sup>+33</sup><sub>-22</sub></td><td>1.11 ± 0.09 ± 1</td></tr><tr><td>J1358-6025</td><td>3.2 ± 0.36</td><td>...</td><td>0.72 ± 0.30</td><td>0.52 ± 0.11</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1410-6132</td><td>2.3 ± 0.71</td><td>...</td><td>0.75 ± 0.43</td><td>1.08 ± 0.36</td><td>...</td><td>500 ± 160<sup>+480</sup><sub>-320</sub></td><td>5 ± 2 ± 5</td></tr><tr><td>J1413-6205</td><td>18.0 ± 0.64</td><td>1.0 ± 0.24</td><td>1.57 ± 0.10</td><td>0.50 ± 0.03</td><td>0.34 ± 0.13</td><td>...</td><td>...</td></tr></tbody></table>
<table><caption>**Table 13**
(Continued)</caption><thead><tr><th>PSR<sup>a</sup></th><th>Energy Flux<br>(erg cm<sup>-2</sup> s<sup>-1</sup>)<br>(×10<sup>-11</sup>)</th><th>Γ<sub>100</sub></th><th>E<sub>p</sub><br>(GeV)</th><th>d<sub>p</sub></th><th>b<sub>free</sub></th><th>Luminosity<br>(10<sup>33</sup> erg s<sup>-1</sup>)</th><th>Efficiency<sup>b</sup><br>(%)</th></tr></thead><tbody><tr><td>J1418-6058</td><td>30.0 ± 1.8</td><td>1.3 ± 0.20</td><td>1.00 ± 0.13</td><td>0.76 ± 0.05</td><td>0.41 ± 0.13</td><td>91.0 ± 5.5<sup>+97</sup><sub>-62</sub></td><td>1.8 ± 0.1<sup>+2</sup><sub>-1</sub></td></tr><tr><td>J1420-6048</td><td>13.0 ± 1.6</td><td>...</td><td>0.73 ± 0.18</td><td>0.78 ± 0.10</td><td>...</td><td>490 ± 61<sup>+470</sup><sub>-310</sub></td><td>4.8 ± 0.6 ± 5</td></tr><tr><td>J1422-6138</td><td>5.3 ± 0.25</td><td>0.55 ± 0.52</td><td>3.66 ± 0.18</td><td>0.95 ± 0.09</td><td>0.56 ± 0.24</td><td>...</td><td>...</td></tr><tr><td>J1429-5911</td><td>11.0 ± 0.36</td><td>1.6 ± 0.17</td><td>0.54 ± 0.08</td><td>0.51 ± 0.04</td><td>0.52 ± 0.17</td><td>...</td><td>...</td></tr><tr><td>J1447-5757</td><td>2.3 ± 0.26</td><td>...</td><td>0.46 ± 0.15</td><td>0.78 ± 0.16</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1459-6053</td><td>12.0 ± 0.37</td><td>1.6 ± 0.16</td><td>0.37 ± 0.07</td><td>0.44 ± 0.03</td><td>0.41 ± 0.15</td><td>...</td><td>...</td></tr><tr><td>J1509-5850</td><td>12.0 ± 0.53</td><td>1.5 ± 0.18</td><td>1.22 ± 0.13</td><td>0.53 ± 0.04</td><td>0.65 ± 0.17</td><td>166.2 ± 7.2<sup>+160</sup><sub>-110</sub></td><td>32 ± 1 ± 30</td></tr><tr><td>J1513-5908‡</td><td>1.2 ± 0.40</td><td>...</td><td>...</td><td>...</td><td>...</td><td>27.8 ± 9.3<sup>+19</sup><sub>-9.2</sub></td><td>0.16 ± 0.05<sup>+0.1</sup><sub>-0.05</sub></td></tr><tr><td>J1522-5735</td><td>7.6 ± 0.40</td><td>1.3 ± 0.29</td><td>0.88 ± 0.11</td><td>0.70 ± 0.07</td><td>0.53 ± 0.21</td><td>...</td><td>...</td></tr><tr><td>J1528-5838</td><td>1.8 ± 0.16</td><td>...</td><td>1.69 ± 0.20</td><td>0.97 ± 0.16</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1531-5610</td><td>1.8 ± 0.30</td><td>...</td><td>1.09 ± 0.20</td><td>1.41 ± 0.34</td><td>...</td><td>17.6 ± 2.9<sup>+17</sup><sub>-11</sub></td><td>1.9 ± 0.3 ± 2</td></tr><tr><td>J1614-5048</td><td>2.0 ± 0.87</td><td>...</td><td>0.97 ± 0.87</td><td>0.94 ± 0.38</td><td>...</td><td>64 ± 28<sup>+61</sup><sub>-41</sub></td><td>4 ± 2 ± 4</td></tr><tr><td>J1615-5137</td><td>3.3 ± 0.30</td><td>...</td><td>2.88 ± 0.22</td><td>1.34 ± 0.21</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1620-4927</td><td>13.0 ± 0.52</td><td>1.3 ± 0.20</td><td>2.86 ± 0.14</td><td>0.91 ± 0.06</td><td>0.94 ± 0.18</td><td>...</td><td>...</td></tr><tr><td>J1623-5005</td><td>6.1 ± 0.50</td><td>0.55 ± 1.1</td><td>3.03 ± 0.40</td><td>0.63 ± 0.09</td><td>0.29 ± 0.35</td><td>...</td><td>...</td></tr><tr><td>J1624-4041</td><td>2.7 ± 0.15</td><td>1.4 ± 0.27</td><td>1.27 ± 0.11</td><td>0.76 ± 0.09</td><td>0.87 ± 0.30</td><td>...</td><td>...</td></tr><tr><td>J1641-5317</td><td>1.5 ± 0.12</td><td>...</td><td>1.06 ± 0.13</td><td>0.81 ± 0.13</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1646-4346 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1648-4611</td><td>4.8 ± 0.44</td><td>1.1 ± 0.66</td><td>2.48 ± 0.31</td><td>0.81 ± 0.13</td><td>0.67 ± 0.45</td><td>114 ± 10<sup>+110</sup><sub>-73</sub></td><td>55 ± 5 ± 50</td></tr><tr><td>J1650-4601</td><td>5.6 ± 0.59</td><td>...</td><td>1.32 ± 0.24</td><td>0.86 ± 0.13</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1702-4128</td><td>2.6 ± 0.64</td><td>...</td><td>0.87 ± 0.32</td><td>1.12 ± 0.30</td><td>...</td><td>49 ± 12<sup>+47</sup><sub>-31</sub></td><td>14 ± 4 ± 10</td></tr><tr><td>J1705-1906</td><td>0.36 ± 0.08</td><td>...</td><td>0.88 ± 0.10</td><td>3.06 ± 1.66</td><td>...</td><td>0.24 ± 0.05<sup>+0.23</sup><sub>-0.15</sub></td><td>3.9 ± 0.8 ± 4</td></tr><tr><td>J1709-4429</td><td>140.0 ± 0.92</td><td>1.3 ± 0.04</td><td>1.43 ± 0.02</td><td>0.37 ± 0.01</td><td>0.43 ± 0.03</td><td>1114.2 ± 7.4 ± 450</td><td>32.1 ± 0.2 ± 10</td></tr><tr><td>J1714-3830</td><td>9.1 ± 0.92</td><td>0.90 ± 0.82</td><td>0.86 ± 0.52</td><td>0.48 ± 0.12</td><td>-0.13 ± 0.28</td><td>...</td><td>...</td></tr><tr><td>J1718-3825</td><td>10.0 ± 0.67</td><td>1.3 ± 0.40</td><td>0.56 ± 0.14</td><td>0.68 ± 0.07</td><td>0.27 ± 0.25</td><td>150.9 ± 9.8<sup>+140</sup><sub>-97</sub></td><td>12.1 ± 0.8 ± 10</td></tr><tr><td>J1730-3350</td><td>4.4 ± 0.73</td><td>...</td><td>0.07 ± 0.24</td><td>0.47 ± 0.15</td><td>...</td><td>63 ± 11<sup>+61</sup><sub>-41</sub></td><td>5.2 ± 0.9 ± 5</td></tr><tr><td>J1731-4744</td><td>0.39 ± 0.12</td><td>...</td><td>0.37 ± 0.07</td><td>3.44 ± 2.49</td><td>...</td><td>0.23 ± 0.07<sup>+0.07</sup><sub>-0.16</sub></td><td>2.0 ± 0.6<sup>+0.6</sup><sub>-1</sub></td></tr><tr><td>J1732-3131</td><td>18.0 ± 0.49</td><td>0.37 ± 0.31</td><td>2.09 ± 0.05</td><td>1.04 ± 0.05</td><td>0.47 ± 0.13</td><td>8.79 ± 0.24<sup>+8.4</sup><sub>-5.6</sub></td><td>6.0 ± 0.2 ± 6</td></tr><tr><td>J1736-3422</td><td>1.7 ± 0.27</td><td>...</td><td>1.80 ± 0.39</td><td>0.75 ± 0.18</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1739-3023</td><td>2.1 ± 0.43</td><td>...</td><td>1.18 ± 0.26</td><td>1.34 ± 0.38</td><td>...</td><td>24.0 ± 4.8<sup>+23</sup><sub>-15</sub></td><td>8 ± 2 ± 8</td></tr><tr><td>J1740+1000</td><td>0.36 ± 0.08</td><td>...</td><td>0.33 ± 0.14</td><td>1.72 ± 0.98</td><td>...</td><td>0.65 ± 0.14<sup>+0.62</sup><sub>-0.42</sub></td><td>0.28 ± 0.06 ± 0.3</td></tr><tr><td>J1741-2054</td><td>12.0 ± 0.26</td><td>0.96 ± 0.15</td><td>0.84 ± 0.02</td><td>1.40 ± 0.05</td><td>0.86 ± 0.13</td><td>1.28 ± 0.03<sup>+13</sup><sub>-0.71</sub></td><td>13.5 ± 0.3<sup>+100</sup><sub>-7</sub></td></tr><tr><td>J1742-3321</td><td>1.5 ± 0.26</td><td>...</td><td>1.76 ± 0.33</td><td>1.18 ± 0.32</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1746-3239</td><td>5.1 ± 0.29</td><td>1.1 ± 0.37</td><td>1.36 ± 0.11</td><td>0.89 ± 0.09</td><td>0.65 ± 0.28</td><td>...</td><td>...</td></tr><tr><td>J1747-2958</td><td>16.0 ± 1.1</td><td>0.62 ± 0.54</td><td>0.53 ± 0.12</td><td>0.68 ± 0.06</td><td>-0.05 ± 0.19</td><td>430 ± 31 ± 120</td><td>17 ± 1 ± 6</td></tr><tr><td>J1748-2815 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1757-2421 ★</td><td>2.5 ± 0.57</td><td>...</td><td>...</td><td>0.09 ± 0.19</td><td>...</td><td>28.7 ± 6.7<sup>+28</sup><sub>-18</sub></td><td>70 ± 20 ± 70</td></tr><tr><td>J1801-2451</td><td>3.2 ± 0.41</td><td>...</td><td>0.70 ± 0.47</td><td>0.46 ± 0.12</td><td>...</td><td>55.2 ± 7.2<sup>+53</sup><sub>-35</sub></td><td>3.1 ± 0.4 ± 3</td></tr><tr><td>J1803-2149</td><td>8.9 ± 0.68</td><td>1.2 ± 0.48</td><td>1.34 ± 0.26</td><td>0.58 ± 0.08</td><td>0.31 ± 0.29</td><td>...</td><td>...</td></tr><tr><td>J1809-2332</td><td>42.0 ± 0.85</td><td>1.1 ± 0.12</td><td>1.29 ± 0.05</td><td>0.50 ± 0.02</td><td>0.34 ± 0.07</td><td>146.9 ± 3.0<sup>+220</sup><sub>-120</sub></td><td>34.2 ± 0.7<sup>+50</sup><sub>-30</sub></td></tr><tr><td>J1813-1246</td><td>25.0 ± 0.62</td><td>1.5 ± 0.12</td><td>0.48 ± 0.05</td><td>0.45 ± 0.02</td><td>0.45 ± 0.11</td><td>...</td><td>...</td></tr><tr><td>J1816-0755 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1817-1742</td><td>2.8 ± 0.45</td><td>...</td><td>1.12 ± 0.54</td><td>0.50 ± 0.14</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1826-1256</td><td>41.0 ± 1.3</td><td>1.6 ± 0.10</td><td>0.87 ± 0.07</td><td>0.63 ± 0.03</td><td>0.69 ± 0.11</td><td>...</td><td>...</td></tr><tr><td>J1827-1446</td><td>1.9 ± 0.18</td><td>...</td><td>2.34 ± 0.14</td><td>2.73 ± 0.44</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1828-1101 ★</td><td>4.8 ± 0.78</td><td>...</td><td>...</td><td>0.38 ± 0.17</td><td>...</td><td>130 ± 21<sup>+120</sup><sub>-83</sub></td><td>8 ± 1 ± 8</td></tr><tr><td>J1831-0952</td><td>5.4 ± 0.78</td><td>...</td><td>0.51 ± 0.10</td><td>1.50 ± 0.31</td><td>...</td><td>88 ± 13<sup>+85</sup><sub>-56</sub></td><td>8 ± 1 ± 8</td></tr><tr><td>J1833-1034</td><td>8.9 ± 0.61</td><td>1.1 ± 0.76</td><td>0.31 ± 0.34</td><td>0.49 ± 0.15</td><td>-0.25 ± 0.32</td><td>179 ± 12 ± 25</td><td>0.53 ± 0.04 ± 0.08</td></tr><tr><td>J1835-1106 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1836+5925</td><td>62.0 ± 0.28</td><td>1.1 ± 0.03</td><td>1.48 ± 0.01</td><td>0.58 ± 0.01</td><td>0.65 ± 0.03</td><td>20.82 ± 0.09<sup>+27</sup><sub>-16</sub></td><td>182.6 ± 0.8<sup>+200</sup><sub>-100</sub></td></tr><tr><td>J1837-0604</td><td>2.8 ± 0.77</td><td>...</td><td>0.33 ± 1.07</td><td>0.41 ± 0.24</td><td>...</td><td>75 ± 21<sup>+72</sup><sub>-48</sub></td><td>4 ± 1 ± 4</td></tr><tr><td>J1838-0537</td><td>12.0 ± 1.3</td><td>0.92 ± 0.66</td><td>1.28 ± 0.35</td><td>0.66 ± 0.09</td><td>0.19 ± 0.27</td><td>...</td><td>...</td></tr><tr><td>J1841-0524 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1844-0346</td><td>4.6 ± 0.53</td><td>...</td><td>1.64 ± 0.23</td><td>1.11 ± 0.18</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1846+0919</td><td>3.6 ± 0.11</td><td>1.2 ± 0.18</td><td>2.04 ± 0.08</td><td>0.86 ± 0.07</td><td>1.05 ± 0.22</td><td>...</td><td>...</td></tr><tr><td>J1846-0258</td><td>1.4 ± 0.46</td><td>...</td><td>...</td><td>...</td><td>...</td><td>55 ± 18 ± 7.4</td><td>0.7 ± 0.2 ± 0.1</td></tr><tr><td>J1853-0004</td><td>0.49 ± 0.11</td><td>...</td><td>3.61 ± 0.49</td><td>2.95 ± 1.49</td><td>...</td><td>16.8 ± 3.8<sup>+16</sup><sub>-11</sub></td><td>8 ± 2 ± 8</td></tr><tr><td>J1856+0113 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1857+0143</td><td>1.2 ± 0.26</td><td>...</td><td>2.41 ± 0.37</td><td>2.55 ± 0.86</td><td>...</td><td>29.2 ± 6.4<sup>+28</sup><sub>-19</sub></td><td>7 ± 1 ± 6</td></tr></tbody></table>
<table><caption>**Table 13**
(Continued)</caption><thead><tr><th>PSR<sup>a</sup></th><th>Energy Flux<br>(erg cm<sup>-2</sup> s<sup>-1</sup>)<br>(×10<sup>-11</sup>)</th><th>Γ<sub>100</sub></th><th>E<sub>p</sub><br>(GeV)</th><th>d<sub>p</sub></th><th>b<sub>free</sub></th><th>Luminosity<br>(10<sup>33</sup> erg s<sup>-1</sup>)</th><th>Efficiency<sup>b</sup><br>(%)</th></tr></thead><tbody><tr><td>J1418-6058</td><td>30.0 ± 1.8</td><td>1.3 ± 0.20</td><td>1.00 ± 0.13</td><td>0.76 ± 0.05</td><td>0.41 ± 0.13</td><td>91.0 ± 5.5<sup>+97</sup><sub>-62</sub></td><td>1.8 ± 0.1<sup>+2</sup><sub>-1</sub></td></tr><tr><td>J1420-6048</td><td>13.0 ± 1.6</td><td>...</td><td>0.73 ± 0.18</td><td>0.78 ± 0.10</td><td>...</td><td>490 ± 61<sup>+470</sup><sub>-310</sub></td><td>4.8 ± 0.6 ± 5</td></tr><tr><td>J1422-6138</td><td>5.3 ± 0.25</td><td>0.55 ± 0.52</td><td>3.66 ± 0.18</td><td>0.95 ± 0.09</td><td>0.56 ± 0.24</td><td>...</td><td>...</td></tr><tr><td>J1429-5911</td><td>11.0 ± 0.36</td><td>1.6 ± 0.17</td><td>0.54 ± 0.08</td><td>0.51 ± 0.04</td><td>0.52 ± 0.17</td><td>...</td><td>...</td></tr><tr><td>J1447-5757</td><td>2.3 ± 0.26</td><td>...</td><td>0.46 ± 0.15</td><td>0.78 ± 0.16</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1459-6053</td><td>12.0 ± 0.37</td><td>1.6 ± 0.16</td><td>0.37 ± 0.07</td><td>0.44 ± 0.03</td><td>0.41 ± 0.15</td><td>...</td><td>...</td></tr><tr><td>J1509-5850</td><td>12.0 ± 0.53</td><td>1.5 ± 0.18</td><td>1.22 ± 0.13</td><td>0.53 ± 0.04</td><td>0.65 ± 0.17</td><td>166.2 ± 7.2<sup>+160</sup><sub>-110</sub></td><td>32 ± 1 ± 30</td></tr><tr><td>J1513-5908‡</td><td>1.2 ± 0.40</td><td>...</td><td>...</td><td>...</td><td>...</td><td>27.8 ± 9.3<sup>+19</sup><sub>-9.2</sub></td><td>0.16 ± 0.05<sup>+0.1</sup><sub>-0.05</sub></td></tr><tr><td>J1522-5735</td><td>7.6 ± 0.40</td><td>1.3 ± 0.29</td><td>0.88 ± 0.11</td><td>0.70 ± 0.07</td><td>0.53 ± 0.21</td><td>...</td><td>...</td></tr><tr><td>J1528-5838</td><td>1.8 ± 0.16</td><td>...</td><td>1.69 ± 0.20</td><td>0.97 ± 0.16</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1531-5610</td><td>1.8 ± 0.30</td><td>...</td><td>1.09 ± 0.20</td><td>1.41 ± 0.34</td><td>...</td><td>17.6 ± 2.9<sup>+17</sup><sub>-11</sub></td><td>1.9 ± 0.3 ± 2</td></tr><tr><td>J1614-5048</td><td>2.0 ± 0.87</td><td>...</td><td>0.97 ± 0.87</td><td>0.94 ± 0.38</td><td>...</td><td>64 ± 28<sup>+61</sup><sub>-41</sub></td><td>4 ± 2 ± 4</td></tr><tr><td>J1615-5137</td><td>3.3 ± 0.30</td><td>...</td><td>2.88 ± 0.22</td><td>1.34 ± 0.21</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1620-4927</td><td>13.0 ± 0.52</td><td>1.3 ± 0.20</td><td>2.86 ± 0.14</td><td>0.91 ± 0.06</td><td>0.94 ± 0.18</td><td>...</td><td>...</td></tr><tr><td>J1623-5005</td><td>6.1 ± 0.50</td><td>0.55 ± 1.1</td><td>3.03 ± 0.40</td><td>0.63 ± 0.09</td><td>0.29 ± 0.35</td><td>...</td><td>...</td></tr><tr><td>J1624-4041</td><td>2.7 ± 0.15</td><td>1.4 ± 0.27</td><td>1.27 ± 0.11</td><td>0.76 ± 0.09</td><td>0.87 ± 0.30</td><td>...</td><td>...</td></tr><tr><td>J1641-5317</td><td>1.5 ± 0.12</td><td>...</td><td>1.06 ± 0.13</td><td>0.81 ± 0.13</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1646-4346 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1648-4611</td><td>4.8 ± 0.44</td><td>1.1 ± 0.66</td><td>2.48 ± 0.31</td><td>0.81 ± 0.13</td><td>0.67 ± 0.45</td><td>114 ± 10<sup>+110</sup><sub>-73</sub></td><td>55 ± 5 ± 50</td></tr><tr><td>J1650-4601</td><td>5.6 ± 0.59</td><td>...</td><td>1.32 ± 0.24</td><td>0.86 ± 0.13</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1702-4128</td><td>2.6 ± 0.64</td><td>...</td><td>0.87 ± 0.32</td><td>1.12 ± 0.30</td><td>...</td><td>49 ± 12<sup>+47</sup><sub>-31</sub></td><td>14 ± 4 ± 10</td></tr><tr><td>J1705-1906</td><td>0.36 ± 0.08</td><td>...</td><td>0.88 ± 0.10</td><td>3.06 ± 1.66</td><td>...</td><td>0.24 ± 0.05<sup>+0.23</sup><sub>-0.15</sub></td><td>3.9 ± 0.8 ± 4</td></tr><tr><td>J1709-4429</td><td>140.0 ± 0.92</td><td>1.3 ± 0.04</td><td>1.43 ± 0.02</td><td>0.37 ± 0.01</td><td>0.43 ± 0.03</td><td>1114.2 ± 7.4 ± 450</td><td>32.1 ± 0.2 ± 10</td></tr><tr><td>J1714-3830</td><td>9.1 ± 0.92</td><td>0.90 ± 0.82</td><td>0.86 ± 0.52</td><td>0.48 ± 0.12</td><td>-0.13 ± 0.28</td><td>...</td><td>...</td></tr><tr><td>J1718-3825</td><td>10.0 ± 0.67</td><td>1.3 ± 0.40</td><td>0.56 ± 0.14</td><td>0.68 ± 0.07</td><td>0.27 ± 0.25</td><td>150.9 ± 9.8<sup>+140</sup><sub>-97</sub></td><td>12.1 ± 0.8 ± 10</td></tr><tr><td>J1730-3350</td><td>4.4 ± 0.73</td><td>...</td><td>0.07 ± 0.24</td><td>0.47 ± 0.15</td><td>...</td><td>63 ± 11<sup>+61</sup><sub>-41</sub></td><td>5.2 ± 0.9 ± 5</td></tr><tr><td>J1731-4744</td><td>0.39 ± 0.12</td><td>...</td><td>0.37 ± 0.07</td><td>3.44 ± 2.49</td><td>...</td><td>0.23 ± 0.07<sup>+0.07</sup><sub>-0.16</sub></td><td>2.0 ± 0.6<sup>+0.6</sup><sub>-1</sub></td></tr><tr><td>J1732-3131</td><td>18.0 ± 0.49</td><td>0.37 ± 0.31</td><td>2.09 ± 0.05</td><td>1.04 ± 0.05</td><td>0.47 ± 0.13</td><td>8.79 ± 0.24<sup>+8.4</sup><sub>-5.6</sub></td><td>6.0 ± 0.2 ± 6</td></tr><tr><td>J1736-3422</td><td>1.7 ± 0.27</td><td>...</td><td>1.80 ± 0.39</td><td>0.75 ± 0.18</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1739-3023</td><td>2.1 ± 0.43</td><td>...</td><td>1.18 ± 0.26</td><td>1.34 ± 0.38</td><td>...</td><td>24.0 ± 4.8<sup>+23</sup><sub>-15</sub></td><td>8 ± 2 ± 8</td></tr><tr><td>J1740+1000</td><td>0.36 ± 0.08</td><td>...</td><td>0.33 ± 0.14</td><td>1.72 ± 0.98</td><td>...</td><td>0.65 ± 0.14<sup>+0.62</sup><sub>-0.42</sub></td><td>0.28 ± 0.06 ± 0.3</td></tr><tr><td>J1741-2054</td><td>12.0 ± 0.26</td><td>0.96 ± 0.15</td><td>0.84 ± 0.02</td><td>1.40 ± 0.05</td><td>0.86 ± 0.13</td><td>1.28 ± 0.03<sup>+13</sup><sub>-0.71</sub></td><td>13.5 ± 0.3<sup>+100</sup><sub>-7</sub></td></tr><tr><td>J1742-3321</td><td>1.5 ± 0.26</td><td>...</td><td>1.76 ± 0.33</td><td>1.18 ± 0.32</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1746-3239</td><td>5.1 ± 0.29</td><td>1.1 ± 0.37</td><td>1.36 ± 0.11</td><td>0.89 ± 0.09</td><td>0.65 ± 0.28</td><td>...</td><td>...</td></tr><tr><td>J1747-2958</td><td>16.0 ± 1.1</td><td>0.62 ± 0.54</td><td>0.53 ± 0.12</td><td>0.68 ± 0.06</td><td>-0.05 ± 0.19</td><td>430 ± 31 ± 120</td><td>17 ± 1 ± 6</td></tr><tr><td>J1748-2815 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1757-2421 ★</td><td>2.5 ± 0.57</td><td>...</td><td>...</td><td>0.09 ± 0.19</td><td>...</td><td>28.7 ± 6.7<sup>+28</sup><sub>-18</sub></td><td>70 ± 20 ± 70</td></tr><tr><td>J1801-2451</td><td>3.2 ± 0.41</td><td>...</td><td>0.70 ± 0.47</td><td>0.46 ± 0.12</td><td>...</td><td>55.2 ± 7.2<sup>+53</sup><sub>-35</sub></td><td>3.1 ± 0.4 ± 3</td></tr><tr><td>J1803-2149</td><td>8.9 ± 0.68</td><td>1.2 ± 0.48</td><td>1.34 ± 0.26</td><td>0.58 ± 0.08</td><td>0.31 ± 0.29</td><td>...</td><td>...</td></tr><tr><td>J1809-2332</td><td>42.0 ± 0.85</td><td>1.1 ± 0.12</td><td>1.29 ± 0.05</td><td>0.50 ± 0.02</td><td>0.34 ± 0.07</td><td>146.9 ± 3.0<sup>+220</sup><sub>-120</sub></td><td>34.2 ± 0.7<sup>+50</sup><sub>-30</sub></td></tr><tr><td>J1813-1246</td><td>25.0 ± 0.62</td><td>1.5 ± 0.12</td><td>0.48 ± 0.05</td><td>0.45 ± 0.02</td><td>0.45 ± 0.11</td><td>...</td><td>...</td></tr><tr><td>J1816-0755 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1817-1742</td><td>2.8 ± 0.45</td><td>...</td><td>1.12 ± 0.54</td><td>0.50 ± 0.14</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1826-1256</td><td>41.0 ± 1.3</td><td>1.6 ± 0.10</td><td>0.87 ± 0.07</td><td>0.63 ± 0.03</td><td>0.69 ± 0.11</td><td>...</td><td>...</td></tr><tr><td>J1827-1446</td><td>1.9 ± 0.18</td><td>...</td><td>2.34 ± 0.14</td><td>2.73 ± 0.44</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1828-1101 ★</td><td>4.8 ± 0.78</td><td>...</td><td>...</td><td>0.38 ± 0.17</td><td>...</td><td>130 ± 21<sup>+120</sup><sub>-83</sub></td><td>8 ± 1 ± 8</td></tr><tr><td>J1831-0952</td><td>5.4 ± 0.78</td><td>...</td><td>0.51 ± 0.10</td><td>1.50 ± 0.31</td><td>...</td><td>88 ± 13<sup>+85</sup><sub>-56</sub></td><td>8 ± 1 ± 8</td></tr><tr><td>J1833-1034</td><td>8.9 ± 0.61</td><td>1.1 ± 0.76</td><td>0.31 ± 0.34</td><td>0.49 ± 0.15</td><td>-0.25 ± 0.32</td><td>179 ± 12 ± 25</td><td>0.53 ± 0.04 ± 0.08</td></tr><tr><td>J1835-1106 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1836+5925</td><td>62.0 ± 0.28</td><td>1.1 ± 0.03</td><td>1.48 ± 0.01</td><td>0.58 ± 0.01</td><td>0.65 ± 0.03</td><td>20.82 ± 0.09<sup>+27</sup><sub>-16</sub></td><td>182.6 ± 0.8<sup>+200</sup><sub>-100</sub></td></tr><tr><td>J1837-0604</td><td>2.8 ± 0.77</td><td>...</td><td>0.33 ± 1.07</td><td>0.41 ± 0.24</td><td>...</td><td>75 ± 21<sup>+72</sup><sub>-48</sub></td><td>4 ± 1 ± 4</td></tr><tr><td>J1838-0537</td><td>12.0 ± 1.3</td><td>0.92 ± 0.66</td><td>1.28 ± 0.35</td><td>0.66 ± 0.09</td><td>0.19 ± 0.27</td><td>...</td><td>...</td></tr><tr><td>J1841-0524 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1844-0346</td><td>4.6 ± 0.53</td><td>...</td><td>1.64 ± 0.23</td><td>1.11 ± 0.18</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1846+0919</td><td>3.6 ± 0.11</td><td>1.2 ± 0.18</td><td>2.04 ± 0.08</td><td>0.86 ± 0.07</td><td>1.05 ± 0.22</td><td>...</td><td>...</td></tr><tr><td>J1846-0258</td><td>1.4 ± 0.46</td><td>...</td><td>...</td><td>...</td><td>...</td><td>55 ± 18 ± 7.4</td><td>0.7 ± 0.2 ± 0.1</td></tr><tr><td>J1853-0004</td><td>0.49 ± 0.11</td><td>...</td><td>3.61 ± 0.49</td><td>2.95 ± 1.49</td><td>...</td><td>16.8 ± 3.8<sup>+16</sup><sub>-11</sub></td><td>8 ± 2 ± 8</td></tr><tr><td>J1856+0113 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1857+0143</td><td>1.2 ± 0.26</td><td>...</td><td>2.41 ± 0.37</td><td>2.55 ± 0.86</td><td>...</td><td>29.2 ± 6.4<sup>+28</sup><sub>-19</sub></td><td>7 ± 1 ± 6</td></tr></tbody></table>
<table><caption>**Table 13**
(Continued)</caption><thead><tr><th>PSR<sup>a</sup></th><th>Energy Flux<br>(erg cm<sup>-2</sup> s<sup>-1</sup>)<br>(×10<sup>-11</sup>)</th><th>Γ<sub>100</sub></th><th>E<sub>p</sub><br>(GeV)</th><th>d<sub>p</sub></th><th>b<sub>free</sub></th><th>Luminosity<br>(10<sup>33</sup> erg s<sup>-1</sup>)</th><th>Efficiency<sup>b</sup><br>(%)</th></tr></thead><tbody><tr><td>J1906+0722</td><td>8.6 ± 0.80</td><td>...</td><td>0.58 ± 0.22</td><td>0.63 ± 0.09</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1907+0602</td><td>30.0 ± 0.76</td><td>1.2 ± 0.16</td><td>0.95 ± 0.06</td><td>0.48 ± 0.02</td><td>0.27 ± 0.10</td><td>235.8 ± 6.1<sup>+230</sup><sub>-150</sub></td><td>8.4 ± 0.2 ± 8</td></tr><tr><td>J1913+0904</td><td>2.0 ± 0.34</td><td>...</td><td>1.69 ± 0.35</td><td>1.19 ± 0.29</td><td>...</td><td>21.2 ± 3.7<sup>+20</sup><sub>-14</sub></td><td>13 ± 2 ± 10</td></tr><tr><td>J1913+1011</td><td>1.8 ± 0.31</td><td>...</td><td>1.65 ± 5.21</td><td>0.13 ± 0.09</td><td>...</td><td>46.6 ± 8.0<sup>+45</sup><sub>-30</sub></td><td>1.6 ± 0.3 ± 2</td></tr><tr><td>J1925+1720</td><td>0.95 ± 0.27</td><td>...</td><td>1.18 ± 0.40</td><td>1.24 ± 0.48</td><td>...</td><td>29.0 ± 8.2<sup>+28</sup><sub>-19</sub></td><td>3.0 ± 0.9 ± 3</td></tr><tr><td>J1928+1746 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1932+1916</td><td>6.5 ± 0.45</td><td>1.2 ± 0.40</td><td>0.72 ± 0.13</td><td>0.77 ± 0.08</td><td>0.41 ± 0.25</td><td>...</td><td>...</td></tr><tr><td>J1932+2220</td><td>0.52 ± 0.15</td><td>...</td><td>1.06 ± 0.53</td><td>0.75 ± 0.33</td><td>...</td><td>73 ± 21<sup>+19</sup><sub>-10</sub></td><td>10 ± 3<sup>+2</sup><sub>-1</sub></td></tr><tr><td>J1935+2025</td><td>2.2 ± 0.31</td><td>...</td><td>0.55 ± 0.18</td><td>0.99 ± 0.26</td><td>...</td><td>54.9 ± 7.8<sup>+53</sup><sub>-35</sub></td><td>1.2 ± 0.2 ± 1</td></tr><tr><td>J1952+3252</td><td>15.0 ± 0.28</td><td>1.3 ± 0.12</td><td>0.99 ± 0.05</td><td>0.42 ± 0.02</td><td>0.34 ± 0.10</td><td>159.0 ± 3.0<sup>+280</sup><sub>-140</sub></td><td>4.27 ± 0.08<sup>+8</sup><sub>-4</sub></td></tr><tr><td>J1954+2836</td><td>11.0 ± 0.32</td><td>1.1 ± 0.28</td><td>1.17 ± 0.09</td><td>0.45 ± 0.03</td><td>0.27 ± 0.15</td><td>...</td><td>...</td></tr><tr><td>J1954+3852 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1957+5033</td><td>2.6 ± 0.08</td><td>0.50 ± 0.40</td><td>0.76 ± 0.03</td><td>1.03 ± 0.07</td><td>0.43 ± 0.20</td><td>...</td><td>...</td></tr><tr><td>J1958+2846</td><td>11.0 ± 0.29</td><td>0.72 ± 0.31</td><td>1.15 ± 0.06</td><td>0.60 ± 0.04</td><td>0.21 ± 0.13</td><td>...</td><td>...</td></tr><tr><td>J2006+3102</td><td>1.1 ± 0.15</td><td>...</td><td>1.47 ± 0.36</td><td>0.79 ± 0.21</td><td>...</td><td>46.3 ± 6.6<sup>+44</sup><sub>-30</sub></td><td>21 ± 3 ± 20</td></tr><tr><td>J2017+3625</td><td>7.5 ± 0.46</td><td>1.4 ± 0.30</td><td>0.95 ± 0.10</td><td>0.92 ± 0.09</td><td>0.74 ± 0.25</td><td>...</td><td>...</td></tr><tr><td>J2021+3651</td><td>49.0 ± 0.79</td><td>0.99 ± 0.10</td><td>1.06 ± 0.03</td><td>0.50 ± 0.01</td><td>0.25 ± 0.06</td><td>190.8 ± 3.0<sup>+530</sup><sub>-180</sub></td><td>5.69 ± 0.09<sup>+20</sup><sub>-5</sub></td></tr><tr><td>J2021+4026</td><td>80.0 ± 1.1</td><td>1.1 ± 0.07</td><td>0.87 ± 0.02</td><td>0.92 ± 0.02</td><td>0.39 ± 0.05</td><td>215.6 ± 2.9 ± 110</td><td>183 ± 2 ± 100</td></tr><tr><td>J2022+3842</td><td>2.7 ± 0.42</td><td>...</td><td>0.20 ± 0.22</td><td>0.61 ± 0.15</td><td>...</td><td>317 ± 50<sup>+300</sup><sub>-110</sub></td><td>1.1 ± 0.2<sup>+1</sup><sub>-0.4</sub></td></tr><tr><td>J2028+3332</td><td>5.7 ± 0.19</td><td>-0.33 ± 0.60</td><td>1.51 ± 0.06</td><td>1.08 ± 0.07</td><td>0.22 ± 0.17</td><td>...</td><td>...</td></tr><tr><td>J2030+3641</td><td>4.2 ± 0.17</td><td>0.55 ± 0.49</td><td>1.87 ± 0.08</td><td>1.03 ± 0.09</td><td>0.63 ± 0.25</td><td>45.5 ± 1.9 ± 25</td><td>142 ± 6 ± 100</td></tr><tr><td>J2030+4415</td><td>4.4 ± 0.22</td><td>0.48 ± 0.57</td><td>1.20 ± 0.07</td><td>1.20 ± 0.11</td><td>0.51 ± 0.27</td><td>1.32 ± 0.06<sup>+2.1</sup><sub>-0.85</sub></td><td>7.8 ± 0.4<sup>+10</sup><sub>-5</sub></td></tr><tr><td>J2032+4127</td><td>14.0 ± 0.47</td><td>1.0 ± 0.21</td><td>2.61 ± 0.10</td><td>0.56 ± 0.03</td><td>0.55 ± 0.14</td><td>52.8 ± 1.7 ± 3.0</td><td>34 ± 1 ± 2</td></tr><tr><td>J2043+2740</td><td>0.9 ± 0.07</td><td>...</td><td>0.83 ± 0.10</td><td>1.06 ± 0.18</td><td>...</td><td>2.37 ± 0.18<sup>+2.3</sup><sub>-1.5</sub></td><td>4.3 ± 0.3 ± 4</td></tr><tr><td>J2055+2539</td><td>5.3 ± 0.10</td><td>0.69 ± 0.17</td><td>1.21 ± 0.03</td><td>0.89 ± 0.04</td><td>0.65 ± 0.12</td><td>...</td><td>...</td></tr><tr><td>J2111+4606</td><td>4.9 ± 0.15</td><td>1.6 ± 0.15</td><td>1.33 ± 0.12</td><td>0.38 ± 0.03</td><td>0.71 ± 0.21</td><td>...</td><td>...</td></tr><tr><td>J2139+4716</td><td>2.7 ± 0.10</td><td>1.1 ± 0.26</td><td>0.98 ± 0.05</td><td>1.17 ± 0.09</td><td>0.98 ± 0.25</td><td>...</td><td>...</td></tr><tr><td>J2208+4056</td><td>0.46 ± 0.11</td><td>...</td><td>0.32 ± 0.13</td><td>1.72 ± 0.75</td><td>...</td><td>0.32 ± 0.07<sup>+0.30</sup><sub>-0.20</sub></td><td>39 ± 9 ± 40</td></tr><tr><td>J2229+6114</td><td>24.0 ± 0.34</td><td>1.5 ± 0.07</td><td>0.74 ± 0.05</td><td>0.29 ± 0.01</td><td>0.31 ± 0.07</td><td>258.6 ± 3.7<sup>+250</sup><sub>-170</sub></td><td>1.20 ± 0.02 ± 1</td></tr><tr><td>J2238+5903</td><td>6.6 ± 0.24</td><td>1.3 ± 0.23</td><td>0.67 ± 0.09</td><td>0.47 ± 0.04</td><td>0.30 ± 0.17</td><td>...</td><td>...</td></tr><tr><td>J2240+5832</td><td>0.98 ± 0.16</td><td>...</td><td>1.14 ± 0.47</td><td>0.57 ± 0.17</td><td>...</td><td>62.2 ± 9.9<sup>+60</sup><sub>-40</sub></td><td>28 ± 4 ± 30</td></tr></tbody></table>

Notes. Unbinned maximum likelihood spectral fit results for the young LAT gamma-ray pulsars, using the PLEC4 model (Equation (15) in Section 6). Column 2 lists the phase-averaged integral energy flux in the 0.1–300 GeV energy band, $G_{100}$. Column 3 lists $\Gamma_{100}$, the photon index at 100 MeV (Equation (23)), reliable only for fits where the $b$ parameter is left free, and not shown when fixed to $b = 2/3$. Columns 4 and 5 list the energy $E_p$ of the maximum of the SED (Equation (21)), and the SED curvature $d_p$ at the maximum (Equation (22)). Column 6 lists the fitted value of $b$ for pulsars with $TS > 1000$ (fixed to $b = 2/3$ otherwise). Tabulated values are from the $b$-free fit when available, and the $b = 2/3$ fit otherwise. Columns 7 and 8 give the total gamma-ray luminosity $L_\gamma$ in the 0.1–100 GeV energy band, and the gamma-ray conversion efficiency $\eta \equiv L_\gamma/\dot{E}$, assuming $f_\Omega = 1$ as described in Section 6.7. The first uncertainties in $L_\gamma$ and $\eta$ come from the statistical uncertainties in the spectral fit, whereas the second are due to the distance uncertainty. The strong dependence of these quantities on distance (see Table 7) and beaming factor means that these values should be considered with care.

<sup>a</sup> A dagger (†) means the point source has $TS < 25$; hence, we show no spectral fit results. A star (⋆) means that the SED slope decreases over the full LAT energy range; hence, $E_p$ is undefined. PSR J1513−5908 (‡ symbol): the pulsar wind nebula (PWN) MSH 15−52 dominates the colocated 4FGL-DR3 source. We use the on-pulse integral energy flux measurement of Kuiper & Hermsen (2015).

<sup>b</sup> Overestimated distances or the assumed beaming factor, $f_\Omega = 1$, can result in an efficiency > 100%.

the field line curvature radius $\rho$ with $E_c \propto \gamma_c^3/\rho$ for curvature radiation within the light cylinder (Romani 1996). Farther out, for example in current sheets, the curvature of the particle trajectory may be quite different. Other emission mechanisms, such as inverse Compton, can also produce peaked spectra. In general, pulsars accelerate particles to a range of energies, and the observed spectrum is a broader superposition of such basic SED shapes. A main goal of gamma-ray spectroscopy is to invert this superposition and reveal properties of the underlying particle energy distribution. In a curvature radiation scenario, e.g., the observed $E_p$ will roughly track the bulk maximum values of $E_c$, while the

width of the peak and the low-energy spectrum ($E \ll E_p$) encode information about the range of $E_c$. A nearly monoenergetic distribution of $E_c$ will produce a narrow SED peak and a low-energy $S(E) \propto E^{4/3}$, while a broad range of $E_c$ will produce a broad gamma-ray peak and $\Gamma_0$ of $\sim 1-2$ (Romani 1996).

Most previous analyses of LAT pulsar spectra have used the PLEC model:

$$ \frac{dN}{dE} \equiv N(E) = N_0 \left(\frac{E}{E_0}\right)^{-\Gamma_0} \exp \left[ - \left(\frac{E}{E_c}\right)^b \right], \quad (14) $$
<table><caption>**Table 13**
(Continued)</caption><thead><tr><th>PSR<sup>a</sup></th><th>Energy Flux<br>(erg cm<sup>-2</sup> s<sup>-1</sup>)<br>(×10<sup>-11</sup>)</th><th>Γ<sub>100</sub></th><th>E<sub>p</sub><br>(GeV)</th><th>d<sub>p</sub></th><th>b<sub>free</sub></th><th>Luminosity<br>(10<sup>33</sup> erg s<sup>-1</sup>)</th><th>Efficiency<sup>b</sup><br>(%)</th></tr></thead><tbody><tr><td>J1906+0722</td><td>8.6 ± 0.80</td><td>...</td><td>0.58 ± 0.22</td><td>0.63 ± 0.09</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1907+0602</td><td>30.0 ± 0.76</td><td>1.2 ± 0.16</td><td>0.95 ± 0.06</td><td>0.48 ± 0.02</td><td>0.27 ± 0.10</td><td>235.8 ± 6.1<sup>+230</sup><sub>-150</sub></td><td>8.4 ± 0.2 ± 8</td></tr><tr><td>J1913+0904</td><td>2.0 ± 0.34</td><td>...</td><td>1.69 ± 0.35</td><td>1.19 ± 0.29</td><td>...</td><td>21.2 ± 3.7<sup>+20</sup><sub>-14</sub></td><td>13 ± 2 ± 10</td></tr><tr><td>J1913+1011</td><td>1.8 ± 0.31</td><td>...</td><td>1.65 ± 5.21</td><td>0.13 ± 0.09</td><td>...</td><td>46.6 ± 8.0<sup>+45</sup><sub>-30</sub></td><td>1.6 ± 0.3 ± 2</td></tr><tr><td>J1925+1720</td><td>0.95 ± 0.27</td><td>...</td><td>1.18 ± 0.40</td><td>1.24 ± 0.48</td><td>...</td><td>29.0 ± 8.2<sup>+28</sup><sub>-19</sub></td><td>3.0 ± 0.9 ± 3</td></tr><tr><td>J1928+1746 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1932+1916</td><td>6.5 ± 0.45</td><td>1.2 ± 0.40</td><td>0.72 ± 0.13</td><td>0.77 ± 0.08</td><td>0.41 ± 0.25</td><td>...</td><td>...</td></tr><tr><td>J1932+2220</td><td>0.52 ± 0.15</td><td>...</td><td>1.06 ± 0.53</td><td>0.75 ± 0.33</td><td>...</td><td>73 ± 21<sup>+19</sup><sub>-10</sub></td><td>10 ± 3<sup>+2</sup><sub>-1</sub></td></tr><tr><td>J1935+2025</td><td>2.2 ± 0.31</td><td>...</td><td>0.55 ± 0.18</td><td>0.99 ± 0.26</td><td>...</td><td>54.9 ± 7.8<sup>+53</sup><sub>-35</sub></td><td>1.2 ± 0.2 ± 1</td></tr><tr><td>J1952+3252</td><td>15.0 ± 0.28</td><td>1.3 ± 0.12</td><td>0.99 ± 0.05</td><td>0.42 ± 0.02</td><td>0.34 ± 0.10</td><td>159.0 ± 3.0<sup>+280</sup><sub>-140</sub></td><td>4.27 ± 0.08<sup>+8</sup><sub>-4</sub></td></tr><tr><td>J1954+2836</td><td>11.0 ± 0.32</td><td>1.1 ± 0.28</td><td>1.17 ± 0.09</td><td>0.45 ± 0.03</td><td>0.27 ± 0.15</td><td>...</td><td>...</td></tr><tr><td>J1954+3852 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1957+5033</td><td>2.6 ± 0.08</td><td>0.50 ± 0.40</td><td>0.76 ± 0.03</td><td>1.03 ± 0.07</td><td>0.43 ± 0.20</td><td>...</td><td>...</td></tr><tr><td>J1958+2846</td><td>11.0 ± 0.29</td><td>0.72 ± 0.31</td><td>1.15 ± 0.06</td><td>0.60 ± 0.04</td><td>0.21 ± 0.13</td><td>...</td><td>...</td></tr><tr><td>J2006+3102</td><td>1.1 ± 0.15</td><td>...</td><td>1.47 ± 0.36</td><td>0.79 ± 0.21</td><td>...</td><td>46.3 ± 6.6<sup>+44</sup><sub>-30</sub></td><td>21 ± 3 ± 20</td></tr><tr><td>J2017+3625</td><td>7.5 ± 0.46</td><td>1.4 ± 0.30</td><td>0.95 ± 0.10</td><td>0.92 ± 0.09</td><td>0.74 ± 0.25</td><td>...</td><td>...</td></tr><tr><td>J2021+3651</td><td>49.0 ± 0.79</td><td>0.99 ± 0.10</td><td>1.06 ± 0.03</td><td>0.50 ± 0.01</td><td>0.25 ± 0.06</td><td>190.8 ± 3.0<sup>+530</sup><sub>-180</sub></td><td>5.69 ± 0.09<sup>+20</sup><sub>-5</sub></td></tr><tr><td>J2021+4026</td><td>80.0 ± 1.1</td><td>1.1 ± 0.07</td><td>0.87 ± 0.02</td><td>0.92 ± 0.02</td><td>0.39 ± 0.05</td><td>215.6 ± 2.9 ± 110</td><td>183 ± 2 ± 100</td></tr><tr><td>J2022+3842</td><td>2.7 ± 0.42</td><td>...</td><td>0.20 ± 0.22</td><td>0.61 ± 0.15</td><td>...</td><td>317 ± 50<sup>+300</sup><sub>-110</sub></td><td>1.1 ± 0.2<sup>+1</sup><sub>-0.4</sub></td></tr><tr><td>J2028+3332</td><td>5.7 ± 0.19</td><td>-0.33 ± 0.60</td><td>1.51 ± 0.06</td><td>1.08 ± 0.07</td><td>0.22 ± 0.17</td><td>...</td><td>...</td></tr><tr><td>J2030+3641</td><td>4.2 ± 0.17</td><td>0.55 ± 0.49</td><td>1.87 ± 0.08</td><td>1.03 ± 0.09</td><td>0.63 ± 0.25</td><td>45.5 ± 1.9 ± 25</td><td>142 ± 6 ± 100</td></tr><tr><td>J2030+4415</td><td>4.4 ± 0.22</td><td>0.48 ± 0.57</td><td>1.20 ± 0.07</td><td>1.20 ± 0.11</td><td>0.51 ± 0.27</td><td>1.32 ± 0.06<sup>+2.1</sup><sub>-0.85</sub></td><td>7.8 ± 0.4<sup>+10</sup><sub>-5</sub></td></tr><tr><td>J2032+4127</td><td>14.0 ± 0.47</td><td>1.0 ± 0.21</td><td>2.61 ± 0.10</td><td>0.56 ± 0.03</td><td>0.55 ± 0.14</td><td>52.8 ± 1.7 ± 3.0</td><td>34 ± 1 ± 2</td></tr><tr><td>J2043+2740</td><td>0.9 ± 0.07</td><td>...</td><td>0.83 ± 0.10</td><td>1.06 ± 0.18</td><td>...</td><td>2.37 ± 0.18<sup>+2.3</sup><sub>-1.5</sub></td><td>4.3 ± 0.3 ± 4</td></tr><tr><td>J2055+2539</td><td>5.3 ± 0.10</td><td>0.69 ± 0.17</td><td>1.21 ± 0.03</td><td>0.89 ± 0.04</td><td>0.65 ± 0.12</td><td>...</td><td>...</td></tr><tr><td>J2111+4606</td><td>4.9 ± 0.15</td><td>1.6 ± 0.15</td><td>1.33 ± 0.12</td><td>0.38 ± 0.03</td><td>0.71 ± 0.21</td><td>...</td><td>...</td></tr><tr><td>J2139+4716</td><td>2.7 ± 0.10</td><td>1.1 ± 0.26</td><td>0.98 ± 0.05</td><td>1.17 ± 0.09</td><td>0.98 ± 0.25</td><td>...</td><td>...</td></tr><tr><td>J2208+4056</td><td>0.46 ± 0.11</td><td>...</td><td>0.32 ± 0.13</td><td>1.72 ± 0.75</td><td>...</td><td>0.32 ± 0.07<sup>+0.30</sup><sub>-0.20</sub></td><td>39 ± 9 ± 40</td></tr><tr><td>J2229+6114</td><td>24.0 ± 0.34</td><td>1.5 ± 0.07</td><td>0.74 ± 0.05</td><td>0.29 ± 0.01</td><td>0.31 ± 0.07</td><td>258.6 ± 3.7<sup>+250</sup><sub>-170</sub></td><td>1.20 ± 0.02 ± 1</td></tr><tr><td>J2238+5903</td><td>6.6 ± 0.24</td><td>1.3 ± 0.23</td><td>0.67 ± 0.09</td><td>0.47 ± 0.04</td><td>0.30 ± 0.17</td><td>...</td><td>...</td></tr><tr><td>J2240+5832</td><td>0.98 ± 0.16</td><td>...</td><td>1.14 ± 0.47</td><td>0.57 ± 0.17</td><td>...</td><td>62.2 ± 9.9<sup>+60</sup><sub>-40</sub></td><td>28 ± 4 ± 30</td></tr></tbody></table>

**Notes.** Unbinned maximum likelihood spectral fit results for the young LAT gamma-ray pulsars, using the PLEC4 model (Equation (15) in Section 6). Column 2 lists the phase-averaged integral energy flux in the 0.1–300 GeV energy band, $G_{100}$. Column 3 lists $\Gamma_{100}$, the photon index at 100 MeV (Equation (23)), reliable only for fits where the $b$ parameter is left free, and not shown when fixed to $b = 2/3$. Columns 4 and 5 list the energy $E_p$ of the maximum of the SED (Equation (21)), and the SED curvature $d_p$ at the maximum (Equation (22)). Column 6 lists the fitted value of $b$ for pulsars with TS > 1000 (fixed to $b = 2/3$ otherwise). Tabulated values are from the $b$-free fit when available, and the $b = 2/3$ fit otherwise. Columns 7 and 8 give the total gamma-ray luminosity $L_\gamma$ in the 0.1–100 GeV energy band, and the gamma-ray conversion efficiency $\eta \equiv L_\gamma/\dot{E}$, assuming $f_\Omega = 1$ as described in Section 6.7. The first uncertainties in $L_\gamma$ and $\eta$ come from the statistical uncertainties in the spectral fit, whereas the second are due to the distance uncertainty. The strong dependence of these quantities on distance (see Table 7) and beaming factor means that these values should be considered with care.

<sup>a</sup> A dagger (†) means the point source has TS < 25; hence, we show no spectral fit results. A star (⋆) means that the SED slope decreases over the full LAT energy range; hence, $E_p$ is undefined. PSR J1513−5908 (‡ symbol): the pulsar wind nebula (PWN) MSH 15−52 dominates the colocated 4FGL-DR3 source. We use the on-pulse integral energy flux measurement of Kuiper & Hermsen (2015).

<sup>b</sup> Overestimated distances or the assumed beaming factor, $f_\Omega = 1$, can result in an efficiency > 100%.

the field line curvature radius $\rho$ with $E_c \propto \gamma_c^3/\rho$ for curvature radiation within the light cylinder (Romani 1996). Farther out, for example in current sheets, the curvature of the particle trajectory may be quite different. Other emission mechanisms, such as inverse Compton, can also produce peaked spectra. In general, pulsars accelerate particles to a range of energies, and the observed spectrum is a broader superposition of such basic SED shapes. A main goal of gamma-ray spectroscopy is to invert this superposition and reveal properties of the underlying particle energy distribution. In a curvature radiation scenario, e.g., the observed $E_p$ will roughly track the bulk maximum values of $E_c$, while the

width of the peak and the low-energy spectrum ($E \ll E_p$) encode information about the range of $E_c$. A nearly monoenergetic distribution of $E_c$ will produce a narrow SED peak and a low-energy $S(E) \propto E^{4/3}$, while a broad range of $E_c$ will produce a broad gamma-ray peak and $\Gamma_0$ of ~1–2 (Romani 1996).

Most previous analyses of LAT pulsar spectra have used the PLEC model:

$$ \frac{dN}{dE} \equiv N(E) = N_0 \left(\frac{E}{E_0}\right)^{-\Gamma_0} \exp \left[ - \left(\frac{E}{E_c}\right)^b \right], \quad (14) $$
<table><caption>Table 14
Spectral Fitting Results for LAT-detected Millisecond Pulsars</caption><thead><tr><th>PSR<sup>a</sup></th><th>Energy Flux<br>(erg cm<sup>-2</sup> s<sup>-1</sup>)<br>(×10<sup>-12</sup>)</th><th>Γ<sub>100</sub></th><th>E<sub>p</sub><br>(GeV)</th><th>d<sub>p</sub></th><th>b<sub>free</sub></th><th>Luminosity<br>(10<sup>33</sup> erg s<sup>-1</sup>)</th><th>Efficiency<sup>b</sup><br>(%)</th></tr></thead><tbody><tr><td>J0023+0923</td><td>7.8 ± 0.6</td><td>...</td><td>1.28 ± 0.15</td><td>0.54 ± 0.11</td><td>...</td><td>3.03 ± 0.21<sup>+2.0</sup><sub>-1.00</sub></td><td>19 ± 1<sup>+10</sup><sub>-6</sub></td></tr><tr><td>J0030+0451</td><td>60.0 ± 1.1</td><td>0.88 ± 0.15</td><td>1.42 ± 0.03</td><td>0.58 ± 0.03</td><td>0.53 ± 0.11</td><td>0.743 ± 0.013 ± 0.026</td><td>21.3 ± 0.4 ± 0.8</td></tr><tr><td>J0034-0534</td><td>20.0 ± 0.6</td><td>1.5 ± 0.16</td><td>0.99 ± 0.09</td><td>0.32 ± 0.03</td><td>0.65 ± 0.23</td><td>4.38 ± 0.14<sup>+4.2</sup><sub>-2.8</sub></td><td>14.7 ± 0.5 ± 10</td></tr><tr><td>J0101-6422</td><td>13.0 ± 0.4</td><td>0.87 ± 0.31</td><td>1.34 ± 0.07</td><td>0.53 ± 0.05</td><td>0.43 ± 0.20</td><td>1.562 ± 0.053<sup>+1.5</sup><sub>-1.00</sub></td><td>13.3 ± 0.4 ± 10</td></tr><tr><td>J0102+4839</td><td>15.0 ± 0.7</td><td>1.2 ± 0.33</td><td>1.70 ± 0.17</td><td>0.41 ± 0.05</td><td>0.48 ± 0.25</td><td>9.59 ± 0.48<sup>+9.2</sup><sub>-6.1</sub></td><td>55 ± 3 ± 50</td></tr><tr><td>J0154+1833 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J0218+4232</td><td>48.0 ± 1.2</td><td>1.9 ± 0.07</td><td>0.33 ± 0.08</td><td>0.26 ± 0.02</td><td>0.76 ± 0.17</td><td>57.4 ± 1.4<sup>+35</sup><sub>-20</sub></td><td>23.5 ± 0.6<sup>+10</sup><sub>-8</sub></td></tr><tr><td>J0248+4230</td><td>1.9 ± 0.3</td><td>...</td><td>1.80 ± 0.26</td><td>1.39 ± 0.41</td><td>...</td><td>0.79 ± 0.11<sup>+0.76</sup><sub>-0.51</sub></td><td>2.1 ± 0.3 ± 2</td></tr><tr><td>J0251+2606</td><td>4.9 ± 0.4</td><td>...</td><td>1.57 ± 0.18</td><td>0.78 ± 0.17</td><td>...</td><td>0.799 ± 0.070<sup>+0.77</sup><sub>-0.51</sub></td><td>4.4 ± 0.4 ± 4</td></tr><tr><td>J0307+7443</td><td>16.0 ± 0.6</td><td>1.2 ± 0.22</td><td>1.63 ± 0.07</td><td>0.99 ± 0.08</td><td>1.12 ± 0.28</td><td>0.293 ± 0.011<sup>+0.28</sup><sub>-0.19</sub></td><td>1.35 ± 0.05 ± 1</td></tr><tr><td>J0312-0921</td><td>5.5 ± 0.4</td><td>...</td><td>1.53 ± 0.13</td><td>0.95 ± 0.18</td><td>...</td><td>0.443 ± 0.034<sup>+0.43</sup><sub>-0.28</sub></td><td>2.9 ± 0.2 ± 3</td></tr><tr><td>J0318+0253</td><td>6.3 ± 0.5</td><td>...</td><td>1.89 ± 0.18</td><td>0.89 ± 0.16</td><td>...</td><td>1.33 ± 0.10<sup>+1.3</sup><sub>-0.85</sub></td><td>27 ± 2 ± 30</td></tr><tr><td>J0340+4130</td><td>19.0 ± 0.7</td><td>0.76 ± 0.35</td><td>2.91 ± 0.14</td><td>0.56 ± 0.05</td><td>0.55 ± 0.23</td><td>5.94 ± 0.22<sup>+5.7</sup><sub>-3.8</sub></td><td>77 ± 3 ± 70</td></tr><tr><td>J0418+6635</td><td>10.0 ± 0.7</td><td>1.3 ± 0.41</td><td>1.80 ± 0.23</td><td>0.42 ± 0.07</td><td>0.55 ± 0.34</td><td>6.02 ± 0.40<sup>+5.8</sup><sub>-3.9</sub></td><td>28 ± 2 ± 30</td></tr><tr><td>J0437-4715</td><td>18.0 ± 0.5</td><td>1.6 ± 0.11</td><td>0.70 ± 0.03</td><td>0.74 ± 0.06</td><td>1.37 ± 0.24</td><td>0.052 ± 0.001 ± 0.006</td><td>0.44 ± 0.01 ± 0.06</td></tr><tr><td>J0533+6759</td><td>9.3 ± 0.5</td><td>1.2 ± 0.27</td><td>2.29 ± 0.17</td><td>0.53 ± 0.07</td><td>0.80 ± 0.30</td><td>6.38 ± 0.32<sup>+6.1</sup><sub>-4.1</sub></td><td>108 ± 5 ± 100</td></tr><tr><td>J0605+3757</td><td>6.4 ± 0.5</td><td>...</td><td>1.95 ± 0.13</td><td>1.39 ± 0.23</td><td>...</td><td>0.036 ± 0.003<sup>+0.034</sup><sub>-0.023</sub></td><td>0.39 ± 0.03 ± 0.4</td></tr><tr><td>J0610-2100</td><td>7.2 ± 0.5</td><td>...</td><td>1.34 ± 0.12</td><td>0.79 ± 0.12</td><td>...</td><td>4.19 ± 0.27 ± 2.2</td><td>50 ± 3 ± 40</td></tr><tr><td>J0613-0200</td><td>38.0 ± 1.1</td><td>1.6 ± 0.16</td><td>1.16 ± 0.07</td><td>0.43 ± 0.03</td><td>0.93 ± 0.27</td><td>2.777 ± 0.078 ± 0.51</td><td>21.1 ± 0.6 ± 4</td></tr><tr><td>J0614-3329</td><td>110.0 ± 1.4</td><td>0.86 ± 0.09</td><td>2.84 ± 0.06</td><td>0.33 ± 0.01</td><td>0.37 ± 0.07</td><td>5.443 ± 0.069 ± 1.6</td><td>24.7 ± 0.3 ± 8</td></tr><tr><td>J0621+2514</td><td>4.1 ± 0.4</td><td>...</td><td>2.69 ± 0.24</td><td>1.83 ± 0.42</td><td>...</td><td>1.31 ± 0.14<sup>+1.3</sup><sub>-0.84</sub></td><td>2.7 ± 0.3 ± 3</td></tr><tr><td>J0636+5128 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J0653+4706</td><td>2.0 ± 0.3</td><td>...</td><td>1.24 ± 0.15</td><td>1.82 ± 0.58</td><td>...</td><td>0.195 ± 0.029<sup>+0.19</sup><sub>-0.12</sub></td><td>2.6 ± 0.4 ± 2</td></tr><tr><td>J0737-3039A †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J0740+6620</td><td>2.8 ± 0.3</td><td>...</td><td>1.88 ± 0.29</td><td>0.59 ± 0.17</td><td>...</td><td>0.448 ± 0.051 ± 0.12</td><td>2.2 ± 0.3 ± 0.7</td></tr><tr><td>J0751+1807</td><td>10.0 ± 0.5</td><td>0.07 ± 1.2</td><td>2.31 ± 0.12</td><td>1.22 ± 0.15</td><td>0.50 ± 0.53</td><td>1.483 ± 0.081 ± 0.49</td><td>20 ± 1 ± 8</td></tr><tr><td>J0931-1902</td><td>1.4 ± 0.2</td><td>...</td><td>1.89 ± 0.19</td><td>2.89 ± 1.16</td><td>...</td><td>2.39 ± 0.35<sup>+2.3</sup><sub>-1.5</sub></td><td>170 ± 20 ± 200</td></tr><tr><td>J0952-0607</td><td>2.4 ± 0.3</td><td>...</td><td>1.83 ± 0.23</td><td>1.29 ± 0.38</td><td>...</td><td>11.0 ± 1.5 ± 1.4</td><td>17 ± 2 ± 2</td></tr><tr><td>J0955-6150</td><td>7.7 ± 0.8</td><td>...</td><td>0.84 ± 0.28</td><td>0.49 ± 0.13</td><td>...</td><td>4.36 ± 0.45<sup>+4.2</sup><sub>-2.8</sub></td><td>6.2 ± 0.6 ± 6</td></tr><tr><td>J1012-4235</td><td>5.6 ± 0.5</td><td>...</td><td>1.30 ± 0.40</td><td>0.40 ± 0.11</td><td>...</td><td>0.093 ± 0.009<sup>+0.089</sup><sub>-0.060</sub></td><td>1.1 ± 0.1 ± 1</td></tr><tr><td>J1024-0719</td><td>4.3 ± 0.4</td><td>...</td><td>1.66 ± 0.24</td><td>0.65 ± 0.16</td><td>...</td><td>0.767 ± 0.075 ± 0.19</td><td>14 ± 1 ± 4</td></tr><tr><td>J1035-6720</td><td>19.0 ± 0.7</td><td>0.55 ± 0.44</td><td>1.65 ± 0.08</td><td>0.87 ± 0.08</td><td>0.46 ± 0.22</td><td>4.81 ± 0.19<sup>+4.6</sup><sub>-3.1</sub></td><td>6.2 ± 0.2 ± 6</td></tr><tr><td>J1036-8317</td><td>4.1 ± 0.4</td><td>...</td><td>2.15 ± 0.25</td><td>0.80 ± 0.19</td><td>...</td><td>2.29 ± 0.23<sup>+1.6</sup><sub>-0.54</sub></td><td>7.5 ± 0.7<sup>+5.2</sup><sub>-2</sub></td></tr><tr><td>J1048+2339</td><td>4.9 ± 0.5</td><td>...</td><td>0.89 ± 0.33</td><td>0.31 ± 0.09</td><td>...</td><td>1.021 ± 0.096<sup>+1.0</sup><sub>-0.32</sub></td><td>8.7 ± 0.8<sup>+9.3</sup><sub>-3</sub></td></tr><tr><td>J1124-3653</td><td>12.0 ± 0.6</td><td>1.4 ± 0.08</td><td>1.96 ± 0.15</td><td>0.51 ± 0.07</td><td>1.01 ± 0.17</td><td>1.465 ± 0.071<sup>+1.4</sup><sub>-0.94</sub></td><td>8.6 ± 0.4 ± 8</td></tr><tr><td>J1125-5825</td><td>6.5 ± 0.7</td><td>...</td><td>3.02 ± 0.36</td><td>0.93 ± 0.21</td><td>...</td><td>2.35 ± 0.24<sup>+2.3</sup><sub>-1.5</sub></td><td>2.9 ± 0.3 ± 3</td></tr><tr><td>J1125-6014</td><td>3.1 ± 0.9</td><td>...</td><td>1.87 ± 0.51</td><td>1.52 ± 0.69</td><td>...</td><td>0.361 ± 0.099<sup>+0.35</sup><sub>-0.23</sub></td><td>4 ± 1 ± 4</td></tr><tr><td>J1137+7528</td><td>0.6 ± 0.1</td><td>...</td><td>3.20 ± 0.64</td><td>1.72 ± 0.78</td><td>...</td><td>1.06 ± 0.24<sup>+1.0</sup><sub>-0.68</sub></td><td>13 ± 3 ± 10</td></tr><tr><td>J1142+0119</td><td>6.4 ± 0.5</td><td>...</td><td>2.86 ± 0.30</td><td>0.46 ± 0.11</td><td>...</td><td>3.63 ± 0.28<sup>+3.5</sup><sub>-2.5</sub></td><td>80 ± 6 ± 80</td></tr><tr><td>J1207-5050</td><td>4.8 ± 0.5</td><td>...</td><td>1.75 ± 0.20</td><td>1.26 ± 0.28</td><td>...</td><td>0.920 ± 0.099<sup>+0.88</sup><sub>-0.59</sub></td><td>43 ± 5 ± 40</td></tr><tr><td>J1221-0633</td><td>5.8 ± 0.5</td><td>...</td><td>1.48 ± 0.22</td><td>0.48 ± 0.11</td><td>...</td><td>1.090 ± 0.092<sup>+1.0</sup><sub>-0.70</sub></td><td>1.8 ± 0.2 ± 2</td></tr><tr><td>J1227-4853</td><td>19.0 ± 1.6</td><td>1.7 ± 0.45</td><td>0.66 ± 0.35</td><td>0.34 ± 0.07</td><td>0.59 ± 0.53</td><td>6.98 ± 0.60<sup>+4.5</sup><sub>-1.5</sub></td><td>6.4 ± 0.5<sup>+1.4</sup><sub>-1</sub></td></tr><tr><td>J1231-1411</td><td>100.0 ± 1.3</td><td>0.69 ± 0.11</td><td>2.02 ± 0.03</td><td>0.57 ± 0.02</td><td>0.53 ± 0.08</td><td>2.133 ± 0.027 ± 0.89</td><td>11.9 ± 0.2 ± 6</td></tr><tr><td>J1301+0833</td><td>7.7 ± 0.5</td><td>...</td><td>1.30 ± 0.13</td><td>0.59 ± 0.10</td><td>...</td><td>2.88 ± 0.18 ± 0.35</td><td>4.3 ± 0.3 ± 0.5</td></tr><tr><td>J1302-3258</td><td>11.0 ± 0.5</td><td>0.78 ± 0.43</td><td>2.54 ± 0.14</td><td>0.84 ± 0.10</td><td>0.86 ± 0.36</td><td>2.67 ± 0.13<sup>+2.6</sup><sub>-1.7</sub></td><td>55 ± 3 ± 50</td></tr><tr><td>J1311-3430</td><td>61.0 ± 1.2</td><td>1.6 ± 0.10</td><td>0.85 ± 0.07</td><td>0.24 ± 0.02</td><td>0.54 ± 0.15</td><td>18.11 ± 0.37<sup>+29</sup><sub>-7.1</sub></td><td>37.0 ± 0.7<sup>+60</sup><sub>-10</sub></td></tr><tr><td>J1312+0051</td><td>15.0 ± 0.7</td><td>1.1 ± 0.27</td><td>1.46 ± 0.08</td><td>0.84 ± 0.09</td><td>0.90 ± 0.30</td><td>3.78 ± 0.17<sup>+3.6</sup><sub>-2.4</sub></td><td>41 ± 2 ± 40</td></tr><tr><td>J1327-0755 †</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1335-5656</td><td>8.2 ± 0.9</td><td>...</td><td>2.09 ± 0.35</td><td>0.52 ± 0.12</td><td>...</td><td>...</td><td>...</td></tr><tr><td>J1400-1431</td><td>6.4 ± 0.5</td><td>...</td><td>1.43 ± 0.14</td><td>0.74 ± 0.13</td><td>...</td><td>0.059 ± 0.004<sup>+0.064</sup><sub>-0.025</sub></td><td>0.61 ± 0.05<sup>+0.7</sup><sub>-0.3</sub></td></tr><tr><td>J1431-4715</td><td>4.7 ± 0.7</td><td>...</td><td>0.44 ± 0.24</td><td>0.80 ± 0.30</td><td>...</td><td>1.74 ± 0.26<sup>+1.2</sup><sub>-0.39</sub></td><td>2.5 ± 0.4<sup>+2</sup><sub>-0.6</sub></td></tr><tr><td>J1446-4701</td><td>7.7 ± 0.7</td><td>...</td><td>1.38 ± 0.29</td><td>0.47 ± 0.11</td><td>...</td><td>2.26 ± 0.20<sup>+2.2</sup><sub>-1.4</sub></td><td>6.2 ± 0.6 ± 6</td></tr><tr><td>J1455-3330</td><td>1.1 ± 0.3</td><td>...</td><td>1.47 ± 0.38</td><td>1.34 ± 0.66</td><td>...</td><td>0.064 ± 0.016<sup>+0.061</sup><sub>-0.041</sub></td><td>3.4 ± 0.9 ± 3</td></tr><tr><td>J1513-2550</td><td>7.6 ± 0.6</td><td>...</td><td>1.05 ± 0.20</td><td>0.55 ± 0.12</td><td>...</td><td>14.3 ± 1.2<sup>+1.4</sup><sub>-9.1</sub></td><td>16 ± 1 ± 20</td></tr><tr><td>J1514-4946</td><td>42.0 ± 1.2</td><td>1.3 ± 0.16</td><td>2.55 ± 0.11</td><td>0.47 ± 0.04</td><td>0.84 ± 0.19</td><td>4.13 ± 0.12<sup>+4.0</sup><sub>-2.6</sub></td><td>25.9 ± 0.7 ± 20</td></tr><tr><td>J1536-4948</td><td>80.0 ± 1.9</td><td>1.4 ± 0.12</td><td>2.14 ± 0.11</td><td>0.29 ± 0.02</td><td>0.56 ± 0.14</td><td>9.14 ± 0.21<sup>+8.8</sup><sub>-5.8</sub></td><td>31.9 ± 0.7 ± 30</td></tr><tr><td>J1543-5149</td><td>18.0 ± 2.2</td><td>...</td><td>0.64 ± 0.29</td><td>0.58 ± 0.13</td><td>...</td><td>2.78 ± 0.35<sup>+2.7</sup><sub>-1.8</sub></td><td>3.8 ± 0.5 ± 4</td></tr><tr><td>J1544+4937</td><td>2.4 ± 0.3</td><td>...</td><td>2.16 ± 0.39</td><td>0.45 ± 0.14</td><td>...</td><td>2.53 ± 0.31<sup>+4.5</sup><sub>-1.4</sub></td><td>23 ± 3<sup>+40</sup><sub>-10</sub></td></tr></tbody></table>