tlpipe.rfi.surface_fit.SurfaceFitMethod

class tlpipe.rfi.surface_fit.SurfaceFitMethod(time_freq_vis, time_freq_vis_mask=None)

Abstract base class for surface fitting methods.

A surface fit to the correlated visibilities \(V(\nu, t)\) as a function of frequency \(\nu\) and time \(t\) can produce a surface \(\hat{V}(\nu, t)\) that represents the astronomical information in the signal. Requiring \(\hat{V}(\nu, t)\) to be a smooth surface is a good assumption for most astronomical continuum sources, as their observed amplitude tend not to change rapidly with time and frequency, whereas specific types of RFI can create sharp edges in the time-frequency domain. The residuals between the fit and the data contain the system noise and the RFI, which can then be thresholded without the chance of flagging astronomical sources that have visibilities with high amplitude.

Note

Because of the smoothing in both time and frequency direction, this method is not directly usable when observing strong line sources or strong pulsars.

__init__(time_freq_vis, time_freq_vis_mask=None)

x.__init__(…) initializes x; see help(type(x)) for signature

Methods

fit()

Abstract method that needs to be implemented by sub-classes.