Chandra Observations of the Anomalous X-ray Pulsar 1E 2259+58.6

S. K. Patel, C. Kouveliotou, P. M. Woods, M. H. Finger (USRA/NSSTC), A. F. Tennant,
M. C. Weisskopf (NASA/MSFC), F. Paerels, J. Vink (Columbia U.), E. Gögüs (UAH),
M. van der Klis (U. Amsterdam), T. Belloni (Osservatorio di Brera)

Abstract

We present X-ray imaging, timing, and phase resolved spectroscopy of the anomalous X-ray pulsar 1E 2259+58.6 using the Chandra X-ray Observatory. Time resolved X-ray spectra show no significant variation as a function of pulsar spin phase. The phase averaged spectrum is well described by a power law plus blackbody model with $\Gamma = 3.6(1)$, $kT_{\rm BB}=0.412(6)$ keV, and $N_{\rm H}=0.93(3)~\times~10^{22}~{\rm cm}^{-2}$; we find no evidence for spectral features (0.5-7.0 keV). We derive a spin period of P=6.978977(24) s. We have detected emission beyond $4^{\prime\prime}$ from the central source extending above $100^{\prime\prime}$, which is due to the supernova remnant (G109.1-1.0) and to dust scattering in the interstellar medium.

CATEGORY: SUPERNOVAE, SUPERNOVA REMNANTS AND ISOLATED NEUTRON STARS