Specifies values for the cleaning parameters. If the string " def" (case-insensitive) is supplied, a set of default configuration parameter values will be used. CONFIG=! disables all cleaning and simply applies apodisation. This is generally not a recommended use of calcnoise.

The supplied value should be either a comma-separated list of strings or the name of a text file preceded by an up-arrow character "$$^" , containing one or more comma-separated lists of strings. Each string is either a " keyword=value" setting, or the name of a text file preceded by an up-arrow character " $$^" . Such text files should contain further comma-separated lists which will be read and interpreted in the same manner (any blank lines or lines beginning with " #" are ignored). Within a text file, newlines can be used as delimiters, as well as commas. Settings are applied in the order in which they occur within the list, with later settings over-riding any earlier settings given for the same keyword.

Each individual setting should be of the form:

$<$keyword$>$=$<$value$>$

The available parameters are identical to the cleaning parameters used by the iterative map-maker (method=ITER) and are are described in the " Configuration Parameters" appendix of SUN/258. Default values will be used for any unspecified parameters. Assigning the value " $<$def$>$" (case insensitive) to a keyword has the effect of resetting it to its default value. Options available to the map-maker but not understood by CALCNOISE will be ignored. Parameters not understood will trigger an error. Use the " cleandk." namespace for configuring cleaning parameters for the dark squids.

If a null value (!) is given all cleaning will be disabled and the full time series will be apodized with no padding. This differs to the behaviour of SC2CLEAN where the defaults will be read and used. [current value]

The effective noise of the .MORE.SMURF.NEP image. See the EFFNOISE parameter for details of how it is calculated.

The effective noise of the primary output image. If this command was run on raw data it will be the current noise and if run on flatfielded data it will be the effective NEP. Calculated as the sqrt of 1/sum(1/sigma$$^2). See also the EFFNEP parameter.

Method to use to calculate the flatfield solution. Options are POLYNOMIAL and TABLE. Polynomial fits a polynomial to the measured signal. Table uses an interpolation scheme between the measurements to determine the power. [POLYNOMIAL]

The order of polynomial to use when choosing POLYNOMIAL method. [1]

Signal-to-noise ratio threshold to use when filtering the responsivity data to determine valid bolometers for the flatfield. [3.0]

If true the previous and following flatfield will be used to determine the overall flatfield to apply to a sequence. If false only the previous flatfield will be used. A null default will use both flatfields for data when we did not heater track at the end, and will use a single flatfield when we did heater track. The parameter value is not sticky and will revert to the default unless explicitly over-ridden. [!]

Frequency to use when determining noise ratio image. The noise ratio image is determined by dividing the power at this frequency by the white noise [0.5]

Frequency range (Hz) to use to calculate the white noise [2,10]

Input files to be transformed. Files from the same sequence will be combined.

Control the verbosity of the application. Values can be NONE (no messages), QUIET (minimal messages), NORMAL, VERBOSE, DEBUG or ALL. [NORMAL]

Flag NEP values this number of standard deviations above the median. If a null (!) value is supplied now high-outlier clipping. [!]

Flag NEP values this number of standard deviations below the median. If a null (!) value is supplied now low-outlier clipping. [3]

Clip based on the log of the NEP. [TRUE]

The number of bolometers with good NEP measurements (see EFFNEP)

Flag NOISE values this number of standard deviations above the median. If a null (!) value is supplied now high-outlier clipping. [!]

Flag NOISE values this number of standard deviations below the median. If a null (!) value is supplied now low-outlier clipping. [3]

Clip based on the log of the NOISE. [TRUE]

The number of bolometers with good NOISE measurements (see EFFNOISE)

Output files (either noise or NEP images depending on the NEP parameter). Number of output files may differ from the number of input files. These will be 2 dimensional.

The name of text file to create, in which to put the names of all the output NDFs created by this application (one per line) from the OUT parameter. If a null (!) value is supplied no file is created. [!]

Output files to contain the power spectra for each processed chunk. There will be the same number of output files as created for the OUT parameter. If a null (!) value is supplied no files will be created. [!]

A group expression containing the resistor settings for each bolometer. Usually specified as a text file using " $$^" syntax. An example can be found in $STARLINK_DIR/share/smurf/resist.cfg [$STARLINK_DIR/share/smurf/resist.cfg]

If true, responsivity data will be used to mask bolometer data when calculating the flatfield. [TRUE]

Output files to contain the cleaned time-series for each processed chunk. There will be the same number of output files as created for the OUT parameter. If a null (!) value is supplied no files will be created. [!]