PSR J0007+7303 is a radio-quiet pulsar / 2004: #apjab14f4bib34) associated with the supernova remnant CTA 1, which is detected in VHE gamma-rays above 500 GeV  Aliu et al / a: #apjab14f4bib17). It is bright at GeV energies and has the second-highest spectral cutoff energy (4.7 GeV) among all young gamma-ray pulsars in the 2PC  Abdo et al / : #apjab14f4bib4). Above the spectral cutoff energy, its HE gamma-ray spectrum is consistent with a subexponential cutoff (Li et al., 2016: #apjab14f4bib45)

PSR J0205+6449 is associated with 3C 58, which is a PWN detected at energies above 400 GeV / 2014: #apjab14f4bib14). It has the third-highest \dot{E} of any gamma-ray pulsar in the 2PC  Abdo et al / : #apjab14f4bib4)

PSR J0357+3205 is the second slowest-rotating gamma-ray pulsar known (see footnote 26) and also one of the nearest known pulsars, at a distance of ~0.5 kpc / 2013: #apjab14f4bib51). It is notable for having a very long X-ray emission tail that extends 9' behind the pulsar (De Luca et al / 2011: #apjab14f4bib29). Its estimated runaway velocity of 1900 km s-1 makes it one of the highest-velocity pulsars known  Manchester et al / : #apjab14f4bib50)

PSR J2021+4026 is a radio-quiet gamma-ray pulsar / 2009: #apjab14f4bib2) located within the radio shell of the supernova remnant G78.2+2.1 (Ladouceur & Pineault, 2008: #apjab14f4bib42). The remnant has also been detected as an extended source in the VHE band by VERITAS  Aliu et al / b: #apjab14f4bib18). The flux above 100 MeV from the pulsar was seen to abruptly decrease by ~20% within less than one week, which coincided with a decrease in the pulsar period time derivative, \dot{P}. After spending about three years in this low-flux, low \dot{P} state, the HE flux and \dot{P} gradually returned to their previous values over the course of a few months Zhao et al / 2017: #apjab14f4bib66). This is currently the only such observation of intermittent behavior (also called mode switching) seen for a pulsar at gamma-ray energies  Allafort et al / : #apjab14f4bib21). The sudden change in HE flux and \dot{P} may be due to a change in the emission beaming from a shift in the magnetic field structure  Allafort et al / : #apjab14f4bib21)

PSR J2032+4127 is a pulsar that was thought to be isolated but was recently found to be in a long-period (P = 45-50 yr Ho et al., 2017: #apjab14f4bib37) binary system / 2015: #apjab14f4bib48), orbiting a 15 M⊙ Be star  Hohle et al / 2010: #apjab14f4bib39) companion. The pulsar is spatially coincident with the extended VHE gamma-ray source TeV J2032+4130, which would generally be interpreted as a PWN powered by the pulsar  Albert et al / : #apjab14f4bib12

: #apjab14f4bib20). In recent observations conducted by VERITAS and MAGIC in fall 2017, both instruments observed a VHE flux elevated by a factor of ~10 over spring/summer 2017 (Mirzoyan & Mukherjee, 2017: #apjab14f4bib53

: #apjab14f4bib5). VERITAS and MAGIC additionally reported a clear detection of a point source at the pulsar location as the system neared periastron, confirming the presence of a gamma-ray binary

Determine the signal and background event rates from VERITAS Crab Nebula data using soft cuts. These event rates are obtained in a reflected-region analysis / : #apjab14f4bib32)

Multiply the rates from step 1 by the source exposure time to get an expected Non and αNoff, then find Nexcess = Non - αNoff, where Nexcess is the number of excess counts, Non is the number of counts in the signal region, Noff is the number in the background region, and α is the ratio of the size of the signal region(s) to the background region

Scale the Crab Nebula excess counts found in step 2 by 0.01 to mimic a 1% Crab Nebula source (the Crab pulsar flux is approximately 1% of the Crab Nebula flux at ~200 GeV)

Obtain the binned pulse profile from the 2PC for the pulsar in question and subtract the value of the lowest bin in the profile from all bins to remove the unpulsed component

Normalize the pulse profile from the previous step and multiply each bin by the scaled excess found in step 3

Add the estimated background expected for the VERITAS observations to the profile by adding αNoff/Nbins to each bin, where Nbins is the total number of bins

Define the number of signal phase gates as one per peak present in the 2PC light curve, and calculate the significance corresponding to all nonoverlapping phase-gate bin combinations—including a background gate. The phase gates selected for the VERITAS analysis are those for which the significance is maximized. As an example, consider a pulsar displaying two HE gamma-ray peaks in its light curve. Two signal phase gates are defined a priori, each with a unique starting and ending edge, which must be located at a bin edge. A background gate is also defined in the same way, and none of these three gates are allowed to overlap. Significances are then calculated for all possible gate combinations by scanning the space of the six possible gate edges. The gate combination with the highest significance is used for the analysis. For cases where two signal phase gates were initially defined but found to be contiguous, the number of gates is reduced to one and the procedure is performed again