Fig. 6
From: A Dataset of Lower Band Whistler Mode Chorus and Exohiss with Instrumental Noise Thresholds
Correction factors and detection thresholds for the simulated trace of the power spectral density matrix obtained from a windowed noise waveform. (a) Correction factors from Eqs. 4 and 5, relevant to the Survey dataset of the EMFISIS Waves instrument on Van Allen Probes. Black dots: average values of the correction factor \({C}_{c\nu }\) for the number of degrees of freedom of the core distribution model; Red dots: average values of the correction factor \({C}_{{cs}}\) for the scale of the core distribution model; Black line with error bars: average values and standard deviations of the correction factor \({C}_{t\nu }\) for the number of degrees of freedom of the tail distribution model; Red line with error bars: average values and standard deviations of the correction factor \({C}_{{ts}}\) for the scale of the tail distribution model. The results are given as a function of the binary logarithm of the number \({n}_{l}\) of averaged spectral estimates; (b) Detection thresholds at P0 = 10−7, for the trace of the magnetic spectral density matrix in na = 3 dimensions, as a function of the binary logarithm of the number \({n}_{l}\) of averaged spectral estimates, assuming a constant sensor noise level of 100 fT2/Hz. Red diamonds: thresholds based on the tail distribution model from Eq. 5, which are used in our procedure, black dots: comparison with thresholds obtained from the core distribution model from Eq. 4, black solid line: comparison with thresholds based on the noise waveform without a window function, according to Eq. 3.
