| illum_pl02 |
|
Table of contents
Procedure
illum_pl02 (illumination angles using DSK type 2 plate model)
void illum_pl02 ( SpiceInt handle,
ConstSpiceDLADescr * dladsc,
ConstSpiceChar * target,
SpiceDouble et,
ConstSpiceChar * abcorr,
ConstSpiceChar * obsrvr,
SpiceDouble spoint [3],
SpiceDouble * phase,
SpiceDouble * solar,
SpiceDouble * emissn )
AbstractDeprecated: This routine has been superseded by the CSPICE routines ilumin_c, illumg_c and illumf_c. This routine is supported for purposes of backward compatibility only. Compute the illumination angles---phase, solar incidence, and emission---at a specified point on a target body at a particular epoch, optionally corrected for light time and stellar aberration. The target body's surface is represented by a triangular plate model contained in a type 2 DSK segment. Required_ReadingFRAMES PCK SPK TIME KeywordsGEOMETRY Brief_I/OVARIABLE I/O DESCRIPTION -------- --- -------------------------------------------------- handle I DSK handle. dladsc I DLA descriptor of target body segment. target I Name of target body. et I Epoch in ephemeris seconds past J2000 TDB. abcorr I Aberration correction. obsrvr I Name of observing body. spoint I Body-fixed coordinates of a target surface point. phase O Phase angle at the surface point. solar O Solar incidence angle at the surface point. emissn O Emission angle at the surface point. Detailed_Input
handle is the DAS file handle of a DSK file open for read
access. This kernel must contain a type 2 segment
that provides a plate model representing the entire
surface of the target body.
dladsc is the DLA descriptor of a DSK segment representing
the surface of the target body.
target is the name of the target body. `target' is
case-insensitive, and leading and trailing blanks in
`target' are not significant. Optionally, you may supply
a string containing the integer ID code for the object.
For example both "MOON" and "301" are legitimate strings
that indicate the moon is the target body.
This routine assumes that the target body's surface is
represented using a plate model, and that a DSK file
containing the plate model has been loaded via dasopr_c.
et is the epoch, represented as seconds past J2000 TDB, at
which the illumination angles are to be computed. When
aberration corrections are used, `et' refers to the
epoch at which radiation is received at the observer.
abcorr indicates the aberration corrections to be applied to
the position and orientation of the target body and the
position of the Sun to account for one-way light time
and stellar aberration. See the discussion in the
Particulars section for recommendations on how to choose
aberration corrections.
`abcorr' may be any of the following:
"NONE" Apply no correction. Use the geometric
positions of the Sun and target body
relative to the observer; evaluate the
target body's orientation at `et'.
The following values of `abcorr' apply to the
"reception" case in which photons depart from the
target's location at the light-time corrected epoch
et-lt and *arrive* at the observer's location at
`et':
"LT" Correct for one-way light time (also
called "planetary aberration") using a
Newtonian formulation. This correction
uses the position and orientation of the
target at the moment it emitted photons
arriving at the observer at `et'. The
position of the Sun relative to the
target is corrected for the one-way light
time from the Sun to the target.
The light time correction uses an
iterative solution of the light time
equation (see Particulars for details).
The solution invoked by the "LT" option
uses one iteration.
"LT+S" Correct for one-way light time and stellar
aberration using a Newtonian formulation.
This option modifies the positions
obtained with the "LT" option to account
for the observer's velocity relative to
the solar system barycenter (note the
target plays the role of "observer" in the
computation of the aberration-corrected
target-Sun vector). The result is that the
illumination angles are computed using
apparent position and orientation of the
target as seen by the observer and the
apparent position of the Sun as seen by
the target.
"CN" Converged Newtonian light time correction.
In solving the light time equation, the
"CN" correction iterates until the
solution converges (three iterations on
all supported platforms).
The "CN" correction typically does not
substantially improve accuracy because the
errors made by ignoring relativistic
effects may be larger than the improvement
afforded by obtaining convergence of the
light time solution. The "CN" correction
computation also requires a significantly
greater number of CPU cycles than does the
one-iteration light time correction.
"CN+S" Converged Newtonian light time
and stellar aberration corrections.
obsrvr is the name of the observing body. This is typically a
spacecraft, the earth, or a surface point on the earth.
`obsrvr' is case-insensitive, and leading and trailing
blanks in `obsrvr' are not significant. Optionally, you
may supply a string containing the integer ID code for
the object. For example both "EARTH" and "399" are
legitimate strings that indicate the earth is the
observer.
spoint is a surface point on the target body, expressed in
rectangular body-fixed (body equator and prime meridian)
coordinates. `spoint' need not be visible from the
observer's location at time `et'.
Detailed_Output
For all of the angles below, if `spoint' does not lie on
one of the *exterior* plates comprising the DSK type 2
surface representation, the "intercept" style
"sub-observer point" corresponding to `spoint' is used
in the illumination angle computations in place of
`spoint'. The selected point will always be on the
*outermost* plate intersected by a ray emanating from
the target body's center and passing through `spoint'.
See the header of subpt_pl02 for details
concerning the definition of the sub-observer point.
In all cases, the normal vector is taken from the plate
on which the sub-point corresponding to `spoint' lies.
If this sub-point lies on an edge or vertex, a normal
vector for one of the bordering plates is selected.
phase is the phase angle at `spoint', as seen from `obsrvr' at
time `et'. This is the angle between the spoint-obsrvr
vector and the spoint-sun vector. Units are radians. The
range of `phase' is [0, pi].
solar is the solar incidence angle at `spoint', as seen from
`obsrvr' at time `et'. This is the angle between the
surface normal vector at `spoint' and the spoint-sun
vector. Units are radians. The range of `solar' is [0,
pi].
emissn is the emission angle at `spoint', as seen from `obsrvr'
at time `et'. This is the angle between the surface
normal vector at `spoint' and the spoint-observer
vector. Units are radians. The range of `emissn' is
is [0, pi].
See Particulars below for a detailed discussion of the
definitions of these angles.
ParametersNone. Exceptions
If any of the listed errors occur, the output arguments are
left unchanged.
1) If `spoint' is the zero vector, the error SPICE(ZEROVECTOR) is
signaled.
2) If either of the input body names `target' or `obsrvr' cannot be
mapped to NAIF integer codes, the error SPICE(IDCODENOTFOUND)
is signaled.
3) If `obsrvr' and `target' map to the same NAIF integer ID codes, the
error SPICE(BODIESNOTDISTINCT) is signaled.
4) If frame definition data enabling the evaluation of the state
of the target relative to the observer in target body-fixed
coordinates have not been loaded prior to calling illum_pl02,
an error is signaled by a routine in the call tree of this
routine.
5) If the specified aberration correction is not recognized, an
error is signaled by a routine in the call tree of this
routine.
6) If insufficient ephemeris data have been loaded prior to
calling illum_pl02, an error is signaled by a
routine in the call tree of this routine.
7) If a DSK providing a DSK type 2 plate model has not been
loaded prior to calling illum_pl02, an error is signaled by a
routine in the call tree of this routine.
8) If the computation method is "near point" and radii of the
target body have not been loaded into the kernel pool, an
error is signaled by a routine in the call tree of this
routine.
9) If PCK data supplying a rotation model for the target body
have not been loaded prior to calling illum_pl02, an error is
signaled by a routine in the call tree of this routine.
10) If the segment associated with the input DLA descriptor does not
contain data for the designated target, the error
SPICE(TARGETMISMATCH) is signaled.
11) If the segment associated with the input DLA descriptor is not
of data type 2, the error SPICE(WRONGDATATYPE) is signaled.
12) If the sub-point associated with `spoint' cannot be computed
because the line segment from a suitably scaled-up `spoint' to
the target body's center fails to intersect the target surface
as defined by the plate model, the error SPICE(NOINTERCEPT) is
signaled. See the routine subpt_pl02 for details.
13) Use of transmission-style aberration corrections is not
permitted. If `abcorr' specified such a correction, the
error SPICE(NOTSUPPORTED) is signaled.
14) The observer is presumed to be outside the target body; no
checks are made to verify this.
15) If any input string pointer is null, the error
SPICE(NULLPOINTER) is signaled.
16) If any input string has length zero, the error
SPICE(EMPTYSTRING) is signaled.
Files
Appropriate DSK, SPK, PCK, and frame data must be available to
the calling program before this routine is called. Typically
the data are made available by loading kernels; however the
data may be supplied via subroutine interfaces if applicable.
The following data are required:
- DSK data: a DSK file containing a plate model representing the
target body's surface must be loaded. This kernel must contain
a type 2 segment that contains data for the entire surface of
the target body.
- SPK data: ephemeris data for target, observer, and Sun must be
loaded. If aberration corrections are used, the states of
target and observer relative to the solar system barycenter
must be calculable from the available ephemeris data. Typically
ephemeris data are made available by loading one or more SPK
files via furnsh_c.
- PCK data: triaxial radii for the target body must be loaded
into the kernel pool if the "Near Point" method is selected.
Typically these data are made available by loading a text PCK
file via furnsh_c.
- Further PCK data: rotation data for the target body must
be loaded. These may be provided in a text or binary PCK file.
Either type of file may be loaded via furnsh_c.
- Frame data: if a frame definition is required to convert
the observer and target states to the body-fixed frame of
the target, that definition must be available in the kernel
pool. Typically the definition is supplied by loading a
frame kernel via furnsh_c.
In all cases, kernel data are normally loaded once per program
run, NOT every time this routine is called.
Particulars
The term "illumination angles" refers to following set of
angles:
solar incidence angle Angle between the surface normal at the
specified surface point and the vector
from the surface point to the Sun.
emission angle Angle between the surface normal at the
specified surface point and the vector
from the surface point to the observer.
phase angle Angle between the vectors from the
surface point to the observing body and
from the surface point to the Sun.
The diagram below illustrates the geometric relationships defining
these angles. The labels for the solar incidence, emission, and
phase angles are "s.i.", "e.", and "phase".
*
Sun
surface normal vector
._ _.
|\ /| Sun vector
\ phase /
\ . . /
. .
\ ___ /
. \/ \/
_\ s.i./
. / \ /
. | e. \ /
* <--------------- * surface point on
viewing vector target body
location to viewing
(observer) location
Note that if the target-observer vector, the target normal vector
at the surface point, and the target-sun vector are coplanar, then
phase is the sum of incidence and emission. This is rarely true;
usually
phase angle < solar incidence angle + emission angle
All of the above angles can be computed using light time
corrections, light time and stellar aberration corrections, or
no aberration corrections. The way aberration corrections
are used is described below.
Care must be used in computing light time corrections. The
guiding principle used here is "describe what appears in
an image." We ignore differential light time; the light times
from all points on the target to the observer are presumed to be
equal.
Observer-target body vector
---------------------------
Let `et' be the epoch at which an observation or remote
sensing measurement is made, and let et - lt ("lt" stands
for "light time") be the epoch at which the photons received
at `et' were emitted from the body (we use the term "emitted"
loosely here).
The correct observer-target vector points from the observer's
location at `et' to the target body's location at et - lt.
The target-observer vector points in the opposite direction.
Since light time corrections are not symmetric, the correct
target-observer vector CANNOT be found by computing the light
time corrected position of the observer as seen from the
target body.
Target body's orientation
-------------------------
Using the definitions of `et' and `lt' above, the target
body's orientation at et - lt is used. The surface
normal is dependent on the target body's orientation, so
the body's orientation model must be evaluated for the correct
epoch.
Target body -- Sun vector
-------------------------
All surface features on the target body will appear in a
measurement made at `et' as they were at the target at epoch
et-lt. In particular, lighting on the target body is dependent
on the apparent location of the Sun as seen from the target body
at et-lt. So, a second light time correction is used in finding
the apparent location of the Sun.
Stellar aberration corrections, when used, are applied as follows:
Observer-target body vector
---------------------------
In addition to light time correction, stellar aberration is
used in computing the apparent target body position as seen
from the observer's location at time `et'. This apparent
position defines the observer-target body vector.
Target body-Sun vector
----------------------
The target body-Sun vector is the apparent position of the Sun,
corrected for light time and stellar aberration, as seen from
the target body at time et-lt. Note that the target body's
position is not affected by the stellar aberration correction
applied in finding its apparent position as seen by the
observer.
Once all of the vectors, as well as the target body's
orientation, have been computed with the proper aberration
corrections, the element of time is eliminated from the
computation. The problem becomes a purely geometric one,
and is described by the diagram above.
Examples
The numerical results shown for this example may differ across
platforms. The results depend on the SPICE kernels used as input,
the compiler and supporting libraries, and the machine specific
arithmetic implementation.
1) Find the illumination angles at both the sub-observer point and
sub-solar point on Phobos as seen from Mars for a specified
sequence of times. Perform each computation twice, using both the
"intercept" and "ellipsoid near point" options for the sub-observer
point and sub-solar point computations. Compute the corresponding
illumination angles using an ellipsoidal surface for comparison.
(Note that the surface points on the plate model generally will
not lie on the ellipsoid's surface, so the emission and solar
incidence angles won't generally be zero at the sub-observer
and sub-solar points, respectively.)
Use the meta-kernel shown below to load the required SPICE
kernels.
KPL/MK
File: illum_pl02_ex1.tm
This meta-kernel is intended to support operation of SPICE
example programs. The kernels shown here should not be
assumed to contain adequate or correct versions of data
required by SPICE-based user applications.
In order for an application to use this meta-kernel, the
kernels referenced here must be present in the user's
current working directory.
The names and contents of the kernels referenced
by this meta-kernel are as follows:
File name Contents
--------- --------
mar097.bsp Mars satellite ephemeris
pck00010.tpc Planet orientation and
radii
naif0010.tls Leapseconds
\begindata
KERNELS_TO_LOAD = ( 'mar097.bsp',
'pck00010.tpc',
'naif0010.tls' )
\begintext
End of meta-kernel
Use the DSK kernel below to provide the plate model representation
of the surface of Phobos.
phobos_3_3.bds
Example code begins here.
/.
Program illum_pl02_ex1
./
#include <stdio.h>
#include <math.h>
#include "SpiceUsr.h"
int main()
{
/.
Local parameters
./
#define FILSIZ 256
#define NCORR 2
#define NSAMP 3
#define NMETHOD 2
#define TOL ( 1.e-12 )
#define CORLEN 15
#define METHLEN 81
#define TIMLEN 41
/.
Local variables
./
SpiceBoolean found;
SpiceChar * abcorr;
SpiceChar * abcorrs[ NCORR ] =
{
"NONE",
"LT+S"
};
SpiceChar dsk [ FILSIZ ];
SpiceChar * emethod;
SpiceChar * emethods[ NMETHOD ] =
{
"Intercept",
"Near point"
};
SpiceChar meta [ FILSIZ ];
SpiceChar * method;
SpiceChar * methods [ NMETHOD ] =
{
"Intercept",
"Ellipsoid near point"
};
SpiceChar * obsrvr = "Mars";
SpiceChar * target = "Phobos";
SpiceChar timstr [ TIMLEN ];
SpiceDLADescr dladsc;
SpiceDouble alt;
SpiceDouble dist;
SpiceDouble emissn;
SpiceDouble et0;
SpiceDouble et;
SpiceDouble phase;
SpiceDouble solar;
SpiceDouble stepsize ;
SpiceDouble xlat;
SpiceDouble xlon;
SpiceDouble xpt [3];
SpiceDouble xr;
SpiceInt coridx;
SpiceInt handle;
SpiceInt i;
SpiceInt midx;
SpiceInt plid;
/.
Prompt for the name of a meta-kernel specifying
all of the other kernels we need. Load the
metakernel.
./
prompt_c ( "Enter meta-kernel name > ", FILSIZ, meta );
furnsh_c ( meta );
/.
Prompt for the name of the DSK to read.
./
prompt_c ( "Enter DSK name > ", FILSIZ, dsk );
/.
Open the DSK file for read access.
We use the DAS-level interface for
this function.
./
dasopr_c ( dsk, &handle );
/.
Begin a forward search through the
kernel, treating the file as a DLA.
In this example, it's a very short
search.
./
dlabfs_c ( handle, &dladsc, &found );
if ( !found )
{
/.
We arrive here only if the kernel
contains no segments. This is
unexpected, but we're prepared for it.
./
setmsg_c ( "No segments found in DSK file #.");
errch_c ( "#", dsk );
sigerr_c ( "SPICE(NODATA)" );
}
/.
If we made it this far, `dladsc' is the
DLA descriptor of the first segment.
Now compute sub-points using both computation
methods. We'll vary the aberration corrections
and the epochs.
./
et0 = 0.0;
stepsize = 1.e6;
for ( i = 0; i < NSAMP; i++ )
{
/.
Set the computation time for the ith
sample.
./
et = et0 + i*stepsize;
timout_c ( et,
"YYYY-MON-DD "
"HR:MN:SC.### ::TDB(TDB)",
TIMLEN,
timstr );
printf ( "\n\nObservation epoch: %s\n",
timstr );
for ( coridx = 0; coridx < NCORR; coridx++ )
{
/.
Select the aberration correction.
./
abcorr = abcorrs[coridx];
printf ( "\n"
" abcorr = %s\n", abcorr );
for ( midx = 0; midx < NMETHOD; midx++ )
{
/.
Select the computation method.
./
method = methods [midx];
emethod = emethods[midx];
printf ( "\n"
" Method = %s\n", method );
/.
Compute the sub-observer point using a plate model
representation of the target's surface.
./
subpt_pl02 ( handle, &dladsc, method,
target, et, abcorr,
obsrvr, xpt, &alt, &plid );
/.
Compute the illumination angles at the sub-observer point.
./
illum_pl02 ( handle, &dladsc, target, et,
abcorr, obsrvr, xpt,
&phase, &solar, &emissn );
/.
Represent the intercept in latitudinal
coordinates.
./
reclat_c ( xpt, &xr, &xlon, &xlat );
printf ( "\n"
" Sub-observer point on plate model surface:\n"
" Planetocentric Longitude (deg): %f\n"
" Planetocentric Latitude (deg): %f\n"
"\n"
" Illumination angles derived using a\n"
" plate model surface:\n"
" Phase angle (deg): %f\n"
" Solar incidence angle (deg): %f\n"
" Emission angle (deg): %f\n",
xlon * dpr_c(),
xlat * dpr_c(),
phase * dpr_c(),
solar * dpr_c(),
emissn * dpr_c() );
/.
Compute the illumination angles using an ellipsoidal
representation of the target's surface. The role of
this representation is to provide an outward surface
normal.
./
illum_c ( target, et, abcorr,
obsrvr, xpt, &phase, &solar, &emissn );
printf (
" Illumination angles derived using an\n"
" ellipsoidal reference surface:\n"
" Phase angle (deg): %f\n"
" Solar incidence angle (deg): %f\n"
" Emission angle (deg): %f\n",
phase * dpr_c(),
solar * dpr_c(),
emissn * dpr_c() );
/.
Now repeat our computations using the sub-solar point.
Compute the sub-solar point using a plate model
representation of the target's surface.
./
subsol_pl02 ( handle, &dladsc, method,
target, et, abcorr,
obsrvr, xpt, &dist, &plid );
/.
Compute the illumination angles at the sub-solar point.
./
illum_pl02 ( handle, &dladsc, target, et,
abcorr, obsrvr, xpt,
&phase, &solar, &emissn );
/.
Represent the intercept in latitudinal
coordinates.
./
reclat_c ( xpt, &xr, &xlon, &xlat );
printf ( "\n"
" Sub-solar point on plate model surface:\n"
" Planetocentric Longitude (deg): %f\n"
" Planetocentric Latitude (deg): %f\n"
"\n"
" Illumination angles derived using a\n"
" plate model surface:\n"
" Phase angle (deg): %f\n"
" Solar incidence angle (deg): %f\n"
" Emission angle (deg): %f\n",
xlon * dpr_c(),
xlat * dpr_c(),
phase * dpr_c(),
solar * dpr_c(),
emissn * dpr_c() );
/.
Compute the illumination angles using an ellipsoidal
representation of the target's surface. The role of
this representation is to provide an outward surface
normal.
./
illum_c ( target, et, abcorr,
obsrvr, xpt, &phase, &solar, &emissn );
printf (
" Illumination angles derived using an\n"
" ellipsoidal reference surface:\n"
" Phase angle (deg): %f\n"
" Solar incidence angle (deg): %f\n"
" Emission angle (deg): %f\n",
phase * dpr_c(),
solar * dpr_c(),
emissn * dpr_c() );
}
}
}
/.
Close the kernel. This isn't necessary in a stand-
alone program, but it's good practice in subroutines
because it frees program and system resources.
./
dascls_c ( handle );
return ( 0 );
}
When this program was executed on a Mac/Intel/cc/64-bit
platform, using the meta-kernel file named illum_pl02_ex1.tm
and the DSK file named phobos_3_3.bds, the output was:
Enter meta-kernel name > illum_pl02_ex1.tm
Enter DSK name > phobos_3_3.bds
Observation epoch: 2000-JAN-01 12:00:00.000 (TDB)
abcorr = NONE
Method = Intercept
Sub-observer point on plate model surface:
Planetocentric Longitude (deg): -0.348118
Planetocentric Latitude (deg): 0.008861
Illumination angles derived using a
plate model surface:
Phase angle (deg): 101.596824
Solar incidence angle (deg): 98.376877
Emission angle (deg): 9.812914
Illumination angles derived using an
ellipsoidal reference surface:
Phase angle (deg): 101.596824
Solar incidence angle (deg): 101.695444
Emission angle (deg): 0.104977
Sub-solar point on plate model surface:
Planetocentric Longitude (deg): 102.413905
Planetocentric Latitude (deg): -24.533127
Illumination angles derived using a
plate model surface:
Phase angle (deg): 101.665306
Solar incidence angle (deg): 13.068798
Emission angle (deg): 98.408735
Illumination angles derived using an
ellipsoidal reference surface:
Phase angle (deg): 101.665306
Solar incidence angle (deg): 11.594741
Emission angle (deg): 98.125499
Method = Ellipsoid near point
Sub-observer point on plate model surface:
Planetocentric Longitude (deg): -0.264850
Planetocentric Latitude (deg): 0.004180
Illumination angles derived using a
plate model surface:
Phase angle (deg): 101.596926
Solar incidence angle (deg): 98.376877
Emission angle (deg): 9.812985
Illumination angles derived using an
ellipsoidal reference surface:
Phase angle (deg): 101.596926
Solar incidence angle (deg): 101.593324
Emission angle (deg): 0.003834
Sub-solar point on plate model surface:
Planetocentric Longitude (deg): 105.857346
Planetocentric Latitude (deg): -16.270558
Illumination angles derived using a
plate model surface:
Phase angle (deg): 101.663675
Solar incidence angle (deg): 16.476730
Emission angle (deg): 118.124981
Illumination angles derived using an
ellipsoidal reference surface:
Phase angle (deg): 101.663675
Solar incidence angle (deg): 0.422781
Emission angle (deg): 101.541470
abcorr = LT+S
Method = Intercept
Sub-observer point on plate model surface:
Planetocentric Longitude (deg): -0.348101
Planetocentric Latitude (deg): 0.008861
Illumination angles derived using a
plate model surface:
Phase angle (deg): 101.592246
Solar incidence angle (deg): 98.372348
Emission angle (deg): 9.812902
Illumination angles derived using an
ellipsoidal reference surface:
Phase angle (deg): 101.592246
Solar incidence angle (deg): 101.690862
Emission angle (deg): 0.104972
Sub-solar point on plate model surface:
Planetocentric Longitude (deg): 102.408894
Planetocentric Latitude (deg): -24.533381
Illumination angles derived using a
plate model surface:
Phase angle (deg): 101.660723
Solar incidence angle (deg): 13.067922
Emission angle (deg): 98.408716
[...]
Warning: incomplete output. Only 100 out of 407 lines have been
provided.
Restrictions
1) This routine assumes that the origin of the body-fixed reference
frame associated with the target body is located in the interior
of that body.
2) This routine does not compute illumination angles for surface
points on interior plates, for example plates representing
the interior of a cave or tunnel. See the -Detailed_Output section.
3) Illumination angles on an irregular target body surface may
differ greatly from those on a reference ellipsoid for the same
surface, as illustrated by the example program shown above.
Users may want to consider using the ellipsoid formulation of
this algorithm, which is implemented in the CSPICE routine
illum_c.
Literature_ReferencesNone. Author_and_InstitutionN.J. Bachman (JPL) J. Diaz del Rio (ODC Space) Version
-CSPICE Version 2.1.0, 26-OCT-2021 (JDR) (NJB)
Bug fix: call to ljust_ is now followed by call to F2C_ConvertStr.
Edited the Examples section to comply with NAIF standard.
Index lines now state that this routine is deprecated.
-CSPICE Version 2.0.0, 22-FEB-2017 (NJB)
Bug fix: the DSK segment's surface ID code is no longer
required to match that of the target. The segment's
center ID must match.
Include file references have been updated. Now calls
zzdsksgr_ instead of dsksgr_. Now calls pltnrm_ instead
of pltrec_.
Added failed_c calls.
-Beta Version 1.3.0, 30-APR-2014 (NJB) (BVS)
Now includes dsk_proto.h. Added failed_c check after
dskgd_ call.
Last update was 07-APR-2014 (BVS)
Changed FRAME to FRAMES in the Required_Reading section.
-Beta Version 1.2.0, 14-MAY-2010 (NJB)
Updated for compatibility with new DSK design.
Updated kernels used in example program.
-Beta Version 1.1.0, 09-FEB-2007 (NJB)
Bug fix: type of local variable fDLADescr was changed to SpiceInt.
-Beta Version 1.0.0, 06-NOV-2006 (NJB)
Index_EntriesDEPRECATED illumination angles using DSK type 2 plate model DEPRECATED lighting angles using DSK type 2 plate model DEPRECATED phase angle using DSK type 2 plate model DEPRECATED emission angle using DSK type 2 plate model DEPRECATED solar incidence angle using DSK type 2 |
Fri Dec 31 18:41:08 2021