2001ApJ...552L.125H -
Astrophys. J., 552, L125-L128 (2001/May-2)
PSR J2229+6114: discovery of an energetic young pulsar in the error box of the EGRET source 3EG J2227+6122.
HALPERN J.P., CAMILO F., GOTTHELF E.V., HELFAND D.J., KRAMER M., LYNE A.G., LEIGHLY K.M. and ERACLEOUS M.
Abstract (from CDS):
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 P{dot}=7.83x10–14 s.s–1. From the measured P and P{dot}, we derive spin-down power E{dot}=2.2x1037 ergs.s–1, magnetic field Bp=2.0x1012 G, and characteristic age P/2P{dot}=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 ~8x10–5, 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.
Abstract Copyright:
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Journal keyword(s):
Gamma Rays: Observations - Stars: Pulsars: Individual: Alphanumeric: PSR J2229+6114 - ISM: Supernova Remnants
Simbad objects:
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