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No Time for Dead Time: Timing Analysis of Bright Black Hole Binaries with NuSTAR

  • Authors: Matteo Bachetti, Fiona A. Harrison, Rick Cook, John Tomsick, Christian Schmid, Brian W. Grefenstette, Didier Barret, Steven E. Boggs, Finn E. Christensen, William W. Craig, Andrew C. Fabian, Felix Fürst, Poshak Gandhi, Charles J. Hailey, Erin Kara, Thomas J. Maccarone, Jon M. Miller, Katja Pottschmidt, Daniel Stern, Phil Uttley, Dominic J. Walton, Jörn Wilms, and William W. Zhang

Bachetti et al. 2015 The Astrophysical Journal 800 109.

  • Provider: AAS Journals

Caption: Figure 3.

Top: variation of the rms of a QPO at different peak frequencies, measured with the various techniques and with and without dead time. Each point represents a simulated QPO with rms = 10% and FWHM = 2 Hz. A total of 281 simulations were used for this plot. (Bottom) Significance measured with each method. The total PDS has about twice the significance of the single-module PDS in the no-dead-time case, as expected, owing to double the number of photons. The CPDS in the no-dead-time case is a factor of higher than the single PDS, and lower than the total PDS by the same amount. The dead-time-affected CPDS, instead, has a much lower level due to the lack of photons. The decrease of significance does not depend on the frequency of the QPO, but only on count rate (see Figure 4).

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