kepwindow: calculate and store the window function for a Kepler time series¶

pyke.kepwindow.
kepwindow
(infile, outfile=None, fcol='SAP_FLUX', fmax=1.0, nfreq=100, plot=False, overwrite=False, verbose=False, logfile='kepwindow.log')¶ kepwindow – Calculate and store the window function for a Kepler time series
Kepler time stamps are not perfectly uniform. There are gaps in the data due to operational pauses and issues, and timestamps are corrected to the barycenter of the solar system. The size of the barycenter correction is timedependent. kepwindow calculates a discrete window function for a userprovided Kepler time series. The result is stored in a new FITS file that is a direct copy of the input file but with an additional table extension containing the window function.
Parameters: infile : str
The name of a MAST standard format FITS file containing a Kepler light curve within the first data extension.
outfile : str
The name of the output FITS file with a new extension containing the window function.
fcol : str
The name of the FITS table column in extension 1 of infile with which the window function should be coupled to. While the window function ostensibly requires the timing information, this particular piece of information is required so that the task can search the fcol array for bad data such as instances of NaN. These will be rejected before the window function is calculated.
fmax : float [1/day]
The maximum frequency on which the window function will be calculated.
nfreq : int
The number of uniform frequency steps between 0 and fmax over which the window function will be calculated.
plot : bool
Plot the output window function?
overwrite : bool
Overwrite the output file?
verbose : bool
Print informative messages and warnings to the shell and logfile?
logfile : str
Name of the logfile containing error and warning messages.
Examples
$ kepwindow kplr0024363242009259160929_llc.fits datacol SAP_FLUX fmax 0.7 nfreq 500 plot verbose