As of Fri Apr 19 2:08:38 2024

SDGRD: Select & grid random-position single-dish measurements


INNAME                             Input UV file name (name)
INCLASS                            Input UV file name (class)
INSEQ             0.0     9999.0   Input UV file name (seq. #)
INDISK            0.0        9.0   Input UV file disk unit #
                                   Cal. info for input:
TIMERANG                           Time range to include
DOCALIB          -1.0        2.0   If >0 calibrate data
GAINUSE                            CS table to apply
FLAGVER                            Flag table version
STOKES                             Stokes' parameter to image.
BIF               0.0              IF (if any) to select
BCHAN             0.0     4096.0   First spectral channel
ECHAN             0.0     4096.0   Last spectral channel
OUTNAME                            Output UV file name (name)
OUTCLASS                           Output UV file name (class)
OUTSEQ            0.0     9999.0   Output UV file name (seq. #)
OUTDISK           0.0        9.0   Output UV file disk unit #.
OPTYPE                             Projection code e.g. '-SIN'
APARM                              1,2,3 = RA (h,m,s)
                                   4,5,6 = Dec (d,m,s)
IMSIZE         32.       4096.     Image size (X,Y) in pixels
CELLSIZE    0.000001     4096.     Cell size in arc seconds
ROTATE                             Rotate image CCW
SHIFT                              (X,Y) image shift in asec
REWEIGHT                           (1) <= 0 -> interp image
                                       =  1 -> convolved image
                                       =  2 -> weight image
                                       =  3 -> 1/sigma**2 image
                                   (2) Min convolved weight
                                       = REWEIGHT(2) *
                                         max(convolved weight)
                                       < 0 => use abs value
XTYPE         -20.         20.     Conv. function type in x
                                     default spheroidal
                                     New round types - SEE HELP
YTYPE         -20.         20.     Conv. function type in y
                                     default spheroidal
XPARM                              Conv. function parms for x
YPARM                              Conv. function parms for y
BADDISK                            Disk drive #'s to avoid


Task:  This task will select random position single-dish data in AIPS uv
       form in a specified field of view about a specified position and
       project the coordinates onto the specified coordinate system.
       Calibration and flagging may be applied during the selection
       process.  It will then convolve the data onto a grid.  If the
       requested image is too large the program will fail.  Use SDIMG
       for such cases.
  INNAME.....Input single-dish data file name (name).
  INCLASS....Input single-dish data file name (class).
  INSEQ......Input single-dish data file name (seq. #).
  INDISK.....Disk drive # of input single-dish data file.
  DOCALIB....If true (>0) then calibrate the data using information in
             the specified CS table.
  GAINUSE....Version number of the CS table to apply to the
             data if DOCALIB=1.  0 = highest numbered.
  FLAGVER....Specifies the version of the flagging table to be
             applied. 0 => highest numbered table.
             <0 => no flagging to be applied.
  STOKES.....Stokes' type of the desired image:
             'I' => I polarization,
             'Q' => Q polarization,
             'U' => U polarization,
             'V' => V polarization,
             'RR' => right circular polarization,
             'LL' => left circular polarization,
             'VV' => vertical linear polarization
             'HH' => horizontal linear polarization
             other => 'I'
  BIF........IF number to grid (only one is done).  0 => 1.
  BCHAN......First spectral channel to grid, 0 => 1.
  ECHAN......Last spectral channel to grid; <BCHAN => max.
  OUTNAME....Output file name (name).  blank => INNAME
  OUTCLASS...Output file name (class).  blank => INCLASS
  OUTSEQ.....Output file name (seq. #). 0 => lowest unique
  OUTDISK....Disk drive # of output UV file.  0 => highest with
             space for the file.
  OPTYPE.....Projection code:
             '-TAN' = tangent projection (optical),
             '-SIN' = sine projection (normal interferometer),
             '-ARC' = arc projection (Schmidt camera, single
                      dish images),
             '-NCP' = North celestial pole (WSRT),
             '-STG' = stereographic projection,
             Those below should have latitude reference value 0.0
             '-AIT' = Aitoff projection, (large field)
             '-GLS' = Global sinusoidal projection (large field)
             '-MER' = Mercator projection (large field)
             '-CAR' = Plate Carree  ("cartesian'")
             '-MOL' = Molweide's (large field)
             '-PAR' = Parabolic (Craster - for large field)
             '    ' => '-SIN'
             See AIPS memo nos. 27 and 46 for more detail and A & A,
             395, 1077-1122 (2002).
  APARM......1,2,3 are the RA as (h,m,s)
             4,5,6 are the Dec, as (d,m,s)
             The specified position is the CENTER of the RA and DEC
             range before the application of the shifts (if any).
             Default: uv data header RA and DEC, or, if they are 0, uv
             data header Observed RA and Dec.  If the data coordinates
             are relative Az-El (i.e. beam switched data), then there is
             no default and 0,0 would be the normal center.
             If APARM(4) is -0 then use APARM(4)=-0.1.
  IMSIZE.....(X,Y) image size in pixels.  Must be even and
             between 32 and 4096.
  CELLSIZE...(X,Y) cell size in arc seconds.
  ROTATE.....Rotate the image CCW by ROTATE degrees.
  SHIFT......Probably wouldn't do what you expect: shifts the reference
             pixel by SHIFT(1)/CELL(1), -SHIFT(2)/CELL(2).  The
             reference value is set by APARM (see above).  For a normal
             Ra-Dec image, if both SHIFTs are > 0, the center of the
             image will be at a higher Ra and higher Dec than the
             reference point.
  REWEIGHT...(1) Selects the kind of output image:
                <= 0 => interpolated image (convolved image
                        divided by a convolved image with the
                        data replaced by 1.0's).
                 = 1 => convolved image of data.
                 = 2 => convolved image with data replaced by 1,
                        i.e an image of the data weights (sum of
                        input data weight * uniform weight
                        correction * convolving function at each
                 = 3 => image of K/sigma**2 for an interpolated
                        image assuming the input weights are
                        K/sigma**2 for the data samples
             (2) Minimum convolved weight (image with data replaced by
                 1.0's) to remain unblanked = REWEIGHT(2) *
                 max(convolved weight).
                 < 0 => use abs(convolved weight) compared to
                        abs(REWEIGHT(2)*max(convolved weight))
                 0 => -0.01. for interpolation output and no blanking
                        for convolution and weight outputs
  XTYPE......Convolution function type in X-direction
                1=Pillbox, 2=exponential, 3=Sinc, 4=Exp*Sinc,
                5=Spheroidal, 6=Exp*BESSJ1(x)/x
                = 0 or > 6 (& < 11) -> 5.
                11 - 16 => circular functions in radius corresponding to
                1 - 6 types above; YTYPE, YPARM are ignored.
             If XTYPE < 0, then abs(xtype) is used and some of the XPARM
             values are assumed to be in arc seconds rather than cells.
             See HELP UV1TYPE through HELP UV6TYPE for details.
  YTYPE.....Convolution function type in Y-direction
  XPARM.....Array containing parameters for XTYPE.
            See HELP UVnTYPE when n=convolution type.
            XPARM(5) is number samples of convolution function
            used per image cell for circular functions - 100 is
            used for X/Y separable functions (types 1-6)
  YPARM.....Array containing parameters for YTYPE.
  BADDISK...Disk drive #'s to avoid for scratch files