Weighing the black holes in ultraluminous X-ray sources through timing
arXiv:0804.3378 · doi:10.1111/j.1365-2966.2008.13372.x
Abstract
We describe a new method to estimate the mass of black holes in Ultraluminous X-ray Sources (ULXs). The method is based on the recently discovered ``variability plane'', populated by Galactic stellar-mass black-hole candidates (BHCs) and supermassive active galactic nuclei (AGNs), in the parameter space defined by the black-hole mass, accretion rate and characteristic frequency. We apply this method to the two ULXs from which low-frequency quasi-periodic oscillations have been discovered, M82 X-1 and NGC 5408 X-1. For both sources we obtain a black-hole mass in the range 100~1300 Msun, thus providing evidence for these two sources to host an intermediate-mass black hole.
5 pages, 2 figures, Accepted by MNRAS
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Cited by in corpus (8)
- A 400 solar mass black hole in the Ultraluminous X-ray source M82 X-1 accreting close to its Eddington limit
- Discovery of mHz X-ray Oscillations in a Transient Ultraluminous X-ray Source in M82
- Roche-lobe overflow systems powered by black holes in young star clusters: the importance of dynamical exchanges
- A geometric origin for quasi-periodic oscillations in black hole X-ray binaries
- Gravitational wave radiation from periodic orbits and quasi-periodic oscillations in Einstein non-linear Maxwell-Yukawa black hole
- Measuring the black hole mass in Ultraluminous X-ray Sources with the X-ray Scaling Method
- Probing the nature of Einstein nonlinear Maxwell Yukawa black hole through gravitational wave forms from periodic orbits and quasiperiodic oscillations
- A supermassive black hole under the radar: Repeating X-ray variability in a Seyfert galaxy