Absorption Features in the X-ray Spectrum of an Ordinary Radio Pulsar

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Science  24 Aug 2012:
Vol. 337, Issue 6097, pp. 946-949
DOI: 10.1126/science.1221378

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  1. Fig. 1

    Period P versus period derivative Embedded Image for pulsars of various types. These parameters are most commonly used to characterize pulsars. The data come from the Australia Telescope National Facility catalog (27). A number of physical indicators can be derived from P and Embedded Image, namely the spin-down power, magnetic field, and spin-down age (overplotted as labeled straight lines). Whereas the vast majority of ordinary, rotation-powered pulsars (black dots) are grouped in the middle of the figure, exotic objects such as magnetars (red squares), RRATs (blue triangles), CCOs (red circles), and XDINSs (orange stars) appear located away from the ordinary pulsar population. We have marked the NSs with reported spectral features (for which both P and Embedded Image have been determined) with large black crosses.

  2. Fig. 2

    Phase-integrated spectra of PSR J1740+1000. (A) The count-rate spectra obtained with XMM-Newton EPIC and Chandra ACIS are shown together with the best-fit absorbed BB+BB+PL model. The error bars shown in this and other figures are 1σ for Poisson statistics. Different colors correspond to different instruments of the two x-ray observatories (as labeled). Here and in other spectral plots, the error bars correspond to the data, and the lines correspond to the best-fit models. (B) The best-fit model photon spectrum, with the individual components shown (dotted lines). See the text for details of the fitting and parameter values. The jumps in the spectrum are the edges due to the interstellar absorption.

  3. Fig. 3

    Pulse profiles and phase-resolved spectra of PSR J1740+1000. (Left) Energy-resolved background-subtracted pulse profiles measured with XMM-Newton EPIC PN in five energy bands. (Top right) Count-rate spectra constructed by selecting the photons from the three chosen phase intervals shown by red, green, and black in the left panel. We also show residuals with respect to the BB component (solid lines) of the best-fit BB×GABS model to emphasize the shape and locations of the lines we observed. (Bottom right) BB×GABS fits and residuals for the three chosen phase intervals. No systematic residuals are seen between 0.5 and 0.8 keV. Here, we have not fitted for the low-energy line, leaving systematic residuals below 0.3 keV. See supplementary materials for details.

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