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Astron. Astrophys. 363, 863-868 (2000)

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7. Summary

The main results of the BeppoSAX observation of Mrk 766 may be summarized as follows:

  • The spectrum of Mrk 766 is well fitted by an absorbed power law (with cold absorption in excess of the Galactic one), a warm absorber, an oxygen line and a further component (mainly accounting for the iron edge) which may be either a second and more ionized warm absorber or a mildly ionized disc. A soft excess is not required by the data, but its inclusion makes the cold absorber closer to the Galactic value.

  • The spectral variability during the observation may be entirely due to variations in the properties of the warm absorber(s), even if the behaviour of the absorber is complex and no obvious correlation with the flux is apparent.

  • The power law is significantly steeper than during the ASCA-ROSAT observation (Leighly et al. 1996). The spectral variability pattern is also very different, indicating that we have observed the source in a different state.

  • There is clear evidence for an O VII emission line, which may originate either in the accretion disc or in the warm absorber, or, most plausibly given the large equivalent width, in both.

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© European Southern Observatory (ESO) 2000

Online publication: December 5, 2000
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