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Doppler tomography can provide a powerful means of determining black holespin when our view to the central regions are revealed and obscured byoptically thick orbiting material, and can provide an independent estimate thatdoes not suffer as many degeneracies as traditional methods. For low mass AGN,time-dependent obscuration is expected to leave a signature in the changingspectrum of the disc emission which extends into the soft X-ray bandpass. Wecreate a spectral model incorporating Doppler tomography and apply it to thecase of the low mass (8 $\times$ 10$^{5}$ M$_{\odot}$) AGN, RX J1301.9+2747which shows unusual timing properties in the form of short-lived flares that weargue are best explained by the orbit of a window through an optically thickwind. Modelling the phase-resolved spectrum over the course of the highest dataquality flare indicates a very low spin even when we relax our constraints.This is the lowest mass AGN for which a spin has been measured and the firstvia this technique. We note that, as the mass and spin are very low, thisappears to favour supermassive black hole (SMBH) growth by chaotic rather thanconstant accretion.

Doppler disc tomography applied to low mass AGN spin