A new direct method for measuring the Hubble constant from reverberating accretion discs in active galaxies

We show how wavelength-dependent time delays between continuum flux variations of AGN can be used to test the standard black hole-accretion disc paradigm, by measuring the temperature structure $T(R)$ of the gaseous material surrounding the purported black hole. Reprocessing of high energy radiation in a steady-state blackbody accretion disc with $T \propto R^{-3/4}$ incurs a wavelength-dependent light travel time delay $\tau \propto \lambda ^{4/3}$. The International AGN Watch multiwavelength monitoring campaign on NGC 7469 showed optical continuum variations lagging behind those in the UV by about 1 day at 4800\AA and about 2 days at 7500\AA. These UV/optical continuum lags imply a radial temperature structure $T \propto R^{-3/4}$, consistent with the classical accretion disc model, and hence strongly supports the existence of a disc in this system. We assume that the observed time delays are indeed due to a classical accretion-disc structure, and derive a redshift independent luminosity distance to NGC 7469. The luminosity distance allows us to estimate a Hubble constant of $H_{0} (\cos i / 0.7)^{1/2} = 42\pm9 \Hubble$. The interpretation of the observed time delays and spectral energy distribution in the context of an accretion disc structure requires further validation. At the same time, efforts to minimize the systematic uncertainties in our method to derive a more accurate measurement of $H_{0}$, e.g by obtaining an independent accurate determination of the disc inclination $i$ or statistical average of a moderate sample of active galaxies, are required. However, this remains a promising new method of determining redshift-independent distances to AGNs.