If TRUE, then the spatial positions of the input data are aligned in the co-ordinate system specified by parameter SYSTEM. Otherwise, they are aligned in the ICRS co-ordinate system. For instance, if the output co-ordinate system is AZEL, then setting ALIGNSYS to TRUE will result in the AZEL values of the input data positions being compared directly, disregarding the fact that a given AZEL will correspond to different positions on the sky at different times. [FALSE]

Only accessed if a null value is supplied for parameter REF. Determines how the dynamic default values should be determined for the projection parameters CROTA, PIXSIZE, REFLAT, REFLON, REFPIX1 and REFPIX2. If TRUE, then default projection parameters are determined by adjusting the grid until as many data samples as possible fall close to the centre of pixels in the output cube. If FALSE, REFLON/REFLAT are set to the first pointing BASE position, CROTA is set to minus the MAP_PA value in the FITS header (converted to the requested sky co-ordinate system), PIXSIZE is set to 6 arcseconds, and REFPIX1/REFPIX2 are both set to zero. [FALSE]

Controls the precise placement of the spatial tangent point on the first pixel axis of the output cube. The position of the tangent point on the sky is specified by REFLON/REFLAT, and this sky position is placed at grid coordinates specified by REFPIX1/REFPIX2. Note, these grid coordinates refer to an interim grid coordinate system that does not depend on the values supplied for LBND, rather than the final grid coordinate system of the output cube. Therefore, if values are supplied for REFPIX1/REFPIX2, they should be copies of the values written to output parameter PIXREF by a previous run of MAKECUBE. The REFPIX and PIXREF parameters allow an initial run of MAKECUBE with AUTOGRID=YES to generate projection parameters that can then be re-used in subsequent runs of MAKECUBE with AUTOGRID=NO in order to force MAKECUBE to use the same pixel grid. If a null (!) value is supplied, default values will be used for REFPIX1/2 - either the autogrid values (if AUTOGRID=YES) or (0,0) (if AUTOGRID=NO). [!]

Controls the precise placement of the spatial tangent point on the second pixel axis of the output cube. See REFPIX1. [!]

A string determining the way in which bad pixels are propagated from input to output. The " AND" scheme uses all input data (thus reducing the noise in the output) and also minimises the number of bad pixels in the output. However, the memory requirements of the " AND" scheme can be excessive. For this reason, two other schemes, " FIRST" and " OR" , are provided which greatly reduce the memory requirements, at the expense either of introducing more bad pixels into the output (" OR" ) or producing higher output noise levels (" FIRST" ). The value supplied for this parameter is used only if SPREAD is set to " Nearest" (otherwise " AND" is always used):

• " FIRST" – The bad-pixel mask in each output spectrum is inherited from the first input spectrum that contributes to the output spectrum. Any subsequent input spectra that contribute to the same output spectrum but which have a different bad-pixel mask are ignored. So an output pixel will be bad if and only if the corresponding pixel in the first input NDF that contributes to it is bad. Since this scheme ignores entire input spectra if they do not conform to the expected bad-pixel mask, the noise in the output can be higher than using the other schemes. However, this scheme has the benefit of using much less memory than the " AND" scheme, and will in general produce fewer bad pixels in the output than the " OR" scheme.

• " OR" – The bad pixel mask in each output spectrum is the union (logical OR) of the bad pixel masks for all input spectra that contribute to the output spectrum. So an output pixel will be bad if any of the input pixels that contribute to it are bad. This scheme will in general produce more bad output pixels than the " FIRST" scheme, but the non-bad output pixels will have a lower noise because, unlike " FIRST" , all the contributing input data are coadded to produce the good output pixels. Like " FIRST" , this scheme uses much less memory than " AND" .

• " AND" – The bad pixel mask for each output spectrum is the intersection (logical AND) of the bad pixel masks for all input spectra that contribute to the output spectrum. So an output pixel will be bad only if all the input pixels that contribute to it are bad. This scheme will produce fewer bad output pixels and will also give lower output noise levels than " FIRST" or " OR" , but at the expense of much greater memory requirements.

[" OR" ]

A string determining the co-ordinate Frame in which positions are to be stored in the output catalogue associated with parameter OUTCAT. The string supplied for CATFRAME can be one of the following:

• A Domain name such as SKY, AXIS, PIXEL, etc.

• An integer value giving the index of the required Frame.

• An IRAS90 Sky Co-ordinate System (SCS) values such as EQUAT(J2000) (see SUN/163).

If a null (!) value is supplied, the positions will be stored in the current Frame of the output NDF. [!]

The epoch at which the sky positions stored in the output catalogue were determined. It will only be accessed if an epoch value is needed to qualify the co-ordinate Frame specified by COLFRAME. If required, it should be given as a decimal years value, with or without decimal places (" 1996.8" for example). Such values are interpreted as a Besselian epoch if less than 1984.0 and as a Julian epoch otherwise.

Only accessed if a null value is supplied for parameter REF. The angle, in degrees, from the second pixel axis in the output cube to north (in the co-ordinate system specified by the SYSTEM parameter), measured north through east. The dynamic default value is determined by the AUTOGRID parameter. []

A group of detector names to include in, or exclude from, the output cube. If the first name starts with a minus sign, then the specified detectors are excluded from the output cube (all other detectors are included). Otherwise, the specified detectors are included in the output cube (all other detectors are excluded). If a null (!) value is supplied, data from all detectors will be used. [!]

A group of names specifying extra columns to be added to the catalogue specified by parameter OUTCAT. Each name should be the name of a component in the JCMTState extension structure. For each name in the group, an extra column is added to the output catalogue containing the value of the named extension item for every table row (i.e. for each data sample). These extra columns can be viewed and manipulated with general-purpose FITS table tools such as TOPCAT, but will not be displayed by the KAPPA:LISTSHOW command. One use for these extra columns is to allow the catalogue to be filtered (e.g. by TOPCAT) to remove samples that meet (or do not meet) some specified requirement specified by the JCMTState contents. No extra columns are added if a null (!) value is supplied. [!]

Sky co-ordinates (radians) of the bottom-left corner of the output cube (the corner with the smallest PIXEL dimension for Axis 1 and the smallest pixel dimension for Axis 2). No check is made that the pixel corresponds to valid data. Note that the position is reported for the centre of the pixel. If SPARSE mode is enabled the positions reported will not be reliable.

Sky co-ordinates (radians) of the bottom right corner of the output cube (the corner with the largest PIXEL dimension for Axis 1 and the smallest pixel dimension for Axis 2). No check is made that the pixel corresponds to valid data. Note that the position is reported for the centre of the pixel. If SPARSE mode is enabled the positions reported will not be reliable.

The lower bounds of the bounding box enclosing the output cube in the selected output WCS Frame. The values are calculated even if no output cube is created. Celestial axis values will be in units of radians, spectral-axis units will be in the same units as the input frameset (matching those used in the SPECBOUNDS parameter). The parameter is named to be consistent with KAPPA:NDFTRACE output. Note, the stored values correspond to the outer edges of the first pixel, not to the pixel centre.

The upper bounds of the bounding box enclosing the output cube in the selected output WCS Frame. The values are calculated even if no output cube is created. Celestial axis values will be in units of radians, spectral-axis units will be in the same units of the input frameset (matching those used in the SPECBOUNDS parameter). The parameter is named to be consistent with KAPPA:NDFTRACE output. Note, the stored values correspond to the outer edges of the first pixel, not to the pixel centre.

Sky co-ordinates (radians) of the top left corner of the output cube (the corner with the smallest PIXEL dimension for Axis 1 and the largest pixel dimension for Axis 2). No check is made that the pixel corresponds to valid data. Note that the position is reported for the centre of the pixel. If SPARSE mode is enabled the positions reported will not be reliable.

Sky co-ordinates (radians) of the top right corner of the output cube (the corner with the largest PIXEL dimension for Axis 1 and the largest pixel dimension for Axis 2). No check is made that the pixel corresponds to valid data. Note that the position is reported for the centre of the pixel. If SPARSE mode is enabled the positions reported will not be reliable.

Indicates how the Variance values in the output NDF are to be calculated. It can take any of the following values:

• " Spread" – the output Variance values are based on the spread of input data values contributing to each output pixel. This option is not available if parameter SPARSE is set TRUE. If the BADMASK value is " OR" or " FIRST" , then a single variance value will be produced for each output spectrum (i.e. all channels in an output spectrum will have the same variance value). If BADMASK is " AND" , then an independent variance value will be calculated for each channel in each output spectrum.

• " Tsys" – the output Variance values are based on the system noise temperature values supplied in the input NDFs. Since each input spectrum is characterised by a single Tsys value, each output spectrum will have a constant Variance value (i.e. all channels in an output spectrum will have the same variance value).

• " None" – no output Variance values are created.

[" Tsys" ]

Input raw data file(s)

Indicates if the input spectra should be weighted when combining two or more input spectra together to form an output spectrum. If TRUE, the weights used are the reciprocal of the variances associated with the input spectra, as determined from the Tsys values in the input. [TRUE]

If TRUE, the output cube is created on the JSA all-sky pixel grid, and is split up into individual JSA tiles. Thus multiple output NDFs may be created, one for each JSA tile that touches the cube. Each of these output NDFs will have the tile index number appended to the end of the path specified by parameter " OUT" . If " JSATILES" is TRUE, the " REF" parameter is ignored. [FALSE]

If parameter " JSATILES" is set TRUE, the zero-based indices of the created JSA tiles will be written to this output parameter. The number of such indices is given the " NTILE" parameter

An array of values giving the lower pixel-index bound on each spatial axis of the output NDF. The suggested default values encompass all the input spatial information. The supplied bounds may be modified if the parameter TRIM takes its default value of TRUE. []

The lower pixel bounds of the output NDF. Note, values will be written to this output parameter even if a null value is supplied for parameter OUT.

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

The number of output tiles used to hold the entire output array (see parameter JSATILES and TILEDIMS). If no input data falls within a specified tile, then no output NDF will be created for the tile, but (if JSATILES is FALSE) the tile will still be included in the tile numbering scheme.

The number of polarisation angle bins used to hold the entire output data (see parameter POLBINSIZE).

Output file. If a null (!) value is supplied, the application will terminate early without creating an output cube, but without reporting an error. Note, the pixel bounds which the output cube would have had will still be written to output parameters LBOUND and UBOUND, even if a null value is supplied for OUT. If the output cube is split up into multiple output NDFs (e.g. an NDF for each tile – see parameter TILEDIMS – or for each polarisation angle bin – see parameter POLBINSIZE), then the value supplied for " OUT" will be used as the root name to which other strings are appended to create the name of each output NDF.

An output catalogue in which to store all the spatial detector positions used to make the output cube (i.e. those selected using the DETECTORS parameter). By default, the stored positions are in the same sky co-ordinate system as the current Frame in the output NDF (but see parameter CATFRAME). The label associated with each row in the catalogue is the detector name. The detector positions in the catalogue are ordered as follows: all the positions for the first input NDF come first, followed by those for the second input NDF, etc. Within the group of positions associated with a single input NDF, the positions for the first time slice come first, followed by the positions for the second time slice, etc. If a null value (!) is supplied, no output catalogue is produced. See also parameter CATFRAME. [!]

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

An optional array which consists of additional parameters required by the Sinc, SincSinc, SincCos, SincGauss, Somb, SombCos, and Gauss spreading methods (see parameter SPREAD).

PARAMS( 1 ) is required by all the above schemes. It is used to specify how many pixels on either side of the output position (that is, the output position corresponding to the centre of the input pixel) are to receive contributions from the input pixel. Typically, a value of 2 is appropriate and the minimum allowed value is 1 (i.e. one pixel on each side). A value of zero or fewer indicates that a suitable number of pixels should be calculated automatically. [0]

PARAMS( 2 ) is required only by the SombCos, Gauss, SincSinc, SincCos, and SincGauss schemes. For the SombCos, SincSinc, and SincCos schemes, it specifies the number of pixels at which the envelope of the function goes to zero. The minimum value is 1.0, and the run-time default value is 2.0. For the Gauss and SincGauss scheme, it specifies the full-width at half-maximum (FWHM) of the Gaussian envelope. The minimum value is 0.1, and the run-time default is 1.0. On astronomical images and spectra, good results are often obtained by approximately matching the FWHM of the envelope function, given by PARAMS(2), to the point-spread function of the input data. []

The grid coordinates used for the reference pixel, within the interim grid coordinate system. See REFPIX1.

Only accessed if a null value is supplied for parameter REF. Pixel dimensions in the output image, in arcseconds. If only one value is supplied, the same value will be used for both axes. The dynamic default value is determined by the AUTOGRID parameter. []

The name of a text file containing corrections to the pointing read from the input data files. If null (!) is supplied, no corrections are used. Note - this parameter is ignored unless parameter USEDETPOS is set to FALSE. If a file is supplied, it should start with one or more lines containing " #" in column one. These are comment lines, but if any comment line has the form " # SYSTEM=AZEL" or " # SYSTEM=TRACKING" then it determines the system in which the pointing correction are specified (SYSTEM defaults to AZEL). The last comment line should be a space-separated list of column names, including " TAI" , " DLON" and " DLAT" . Each remaining line should contain numerical values for each column, separated by white space. The TAI column should contain the TAI time given as an MJD. The DLON and DLAT columns should give arc-distance offsets parallel to the longitude and latitude axes, in arc-seconds. The TAI values should be monotonic increasing with row number. The longitude and latitude axes are either AZEL or TRACKING as determined by the SYSTEM value in the header comments. Blank lines are ignored. The DLON and DLAT values are added onto the SMU jiggle positions stored in the JCMTSTATE extension of the input NDFs. DLON and DLAT values for non-tabulated times are determined by interpolation.

If you need to apply two sets of pointing corrections, one in TRACKING and one in AZEL, you can include two tables (one for each system) in a single text file. Both tables should use the format described above. The two tables must be separated by a line containing two or more minus signs with no leading spaces. [!]

This parameter is only prompted for if the input files contain polarisation data. The supplied value is used as the bin size (in degrees) for grouping polarisation analyser angles. The first bin is centred at the angle given by parameter POLBINZERO. The " analyser angle" is the anti-clockwise angle from celestial north (in the system chosen by parameter SYSTEM) to the axis of the " effective analyser" - a rotating analyser that would have the same effect as the combination of fixed analyser and half-wave plate actually present in the polarimeter. The supplied value for POLBINSIZE will be modified if required to ensure that a whole number of bins is used to cover the complete range of analyser angles (0 to 360 degrees). A separate output cube will be created for each bin that is not empty, and each output NDF will contain a POLPACK extension suitable for use with the POLPACK:POLCAL command. These NDFs are all stored in a single HDS container file (one per tile) with the name specified by parameter OUT. Within this container file, each cube will be held in a component with name of the form " P$<$N$>$" appended to the end, where "$<$N$>$" is an integer bin index. The largest value of N is written to output parameter NPOLBIN. If a null value (!) is supplied, then a single output NDF (without POLPACK extension) is created for each tile, containing all input data.

This parameter is only prompted for if the input files contain polarisation data. It is the analyser angle (in degrees) at the centre of the first analyser angle bin. A value of zero corresponds to north in the celestial co-ordinate system specified by parameter SYSTEM. [0]

If a true value is supplied, then an error is reported and the application terminates if a significant difference is found between the detector positions array (RECEPPOS) and positions implied by the FPLANEX/Y arrays. If a false value is supplied, a warning is issued but the application proceeds. See also parameters POSERRMAX and USEDETPOS. [FALSE]

Defines the maximum insignificant discrepancy between the detector positions array (RECEPPOS) and positions implied by the FPLANEX/Y arrays, in units of arc-seconds. See parameter POSERRFATAL. [3.0]

An existing NDF that is to be used to define the output grid, or the string " JSA" . If an NDF is supplied, the output grid will be aligned with the supplied reference NDF. The NDF need not be three-dimensional. For instance, a two-dimensional image can be supplied in which case the spatial axes of the output cube will be aligned with the reference image and the spectral axis will be inherited form the first input NDF. If " JSA" is supplied, the JSA all-sky pixel grid will be used (note, the cube will still be created as a single NDF - if multiple NDFs, one for each JSA tile, are required, the " JSATILES" parameter should beset TRUE instead of using the " REF" parameter). If a null (!) value is supplied then the output grid is determined by parameters AUTOGRID, REFLON, REFLAT, etc. [!]

Only accessed if a null value is supplied for parameter REF. The formatted celestial-latitude value at the tangent point of the spatial projection in the output cube. This should be provided in the system specified by parameter SYSTEM. The dynamic-default value is determined by the AUTOGRID parameter. []

Only accessed if a null value is supplied for parameter REF. The formatted celestial-longitude value at the tangent point of the spatial projection in the output cube. This should be provided in the system specified by parameter SYSTEM. The dynamic-default value is determined by the AUTOGRID parameter. []

Indicates if the spectra in the output cube should be stored as a sparse array, or as a regularly gridded array. If FALSE, pixel Axes 1 and 2 of the output cube represent a regularly gridded tangent plane projection of the sky, with parameters determined by CROTA, PIXSIZE, REFLON and REFLAT. Each input spectrum is placed at the appropriate pixel position in this three-dimensional projection, as given by the celestial co-ordinates associated with the spectrum. If SPARSE is TRUE, then each input spectrum is given an associated index, starting from 1, and the spectrum with index " I" is stored at pixel position (I,1) in the output cube (pixel Axis 2 will always have the value 1 – that is, Axis 2 is a degenerate axis that spans only a single pixel).

In both cases, the third pixel axis in the output cube corresponds to spectral position (frequency, velocity, etc).

Whatever the setting of SPARSE, the output NDF’ s WCS component can be used to transform pixel position into the corresponding (celestial longitude, celestial latitude, spectral position) values. However, if SPARSE is TRUE, then the inverse transformation (i.e. from (long,lat,spec) to pixel co-ordinates) will not be defined. This means, for instance, that if a sparse array is displayed as a two-dimensional image, then it will not be possible to annotate the axes with WCS values. Also, whilst KAPPA:WCSMOSAIC will succesfully align the data in a sparse array with a regularly gridded cube, KAPPA:WCSALIGN will not, since WCSALIGN needs the inverse transformation to be defined.

The dynamic default value for SPARSE depends on the value supplied for parameter AUTOGRID. If AUTOGRID is set FALSE, then SPARSE defaults to FALSE. If AUTOGRID is set TRUE, then the default for SPARSE will be TRUE if the algorithm described under the AUTOGRID parameter fails to find useful default grid parameters. If the AUTOGRID algorithm succeeds, the default for SPARSE will be FALSE. []

The bounds of the output cube on the spectral axis. Input data that falls outside the supplied range will not be included in the output cube. The supplied parameter value should be a string containing a pair of axis values separated by white space or commas. The first should be the spectral value corresponding to the lower edge of the first spectral channel in the output cube, and the second should be the spectral value corresponding to the upper edge of the last spectral channel. The supplied values should refer to the spectral system described by the WCS FrameSet of the first input NDF. To see what this is, supply a single colon (" :" ) for the parameter value. This will display a description of the required spectral co-ordinate system, and then re-prompt for a new parameter value. The dynamic default is determined by the SPECUNION parameter. []

Determines how the default spectral bounds for the output are chosen. If a TRUE value is supplied, then the defaults for the SPECBOUNDS parameter represent the union of the spectral ranges in the input data. Otherwise, they represent the intersection of the spectral ranges in the input data. This option is only available if parameter BADMASK is set to AND. For any other value of BADMASK, a value of FALSE is always used for SPECUNION. [FALSE]

The method to use when spreading each input pixel value out between a group of neighbouring output pixels. If SPARSE is set TRUE, then SPREAD is not accessed and a value of " Nearest" is always assumed. SPREAD can take the following values:

• " Linear" – The input pixel value is divided bi-linearly between the four nearest output pixels. Produces smoother output NDFs than the nearest-neighbour scheme.

• " Nearest" – The input pixel value is assigned completely to the single nearest output pixel. This scheme is much faster than any of the others.

• " Sinc" – Uses the sinc(pi$\ast$x) kernel, where x is the pixel offset from the interpolation point (resampling) or transformed input pixel centre (rebinning), and sinc(z)=sin(z)/z. Use of this scheme is not recommended.

• " SincSinc" – Uses the sinc(pi$\ast$x)sinc(k$\ast$pi$\ast$x) kernel. A valuable general-purpose scheme, intermediate in its visual effect on NDFs between the bi-linear and nearest-neighbour schemes.

• " SincCos" – Uses the sinc(pi$\ast$x)cos(k$\ast$pi$\ast$x) kernel. Gives similar results to the " Sincsinc" scheme.

• " SincGauss" – Uses the sinc(pi$\ast$x)exp(-k$\ast$x$\ast$x) kernel. Good results can be obtained by matching the FWHM of the envelope function to the point-spread function of the input data (see parameter PARAMS).

• " Somb" – Uses the somb(pi$\ast$x) kernel, where x is the pixel offset from the transformed input pixel centre, and somb(z)=2$\ast$J1(z)/z (J1 is the first-order Bessel function of the first kind). This scheme is similar to the " Sinc" scheme.

• " SombCos" – Uses the somb(pi$\ast$x)cos(k$\ast$pi$\ast$x) kernel. This scheme is similar to the " SincCos" scheme.

• " Gauss" – Uses the exp(-k$\ast$x$\ast$x) kernel. The FWHM of the Gaussian is given by parameter PARAMS(2), and the point at which to truncate the Gaussian to zero is given by parameter PARAMS(1).

For further details of these schemes, see the descriptions of routine AST_REBINx in SUN/211. [" Nearest" ]

The celestial co-ordinate system for the output cube. One of ICRS, GAPPT, FK5, FK4, FK4-NO-E, AZEL, GALACTIC, ECLIPTIC. It can also be given the value " TRACKING" , in which case the system used will be which ever system was used as the tracking system during in the observation. The value supplied for the CROTA parameter should refer to the co-ordinate system specified by this parameter.

The choice of system also determines if the telescope is considered to be tracking a moving object such as a planet or asteroid. If system is GAPPT or AZEL, then each time slice in the input data will be shifted in order to put the base telescope position (given by TCS_AZ_BC1/2 in the JCMTSTATE extension of the input NDF) at the same pixel position that it had for the first time slice. For any other system, no such shifts are applied, even if the base telescope position is changing through the observation. [TRACKING]

Maximum separation between the actual position (TCS_TR_AC1/2) and demand position (TCS_TR_DC1/2) in the JCMTSTATE extension (arcsec). If non-zero, time slices which exceed this separation will be excluded. [0.0]

Only accessed if a non-null value is supplied for parameter TILEDIMS. It gives the width, in pixels, of a border to add to each output tile. These borders contain data from the adjacent tile. This results in an overlap between adjacent tiles equal to twice the supplied border width. If the default value of zero is accepted, then output tiles will abut each other in pixel space without any overlap. If a non-zero value is supplied, then each pair of adjacent tiles will overlap by twice the given number of pixels. Pixels within the overlap border will be given a quality name of " BORDER" (see KAPPA:SHOWQUAL). [0]

This parameter is ignored if parameter " JSATILES" is set TRUE.

For large data sets, it may sometimes be beneficial to break the output array up into a number of smaller rectangular tiles, each created separately and stored in a separate output NDF. This can be accomplished by supplying non-null values for the TILEDIMS parameter. If supplied, these values give the nominal spatial size of each output tile, in pixels. Edge tiles may be thinner if the TRIMTILES parameter is set TRUE. In order to avoid creating very thin tiles around the edges, the actual tile size used for the edge tiles may be up to 10 % larger than the supplied value. This creation of " fat" edge tiles may be prevented by supplying a negative value for the tile size, in which case edge tiles will never be wider than the supplied absolute value.

If only one value is supplied, the supplied value is duplicated to create square tiles. Tiles are created in a raster fashion, from bottom left to top right of the spatial extent. The NDF file name specified by " out" is modified for each tile by appending " _$<$N$>$" to the end of it, where $<$N$>$ is the integer tile index (starting at 1). The number of tiles used to cover the entire output cube is written to output parameter NTILES. The tiles all share the same projection and so can be simply pasted together in pixel co-ordinates to reconstruct the full size output array. The tiles are centred so that the reference position (given by REFLON and REFLAT) falls at the centre of a tile. If a tile receives no input data, then no corresponding output NDF is created, but the tile is still included in the tile numbering scheme. If a null (!) value is supplied for TILEDIMS, then the entire output array is created as a single tile and stored in a single output NDF with the name given by parameter OUT (without any " _$<$N$>$" appendage). [!]

If TRUE, then the output cube will be trimmed to exclude any borders filled with bad values. Such borders can be caused, for instance, by one or more detectors having been excluded (see parameter DETECTORS), or by the supplied LBND and/or UBND parameter values extending beyond the available data. [TRUE]

Only accessed if the output is being split up into more than one spatial tile (see parameter TILEDIMS and JSATILES). If TRUE, then the tiles around the border will be trimmed to exclude areas that fall outside the bounds of the full sized output array. This will result in the border tiles being smaller than the central tiles. [FALSE]

An array of values giving the upper pixel-index bound on each spatial axis of the output NDF. The suggested default values encompass all the input spatial information. The supplied bounds may be modified if the parameter TRIM takes its default value of TRUE. []

The upper pixel bounds of the output NDF. Note, values will be written to this output parameter even if a null value is supplied for parameter OUT.

If a true value is supplied, then the detector positions are read from the detector position arrays in each input NDF. Otherwise, the detector positions are calculated on the basis of the FPLANEX/Y arrays. Both methods should (in the absence of bugs) result in identical cubes. See also parameter POSERRFATAL. [TRUE]

If TRUE, then the weights associated with the array of output pixels are stored in an extension named ACSISRED, within the output NDF. If FALSE the weights are discarded once they have been used. These weights record the relative weight of the input data associated with each output pixel. If SPARSE is set TRUE, then WEIGHTS is not accessed and a FALSE value is assumed. [FALSE]