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

TL;DR

This study analyzes Suzaku and Swift data of the Seyfert 1 galaxy CBS 126, revealing a soft excess, Fe emission line, and potential absorption features, and explores relativistic reflection models with implications for warm absorbers.

Contribution

It provides the first detailed spectral analysis of CBS 126 using simultaneous Suzaku and Swift data, highlighting the role of relativistic reflection and absorption features in BLS1 galaxies.

Findings

Detection of a strong soft excess and Fe emission line.

Evidence for an absorption edge at ~0.89 keV.

Relativistic reflection models can explain the spectra with high iron abundance.

Abstract

We analysed new simultaneous \emph{Suzaku} and \emph{Swift} data of the Broad Line Seyfert 1 (BLS1) galaxy CBS 126. A clear Fe emission line and a strong 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 possibly due to the large soft excess present. 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 in order to examine the existence of the edge. Although high iron abundance is required more in the time-resolved spectra, a model of solar iron abundance together with an absorption edge gives a more physical explanation. Variation of the ionisation parameter is an alternative, plausible explanation for the excess seen in the difference spectra. It is difficult to know if there are warm absorbers in this source from the current data. To further investigate the presence of possible warm absorbers, higher signal-to-noise low-energy data are needed. The work presented here tentatively suggests that the spectra of a BLS1 can be explained by a relativistic reflection model similar to that often seen in their narrow-line cousins.