.help ccfind Jun99 images.imcoords
.ih
NAME
ccfind -- locate objects in an image given a celestial coordinate list and
the image wcs
.ih
USAGE
ccfind input output image
.ih
PARAMETERS
.ls input
The list of input celestial coordinate files. Coordinates may be entered
by hand by setting input to "STDIN". A STDIN coordinate list is terminated
by typing <EOF> (usually <ctrl/d> or <ctrl/z>).
.le
.ls output
The list of output matched coordinate files. The computed pixel values
are appended to the input coordinate file line and written to output. The number
of output files must equal the number of input files. Results may be
printed on the terminal by setting output to "STDOUT".
.le
.ls image
The list of input images associated with the input coordinate files. The number
of input images must equal the number of input coordinate files.
.le
.ls lngcolumn = 1, latcolumn = 2
The input coordinate file columns containing the celestial ra / longitude and
dec / latitude coordinates respectively.
.le
.ls lngunits = "", latunits = ""
The units of the input ra / longitude and dec / latitude coordinates. The
options are "hours", "degreees", and "radians" for ra / longitude and
"degrees" and "radians" for dec / latitude. If lngunits and latunits are
undefined they default to the preferred units for the coordinates
system specified by \fIinsystem\fR, e.g. "hours" and "degrees" for
equatorial systems and "degrees" and "degrees" for ecliptic, galactic, and
supergalactic systems.
.le
.ls insystem = "j2000"
The input celestial coordinate system. The \fIinsystem\fR parameter
sets the preferred units for the input celestial coordinates, and
tells CCFIND how to transform the input celestial coordinates 
the input image celestial coordinate system. The systems of most
interest to users are "icrs", "j2000", and "b1950".  The full set
of options are the following:

.ls equinox [epoch]
The equatorial mean place post-IAU 1976 (FK5) system if equinox is a
Julian epoch, e.g. J2000.0 or 2000.0, or the equatorial mean place
pre-IAU 1976 system (FK4) if equinox is a Besselian epoch, e.g. B1950.0
or 1950.0. Julian equinoxes are prefixed by a J or j, Besselian equinoxes
by a B or b. Equinoxes without the J / j or B / b prefix are treated as
Besselian epochs if they are < 1984.0, Julian epochs if they are >= 1984.0.
Epoch is the epoch of the observation and may be a Julian
epoch, a Besselian epoch, or a Julian date. Julian epochs
are prefixed by a J or j, Besselian epochs by a B or b.
Epochs without the J / j or B / b prefix default to the epoch type of
equinox if the epoch value <= 3000.0, otherwise epoch is interpreted as
a Julian date.  If undefined epoch defaults to equinox.
.le
.ls icrs [equinox] [epoch]
The International Celestial Reference System (ICRS) where equinox is
a Julian or Besselian epoch e.g. J2000.0  or B1980.0.
Equinoxes without the J / j or B / b prefix are treated as Julian epochs.
The default value of equinox is J2000.0.
Epoch is a Besselian epoch, a Julian epoch, or a Julian date.
Julian epochs are prefixed by a J or j, Besselian epochs by a B or b.
Epochs without the J / j or B / b prefix default to Julian epochs
if the epoch value <= 3000.0, otherwise epoch is interpreted as
a Julian date.  If undefined epoch defaults to equinox.
.le
.ls fk5 [equinox] [epoch]
The equatorial mean place post-IAU 1976 (FK5) system where equinox is
a Julian or Besselian epoch e.g. J2000.0  or B1980.0.
Equinoxes without the J / j or B / b prefix are treated as Julian epochs.
The default value of equinox is J2000.0.
Epoch is a Besselian epoch, a Julian epoch, or a Julian date.
Julian epochs are prefixed by a J or j, Besselian epochs by a B or b.
Epochs without the J / j or B / b prefix default to Julian epochs
if the epoch value <= 3000.0, otherwise epoch is interpreted as
a Julian date.  If undefined epoch defaults to equinox.
.le
.ls fk4 [equinox] [epoch]
The equatorial mean place pre-IAU 1976 (FK4) system where equinox is a
Besselian or Julian epoch e.g. B1950.0  or J2000.0,
and epoch is the Besselian epoch, the Julian epoch, or the Julian date of the
observation.
Equinoxes without the J / j or B / b prefix are treated
as Besselian epochs. The default value of equinox is B1950.0. Epoch
is a Besselian epoch, a Julian epoch, or a Julian date.
Julian epochs are prefixed by a J or j, Besselian epochs by a B or b.
Epochs without the J / j or B / b prefix default to Besselian epochs
if the epoch value <= 3000.0, otherwise epoch is interpreted as
a Julian date.  If undefined epoch defaults to equinox.
.le
.ls noefk4 [equinox] [epoch]
The equatorial mean place pre-IAU 1976 (FK4) system but without the E-terms
where equinox is a Besselian or Julian epoch e.g. B1950.0 or J2000.0,
and epoch is the Besselian epoch, the Julian epoch, or the Julian date of the
observation.
Equinoxes without the J / j or B / b prefix are treated
as Besselian epochs. The default value of equinox is B1950.0.
Epoch is a Besselian epoch, a Julian epoch, or a Julian date.
Julian epochs are prefixed by a J or j, Besselian epochs by a B or b.
Epochs without the J / j or B / b prefix default to Besselian epochs
if the epoch value <= 3000.0, otherwise epoch is interpreted as
a Julian day.  If undefined epoch defaults to equinox.
.le
.ls apparent epoch
The equatorial geocentric apparent place post-IAU 1976 system where
epoch is the epoch of observation.
Epoch is a Besselian epoch, a Julian epoch or a Julian date.
Julian epochs are prefixed by a J or j, Besselian epochs by a B or b.
Epochs without the J / j or B / b prefix default to Besselian
epochs if the epoch value < 1984.0, Julian epochs
if the epoch value <= 3000.0, otherwise epoch is interpreted as
a Julian date.
.le
.ls ecliptic epoch
The ecliptic coordinate system where epoch is the epoch of observation.
Epoch is a Besselian epoch, a Julian epoch, or a Julian date.
Julian epochs are prefixed by a J or j, Besselian epochs by a B or b.
Epochs without the J / j or B / b prefix default to Besselian epochs
if the epoch values < 1984.0, Julian epochs
if the epoch value <= 3000.0, otherwise epoch is interpreted as
a Julian day.
.le
.ls galactic [epoch]
The IAU 1958 galactic coordinate system.
Epoch is a Besselian epoch, a Julian epoch or a Julian date.
Julian epochs are prefixed by a J or j, Besselian epochs by a B or b.
Epochs without the J / j or B / b prefix default to Besselian
epochs if the epoch value < 1984.0, Julian epochs
if the epoch value <= 3000.0, otherwise epoch is interpreted as
a Julian date. The default value of epoch is B1950.0.
.le
.ls supergalactic [epoch]
The deVaucouleurs supergalactic coordinate system.
Epoch is a Besselian epoch, a Julian epoch or a Julian date.
Julian epochs are prefixed by a J or j, Besselian epochs by a B or b.
Epochs without the J / j or B / b prefix default to Besselian
epochs if the epoch value < 1984.0, Julian epochs
if the epoch value <= 3000.0, otherwise epoch is interpreted as
a Julian date. The default value of epoch is B1950.0.
.le

In all the above cases fields in [] are optional with the defaults as
described. The epoch field for the icrs, fk5, galactic, and supergalactic
coordinate systems is only used if the input coordinates are in the
equatorial fk4, noefk4, fk5, or icrs systems and proper motions are supplied.
Since CCFIND does not currently support proper motions these fields are
not required.
.le
.ls usewcs = no
Use image header information to compute the input image celestial coordinate
system ? If usewcs is "yes", the image coordinate system is read from the
image header.  If usewcs is "no", the input image celestial coordinates
system is defined by \fIxref\fR, \fIyref\fR, \fIxmag\fR, \fIymag\fR,
\fIxrotation\fR, \fIyrotation\fR, \fIlngref\fR, \fIlatref\fR, 
\fIlngrefunits\fR, \fIlatrefunits\fR, \fIrefsystem\fR, and \fIprojection\fR
parameters respectively.
.le
.ls xref = INDEF, yref = INDEF
The x and y pixel coordinates of the reference point.
xref and yref default to the center of the image in pixel coordinates.
.le
.ls xmag = INDEF, ymag = INDEF
The x and y scale factors in arcseconds per pixel.  xmag and ymag default
to 1.0 and 1.0 arcseconds per pixel.
.le
.ls xrotation = INDEF, yrotation = INDEF
The x and y rotation angles in degrees. xrotation and yrotation are
interpreted as the rotation of the ra / longitude and dec / latitude
coordinates with respect to the x and y axes, and default 0.0 and 0.0 degrees
respectively. To set east to the up, down, left, and right directions,
set xrotation to 90, 270, 180, and 0 respectively. To set north to the
up, down, left, and right directions, set yrotation to  0, 180, 90, and 270
degrees respectively. Any global rotation must be added to both the
xrotation and yrotation values.
.le
.ls lngref = "INDEF", latref = "INDEF"
The ra / longitude and dec / latitude of the reference point. Lngref and latref
may be numbers, e.g 13:20:42.3 and -33:41:26, or keywords for the
appropriate parameters in the image header, e.g. RA and DEC for NOAO
image data. If lngref and latref are undefined they default to 0.0 and 0.0
respectively.
.le
.ls lngrefunits = "", latrefunits = ""
The units of the reference point celestial  coordinates. The options
are "hours", "degrees", and "radians" for the ra / longitude coordinates,
and "degrees" and "radians" for the dec /latitude coordinates.
If lngrefunits and latrefunits are undefined they default to the preferred
units of the reference system.
.le
.ls refsystem = "INDEF"
The celestial coordinate system of the reference point. Refsystem may
be any one of the options listed under the \fIinsystem\fR parameter, e.g.
"b1950", or an image header keyword containing the epoch of the observation
in years, e.g. EPOCH for NOAO data.  If refsystem is undefined
the celestial coordinate system of the reference point defaults to the
celestial coordinate system of the input coordinates \fIinsystem\fR.
.le
.ls projection = "tan"
The sky projection geometry. The most commonly used projections in
astronomy are "tan", "arc", "sin", and "lin". Other supported projections
are "ait", "car", "csc", "gls", "mer", "mol", "par", "pco", "qsc", "stg",
"tsc", and "zea".
.le
.ls center = yes
Center the object pixel coordinates using an x and y marginal centroiding
algorithm ?
.le
.ls sbox = 21
The search box width in pixels. Sbox defines the region of the input image
searched and used to compute the initial x and y marginal centroids. Users
worried about contamination can set sbox = cbox, so that the first
centering iteration will be the same as the others.
.le
.ls cbox = 9
The centering box width in pixels. Cbox defines the region of the input
image used to compute the final x and y marginal centroids.
.le
.ls datamin = INDEF, datamax = INDEF
The minimum and maximum good data values. Values outside this range
are exclude from the x and y marginal centroid computation.
.le
.ls background = INDEF
The background value used by the centroiding algorithm. If background is
INDEF, a value equal to the mean value of the good data pixels for
each object is used.
.le
.ls maxiter = 5
The maximum number of centroiding iterations to perform. The centroiding
algorithm will halt when this limit is reached or when the desired tolerance
is reached.
.le
.ls tolerance = 0
The convergence tolerance of the centroiding algorithm. Tolerance is
defined as the maximum permitted integer shift of the centering box in
pixels from one iteration to the next.
.le
.ls verbose
Print messages about actions taken by the task?
.le

.ih
DESCRIPTION

CCFIND locates the objects in the input celestial coordinate lists \fIinput\fR
in the input images \fIimage\fR using the image world coordinate system,
and writes the located objects to the output matched coordinates files
\fIoutput\fR. CCFIND computes the pixel coordinates of each object by,
1) transforming the input celestial coordinates to image celestial coordinate
system, 2) using the image celestial coordinate system to compute the
initial pixel coordinates, and 3) computing the final pixel coordinates
using a centroiding algorithm. The image celestial coordinate system may
be read from the image header or supplied by the user. The CCFIND output
files are suitable for input to the plate solution computation task CCMAP.

The input ra / longitude and dec / latitude coordinates are read from
columns \fIlngcolumn\fR and \fIlatcolumn\fR in the input coordinate
file respectively.

The input celestial coordinate system is set by the \fIinsystem\fR parameter,
and must be one of the following: equatorial, ecliptic, galactic, or
supergalactic.  The equatorial coordinate systems must be one of: 1) FK4,
the mean place pre-IAU 1976 system, 2) FK4-NO-E, the same as FK4 but without
the E-terms, 3) FK5, the mean place post-IAU 1976 system, 4) ICRS the
International Celestial Reference System, 5) GAPPT, the geocentric apparent
place in the post-IAU 1976 system.

The \fIlngunits\fR and \fIlatunits\fR parameters set the units of the input
celestial coordinates. If undefined, lngunits and latunits assume sensible
defaults for the input celestial coordinate system set by the \fIinsystem\fR
parameter, e.g. "hours" and "degrees" for equatorial coordinates and "degrees"
and "degrees" for galactic coordinates.

If the \fIusewcs\fR parameter is "yes", the image celestial coordinate
system is read from the image header keywords CRPIX, CRVAL, CD or CDELT/CROTA,
RADECSYS, EQUINOX or EPOCH, and MJD-OBS or DATE-OBS, where the mathematical
part of this transformation is shown below.

.nf
        xi = a + b * x + c * y
       eta = d + e * x + f * y
         b = CD1_1
         c = CD1_2
         e = CD2_1
         f = CD2_2
         a = - b * CRPIX1 - c * CRPIX2
         d = - e * CRPIX1 - f * CRPIX2 
       lng = CRVAL1 + PROJ (xi, eta)
       lat = CRVAL2 + PROJ (xi, eta)
.fi

If usewcs is "no", then the image celestial coordinate system is computed
using the values of the \fIxref\fR, \fIyref\fR, \fIxmag\fR, \fIymag\fR,
\fIxrotation\fR, \fIyrotation\fR, \fIlngref\fR, \fIlatref\fR,
\fIlngrefunits\fR, \fIlatrefunits\fR, \fIrefsystem\fR, and \fIprojection\fR
supplied by the user, where the mathematical part of this transformation is
shown below.

.nf
        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 = - b * xref - c * yref 
         d = - e * xref - f * yref
       lng = lngref + PROJ (xi, eta)
       lat = latref + PROJ (xi, eta)
.fi

In both the above examples, x and y are the pixel coordinates, xi and eta
are the usual projected (standard) coordinates, lng and lat are the celestial
coordinates, and PROJ stands for the projection function,  usually
the tangent plane projection function.

Once the image celestial coordinate system is determined, CCFIND transforms
the input celestial coordinates to the image celestial coordinate system
using the value of the \fIinsystem\fR parameter, and either the values of
the image header keywords RADECSYS, EQUINOX / EPOCH, and MJD-OBS / DATE-OBS
(if \fIusewcs\fR = "yes"), or the value of the \fIrefsystem\fR parameter (if
\fIusewcs\fR = "no"), and then transforms the image celestial coordinates
to pixel coordinates using the inverse of the transformation functions
shown above.

If \fIcenter\fR is yes, CCFIND locates the objects in the input
image using an  xn and y marginal centroiding algorithm. Pixels
inside a box \fIsbox\fR pixels wide centered in the initial coordinates,
are used to locate the objects in the image. Accurate final centering
is done using pixels inside a region \fIcbox\fR pixels wide centered on
these initial coordinates. Sbox should be set to a value large enough
to locate the object, but small enough to exclude other bright sources.
Cbox should be set to a value small enough to exclude sky values and other
bright sources, but large enough to include the wings of point sources.
Bad data can be excluded from the centroiding algorithm by setting
the \fIdatamin\fR and \fIdatamax\fR parameters. If \fIbackground\fR is
undefined then the centroiding algorithm sets the background value to
the mean of the good data values inside the centering box.
The centroiding algorithm iterates until the maximum number of
iterations \fImaxiter\fR limit is reached, or until the tolerance
criteria \fItolerance\fR is achieved.

Only objects whose coordinates are successfully located in the 
input image are written to the output coordinate file. The computed
output pixel coordinates are appended to the input image line using
the format parameters \fIxformat\fR and \fIyformat\fR parameters,
whose default values are "%10.3f" and "%10.3f" respectively

.ih
FORMATS

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:
   
.nf
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
cctran.hlp-(67%)-line 268-file 1 of 1
%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
.fi

.ih
EXAMPLES

1. Locate the object in the list wpix.coords in the image wpix using
the existing image header wcs. The input celestial coordinates file
contains j2000 GSC catalog coordinates of 5 objects in the field.
The image wcs is in b1950.

.nf
cl> imcopy dev$wpix wpix
    ... copy the test image into the current directory

cl> hedit wpix equinox 1950.0 add+
    ... change the epoch keyword value to the correct number

cl> type wpix.coords
13:29:47.297  47:13:37.52
13:29:37.406  47:09:09.18
13:29:38.700  47:13:36.23
13:29:55.424  47:10:05.15
13:30:01.816  47:12:58.79

cl> ccfind wpix.coords wpix.match wpix usewcs+

Input File: wpix.coords  Output File: wpix.match
    Image: wpix  Wcs: 
Insystem: j2000  Coordinates: equatorial FK5
    Equinox: J2000.000 Epoch: J2000.00000000 MJD: 51544.50000
Refsystem: wpix.imh logical  Projection: TAN  Ra/Dec axes: 1/2
    Coordinates: equatorial FK4 Equinox: B1950.000
    Epoch: B1987.25767884 MJD: 46890.00000
Located 5 objects in image wpix

cl> type wpix.match
# Input File: wpix.coords  Output File: wpix.match
#     Image: wpix  Wcs: 
# Insystem: j2000  Coordinates: equatorial FK5
#     Equinox: J2000.000 Epoch: J2000.00000000 MJD: 51544.50000
# Refsystem: wpix.imh logical  Projection: TAN  Ra/Dec axes: 1/2
#     Coordinates: equatorial FK4 Equinox: B1950.000
#     Epoch: B1987.25767884 MJD: 46890.00000

13:29:47.297  47:13:37.52     327.504    410.379
13:29:37.406  47:09:09.18     465.503     62.101
13:29:38.700  47:13:36.23     442.013    409.654
13:29:55.424  47:10:05.15     224.351    131.200
13:30:01.816  47:12:58.79     134.373    356.327

cl> ccmap wpix.match ccmap.db xcol=3 ycol=4 lngcol=1 latcol=2 ...
.fi

2. Repeat the previous example but input the image coordinate system by hand.
The scale is known to be ~0.77 arcseconds per pixel, north is up, east is left,
and the center of the image is near ra = 13:27:47, dec = 47:27:14 in 1950
coordinates.

.nf
cl> ccfind wpix.coords wpix.match wpix xmag=-0.77 ymag=.77 lngref=13:27:47 \
latref=47:27:14 refsystem=b1950.

Input File: wpix.coords  Output File: wpix.match.1
    Image: wpix  Wcs: 
Insystem: j2000  Coordinates: equatorial FK5
    Equinox: J2000.000 Epoch: J2000.00000000 MJD: 51544.50000
Refsystem: b1950  Coordinates: equatorial FK4
    Equinox: B1950.000 Epoch: B1950.00000000 MJD: 33281.92346
Located 5 objects in image wpix


cl> type wpix.match 

# Input File: wpix.coords  Output File: wpix.match
#     Image: wpix  Wcs: 
# Insystem: j2000  Coordinates: equatorial FK5
#     Equinox: J2000.000 Epoch: J2000.00000000 MJD: 51544.50000
# Refsystem: b1950  Coordinates: equatorial FK4
#     Equinox: B1950.000 Epoch: B1950.00000000 MJD: 33281.92346

13:29:47.297  47:13:37.52     327.504    410.379
13:29:37.406  47:09:09.18     465.503     62.101
13:29:38.700  47:13:36.23     442.013    409.654
13:29:55.424  47:10:05.15     224.351    131.200
13:30:01.816  47:12:58.79     134.373    356.327
.fi

3. Repeat the previous example but read the ra, dec, and epoch from the
image header keywords RA, DEC, and EPOCH. It turns out the telescope
RA and DEC recorded in the image header are not very accurate and that
EPOCH is 0.0 instead of 1987.26 so we will fix up the header before
trying out the example.

.nf
cl> hedit wpix EPOCH 1987.26
cl> hedit wpix RA '13:29:21'
cl> hedit wpix DEC '47:15:42'

cl> ccfind wpix.coords wpix.match wpix xmag=-0.77 ymag=.77 lngref=RA \
latref=DEC refsystem=EPOCH

Input File: wpix.coords  Output File: wpix.match
    Image: wpix  Wcs: 
Insystem: j2000  Coordinates: equatorial FK5
    Equinox: J2000.000 Epoch: J2000.00000000 MJD: 51544.50000
Refsystem: 1987.26  Coordinates: equatorial FK5
    Equinox: J1987.260 Epoch: J1987.26000000 MJD: 46891.21500
Located 5 objects in image wpix

# Input File: wpix.coords  Output File: wpix.match
#     Image: wpix  Wcs: 
# Insystem: j2000  Coordinates: equatorial FK5
#     Equinox: J2000.000 Epoch: J2000.00000000 MJD: 51544.50000
# Refsystem: 1987.26  Coordinates: equatorial FK5
#     Equinox: J1987.260 Epoch: J1987.26000000 MJD: 46891.21500

13:29:47.297  47:13:37.52     327.504    410.379
13:29:37.406  47:09:09.18     465.503     62.101
13:29:38.700  47:13:36.23     442.013    409.654
13:29:55.424  47:10:05.15     224.351    131.200
13:30:01.816  47:12:58.79     134.373    356.327
.fi

4. Use ccfind to predict the pixel coordinate in the last example by
turning off the object centering, and mark the predicted coordinates
on the image display with red dots.

.nf
cl> ccfind wpix.coords wpix.match wpix xmag=-0.77 ymag=.77 lngref=RA \
latref=DEC refsystem=EPOCH center-

Input File: wpix.coords  Output File: wpix.match
    Image: wpix  Wcs: 
Insystem: j2000  Coordinates: equatorial FK5
    Equinox: J2000.000 Epoch: J2000.00000000 MJD: 51544.50000
Refsystem: 1987.26  Coordinates: equatorial FK5
    Equinox: J1987.260 Epoch: J1987.26000000 MJD: 46891.21500
Located 5 objects in image wpix

cl> type wpix.match

# Input File: wpix.coords  Output File: wpix.match
#     Image: wpix  Wcs: 
# Insystem: j2000  Coordinates: equatorial FK5
#     Equinox: J2000.000 Epoch: J2000.00000000 MJD: 51544.50000
# Refsystem: 1987.26  Coordinates: equatorial FK5
#     Equinox: J1987.260 Epoch: J1987.26000000 MJD: 46891.21500

13:29:47.297  47:13:37.52     333.954    401.502
13:29:37.406  47:09:09.18     465.338     53.175
13:29:38.700  47:13:36.23     447.687    399.967
13:29:55.424  47:10:05.15     226.600    125.612
13:30:01.816  47:12:58.79     141.892    351.084

cl> display wpix 1

cl> fields wpix.match 3,4 | tvmark 1 STDIN col=204

.fi

.ih
TIME REQUIREMENTS
.ih
BUGS
.ih
SEE ALSO
starfind, ccxymatch, ccmap, ccsetwcs, cctran
.endhelp