1998A&A...330..175P

The 7 s X-ray pulsar 1E 2259+586 and the supernova remnant (SNR) G109.1-1.0 (CTB 109) were observed by BeppoSAX in 1996 November. The pulse period of 6.978914±0.000006 s implies that 1E 2259+586 continues its near constant spin-down trend. The 0.5-10keV pulse shape is characterized by a double peaked profile, with the amplitude of the second peak ∼50% of that of the main peak. The pulse profile does not exhibit any strong energy dependence. We confirm the ASCA discovery of an additional low-energy spectral component from 1E 2259+586. This can best be modeled as a 0.44keV blackbody, but we cannot exclude that some, or all, of this emission arises from the part of the SNR that lies within the pulsar's extraction region. The spectrum of G109.1-1.0 is well fit with a non-equilibrium ionization plasma model with a best-fit temperature of 0.95keV. The derived mass for the X-ray emitting plasma (∼15-20M_☉) and its near cosmic abundances imply that the X-ray emission comes mainly from mildly enriched, swept-up circumstellar material. The spectrum is strongly out of equilibrium with an ionization age of only 3000 yr. This age is in good agreement with that derived from hydrodynamic simulations of the SNR using the above X-ray temperature.