Chandra X-Ray Observations of G11.2-0.3: Implications for Pulsar Ages
Abstract
We 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. 18h11m29.22s, decl. -19°25'27.6", with 1 σ error radius of 0.6". 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.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- October 2001
- DOI:
- arXiv:
- arXiv:astro-ph/0107292
- Bibcode:
- 2001ApJ...560..371K
- Keywords:
-
- Stars: Pulsars: General;
- pulsars: individual (AX J1811.5-1926;
- PSR J1811-1925);
- supernovae: individual (G11.2-0.3);
- X-Rays: General;
- Astrophysics
- E-Print:
- 16 pages, 3 figures, Accepted for publication in ApJ. For a full resolution version of Fig 1, see http://www.physics.mcgill.ca/~vkaspi/G11.2-0.3/f1.eps
