Chia-Ying Chiang, R. C. Reis, A. C. Fabian, D. Grupe, S. Tsuruta
We analysed the new simultaneous \emph{Suzaku} and \emph{Swift} data of the
Broad Line Seyfert 1 (BLS1) galaxy CBS 126. A clear Fe emission line and an
enormous soft excess are present in the source spectra. We fit the spectra with
a relativistic reflection model and find the model tends to fit the data with a
high iron abundance due to the large soft excess. By checking the difference
and the RMS spectra, we find there is likely an absorption edge at $\sim$ 0.89
keV, which might be caused by Oxygen or Neon. We also produced an analysis of
the time-resolved spectra to examine the existence of the edge. Although a
model with a high iron abundance is more desired in the time-resolved spectra,
a model of solar iron abundance together with an absorption edge is a more
physical explanation. Variation of the ionisation parameter in difference
periods of spectra could be an alternative explanation of the excess seen in
the difference spectra. We find the lack of low-energy ($<$ 0.5 keV) data
coverage in the time-resolved spectra to be the reason for the high iron
abundance tendency. It is difficult to know if there are warm absorbers in this
source from the current data. To further investigate the presence of warm
absorbers and constrain the iron abundance, more detailed low-energy data are
needed. The work presents that the spectra of a BLS1 can be explained by the
standard reflection model.
View original:
http://arxiv.org/abs/1110.6047
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