Analysing the Spectra of the Broad-Line Seyfert 1 Galaxy CBS 126

Details Analysing the Spectra of the Broad-Line Seyfert 1 Galaxy CBS 126 Analysing the Spectra of the Broad-Line Seyfert 1 Galaxy CBS 126

2011-10-27

arxiv.org/abs/1110.6047v1

Astronomy and Astrophysics

Astrophysics

High Energy Astrophysical Phenomena

7 pages, 10 figures, submitted to MNRAS

Scientific paper

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.

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