High-frequency X-ray variability as a mass estimator of stellar and supermassive black holes

Marek Gierliński (Lead / Corresponding author), Marek Nikołajuk, Boena Czerny

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Abstract

There is increasing evidence that supermassive black holes in active galactic nuclei (AGN) are scaled-up versions of Galactic black holes. We show that the amplitude of high-frequency X-ray variability in the hard spectral state is inversely proportional to the black hole mass over eight orders of magnitude. We have analysed all available hard-state data from RXTE of seven Galactic black holes. Their power density spectra change dramatically from observation to observation, except for the high-frequency (≳10 Hz) tail, which seems to have a universal shape, roughly represented by a power law of index -2. The amplitude of the tail, CM (extrapolated to 1 Hz), remains approximately constant for a given source, regardless of the luminosity, unlike the break or quasi-periodic oscillation frequencies, which are usually strongly correlated with luminosity. Comparison with a moderate-luminosity sample of AGN shows that the amplitude of the tail is a simple function of black hole mass, CM = C/M, where C ≈ 1.25 M Hz -1. This makes CM a robust estimator of the black hole mass which is easy to apply to low- to moderate-luminosity supermassive black holes. The high-frequency tail with its universal shape is an invariant feature of a black hole and, possibly, an imprint of the last stable orbit.

Original languageEnglish
Pages (from-to)741-749
Number of pages9
JournalMonthly Notices of the Royal Astronomical Society
Volume383
Issue number2
DOIs
Publication statusPublished - 11 Jan 2008

Keywords

  • Accretion, accretion discs
  • Galaxies: active
  • X-rays: binaries

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