Testing the Keplerian disk hypothesis using X-ray reflection spectroscopy

Abstract

The Novikov-Thorne model is the standard framework for the description of geometrically thin and optically thick accretion disks around black holes and is widely used to study the electromagnetic spectra of accreting black holes. One of the assumptions of the model is that the particles of the gas move on nearly-geodesic circular orbits on the equatorial plane. In this work, we propose to test the Keplerian velocity of the particles in the accretion disk using X-ray reflection spectroscopy. We present a modified version of RELXILL in which we introduce a phenomenological parameter, $\alpha$, to quantify possible deviations from Keplerian motion. We use our model to fit a Suzaku observation of the black hole binary GRS 1915+105. We find that the estimate of $\alpha$ is correlated to that of the inclination angle of the disk, $i$, and that we could test the Keplerian disk hypothesis in the presence of a robust and independent measurement of $i$.

9 pages, 5 figures. v2: refereed version

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• Constraints on Einstein-Maxwell dilaton-axion gravity from X-ray reflection spectroscopy
• Testing General Relativity with X-ray reflection spectroscopy: The Konoplya-Rezzolla-Zhidenko parametrization
• Testing relativistic reflection models with GRMHD simulations of accreting black holes
• Towards more accurate synthetic reflection spectra: improving the calculations of returning radiation
• Probing the near-horizon region of Cygnus X-1 with Suzaku and NuSTAR
• Impact of the returning radiation in current tests of the Kerr black hole hypothesis using X-ray reflection spectroscopy
• Impact of ionization and electron density gradients in X-ray reflection spectroscopy measurements
• Measuring black hole spins with x-ray reflection spectroscopy: A GRMHD outlook