| ccstd | images.imcoords | ccstd |
ccstd -- transform pixel and celestial coordinates to standard coordinates and vice versa
ccstd input output database solutions
CCSTD transforms the list of input coordinates in the text file input and writes the transformed coordinates to the text file output . The input coordinates are read from and the output coordinates written to, the columns xcolumn , ycolumn , lngcolumn , and latcolumn in the input and output files. The format of the output coordinates can be specified using the xformat , yformat , lngformat and latformat parameters. If the output formats are unspecified the coordinates are written out with reasonable default formats, e.g. "%10.3f" for standard coordinates, "%12.2h" and "11.1h" for celestial coordinates in hours or degrees, and "%13.7g" for celestial coordinates in radians. All the remaining fields in the input file are copied to the output file without modification. Blank lines and comment lines are also passed to the output file unaltered.
The plate solution can either be read from record solutions in the database file database written by CCMAP, or specified by the user via the xref , yref , xmag , ymag , xrotation , yrotation , lngref , latref , and projection parameters. lngunits and latunits define the units of the input celestial coordinates. If undefined they default to to the values in the database or to the quantities "hours" and "degrees" respectively. The standard coordinates are always written and read in units of arcseconds.
If the forward parameter is "yes", the input coordinates are assumed to be pixel coordinates and celestial coordinates. The pixel coordinates are transformed to standard coordinates using the plate solution, and celestial coordinates are transformed to standard coordinates using the position of the reference point lngref , latref , and the projection specified by projection . If forward is "no", then the input coordinates are assumed to be standard coordinates and those in xcolumn and ycolumn are transformed to pixel coordinates by inverting the plate solution, and those in lngcolumn and latcolumn are transformed to celestial coordinates using the position of the reference point and the specified projection.
The plate solution computed by CCMAP has the following form where x and y are the pixel coordinates and xi and eta are the corresponding fitted standard coordinates in arcseconds per pixel. The observed standard coordinates are computed by applying the appropriate sky projection to the celestial coordinates.
xi = f (x, y) eta = g (x, y)
The functions f and g are either power series, Legendre, or Chebyshev polynomials whose order and region of validity were set by the user when CCMAP was run. The plate solution is arbitrary and does not correspond to any physically meaningful model. However the first order terms can be given the simple geometrical interpretation shown below.
xi = a + b * x + c * y eta = d + e * x + f * y b = xmag * cos (xrotation) c = ymag * sin (yrotation) e = -xmag * sin (xrotation) f = ymag * cos (yrotation) a = xi0 - b * xref - c * yref = xshift d = eta0 - e * xref - f * yref = yshift xi0 = 0.0 eta0 = 0.0
xref, yref, xi0, and eta0 are the origins of the reference and output coordinate systems respectively. xi0 and eta0 are both 0.0 by default. xmag and ymag are the x and y scales in " / pixel, and xrotation and yrotation are the x and y axes rotation angles measured counter-clockwise from original x and y axes.
If the CCMAP database is undefined then CCSTD computes a linear plate solution using the the parameters xref , yref , xmag , ymag , xrotation , yrotation , lngref , latref , lngunits , latunits and projection as shown below. Note that in this case xrotation and yrotation are interpreted as the rotation of the coordinates not the rotation of the coordinate axes.
xi = a + b * x + c * y eta = d + e * x + f * y b = xmag * cos (xrotation) c = -ymag * sin (yrotation) e = xmag * sin (xrotation) f = ymag * cos (yrotation) a = xi0 - b * xref - c * yref = xshift d = eta0 - e * xref - f * yref = yshift xi0 = 0.0 eta0 = 0.0
Linear plate solutions are evaluated in the forward and reverse sense using the appropriate iraf mwcs system routines. Higher order plate solutions are evaluated in the forward sense using straight-forward evaluation of the polynomial terms, in the reverse sense by applying Newton's method to the plate solution.
A format specification has the form "%w.dCn", where w is the field width, d is the number of decimal places or the number of digits of precision, C is the format code, and n is radix character for format code "r" only. The w and d fields are optional. The format codes C are as follows:
b boolean (YES or NO)
c single character (c or '\c' or '\0nnn')
d decimal integer
e exponential format (D specifies the precision)
f fixed format (D specifies the number of decimal places)
g general format (D specifies the precision)
h hms format (hh:mm:ss.ss, D = no. decimal places)
m minutes, seconds (or hours, minutes) (mm:ss.ss)
o octal integer
rN convert integer in any radix N
s string (D field specifies max chars to print)
t advance To column given as field W
u unsigned decimal integer
w output the number of spaces given by field W
x hexadecimal integer
z complex format (r,r) (D = precision)
Conventions for w (field width) specification:
W = n right justify in field of N characters, blank fill
-n left justify in field of N characters, blank fill
0n zero fill at left (only if right justified)
absent, 0 use as much space as needed (D field sets precision)
Escape sequences (e.g. "\n" for newline):
\b backspace (not implemented)
\f formfeed
\n newline (crlf)
\r carriage return
\t tab
\" string delimiter character
\' character constant delimiter character
\\ backslash character
\nnn octal value of character
Examples
%s format a string using as much space as required
%-10s left justify a string in a field of 10 characters
%-10.10s left justify and truncate a string in a field of 10 characters
%10s right justify a string in a field of 10 characters
%10.10s right justify and truncate a string in a field of 10 characters
%7.3f print a real number right justified in floating point format
%-7.3f same as above but left justified
%15.7e print a real number right justified in exponential format
%-15.7e same as above but left justified
%12.5g print a real number right justified in general format
%-12.5g same as above but left justified
%h format as nn:nn:nn.n
%15h right justify nn:nn:nn.n in field of 15 characters
%-15h left justify nn:nn:nn.n in a field of 15 characters
%12.2h right justify nn:nn:nn.nn
%-12.2h left justify nn:nn:nn.nn
%H / by 15 and format as nn:nn:nn.n
%15H / by 15 and right justify nn:nn:nn.n in field of 15 characters
%-15H / by 15 and left justify nn:nn:nn.n in field of 15 characters
%12.2H / by 15 and right justify nn:nn:nn.nn
%-12.2H / by 15 and left justify nn:nn:nn.nn
\n insert a newline
1. Compute the standard coordinates in arcseconds per pixel given a list of
pixel and equatorial coordinates and the position of the reference point in
pixel and equatorial coordinates.
cl> type coords
13:29:47.297 47:13:37.52 327.50 410.38
13:29:37.406 47:09:09.18 465.50 62.10
13:29:38.700 47:13:36.23 442.01 409.65
13:29:55.424 47:10:05.15 224.35 131.20
13:30:01.816 47:12:58.79 134.37 356.33
cl> ccstd coords STDOUT "" xref=256.5 yref=256.5 lngref=13:29:48.1 \
latref = 47:11:53.4 xcol=3 ycol=4 lngcol=1 latcol=2
-8.180 104.120 71.000 153.880
-109.087 -164.189 209.000 -194.400
-95.753 102.854 185.510 153.150
74.688 -108.235 -32.150 -125.300
139.745 65.441 -122.130 99.830
2. Repeat the previous example but output the results in polar coordinates.
The first and third columns contain the radius coordinate in arcseconds,
the second and fourth columns contain the position angle in degrees measured
counter-clockwise with respect to the standard coordinates.
cl> ccstd coords STDOUT "" xref=256.5 yref=256.5 lngref=13:29:48.1 \
latref = 47:11:53.4 xcol=3 ycol=4 lngcol=1 latcol=2 polar+
104.441 94.492 169.470 65.231
197.124 236.400 285.434 317.073
140.526 132.952 240.560 39.542
131.504 304.608 129.359 255.609
154.309 25.093 157.740 140.737
3. Compute the plate solution and use it to evaluate the Cartesian and
polar standard coordinates for the input coordinate list used in example 1.
cl> ccmap coords coords.db xcol=3 ycol=4 lngcol=1 latcol=2 inter-
Coords File: coords Image:
Database: coords.db Record: coords
Refsystem: j2000 Coordinates: equatorial FK5
Equinox: J2000.000 Epoch: J2000.00000000 MJD: 51544.50000
Insystem: j2000 Coordinates: equatorial FK5
Equinox: J2000.000 Epoch: J2000.00000000 MJD: 51544.50000
Coordinate mapping status
Ra/Dec or Long/Lat fit rms: 0.229 0.241 (arcsec arcsec)
Coordinate mapping parameters
Sky projection geometry: tan
Reference point: 13:29:48.129 47:11:53.37 (hours degrees)
Reference point: 318.735 273.900 (pixels pixels)
X and Y scale: 0.764 0.767 (arcsec/pixel arcsec/pixel)
X and Y axis rotation: 179.110 358.958 (degrees degrees)
cl> type coords.db
# Mon 10:29:13 24-Nov-97
begin coords
xrefmean 318.7460000000001
yrefmean 273.9320000000001
lngmean 13.49670238888889
latmean 47.19815944444444
coosystem j2000
projection tan
lngref 13.49670238888889
latref 47.19815944444444
lngunits hours
latunits degrees
xpixref 318.7352667484295
ypixref 273.9002619912411
geometry general
function polynomial
xishift 247.3577084680361
etashift -206.1795977453246
xmag 0.7641733802338992
ymag 0.7666917500560622
xrotation 179.1101291109185
yrotation 358.9582148846163
wcsxirms 0.2288984454992771
wcsetarms 0.2411034140453112
xirms 0.2288984454992771
etarms 0.2411034140453112
surface1 11
3. 3.
2. 2.
2. 2.
0. 0.
134.3700000000001 134.3700000000001
465.5000000000002 465.5000000000002
62.1 62.1
410.3800000000001 410.3800000000001
247.3577084680361 -206.1795977453246
-0.7640812161068504 -0.011868034832272
-0.01393966623835092 0.7665650170136847
surface2 0
cl> ccstd coords STDOUT coords.db coords xcol=3 ycol=4 lngcol=1 latcol=2
-8.471 104.146 -8.599 104.517
-109.378 -164.163 -109.188 -164.100
-96.044 102.880 -96.084 102.598
74.397 -108.210 74.107 -108.269
139.454 65.467 139.721 65.376
cl> ccstd coords STDOUT coords.db coords xcol=3 ycol=4 lngcol=1 latcol=2 \
polar+
104.490 94.650 104.870 94.704
197.264 236.325 197.106 236.361
140.744 133.032 140.565 133.122
131.317 304.509 131.202 304.391
154.056 25.148 154.259 25.075
4. Use the previous plate solution to transform the pixel and equatorial
coordinates to standard coordinates but enter the plate solution by hand.
cl> ccstd coords STDOUT "" xref=318.735 yref=273.900 lngref=13:29:48.129 \
latref=47:11:53.37 xmag=.764 ymag=.767 xrot=180.890 yrot=1.042 xcol=3 \
ycol=4 lngcol=1 latcol=2
-8.475 104.150 -8.599 104.559
-109.382 -164.159 -109.161 -164.165
-96.048 102.884 -96.064 102.640
74.393 -108.206 74.092 -108.313
139.450 65.471 139.688 65.401
cl> ccstd coords STDOUT "" xref=318.735 yref=273.900 lngref=13:29:48.129 \
latref=47:11:53.37 xmag=.764 ymag=.767 xrot=180.890 yrot=1.042 xcol=3 \
ycol=4 lngcol=1 latcol=2 polar+
104.494 94.652 104.912 94.702
197.263 236.324 197.145 236.378
140.750 133.032 140.582 133.105
131.311 304.509 131.230 304.374
154.054 25.150 154.240 25.089
Note that there are minor differences between the results of examples 3 and
4 due to precision differences in the input, and that the angles input
to ccstd in example 4 are the coordinate rotation angles not the axes
rotation angles as printed by ccmap. The difference is exactly 180 degrees
in both cases.
5. Use the plate solution computed in example 3 to convert a list
of standard coordinates into the equivalent pixel and celestial coordinates.
cl> type stdcoords
-8.471 104.146 -8.599 104.517
-109.378 -164.163 -109.188 -164.100
-96.044 102.880 -96.084 102.598
74.397 -108.210 74.107 -108.269
139.454 65.467 139.721 65.376
cl> ccstd stdcoords STDOUT coords.db coords xcol=3 ycol=4 lngcol=1 latcol=2 \
forward-
13:29:47.30 47:13:37.5 327.499 410.381
13:29:37.41 47:09:09.2 465.500 62.101
13:29:38.70 47:13:36.2 442.010 409.650
13:29:55.42 47:10:05.1 224.350 131.200
13:30:01.82 47:12:58.8 134.370 356.330
ccmap, ccsetwcs, cctran, finder.tastrom, skyctran