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Kepler Guest Observer Program

Contributed Software - KEPSMOOTH

Software: PyKE
Version: 2.0.2
Contributor:

Figure 1: The SAP light curve of a rapidly-rotating spotty star observed during quarter 2 is plotted in orange. The blue curve is the same data smoothed by convolution with a Hanning function of width 1 day.

NAME
kepsmooth -- Smooth Kepler light curve data by convolution

USAGE
kepsmooth infile outfile datacol function fscale plot plotlab clobber verbose logfile status

PARAMETERS
infile = string
The name of a MAST standard format FITS file containing Kepler light curve data within the first data extension.

outfile = string
The name of the output FITS file. The output file is identical in format to the input file. The data to be smoothed will be overwritten in the output file by its convolved version.

datacol = string
The name of the data column in the input FITS file to be smoothed, e.g. SAP_FLUX, PDCSAP_FLUX, MOM_CENTR1 etc. A full list of archived data columns is provided in the Kepler Archive Manual.

function = string
The form of the smoothing function. A flat function is a moving average. The Options are:
flat | hanning | hamming | bartlett | blackman

fscale = float
The width of the convolution function in units of days.

plot = boolean
Plot the original light curve and the result of the smoothing?

plotlab = string
vertical axis label for plot

clobber = boolean (optional)
Overwrite the output file? if clobber = no and an existing file has the same name as outfile then the task will stop with an error.

verbose = boolean (optional)
Print informative messages and warnings to the shell and logfile?

logfile = string (optional)
Name of the logfile containing error and warning messages.

status = integer
Exit status of the script. It will be non-zero if the task halted with an error. This parameter is set by the task and should not be modified by the user.

DESCRIPTION
kepsmooth smooths Kepler light curve data by convolution with a choice of analytical functions. The smoothed data is copied to a new FITS file with the same structure as the input file.

EXAMPLE

  • kepsmooth infile=kplr005110407-2009259160929_llc.fits outfile=kplr005110407-2009259160929-smooth.fits datacol=SAP_FLUX function=hanning cutoff=1.0 plot=y plotlab='e$^-$ s$^{-1}$' clobber=yes

TIME REQUIREMENTS
Completion upon one target pixel file using a 2.66 GHz Intel Core 2 i7 Mac running OS 10.6.7, takes a few seconds in addition to the manual input required by the tool.

BUGS AND LIMITATIONS
Statistical uncertainties are not propagated through the convolution. The Kepler PyRAF package is privately-developed software made available to the community through the contributed software page of the Kepler astrophysics program at http://keplergo.arc.nasa.gov/ContributedSoftware.shtml. It is not an official software product of the Kepler mission or NASA. Bugs and errors are not the responsibility of the Kepler Team or NASA. Please send bug reports and suggestions to keplergo@mail.arc.nasa.gov.

HISTORY

Date
Version
Description
2011-06-25
1.0.0
Initial software release (MS)
2011-07-03
1.0.1
Updated for Kepler FITS v2.0 (MS)
2011-09-21
1.0.2
The plot axes can now be re-sized using the menu accessible from the plotting window (MS)
2012-03-27
2.0.0
Code can now be run from the command line (TB)
2012-06-07
2.0.1
more reliable plot rendering on linux operating systems (MS)
2012-10-23
2.0.2
fscale and plotlab functionality added to shell-mode operation (MS)

SEE ALSO
kepmask, kepextract, keppixseries


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Editor: Martin Still
NASA Official: Jessie Dotson
Last Updated: Jan 11, 2013
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