Fitting Pulsar Wind Tori. II. Error Analysis and Applications

Abstract

We have applied the torus fitting procedure described in Ng & Romani (2004) to PWNe observations in the Chandra data archive. This study provides quantitative measurement of the PWN geometry and we characterize the uncertainties in the fits, with statistical errors coming from the fit uncertainties and systematic errors estimated by varying the assumed fitting model. The symmetry axis $\Psi$ of the PWN are generally well determined, and highly model-independent. We often derive a robust value for the spin inclination $\zeta$. We briefly discuss the utility of these results in comparison with new radio and high energy pulse measurements

15 pages, 3 figures, ApJ in press

References in corpus (1)

• The Origin and Motion of PSR J0538+2817 in S147

Cited by in corpus (7)

• Fermi LAT Observations of the Vela Pulsar
• Optical polarisation of the Crab pulsar: precision measurements and comparison to the radio emission
• Deep Chandra Observation of the Pulsar Wind Nebula Powered by the Pulsar J1846-0258 in the Supernova Remnant Kes 75
• Fourier Modeling of the Radio Torus Surrounding Supernova 1987A
• Discovery of High-Energy Gamma-Ray Pulsations from PSR J2021+3651 with AGILE
• Rings and Jets around PSR J2021+3651: the `Dragonfly Nebula'
• Discovery of Pulsations from the Pulsar J0205+6449 in SNR 3C 58 with the Fermi Gamma-Ray Space Telescope