Index of Functions: A B C D E F G H I J K L M N O P Q R S T U V W X
Index Page illum_pl02
Table of contents
Procedure Abstract Required_Reading Keywords Brief_I/O Detailed_Input | Detailed_Output Parameters Exceptions Files Particulars Examples | Restrictions Literature_References Author_and_Institution Version Index_Entries
#### 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      )
#### Abstract
       Deprecated: This routine has been superseded by the CSPICE routines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_Reading
       FRAMES
       PCK
       SPK
       TIME
#### Keywords
       GEOMETRY
#### Brief_I/O
       VARIABLE  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.
#### Parameters
       None.
#### 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_References
       None.
#### Author_and_Institution
       N.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_Entries
       DEPRECATED 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
#### Link to routine illum_pl02 source file illum_pl02.c

    Fri Dec 31 18:41:08 2021