PSR J2229+6114: Discovery of an energetic young pulsar in the error box of the EGRET source 3EG J2227+6122

J. P. Halpern, F. Camilo, E. V. Gotthelf, D. J. Helfand, M. Kramer, A. G. Lyne, K. M. Leighly, M. Eracleous

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Abstract

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.

Original languageEnglish (US)
Pages (from-to)L125-L128
JournalAstrophysical Journal
Volume552
Issue number2 PART 2
DOIs
StatePublished - May 10 2001

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pulsars
boxes
energetics
rays
x rays
radio
supernova remnants
nebulae
erg
point sources
point source
observatories
observatory
luminosity
time measurement
young
shell
magnetic field
trends
magnetic fields

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Halpern, J. P., Camilo, F., Gotthelf, E. V., Helfand, D. J., Kramer, M., Lyne, A. G., ... Eracleous, M. (2001). PSR J2229+6114: Discovery of an energetic young pulsar in the error box of the EGRET source 3EG J2227+6122. Astrophysical Journal, 552(2 PART 2), L125-L128. https://doi.org/10.1086/320347
Halpern, J. P. ; Camilo, F. ; Gotthelf, E. V. ; Helfand, D. J. ; Kramer, M. ; Lyne, A. G. ; Leighly, K. M. ; Eracleous, M. / PSR J2229+6114 : Discovery of an energetic young pulsar in the error box of the EGRET source 3EG J2227+6122. In: Astrophysical Journal. 2001 ; Vol. 552, No. 2 PART 2. pp. L125-L128.
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Halpern, JP, Camilo, F, Gotthelf, EV, Helfand, DJ, Kramer, M, Lyne, AG, Leighly, KM & Eracleous, M 2001, 'PSR J2229+6114: Discovery of an energetic young pulsar in the error box of the EGRET source 3EG J2227+6122', Astrophysical Journal, vol. 552, no. 2 PART 2, pp. L125-L128. https://doi.org/10.1086/320347

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.; Eracleous, M.

In: Astrophysical Journal, Vol. 552, No. 2 PART 2, 10.05.2001, p. L125-L128.

Research output: Contribution to journalArticle

TY - JOUR

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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.

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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Halpern JP, Camilo F, Gotthelf EV, Helfand DJ, Kramer M, Lyne AG et al. PSR J2229+6114: Discovery of an energetic young pulsar in the error box of the EGRET source 3EG J2227+6122. Astrophysical Journal. 2001 May 10;552(2 PART 2):L125-L128. https://doi.org/10.1086/320347