TY - JOUR
T1 - PSR J2229+6114
T2 - Discovery of an energetic young pulsar in the error box of the EGRET source 3EG J2227+6122
AU - Halpern, J. P.
AU - Camilo, F.
AU - Gotthelf, E. V.
AU - Helfand, D. J.
AU - Kramer, M.
AU - Lyne, A. G.
AU - Leighly, K. M.
AU - Eracleous, M.
N1 - Funding Information:
We thank Christine Jordan and Benjamin Collins for help with reduction of radio data and X-ray data, respectively. An anonymous referee supplied many helpful comments. This work was supported by NASA grants NAG5-9095 and CXO GO1-2049X to the Columbia Astrophysics Laboratory.
PY - 2001/5/10
Y1 - 2001/5/10
N2 - 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 = 7.83 × 10-14 s s-1. From the measured P and Ṗ, we derive spin-down power Ė = 2.2 × 1037 ergs s-1, magnetic field Bp = 2.0 × 1012 G, and characteristic age P/2Ṗ = 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.
AB - 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 = 7.83 × 10-14 s s-1. From the measured P and Ṗ, we derive spin-down power Ė = 2.2 × 1037 ergs s-1, magnetic field Bp = 2.0 × 1012 G, and characteristic age P/2Ṗ = 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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U2 - 10.1086/320347
DO - 10.1086/320347
M3 - Article
AN - SCOPUS:0035638645
SN - 0004-637X
VL - 552
SP - L125-L128
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2 PART 2
ER -