pint.models.noise_model
Pulsar timing noise models.
Functions
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Create quantization matrix mapping TOAs to observing epochs. |
Construct a Fourier design matrix from a given set of frequencies. |
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Find only epochs with more than 1 TOA for applying ECORR. |
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Get the number of epochs associated with each ECORR. |
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Compute an array of red-noise frequencies, optionally mixing log- and linearly spaced frequencies. |
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Construct an interpolation basis for the given TOAs and interpolation parameters using scipy.interpolate.interp1d. |
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Matérn covariance matrix. |
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Quasi-periodic (SE × periodic) covariance matrix. |
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Power-law PSD. |
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Project basis-space covariance to data-space covariance. |
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Ridge (diagonal) covariance matrix. |
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Squared-exponential (RBF) covariance matrix. |
Classes
Abstract base class for all correlated noise components. |
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Noise correlated between nearby TOAs. |
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Model of a radio frequency-dependent noise with a power-law spectrum and arbitrary chromatic index. |
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Model of DM variations as radio frequency-dependent noise with a power-law spectrum. |
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Timing noise with a power-law spectrum. |
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Model of solar wind DM variations as radio frequency-dependent noise with a power-law spectrum. |
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Correction for estimated wideband DM measurement uncertainty. |
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Correct the reported TOA uncertainties. |
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Time-domain solar wind noise model with a selectable GP kernel. |
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Abstract base class for all white noise components. |