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Title:
Chandra X-Ray Observations of G11.2-0.3: Implications for Pulsar Ages
Authors:
Kaspi, V. M.; Roberts, M. E.; Vasisht, G.; Gotthelf, E. V.; Pivovaroff, M.; Kawai, N.
Affiliation:
AA(; Department of Physics, Rutherford Physics Building, McGill University, 3600 University Street, Montreal, QC H3A 2T8, Canada.; Department of Physics and Center for Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139.; Alfred P. Sloan Research Fellow.), AB(; Department of Physics, Rutherford Physics Building, McGill University, 3600 University Street, Montreal, QC H3A 2T8, Canada.; Department of Physics and Center for Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139.; Quebec Merit Fellow.), AC(; Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109.), AD(; Astronomy Department, Pupin Hall, Columbia University, 550 West 120th Street, New York, NY 10027.), AE(; Therma-Wave, Inc., 1250 Reliance Way, Fremont, CA 94539.), AF(; Department of Physics, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, 152-8551 Tokyo, Japan.; RIKEN (The Institute of Physical and Chemical Research), 2-1 Hirosawa, Wako, 351-0198 Saitama, Japan.)
Publication:
The Astrophysical Journal, Volume 560, Issue 1, pp. 371-377. (ApJ Homepage)
Publication Date:
10/2001
Origin:
UCP
ApJ Keywords:
Stars: Pulsars: General, pulsars: individual (AX J1811.5-1926, PSR J1811-1925), supernovae: individual (G11.2-0.3), X-Rays: General
DOI:
10.1086/322515
Bibliographic Code:
2001ApJ...560..371K

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.
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