Description:
Calculate the areas of the output map that will be affected by points in the input
data array. This is used to generate a mask so that the rebinned output map only contains
data points close to input data. Similar to SCULIB_WTFN_REGRID_1.
Invocation
CALL
SCULIB_SPLINE_REGRID_1 (DIAMETER, WAVELENGTH, IN_DATA, X, Y, NPIX, PIXSPACE, NI, NJ,
ICEN, JCEN, QUALITY, STATUS)
Arguments
DIAMETER = REAL (Given)
Diameter of
telescope
WAVELENGTH = REAL (Given)
Wavelength of the observation
IN_DATA
(NPIX) = REAL (Given)
The input data values. (Used to define quality)
X( NPIX ) =
REAL (Given)
The x coordinates of the input pixels
Y( NPIX ) = REAL (Given)
The y
coordinates of the input pixels
NPIX = INTEGER (Given)
the number of input pixels
PIXSPACE = DOUBLE PRECISION (Given)
the pixel spacing of the output pixels
NI
= INTEGER (Given)
The number of output pixels in the x direction
NJ = INTEGER
(Given)
The number of output pixels in the y direction
ICEN = INTEGER (Given)
the x
index of the centre of the output array
JCEN = INTEGER (Given)
the y index of the
centre of the output array
SCRATCH (NI, NJ) = UBYTE (Returned)
Quality mask
STATUS = INTEGER (Given and Returned)
The global status.
Copyright
Copyright
©1995,1996,1997,1998,1999 Particle Physics and Astronomy Research Council. All Rights Reserved.