V. M. Kaspi et al. 2001 ApJ 560 371 doi:10.1086/322515
Chandra X-Ray Observations of G11.2–0.3: Implications for Pulsar Ages
FREEV. M. Kaspi1,2,3, M. E. Roberts1,2,4, G. Vasisht5, E. V. Gotthelf6, M. Pivovaroff7 and N. Kawai8,9
Show affiliationsWe present Chandra X-Ray Observatory imaging observations of the young Galactic supernova remnant G11.2-0.3. The image shows that the previously known young 65 ms X-ray pulsar is at position (J2000) R.A. 18h11m29.s22, decl. -19°25'27
6, with 1 σ error radius of 06. This is within 8'' of the geometric center of the shell. This provides strong confirming evidence that the system is younger, by a factor of ~12, than the characteristic age of the pulsar. The age discrepancy suggests that pulsar characteristic ages can be poor age estimators for young pulsars. Assuming conventional spin-down with constant magnetic field and braking index, the most likely explanation for the age discrepancy in G11.2-0.3 is that the pulsar was born with a spin period of ~62 ms. The Chandra image also reveals, for the first time, the morphology of the pulsar wind nebula. The elongated hard X-ray structure can be interpreted as either a jet or a Crab-like torus seen edge-on. This adds to the growing list of highly aspherical pulsar wind nebulae and argues that such structures are common around young pulsars.
- Subject headings
pulsars: general; pulsars: individual (AX J1811.5–1926, PSR J1811–1925); supernovae: individual (G11.2–0.3); X-rays: general
- Dates
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Issue 1 (2001 October 10)
Received 2001 April 20, accepted for publication 2001 June 12
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Chandra X-Ray Observations of G11.2–0.3: Implications for Pulsar Ages
V. M. Kaspi et al. 2001 ApJ 560 371
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