We report the results of temporal and spectral analysis performed on the X-ray pulsar 4U 1538-52 observed by BeppoSAX. We obtained a new estimate of the spin period of the neutron star P = 528.24 +/- 0.01 s (corrected for the orbital motion of the X-ray source): the source is still in the spin-up state, as it has been since 1988. The pulse profile is double peaked, although significant variations of the relative intensity of the peaks with energy are present. The broadband (0.12-100 keV) out-of-eclipse spectrum is well described by an absorbed power law modified by a high-energy cutoff at similar to 16 keV (e-folding energy similar to 10 keV) plus an iron emission line at similar to6.4 keV. A cyclotron line at similar to 21 keV is present. The width of the line is consistent with thermal Doppler broadening at the temperature of the exponential cutoff. We searched for the presence of the second harmonic, previously reported for this source. We found no evidence of lines at similar to 42 keV, although an absorption feature at 51 keV seems to be present (at 99% confidence level). A soft excess, modeled by a blackbody with a temperature of similar to0.08 keV could be present, probably emitted by the matter at the magnetosphere. We also performed a spectral analysis during the X-ray eclipse. The spectral evolution during the eclipse can be well described by a progressive covering of the primary Comptonization spectrum that is scattered into the line of sight. During the deep eclipse this spectrum also softens, suggesting that the dust-scattered component becomes important. An alternative, more complex model, with an emission iron line and scattered components (as the one that has been used to fit the eclipse of Cen X-3), also gives a good fit of the deep-eclipse data.
The BeppoSAX 0.1-100 keV spectrum of the X-ray pulsar 4U 1538-52
BURDERI, LUCIANO;
2001-01-01
Abstract
We report the results of temporal and spectral analysis performed on the X-ray pulsar 4U 1538-52 observed by BeppoSAX. We obtained a new estimate of the spin period of the neutron star P = 528.24 +/- 0.01 s (corrected for the orbital motion of the X-ray source): the source is still in the spin-up state, as it has been since 1988. The pulse profile is double peaked, although significant variations of the relative intensity of the peaks with energy are present. The broadband (0.12-100 keV) out-of-eclipse spectrum is well described by an absorbed power law modified by a high-energy cutoff at similar to 16 keV (e-folding energy similar to 10 keV) plus an iron emission line at similar to6.4 keV. A cyclotron line at similar to 21 keV is present. The width of the line is consistent with thermal Doppler broadening at the temperature of the exponential cutoff. We searched for the presence of the second harmonic, previously reported for this source. We found no evidence of lines at similar to 42 keV, although an absorption feature at 51 keV seems to be present (at 99% confidence level). A soft excess, modeled by a blackbody with a temperature of similar to0.08 keV could be present, probably emitted by the matter at the magnetosphere. We also performed a spectral analysis during the X-ray eclipse. The spectral evolution during the eclipse can be well described by a progressive covering of the primary Comptonization spectrum that is scattered into the line of sight. During the deep eclipse this spectrum also softens, suggesting that the dust-scattered component becomes important. An alternative, more complex model, with an emission iron line and scattered components (as the one that has been used to fit the eclipse of Cen X-3), also gives a good fit of the deep-eclipse data.
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