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We present the first long \emph{Suzaku} observation of the hyperluminousinfrared galaxy IRAS 09104+4109 which is dominated by a Type 2 AGN. Theinfrared to X-ray SED indicates that the source is an obscured quasar with aCompton-thin absorber. However, the 3$\sigma$ hard X-ray detection of thesource with the \emph{BeppoSAX} PDS suggested a reflection-dominated,Compton-thick view. The high-energy detection was later found to be possiblycontaminated by another Type 2 AGN, NGC 2785, which is only 17 arcmin away. Ournew \emph{Suzaku} observation offers simultaneous soft and hard X-ray coverageand excludes contamination from NGC 2785. We find that the hard X-ray componentis not detected by the \emph{Suzaku} HXD/PIN (effective energy band 14-45 keV).Both reflection and transmission models have been tested on the latest\emph{Suzaku} and \emph{Chandra} data. The 0.5-10 keV spectrum can be wellmodelled by the two scenarios. In addition, our analysis implied that theabsorption column required in both models is $N_{\rm H} \sim 5 \times 10^{23}$cm$^{-2}$. Unless IRAS 09104+4109 is a "changing-look" quasar, we confirm thatit is a Compton-thin AGN. Although the lack of detection of X-ray emissionabove 10 keV seems to favour the transmission scenario, we found that the twomodels offer fairly similar flux predictions over the X-ray band below $\sim$40 keV. We also found that the strong iron line shown in the \emph{Suzaku}spectrum is in fact a blend of two emission lines, in which the 6.4 keV one ismostly contributed from the AGN and the 6.7 keV from the hot cluster gas. Thisimplies that the neutral line is perhaps caused by disc reflection, and thereflection-dominated model is more likely the explanation. The transmissionmodel should not be completely ruled out, but a deeper hard X-ray spectrumobservation is needed to discriminate between the two scenarios.

Confirmation of the nature of the absorber in IRAS 09104+4109