Context : Pulsars PSR J0248+6021 ( with a rotation period P = 217 ms and spin-down power \dot { E } = 2.13 \times 10 ^ { 35 } erg s ^ { -1 } ) and PSR J2240+5832 ( P = 140 ms , \dot { E } = 2.12 \times 10 ^ { 35 } erg s ^ { -1 } ) were discovered in 1997 with the Nançay radio telescope during a northern Galactic plane survey , using the Navy-Berkeley Pulsar Processor ( NBPP ) filter bank .
The GeV gamma-ray pulsations from both were discovered using the Fermi Large Area Telescope .

Aims : We characterize the neutron star emission using radio and gamma-ray observations , and explore the rich environment of PSR J0248+6021 .

Methods : Twelve years of radio timing data , including glitches , with steadily improved instrumentation , such as the Berkeley-Orleans-Nançay pulsar backend , and a gamma-ray data set 2.6 times larger than previously published allow detailed investigations of these pulsars .
Radio polarization data allow comparison with the geometry inferred from gamma-ray emission models .

Results : The two pulsars resemble each other in both radio and gamma-ray data .
Both are rare in having a single gamma-ray pulse offset far from the radio peak .
The anomalously high dispersion measure for PSR J0248+6021 ( DM = 370 pc cm ^ { -3 } ) is most likely due to its being within the dense , giant HII region W5 in the Perseus arm at a distance of 2 kpc , as opposed to being beyond the edge of the Galaxy as obtained from models of average electron distributions .
Its large transverse velocity and the low magnetic field along the line-of-sight favor this small distance .
Neither gamma-ray , X-ray , nor optical data yield evidence of a pulsar wind nebula surrounding PSR J0248+6021 .
We report the discovery of gamma-ray pulsations from PSR J2240+5832 .
We argue that it could be in the outer arm , although slightly nearer than its DM-derived distance , but that it may be in the Perseus arm at half the distance .

Conclusions : The energy flux and distance yield a gamma-ray luminosity for PSR J0248+6021 of L _ { \gamma } = ( 1.4 \pm 0.3 ) \times 10 ^ { 34 } erg s ^ { -1 } .
For PSR J2240+5832 , we find either L _ { \gamma } = ( 7.9 \pm 5.2 ) \times 10 ^ { 34 } erg s ^ { -1 } if the pulsar is in the outer arm , or L _ { \gamma } = ( 2.2 \pm 1.7 ) \times 10 ^ { 34 } erg s ^ { -1 } for the Perseus arm .
These luminosities are consistent with an L _ { \gamma } \propto \sqrt { \dot { E } } rule .
Comparison of the gamma-ray pulse profiles with model predictions , including the constraints obtained from radio polarization data , implies outer magnetosphere emission .
These two pulsars differ mainly by their inclination angles and acceleration gap widths , which in turn explain the observed differences in the gamma-ray peak widths .