EX: INP=PIC where PIC is the image to be navigated. PIC must be a Voyager, Galileo or Cassini image in either byte or halfword (16-bit integer) data format. The frame must be in image-space or object-space (no picture size reduction or map-projection allowed). Voyager images should be 800x800 for image-space frames and 1000x1000 for object-space frames. Galileo images are always in image-space and are 800x800 for full-frame images and 400x400 for summation-mode images. Cassini images can be 1024x1024, 512x512 or 256x256 and are always in image-space. The frame does not have to be radiometrically corrected. It will be desirable to do so, however, if the PROFILE option is used to gather ring-profile data.
SPICEMODE=LOCAL specifies that SPICE data is to be accessed from local SPICE kernels. SPICEMODE=REMOTE specifies that SPICE data is to be accessed via the SPICE server. If SPICEMODE is defaulted, the logical name (or environmental variable) DEFAULTSPICE is used to determine whether LOCAL or REMOTE is used. Note that if SPICE data is not found in LOCAL or REMOTE mode, the other mode is attempted in order to retrieve SPICE data. However, when improved camera pointing data is stored, only the specified or default mode is used.
CKNAME is a four character string specifying the C-kernel to be used in reading camera pointing data: CKNAME C KERNEL -------- ------------- DAVI MIPS_DAVI.CK NAV MIPS_NAV.CK FARE MIPS_FARENC.CK NAV2 MIPS_NAV2.CK NEAR MIPS_NEAR.CK AMOS MIPS_AMOS.CK NAIF the best NAIF kernel is used If defaulted, the kernels are searched in the above order.
CKID is an alternative way to specify the prefered C-kernel for reading
camera pointing data (see CKNAME parameter):
CKID CKNAME C KERNEL
---- -------- -------------
M906 DAVI MIPS_DAVI.CK
M905 NAV MIPS_NAV.CK
M904 FARE MIPS_FARENC.CK
M903 NAV2 MIPS_NAV2.CK
M902 NEAR MIPS_NEAR.CK
M901 AMOS MIPS_AMOS.CK
varies NAIF there are a large number of these files
Ex: CKID=M901 specifies the four character ID which uniquely identifies the
C-kernel MIPS_AMOS.CK.
A complete list of the C-kernel IDs is located in the ASCII file assigned the
logical name (or environmental variable) KERNELDB.
If specified, CKID overrides the CKNAME parameter.
INSTITUTE is a four character string identifying the facility which creates
the improved (C-Smithed) camera pointing. If defaulted, the value of the
logical name (or environmental variable) VICAR_SITE is used.
Ex: INSTITUTE=ASU identifies ASU as the creator of the improved camera
pointing.
PURPOSE is a four character string identifying the purpose of the observation or the purpose of processing. For example, PURPOSE=MOSA identifies the image as part of a mosaic sequence PURPOSE=COLO identifies the image as part of a color sequence
REQUNUM is a four character string identifying the IPL request number for which the camera pointing was created. REQNUM must contain exactly 4 digits. Ex: REQNUM=0123 identifies (somewhat) request number R000123
Date and time the camera pointing was created in the form 'YEARMMDDHHMM'.
The date string must contain exactly 12 digits.
Ex: CDATE=199602291200 specifies that the pointing was created at noon
on February 29, 1996.
If defaulted, the current date and time is used.
GROUPID is a three character string which identifies the group of the user running this program to store improved camera pointing. (The user ID is automatically determined by the program). Ex: GROUPID=040 identifies group 040 as the creator of the camera pointing. On VMS, this parameter is ignored since the program automatically determines the group ID of the current user. If GROUPID is defaulted on Unix, the program uses the value of the environmental variable GROUPID. Note that GROUPID is not a system-defined variable, and should be defined in your .cshrc as in the following example: Ex: setenv GROUPID 040
INTEGER - Frame number of the input image. For Voyager, this is the FDS Count specified as XXXXXYY where XXXXX is the Mod16 count and YY is the Mod60 count. Default is the value in the picture label.
INTEGER - Camera serial number. Default is the value in the picture
label. Valid Voyager camera serial numbers are:
4 = VGR-2 WA 6 = VGR-1 WA
5 = VGR-2 NA 7 = VGR-1 NA
Galileo SSI has only one camera (serial number always 1).
However, serial number of 2 is used for summation mode.
Valid Cassini camera serial numbers are:
1=NAC 21=NAC 2x2 summation mode 41=NAC 4x4 summation mode
2=WAC 22=WAC 2x2 summation mode 42=WAC 4x4 summation mode
STRING--OPTIONAL
Input reseau locations:
Ex: RESLOC (PIC,RESFILE) R !Locate the reseau
NAV PIC RES=R !Input the reseau to NAV
The reseau locations must be input if the image contains geometric camera
distortions (i.e. if it is an image-space frame).
STRING--OPTIONAL
Input blemish locations:
Ex: VGRBLEM PIC B !Retrieve the blemish locations
NAV PIC BLEMS=B !Input the blemishes to NAV
If defaulted, the program automatically accesses blemish files located
in WMS_VGR:[VGR1.NA], WMS_VGR:[VGR1.WA], and WMS_VGR:[VGR2], or the
equivalent directories /project/vgr/vgr1/wa, /project/vgr/vgr1/na, and
/project/vgr/vgr2 under Unix.
The program checks to ensure that the camera serial number associated
with the file (as extracted from the label) matches the camera serial
number associated with the image.
EX: SAO=VGR:[UID123]SAO.CAT Specifies the file location of the Smithsonian Astrophysical Observatory (SAO) or other star catalog. The catalog is required for star navigation only. At MIPS the file sao_idl.str is located in WMS_VGR:[000000] if VMS, or /project/vgr under Unix. Other star catalogs are available. Outside users can get the sao.cat file from FEI using fei -g vgrrad/sao_idl.str See HELP file for details on file contents and format.
EX: GSCPFX=GSCVOL !VMS
GSCPFX="/cdrom/gscvol" !Eunuchs(tm)
Specifies the prefix for ths location of the Guide Star Catalog CDROM's put
out by the Space Telescope Science Institute. If this parameter is specified
then it will override the SAO parameter.
See HELP file for details on mounting the CDROM's.
EX: OEF=VGR:[UID123]OEF.DAT Specifies the file location of the Orbital Elements File, which defines the ring systems of the outer planets. At MIPS, the orbital elements file is located in WMS_VGR:[000000] if VMS, or /project/vgr under Unix. This parameter is required when the parameter RING is specified. Outside users can get the ROEF.DAT file from FEI using fei -g vgrrad/roef.dat.
INTEGER - Length of correlation window in pixels.
High contrast points (limb or ring) are determined by correlating
with an edge function of area NLWxNSW. Note that both NLW and
NSW must be positive odd integers.
INTEGER - Search radius (pixels).
Example: NSEARCH=11
Starting at each computed limb (or ring) point, scan in a direction
normal to the limb a distance + and - 11 pixels for high-contrast
points.
INTEGER - Center display and zoom
Example: CZOOM=2
Center the display around the current cursor position and magnify
the image to twice normal resolution.
Display entire image. The image may be displayed at reduced resolution to accomplish this.
Read cursor positon. Reports (line,sample) and (lat,lon) or (radius,lon) coordinates.
KEYWORD - Overlay (in graphics plane) histogram of displayed image area. A logrithmic frequency scale is used.
INTEGER - Ex: SPIKES=n will scale the frequencies so that the n'th largest frequency corresponds to maximum scale.
INTEGER - Stretch the displayed image
Example: STRETCH=(25,100)
A hardware stretch (linear transformation) is applied to the displayed
image.
ASTR=(lopercent,hipercent)
Entering ASTR=(0.5,1.5) will perform an "ends-in" stretch: The
histogram of the displayed image area is first computed. Low and
high stretch limits are then chosen so as to saturate 0.5 and
1.5 percent of the data at the low and high ends of the histogram
(respectively). The algorithm is described in detail in the
help information for VICAR program FIT.
INTEGER - Draw latitude-longitude grid Ex: OVERLAY=30 draws parallels and meridians at 30 deg intervals
REAL - Draw a parallel Ex: LATI=35.5 draws a parallel at latitude 35.5 degrees
REAL - Draw a meridian Ex: LONG=180.0 draws a meridian a longitude 180.0 degrees
REAL - Convert from lat-lon to line-sample Ex: LL=(-35.2,183)
REAL - Convert from line-sample to lat-lon Ex: LS=(341,789.3)
REAL - Ring radius (km)
Example: RADIUS=136776
A ring of radius 136776 km is displayed in graphics.
STRING - Ring name. The ten Uranian rings are identified by the
following nomenclature:
6 = ring 6 N = eta ring
5 = ring 5 G = gamma ring
4 = ring 4 D = delta ring
A = alpha ring L = lambda ring (1986U1R)
B = beta ring E = epsilon ring
Saturns ring features are as follows:
F = F ring K = Outer Keeler gap
E = Outer Encke gap A = Inner A ring edge
N = Cassini inner edge of outer ring
S = Cassini inner edge of 4th outer ring
W = Outer B feature B = Inner B ring edge
M = Maxwell gap R = Mid C ring feature
T = Titan gap C = Inner C ring edge
For Neptune, nine test orbits have been defined, the first three with
polar orbits and the remainder with equatorial orbits. These rings are
idenditied as follows:
Polar rings New Satellites Previous
A = 50000 Km 5 = 1989N5 orbit T = Triton orbit
B = 100000 Km 3 = 1989N3 N = Nereid orbit
C = 150000 Km 4 = 1989N4
2 = 1989N2
1 = 1989N1
E.g. RING=E
When RING is specified, the parameter OEF is required.
KEYWORD - Show ring system. For Uranus, the ten known rings will be displayed in graphics, their positions based upon current pointing knowledge.
REAL (3) - PREDICT=FRAME: Longitude of cursored object is predicted for FRAME assuming MASTER ring orbit. Cursor determines current object's MASTER radius and longitude. PREDICT=(FRAME,RADIUS): Longitude of cursored object is predicted for FRAME assuming circular orbit of RADIUS in MASTER ring plane. Cursor determines objects current MASTER longitude. PREDICT=(FRAME,LONGITUDE): Position in current frame is determined from MASTER longitude at different FRAME. PREDICT=(FRAME,LONGITUDE,RADIUS): Position in current frame is determined from MASTER longitude assuming circular orbit of RADIUS in MASTER plane at different FRAME.
KEYWORD - Plot radial or longitudinal profile of specified ring sector. The user will be prompted for radius and longitude boundaries of sector.
STRING - Specifies master C-matrix. All C-matrices are replaced by the master C-matrix. Ex: MASTER=D
KEYWORD - Enables editing of ring orbital parameters.
Inner edge of ring.
Keywords INNER, OUTER, or THIN specity the type of edge function
to apply when scanning for a ring radius.
Typing STAR invokes the STARFIT routine which navigates the image by matching the stars in the image with a starmap computed from data retrieved from the SAO catalog.
INT - highest magnitude star displayed. !CBTC REAL - highest magnitude star displayed.
KEYWORD - Display starmap.
KEYWORD - Move (register) starmap.
Typing RD=(76.7,15.5) will cause the cursor to be moved to that right-ascension and declination on the display screen. The corresponding line-sample coordinates are reported.
All input and output latitudes are reported as planetographic. The default for Voyager is GEODET. For all other projects, the default is GEOCEN.
All input and output latitudes are reported as planetocentric.
REAL - Object-space planet-center (line,sample)
Example: PC=(433.2,315.3)
The camera pointing is updated so that the planet-center is
located at (line,sample)=(433.2,315.3) in the image.
REAL - Image-space planet-center (line,sample)
Example: ISPC=(433.2,315.3)
The camera pointing is updated so that the planet-center is
located at (line,sample)=(433.2,315.3) in the image. The input
image must be an image-space frame.
REAL - Object-space planet-center of VGR wide-angle frame. The input frame is assumed to be the narrow-angle frame of a WA-NA simultaneous exposure. WAPC permits input of the planet-center (line,sample) of the corresponding wide-angle frame. The planet-center for the narrow-angle frame is then derived using the known transformation between the to camera fields-of-view. EX: WAPC=(235.3,335.8)
REAL - Image-space planet-center of VGR wide-angle frame. The input frame must be in image-space and is assumed to be the narrow-angle frame of a WA-NA simultaneous exposure. WAISPC permits input of the planet-center (line,sample) of the corresponding wide-angle frame. The planet-center for the narrow-angle frame is then derived using the known transformation between the to camera fields-of-view. EX: WAISPC=(235.3,335.8)
REAL - North angle
Example: ANGLN=45.3
The camera pointing is updated so that the planet's projected
spin axis is oriented at a 45.3 degree angle, measured
clockwise from up in the image.
REAL - Spacecraft range (km).
Distance from spacecraft to planet center.
REAL - Minimum and maximum ring radii. Used only to flag ring-obscured limb points during limb scans. EX: RLIM=(80000.,140000.)
STRING - Target body name Example: TARGET=SATURN
KEYWORD - Save current navigation or orbital data.
KEYWORD - Restore previously saved navigation or orbital data. If no previous values were saved, initial values are retrieved.
KEYWORD - Retrieve navigation data from SEDR. This restores the nominal camera pointing.
REAL - Longitude of periapse measured at Epoch. For Uranus, French's epoch is 20:00 UT on 10 March 1977. For Saturn, Porco's epoch is time of Voyager 1 closest approach. For Neptune, the epoch is time of Voyager 2 closest approach.
REAL - Longitude of ascending node measured at Epoch. For Uranus, French's epoch is 20:00 UT on 10 March 1977. For Saturn, Porco's epoch is time of Voyager 1 closest approach. For Neptune, the epoch is time of Voyager 2 closest approach.
REAL - Right ascension of planet's pole (assumed constant)
REAL - Declination of planet's pole (assumed constant)
Sub spacecraft planetocentric latitude in degrees. Normally this is obtained from the input label(s). Only valid for non-flight projects.
Sub spacecraft longitude in degrees east. Normally this is obtained from the input label(s). Only valid for non-flight projects.
Sub solar planetocentric latitude in degrees. Normally this is obtained from the input label(s). Only valid for non-flight projects.
Sub solar longitude in degrees east. Normally this is obtained from the input label(s). Only valid for non-flight projects.
Line of planet center. Normally this is obtained from the input label(s). Only valid for non-flight projects.
Sample of planet center Normally this is obtained from the input label(s). Only valid for non-flight projects.
Distance from spacecraft to planet center in KM. Normally this is obtained from the input label(s). Only valid for non-flight projects.
Camera focal length in mm. Normally this is obtained from the input label(s). Only valid for non-flight projects.
Camera scale in pixels/mm. Normally this is obtained from the input label(s). Only valid for non-flight projects.
The angle measured in degrees clockwise from up of the projection of the planet spin axis (north end) normally onto the image plane. Normally this is obtained from the input label(s). Only valid for non-flight projects.
Line of the camera optical axis. Normally this is obtained from the input label(s). Only valid for non-flight projects.
Sample of the camera optical axis. Normally this is obtained from the input label(s). Only valid for non-flight projects.
INTEGER - Clean bad points
Example: CLEAN=5
All high-contrast points within a 5 pixel radius of the current
cursor position are deleted from the acquired curve.
The SEF command is for program development only. Don't try it.