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Maximum Likelihood Fitting of X-Ray Power Density Spectra: Application to High-frequency Quasi-periodic Oscillations from the Neutron Star X-Ray Binary 4U1608-522

  • Authors: Didier Barret and Simon Vaughan

Barret & Vaughan 2012 The Astrophysical Journal 746 131.

  • Provider: AAS Journals

Caption: Figure 3.

Measured biases on the four model parameters (top left, ν 0; bottom left, a; top right, w; bottom right, R), as a function of the number of 8 s PDS averaged (same y-axis scale as Figure 2). Those biases are derived from the difference between the sample mean of 4096 MLEs (each one from fitting the average of M PDS), and an estimate of the average QPO parameters generated by the simulation over the entire set of 4096 × M PDS simulated. The biases are expressed in percentage of these average values. Error bars on the bias are derived from the standard error on the MLEs; they do not account for error on the fits to the averaged periodograms (which are generated from the same data and so are not independent of the averaged MLEs). Clearly, all the biases converge to zero.

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