We report the detection of radio and X-ray pulsations at a period of 51.6 ms from the X-ray source RX/AX J2229.0+6114 in the error box of the EGRET source 3EG J2227+6122. An ephemeris derived from a single ASCA observation and multiple epochs at 1412 MHz from Jodrell Bank indicates steady spin-down with = 7.83 × 10 -14 s s -1 . From the measured P and , we derive spin-down power = 2.2 × 10 37 ergs s -1 , magnetic field B p = 2.0 × 10 12 G, and characteristic age P /2 = 10,460 yr. An image from the Chandra X-Ray Observatory reveals a point source surrounded by centrally peaked diffuse emission that is contained within an incomplete radio shell. We assign the name G106.6+2.9 to this new supernova remnant, which is evidently a pulsar wind nebula. For a distance of 3 kpc estimated from X-ray absorption, the ratio of X-ray luminosity to spin-down power is ≈8 × 10 -5 , smaller than that of most pulsars but similar to the Vela pulsar. If PSR J2229+6114 is the counterpart of 3EG J2227+6122, then its efficiency of γ-ray production, if isotropic, is 0.016 ( d /3 kpc) 2 . It obeys an established trend of γ-ray efficiency among known γ-ray pulsars, which, in combination with the demonstrated absence of any other plausible counterpart for 3EG J2227+6122, makes the identification compelling. If confirmed, this identification bolsters the pulsar model for unidentified Galactic EGRET sources.
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Halpern et al. (2001) studied this question.