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We present new broadband X-ray observations of the type-I Seyfert galaxy IRAS09149-6206, taken in 2018 with $XMM$-$Newton$, $NuSTAR$ and $Swift$. The sourceis highly complex, showing a classic 'warm' X-ray absorber, additionalabsorption from highly ionised iron, strong relativistic reflection from theinnermost accretion disc and further reprocessing by more distant material. Bycombining X-ray timing and spectroscopy, we have been able to fullycharacterise the supermassive black hole in this system, constraining both itsmass and - for the first time - its spin. The mass is primarily determined byX-ray timing constraints on the break frequency seen in the power spectrum, andis found to be $\log[M_{\rm{BH}}/M_{\odot}] = 8.0 \pm 0.6$ (1$\sigma$uncertainties). This is in good agreement with previous estimates based on theH$\alpha$ and H$\beta$ line widths, and implies that IRAS 09149-6206 isradiating at close to (but still below) its Eddington luminosity. The spin isconstrained via detailed modelling of the relativistic reflection, and is foundto be $a^* = 0.94^{+0.02}_{-0.07}$ (90% confidence), adding IRAS 09149-6206 tothe growing list of radio-quiet AGN that host rapidly rotating black holes. Theoutflow velocities of the various absorption components are all relativelymodest ($v_{\rm{out}} \lesssim 0.03c$), implying these are unlikely to drivesignificant galaxy-scale AGN feedback.

A Full Characterisation of the Supermassive Black Hole in IRAS 09149-6206