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XMM-Newton Science Analysis System


colimplot (colimplot-3.13.2) [xmmsas_20080701_1801-8.0.0]

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Parameters

This section documents the parameters recognized by this task (if any).

Parameter	Mand	Type	Default	Constraints
insets	yes	dataset list
List (in order of increasing hardness) of input image sets.
withmask	no	boolean	yes	yes|no
If `yes', the task attempts to access or create a mask, depending on the setting of maskstyle. Parameters greylevel and expandtomask are also enabled by this switch.
maskstyle	no	string	self	self|user
If `self', the task attempts to create the mask by using the input images. If `user', the task looks for the name of the mask image set in the parameter maskset.
maskset	no	dataset	mask.ds
The name of the mask set (usually an exposure map).
greylevel	no	real	0.0	$0.0\le$ greylevel$\le 1.0$
The grey level to paint those areas of the output image that fall outside the mask. Where the background level of the image is visible, the default value (= black) is preferable; however, in the case that large areas of the image fall outside the mask (but see also the parameter expandtomask), a value of 1.0 may be better, if only to save ink on printed output.
expandtomask	no	boolean	yes	yes|no
When set, that part of the image where the mask is true is expanded until it just fits into the frame. This is to prevent large areas of non-mask and therefore blank image from being displayed.
rebinimage	no	boolean	no	yes|no
Rebin the image to the specifications dictated by the parameters dividexby and divideyby or newnxbins and newnybins.
rebinstyle	no	string	tonumber	tonumber|divideby
This parameter controls the style in which the image rebinning occurs. If `tonumber', the parameters newnxbins and newnybins are read; if `divideby', the parameters dividexby and divideyby are read.
dividexby	no	real	5.0	$1.0\le$ dividexby$\le 50.0$
Divide the number of x pixels by this value, and convert to integer; the result is the number of x pixels in the rebinned image.
divideyby	no	real	5.0	$1.0\le$ divideyby$\le 50.0$
Divide the number of y pixels by this value, and convert to integer; the result is the number of y pixels in the rebinned image.
newnxbins	no	integer	100	$10\le$ newnxbins$\le 1000$
The number of x pixels in the rebinned image.
newnybins	no	integer	100	$10\le$ newnybins$\le 1000$
The number of y pixels in the rebinned image.
negremovalstyle	no	string	truncate	truncate|offset
If negative values are detected in any of the input images, the task removes them by whichever of these two methods is specified.
refclrstyle	no	string	internal	internal|bb|none|user
Dictates the style in which the reference multiplet is calculated.
internalrefstyle	no	string	rms	rms|mean
If refclrstyle=`internal', this is read, and controls whether the reference multiplet is calculated from the root mean squared (rms) or the mean of all pixels which have a total flux above the cutoff value (see parameter cutoff).
cutoff	no	real	0.05	$0.0\le$ cutoff$\le 1.0$
Pixels which have a total flux which is less than cutoff times the maximum total flux are not included in calculations of the reference multiplet. The purpose of this is to prevent such calculations being skewed by background values, which usually dominate an image in terms of numbers of pixels involved.
bbrefstyle	no	string	kev	kev|angstroms|kelvin
For refclrstyle=`bb', the value of the reference multiplet is set to the image multiplet that would have been observed from a black-body source with a given temperature. The different values possible to bbrefstyle just allow the user some flexibility in entering the temperature. For bbrefstyle=`kelvin' the temperature is entered directly in millions of degrees kelvin; for bbrefstyle=`kev' the peak of the BB curve is given in keV; whereas for bbrefstyle=`angstroms' the peak is given in angstroms. Note that these peak values refer to the peak of the BB spectrum as a function of energy or frequency, rather than wavelength.
whitekev	no	real	2.0	$0.01\le$ whitekev$\le 20.0$
Enabled if refclrstyle=`bb' and bbrefstyle=`kev'. It is the energy of a photon at the peak of the reference black body spectrum.
whiteangstroms	no	real	100.0	$0.01\le$ whiteangstroms$\le 8000.0$
Enabled if refclrstyle=`bb' and bbrefstyle=`angstroms'. It is the wavelength of a photon at the peak of the reference black body spectrum.
whitemegakelvin	no	real	1.0	$0.01\le$ whitemegakelvin$\le 100.0$
Enabled if refclrstyle=`bb' and bbrefstyle=`kelvin'. It is the temperature of the reference black body spectrum.
refclr	no	real list		$>0$
List of 3 RGB weights to use for reference colour.
weirdness	no	real	-0.7	$-1.0\le$ weirdness$\le 1.0$
This parameter exerts control over the colour values of the plot. Values of weirdness that approach -1 give output colours in the so-called `thermal' sequence, ie that are similar to those acquired by heated black bodies; values that approach 1 give highly non-thermal colours such as greens and violets.
heat	no	real	0.0	$-1.0\le$ heat$\le 1.0$
This parameter exerts control over the colour values of the plot. Smaller values of heat make all the pixels `cooler' in the thermal sequence of colours (ie redder); larger values in contrast `heat up' the colour values, ie make them bluer.
heatspread	no	real	0.3	$-1.0\le$ heatspread$\le 1.0$
This parameter exerts control over the colour values of the plot. Smaller values of heatspread pull all the pixels in towards white, larger values spread them out more along the thermal sequence of colours.
rgbsysstyle	no	string	polar	cartesian|polar
This parameter controls whether the colour points are described in a RGB basis or in a brightness-saturation-hue basis when an 8-bit colour palette is shared out.
gainstyle	no	string	auto	user|auto
If `user', a value of gain can be entered directly via the parameter usergain. If gainstyle=`auto', the task attempts to calculate it such that the background is just bright enough to be visible.
usergain	no	real	8.0	$0.0<$ usergain
The value by which the net flux values should be multiplied before display.
pixelfraction	no	real	0.5	$0.0<$ pixelfraction$\le 1.0$
For gainstyle=`auto', the task calculates the gain required to bring the maximum net flux fraction of the dimmest pixelfraction pixels to the value of tofluxfraction.
tofluxfraction	no	real	0.4	$0.0<$ tofluxfraction$\le 1.0$
For gainstyle=`auto', the task calculates the gain required to bring the maximum net flux fraction of the dimmest pixelfraction pixels to the value of tofluxfraction.
nhotpixels	no	integer	10	$0\le$ nhotpixels
The image brightness is scaled so as to saturate the nhotpixels brightest pixels.
pgdev	no	string	/cps
The pgplot device name.
plotfile	no	string	test.ps
If the pgplot device is one that requires an output file, this gives the name of the file.
withframe	no	boolean	no	yes|no
If pgdev=`/ppm' and withframe=`yes', the task constructs a frame plot around the image, containing various pieces of information such as the name of the observer and the target. This is written to a .gif file named frame.gif, which can be combined with the output image by colimchain.
Parameter	Mand	Type	Default	Constraints