Discovery of a young, 267 millisecond pulsar in the supernova remnant W44

A. Wolszczan, J. M. Cordes, R. J. Dewey

Research output: Contribution to journalArticle

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Abstract

We report the discovery of a 267 ms pulsar, PSR 1853+01, in the supernova remnant W44 (G34.7-0.4). The pulsar is located south of the center of W44, well within its radio shell and at the southern edge of the X-ray emission region which fills the interior of the remnant. The period derivative Ṗ ≈ 208 x 10-15 s s-1 leads to a characteristic age of ∼20,000 yr for the pulsar, which agrees well with the estimated age of W44 (≥ 10,000 yr). Similarly, the dispersion measure derived distance of the pulsar, ∼3.2 kpc, is almost identical with the kinematic distance of the remnant, 3.1 kpc. As expected in the case of a young pulsar, PSR 1853+01 exhibits large timing activity. These data clearly indicate that the two objects are physically related and form the sixth known pulsar-supernova remnant association. We also discuss the possibility that PSR 1853+01 and a nearby older pulsar PSR 1854+00 may have a common origin in a binary system disrupted by the explosion that produced W44.

Original languageEnglish (US)
Pages (from-to)L99-L102
JournalAstrophysical Journal
Volume372
Issue number2 PART 2
DOIs
StatePublished - May 10 1991

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supernova remnants
pulsars
explosion
fill
kinematics
shell
radio
young
explosions
time measurement
x rays

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Wolszczan, A. ; Cordes, J. M. ; Dewey, R. J. / Discovery of a young, 267 millisecond pulsar in the supernova remnant W44. In: Astrophysical Journal. 1991 ; Vol. 372, No. 2 PART 2. pp. L99-L102.
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abstract = "We report the discovery of a 267 ms pulsar, PSR 1853+01, in the supernova remnant W44 (G34.7-0.4). The pulsar is located south of the center of W44, well within its radio shell and at the southern edge of the X-ray emission region which fills the interior of the remnant. The period derivative Ṗ ≈ 208 x 10-15 s s-1 leads to a characteristic age of ∼20,000 yr for the pulsar, which agrees well with the estimated age of W44 (≥ 10,000 yr). Similarly, the dispersion measure derived distance of the pulsar, ∼3.2 kpc, is almost identical with the kinematic distance of the remnant, 3.1 kpc. As expected in the case of a young pulsar, PSR 1853+01 exhibits large timing activity. These data clearly indicate that the two objects are physically related and form the sixth known pulsar-supernova remnant association. We also discuss the possibility that PSR 1853+01 and a nearby older pulsar PSR 1854+00 may have a common origin in a binary system disrupted by the explosion that produced W44.",
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Discovery of a young, 267 millisecond pulsar in the supernova remnant W44. / Wolszczan, A.; Cordes, J. M.; Dewey, R. J.

In: Astrophysical Journal, Vol. 372, No. 2 PART 2, 10.05.1991, p. L99-L102.

Research output: Contribution to journalArticle

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N2 - We report the discovery of a 267 ms pulsar, PSR 1853+01, in the supernova remnant W44 (G34.7-0.4). The pulsar is located south of the center of W44, well within its radio shell and at the southern edge of the X-ray emission region which fills the interior of the remnant. The period derivative Ṗ ≈ 208 x 10-15 s s-1 leads to a characteristic age of ∼20,000 yr for the pulsar, which agrees well with the estimated age of W44 (≥ 10,000 yr). Similarly, the dispersion measure derived distance of the pulsar, ∼3.2 kpc, is almost identical with the kinematic distance of the remnant, 3.1 kpc. As expected in the case of a young pulsar, PSR 1853+01 exhibits large timing activity. These data clearly indicate that the two objects are physically related and form the sixth known pulsar-supernova remnant association. We also discuss the possibility that PSR 1853+01 and a nearby older pulsar PSR 1854+00 may have a common origin in a binary system disrupted by the explosion that produced W44.

AB - We report the discovery of a 267 ms pulsar, PSR 1853+01, in the supernova remnant W44 (G34.7-0.4). The pulsar is located south of the center of W44, well within its radio shell and at the southern edge of the X-ray emission region which fills the interior of the remnant. The period derivative Ṗ ≈ 208 x 10-15 s s-1 leads to a characteristic age of ∼20,000 yr for the pulsar, which agrees well with the estimated age of W44 (≥ 10,000 yr). Similarly, the dispersion measure derived distance of the pulsar, ∼3.2 kpc, is almost identical with the kinematic distance of the remnant, 3.1 kpc. As expected in the case of a young pulsar, PSR 1853+01 exhibits large timing activity. These data clearly indicate that the two objects are physically related and form the sixth known pulsar-supernova remnant association. We also discuss the possibility that PSR 1853+01 and a nearby older pulsar PSR 1854+00 may have a common origin in a binary system disrupted by the explosion that produced W44.

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