Radio detection of LAT PSRs J1741-2054 and J2032+4127: no longer just
  gamma-ray pulsars
  Sixteen pulsars have been discovered so far in blind searches of photons
collected with the Large Area Telescope on the Fermi Gamma-ray Space Telescope.
We here report the discovery of radio pulsations from two of them. PSR
J1741-2054, with period P=413ms, was detected in archival Parkes telescope data
and subsequently has been detected at the Green Bank Telescope (GBT). Its
received flux varies greatly due to interstellar scintillation and it has a
very small dispersion measure of DM=4.7pc/cc, implying a distance of ~0.4kpc
and possibly the smallest luminosity of any known radio pulsar. At this
distance, for isotropic emission, its gamma-ray luminosity above 0.1GeV
corresponds to 25% of the spin-down luminosity of dE/dt=9.4e33erg/s. The
gamma-ray profile occupies 1/3 of pulse phase and has three closely-spaced
peaks with the first peak lagging the radio pulse by delta=0.29P. We have also
identified a soft Swift source that is the likely X-ray counterpart. In many
respects PSR J1741-2054 resembles the Geminga pulsar. The second source, PSR
J2032+4127, was detected at the GBT. It has P=143ms, and its DM=115pc/cc
suggests a distance of ~3.6kpc, but we consider it likely that it is located
within the Cyg OB2 stellar association at half that distance. The radio
emission is nearly 100% linearly polarized, and the main radio peak precedes by
delta=0.15P the first of two narrow gamma-ray peaks that are separated by
Delta=0.50P. Faint, diffuse X-ray emission in a Chandra image is possibly its
pulsar wind nebula. PSR J2032+4127 likely accounts for the EGRET source 3EG
J2033+4118, while its pulsar wind is responsible for the formerly unidentified
HEGRA source TeV J2032+4130.
