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Abstract
I/O
Examples
Particulars
Required Reading
Version
Index_Entries

Abstract


   CSPICE_ILUMIN computes the illumination angles (phase, solar incidence,
   and emission) at a specified surface point of a target body.

   This routine supersedes cspice_illum, which lacks an input
   argument for the target body-fixed frame name.

I/O


   Given:

      method   is a short string providing parameters defining
               the computation method to be used. In the syntax
               descriptions below, items delimited by brackets
               are optional.

               [1,c1] = size(method); char = class(method)

                or

               [1,1] = size(method); cell = class(method)

               `method' may be assigned the following values:

                  'ELLIPSOID'

                     The illumination angle computation uses a
                     triaxial ellipsoid to model the surface of the
                     target body. The ellipsoid's radii must be
                     available in the kernel pool.


                  'DSK/UNPRIORITIZED[/SURFACES = <surface list>]'

                     The illumination angle computation uses
                     topographic data to model the surface of the
                     target body. These data must be provided by
                     loaded DSK files.

                     The surface list specification is optional. The
                     syntax of the list is

                        <surface 1> [, <surface 2>...]

                     If present, it indicates that data only for the
                     listed surfaces are to be used; however, data
                     need not be available for all surfaces in the
                     list. If absent, loaded DSK data for any surface
                     associated with the target body are used.

                     The surface list may contain surface names or
                     surface ID codes. Names containing blanks must
                     be delimited by double quotes, for example

                        'SURFACES = "Mars MEGDR 128 PIXEL/DEG"'

                     If multiple surfaces are specified, their names
                     or IDs must be separated by commas.

                     See the Particulars section below for details
                     concerning use of DSK data.


               Neither case nor white space are significant in
               `method', except within double-quoted strings
               representing surface names. For example, the string
               ' eLLipsoid ' is valid.

               Within double-quoted strings representing surface names,
               blank characters are significant, but multiple
               consecutive blanks are considered equivalent to a single
               blank. Case is not significant. So

                  "Mars MEGDR 128 PIXEL/DEG"

               is equivalent to

                  " mars megdr  128  pixel/deg "

               but not to

                  "MARS MEGDR128PIXEL/DEG"

      target   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.

               [1,c2] = size(target); char = class(target)

      et       epoch specified in ephemeris is seconds past J2000, at which
               the apparent illumination angles at the specified surface point
               on the target body, as seen from the observing body, are to be
               computed.

               [1,1] = size(et); double = class(et)

      fixref   name of body-fixed, body-centered reference frame associated
               with the target body. The input surface point `spoint' and the
               output vector 'srfvec' are expressed relative to this reference
               frame.

               [1,c3] = size(fixref); char = class(fixref)

               'fixref' is case-insensitive, and leading and trailing
               blanks are not significant.

      abcorr   aberration correction to be used in computing the location of
               the surface point, the orientation of the target body, and the
               location of the Sun.

               [1,m] = size(abcorr); char = class(abcorr)

               For remote sensing applications, where the apparent
               illumination angles seen by the observer are desired,
               normally either of the corrections

                  'LT+S'
                  'CN+S'

               should be used. These and the other supported options
               are described below. `abcorr' may be any of the
               following:

                  'NONE'     No aberration correction.

                  'LT'       Correct the position of the input
                             surface point SPOINT and orientation of
                             target body for light time, and correct
                             the position of the Sun as seen
                             from the target for light time.

                  'LT+S'     Correct the position of the surface
                             point SPOINT for light time and stellar
                             aberration, correct the orientation of
                             the target body for light time, and
                             correct the position of the Sun as seen
                             from the target for light time and
                             stellar aberration.

                  'CN'       Converged Newtonian light time
                             correction. In solving the light time
                             equation, the 'CN' correction iterates
                             until the solution converges. Both the
                             position of the surface point SPOINT c
                             and rotation of the target body, as
                             well as the position of the Sun as seen
                             from the target, are corrected for
                             light time.

                  'CN+S'     Converged Newtonian light time and
                             stellar aberration corrections. This
                             option produces a solution that is at
                             least as accurate at that obtainable
                             with the 'LT+S' option. Whether the
                             'CN+S' solution is substantially more
                             accurate depends on the geometry of the
                             participating objects and on the
                             accuracy of the input data. In all
                             cases this routine will execute more
                             slowly when a converged solution is
                             computed.

               Neither case nor white space are significant in
               `abcorr'. For example, the string

                 'Lt + s'

               is valid.

      obsrvr   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.

               [1,c4] = size(obsrvr); char = class(obsrvr)

               `obsrvr' may be not be identical to `target'.

      spoint   a surface location on the target body, expressed in Cartesian
               coordinates, relative to the body-fixed target frame designated
               by `fixref'.

               [3,1] = size(spoint); double = class(spoint)

               `spoint' need not be visible from the observer's
               location at the epoch `et'.

               The components of `spoint' have units of km.

   the call:

      [trgepc, srfvec, phase, solar, emissn] = cspice_ilumin( method,  ...
                                              target, et,     fixref,  ...
                                              abcorr, obsrvr, spoint)

   returns:

      trgepc   "surface point epoch." 'trgepc' is defined as follows: letting
               'lt' be the one-way light time between the observer and the
               input surface point 'spoint', 'trgepc' is either the epoch
               et-lt or 'et' depending on whether the requested aberration
               correction is, respectively, for received radiation or omitted.
               'lt' is computed using the method indicated by 'abcorr'.

               [1,1] = size(trgepc); double = class(trgepc)

               'trgepc' is expressed as seconds past J2000 TDB.


      srfvec   the position vector from the observer at 'et' to 'spoint'.
               'srfvec' is expressed in the target body-fixed  reference frame
               designated by 'fixref', evaluated at  'trgepc'.

               [3,1] = size(srfvec); double = class(srfvec)

               The components of 'srfvec' are given in units of km.

               One can use the function norm to obtain the
               distance between the observer and 'spoint':

                     dist = norm( srfvec )

               The observer's position 'obspos', relative to the
               target body's center, where the center's position is
               corrected for aberration effects as indicated by
               'abcorr', can be computed with:

                     obspos = spoint - srfvec

               To transform the vector 'srfvec' from a reference frame
               'fixref' at time 'trgepc' to a time-dependent reference
               frame 'ref' at time 'et', the routine 'cspice_pxfrm2' should be
               called. Let 'xform' be the 3x3 matrix representing the
               rotation from the reference frame 'fixref' at time
               'trgepc' to the reference frame 'ref' at time 'et'. Then
               'srfvec' can be transformed to the result 'refvec' as
               follows:

                     xform  = cspice_pxfrm2 ( fixref, ref, trgepc, et )
                     refvec = xform * srfvec

      phase    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].

               [1,1] = size(phase); double = class(phase)

      solar    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].

               [1,1] = size(solar); double = class(solar)

      emissn   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 [0, pi].

               [1,1] = size(emissn); double = class(emissn)

Examples


   Any numerical results shown for this example may differ between
   platforms as the results depend on the SPICE kernels used as input
   and the machine specific arithmetic implementation.

      Find the phase, solar incidence, and emission angles at the 
      sub-solar and sub-spacecraft points on Mars as seen from the Mars
      Global Surveyor spacecraft at a specified UTC time.
 
      Use both an ellipsoidal Mars shape model and topographic data
      provided by a DSK file.  For both surface points, use the "near
      point" and "nadir" definitions for ellipsoidal and DSK shape
      models, respectively.
 
      Use converged Newtonian light time and stellar aberration
      corrections.
  
      The topographic model is based on data from the MGS MOLA DEM 
      megr90n000cb, which has a resolution of 4 pixels/degree. A 
      triangular plate model was produced by computing a 720 x 1440 
      grid of interpolated heights from this DEM, then tessellating 
      the height grid. The plate model is stored in a type 2 segment 
      in the referenced DSK file. 
 
      Use the meta-kernel shown below to load the required SPICE 
      kernels. 
 
         KPL/MK 
 
         File: illum_t2.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 
            ---------                        -------- 
            de430.bsp                        Planetary ephemeris 
            mar097.bsp                       Mars satellite ephemeris 
            pck00010.tpc                     Planet orientation and 
                                             radii 
            naif0011.tls                     Leapseconds 
            mgs_ext12_ipng_mgs95j.bsp        MGS ephemeris 
            megr90n000cb_plate.bds           Plate model based on 
                                             MEGDR DEM, resolution 
                                             4 pixels/degree. 
 
         \begindata 
 
            KERNELS_TO_LOAD = ( 'de430.bsp', 
                                'mar097.bsp', 
                                'pck00010.tpc', 
                                'naif0011.tls', 
                                'mgs_ext12_ipng_mgs95j.bsp', 
                                'megr90n000cb_plate.bds'      ) 
         \begintext 
 
   Example(1): 

      function illumf_t2()
      
            %
            % Load kernel files.
            %
            cspice_furnsh( 'illum_t2.tm' )
      
      
            %
            % Convert the UTC request time string to seconds past
            % J2000 TDB.
            %
            utc = '2003 OCT 13 06:00:00 UTC';
      
            et = cspice_str2et( utc );
      
            %
            % Assign observer and target names. The acronym MGS
            % indicates Mars Global Surveyor. See NAIF_IDS for a
            % list of names recognized by SPICE.
            %
            % Also set the target body-fixed frame and
            % the aberration correction flag.
            %
      
            target = 'Mars';
            obsrvr = 'MGS';
            fixref = 'IAU_MARS';
            abcorr = 'CN+S';
      
            ilumth  = {'Ellipsoid', 'DSK/Unprioritized' };
            submth =  {'Near Point/Ellipsoid', 'DSK/Nadir/Unprioritized' };
      
            for i=1:numel(ilumth)
      
               %
               % Find the sub-solar point on the Earth as seen from
               % the MGS spacecraft at et. Use the 'near point'
               % style of sub-point definition.
               %
               [ssolpt, trgepc, srfvec] = ...
                                        cspice_subslr( submth(i), ...
                                             target, et, fixref,  ...
                                             abcorr, obsrvr );
      
               %
               % Now find the sub-spacecraft point.
               %
               [sscpt, trgepc, srfvec] = ...
                                        cspice_subpnt( submth(i), ...
                                              target, et, fixref, ...
                                              abcorr, obsrvr );
      
               %
               % Find the phase, solar incidence, and emission
               % angles at the sub-solar point on the Earth as seen
               % from MGS at time et.
               %
               [ trgepc, srfvec, sslphs, sslsol, sslemi ] = ...
                                cspice_ilumin( ilumth(i),   ...
                                       target, et,  fixref, ...
                                       abcorr, obsrvr, ssolpt );
      
               %
               % Do the same for the sub-spacecraft point.
               %
               [ trgepc, srfvec, sscphs, sscsol, sscemi ] = ...
                                  cspice_ilumin( ilumth(i), ...
                                        target, et, fixref, ...
                                        abcorr, obsrvr, sscpt );
      
               %
               % Convert the angles to degrees and write them out.
               %
               sslphs = sslphs * cspice_dpr;
               sslsol = sslsol * cspice_dpr;
               sslemi = sslemi * cspice_dpr;
               sscphs = sscphs * cspice_dpr;
               sscsol = sscsol * cspice_dpr;
               sscemi = sscemi * cspice_dpr;
      
               fprintf( [ '\n'                                         ...
                       '   cspice_ilumin method: %s\n'                 ...
                       '   cspice_subpnt method: %s\n'                 ...
                       '   cspice_subslr method: %s\n'                 ...
                       '\n'                                            ...
                       '      Illumination angles at the '             ...
                       'sub-solar point:\n'                            ...
                       '\n'                                            ...
                       '      Phase angle            (deg): %15.9f\n'  ...
                       '      Solar incidence angle  (deg): %15.9f\n'  ...
                       '      Emission angle         (deg): %15.9f\n'],...
                              char(ilumth(i)),   ...
                              char(submth(i)),   ...
                              char(submth(i)),   ...
                              sslphs,      ...
                              sslsol,      ...
                              sslemi                                    );
      
               if ( i == 0 )
      
                  fprintf( [ '        The solar incidence angle ' ...
                             'should be 0.\n'                     ...
                             '        The emission and phase '    ...
                             'angles should be equal.\n' ] );
               end
      
               fprintf( [ '\n'                                            ...
                          '      Illumination angles at the '             ...
                          'sub-s/c point:\n'                              ...
                          '\n'                                            ...
                          '      Phase angle            (deg): %15.9f\n'  ...
                          '      Solar incidence angle  (deg): %15.9f\n'  ...
                          '      Emission angle         (deg): %15.9f\n'],...
                          sscphs, ...
                          sscsol, ...
                          sscemi                                    );
      
               if ( i == 0 )
      
                 fprintf( [ '        The emission angle '  ...
                            'should be 0.\n'               ...
                            '        The solar incidence ' ...
                            'and phase angles should be equal.\n' ] );
                 end
      
                 fprintf ( '\n' );
      
            end
      
            %
            % It's always good form to unload kernels after use,
            % particularly in Matlab due to data persistence.
            %
            cspice_kclear

   MATLAB outputs:

      cspice_ilumin method: Ellipsoid
      cspice_subpnt method: Near Point/Ellipsoid
      cspice_subslr method: Near Point/Ellipsoid
   
         Illumination angles at the sub-solar point:
   
         Phase angle            (deg):   138.370270685
         Solar incidence angle  (deg):     0.000000000
         Emission angle         (deg):   138.370270685
   
         Illumination angles at the sub-s/c point:
   
         Phase angle            (deg):   101.439331040
         Solar incidence angle  (deg):   101.439331041
         Emission angle         (deg):     0.000000002
   
   
      cspice_ilumin method: DSK/Unprioritized
      cspice_subpnt method: DSK/Nadir/Unprioritized
      cspice_subslr method: DSK/Nadir/Unprioritized
   
         Illumination angles at the sub-solar point:
   
         Phase angle            (deg):   138.387071678
         Solar incidence angle  (deg):     0.967122745
         Emission angle         (deg):   137.621480599
   
         Illumination angles at the sub-s/c point:
   
         Phase angle            (deg):   101.439331359
         Solar incidence angle  (deg):   101.555993667
         Emission angle         (deg):     0.117861156

Particulars


   Mice contains four routines that compute illumination angles:

      cspice_illumf (same as cspice_illumg, except that illumination 
                    and visibility flags are returned) 
                
      cspice_illumg (same as this routine, except that the caller
                    specifies the illumination source) 

      cspice_ilumin (this routine) 
 
      cspice_illum  (deprecated) 
 
   
   cspice_illumf is the most capable of the set. 


   Illumination angles
   ===================

   The term "illumination angles" refers to following set of
   angles:


      phase angle              Angle between the vectors from the
                               surface point to the observer and
                               from the surface point to the
                               illumination source.

      incidence angle          Angle between the surface normal at
                               the specified surface point and the
                               vector from the surface point to the
                               illumination source.

      emission angle           Angle between the surface normal at
                               the specified surface point and the
                               vector from the surface point to the
                               observer.

   The diagram below illustrates the geometric relationships
   defining these angles. The labels for the incidence, emission,
   and phase angles are "inc.", "e.", and "phase".


                                                    *
                                            illumination source

                  surface normal vector
                            ._                 _.
                            |\                 /|  illumination
                              \    phase      /    source vector
                               \   .    .    /
                               .            .
                                 \   ___   /
                            .     \/     \/
                                  _\ inc./
                           .    /   \   /
                           .   |  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-illumination source vector
   are coplanar, then phase is the sum of the incidence and emission
   angles. This rarely occurs; usually

      phase angle  <  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. In order to describe apparent geometry as
   observed by a remote sensing instrument, both light time and
   stellar aberration corrections should be used.

   The way aberration corrections are applied by this routine
   is described below.

      Light time corrections
      ======================

         Observer-target surface point 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 surface point `spoint'.
         Note that the light time between the surface point and
         observer will generally differ from the light time between
         the target body's center and the observer.


         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 -- illumination source vector
         -----------------------------------------

         The surface features on the target body near `spoint' will
         appear in a measurement made at `et' as they were at et-lt.
         In particular, lighting on the target body is dependent on
         the apparent location of the illumination source as seen
         from the target body at et-lt. So, a second light time
         correction is used to compute the position of the
         illumination source relative to the surface point.


      Stellar aberration corrections
      ==============================

      Stellar aberration corrections are applied only if
      light time corrections are applied as well.

         Observer-target surface point body vector
         -----------------------------------------

         When stellar aberration correction is performed, the
         direction vector `srfvec' is adjusted so as to point to the
         apparent position of `spoint': considering `spoint' to be an
         ephemeris object, `srfvec' points from the observer's
         position at `et' to the light time and stellar aberration
         corrected position of `spoint'.

         Target body-illumination source vector
         --------------------------------------

         The target body-illumination source vector is the apparent
         position of the illumination source, corrected for light
         time and stellar aberration, as seen from the target body
         at time et-lt.


   Using DSK data
   ==============

      DSK loading and unloading
      -------------------------

      DSK files providing data used by this routine are loaded by
      calling cspice_furnsh and can be unloaded by calling cspice_unload or
      cspice_kclear. See the documentation of cspice_furnsh for limits on 
      numbers of loaded DSK files.

      For run-time efficiency, it's desirable to avoid frequent
      loading and unloading of DSK files. When there is a reason to
      use multiple versions of data for a given target body---for
      example, if topographic data at varying resolutions are to be
      used---the surface list can be used to select DSK data to be
      used for a given computation. It is not necessary to unload
      the data that are not to be used. This recommendation presumes
      that DSKs containing different versions of surface data for a
      given body have different surface ID codes.


      DSK data priority
      -----------------

      A DSK coverage overlap occurs when two segments in loaded DSK
      files cover part or all of the same domain---for example, a
      given longitude-latitude rectangle---and when the time
      intervals of the segments overlap as well.

      When DSK data selection is prioritized, in case of a coverage
      overlap, if the two competing segments are in different DSK
      files, the segment in the DSK file loaded last takes
      precedence. If the two segments are in the same file, the
      segment located closer to the end of the file takes
      precedence.

      When DSK data selection is unprioritized, data from competing
      segments are combined. For example, if two competing segments
      both represent a surface as a set of triangular plates, the
      union of those sets of plates is considered to represent the
      surface.

      Currently only unprioritized data selection is supported.
      Because prioritized data selection may be the default behavior
      in a later version of the routine, the UNPRIORITIZED keyword is
      required in the `method' argument.


      Syntax of the `method' input argument
      -----------------------------------

      The keywords and surface list in the `method' argument
      are called "clauses." The clauses may appear in any
      order, for example

         'DSK/<surface list>/UNPRIORITIZED'
         'DSK/UNPRIORITIZED/<surface list>'
         'UNPRIORITIZED/<surface list>/DSK'

      The simplest form of the `method' argument specifying use of
      DSK data is one that lacks a surface list, for example:

         'DSK/UNPRIORITIZED'

      For applications in which all loaded DSK data for the target
      body are for a single surface, and there are no competing
      segments, the above string suffices. This is expected to be
      the usual case.

      When, for the specified target body, there are loaded DSK
      files providing data for multiple surfaces for that body, the
      surfaces to be used by this routine for a given call must be
      specified in a surface list, unless data from all of the
      surfaces are to be used together.

      The surface list consists of the string

         'SURFACES ='

      followed by a comma-separated list of one or more surface
      identifiers. The identifiers may be names or integer codes in
      string format. For example, suppose we have the surface
      names and corresponding ID codes shown below:

         Surface Name                              ID code
         ------------                              -------
         "Mars MEGDR 128 PIXEL/DEG"                1
         "Mars MEGDR 64 PIXEL/DEG"                 2
         "Mars_MRO_HIRISE"                         3

      If data for all of the above surfaces are loaded, then
      data for surface 1 can be specified by either

         "SURFACES = 1"

      or

         'SURFACES = "Mars MEGDR 128 PIXEL/DEG"'

      Double quotes are used to delimit the surface name
      because it contains blank characters.

      To use data for surfaces 2 and 3 together, any
      of the following surface lists could be used:

         'SURFACES = 2, 3'

         'SURFACES = "Mars MEGDR  64 PIXEL/DEG", 3'

         'SURFACES = 2, Mars_MRO_HIRISE'

         'SURFACES = "Mars MEGDR 64 PIXEL/DEG", Mars_MRO_HIRISE'

      An example of a `method' argument that could be constructed
      using one of the surface lists above is

         'DSK/UNPRIORITIZED/SURFACES = "Mars MEGDR 64 PIXEL/DEG", 3'


      Aberration corrections using DSK data
      -------------------------------------

      For irregularly shaped target bodies, the distance between the
      observer and the nearest surface intercept need not be a
      continuous function of time; hence the one-way light time
      between the intercept and the observer may be discontinuous as
      well. In such cases, the computed light time, which is found
      using iterative algorithm, may converge slowly or not at all.
      In all cases, the light time computation will terminate, but
      the result may be less accurate than expected.

   Please refer to the Aberation Corrections Required Reading (ABCORR.REQ)
   for detailed information describing the nature and calculation of the
   applied corrections.

Required Reading


   For important details concerning this module's function, please refer to
   the Mice routine cspice_ilumin.

   MICE.REQ
   ABCORR.REQ
   DSK.REQ
   FRAMES.REQ
   NAIF_IDS.REQ
   PCK.REQ
   SPK.REQ
   TIME.REQ

Version


   -Mice Version 1.1.0, 04-APR-2017, EDW (JPL)

       Changed field name, in 'ilumin' return argument, corresponding
       to the 'solar' incidence angle from "solar to "incdnc" (incident).
       This change corresponds to the modification made to the MiceIlum
       return structure.

       Particulars updated to refer to Aberration Corrections
       Required Reading document.

       I/O updated to describe use of DSKs.

   -Mice Version 1.0.4, 12-MAR-2012, SCK (JPL), EDW (JPL)

       References to the new 'cspice_pxfrm2' routine were added to the
       'I/O returns' section. A problem description was added to the
       'Examples' section.

       Edited I/O section to conform to NAIF standard for Mice documentation.

   -Mice Version 1.0.3, 29-APR-2011, EDW (JPL)

       Corrected minor typo in header and another in the usage string.

   -Mice Version 1.0.2, 12-MAY-2009, EDW (JPL)

       Edited I/O section; added 'fixref' description.

   -Mice Version 1.0.1, 30-DEC-2008, EDW (JPL)

       Added typography markers to usage string descriptor.

       Minor edit to Example comments.

       Corrected misspellings.

   -Mice Version 1.0.0, 14-FEB-2008, EDW (JPL)

Index_Entries


   illumination angles
   lighting angles
   phase angle
   emission angle
   solar incidence angle


Wed Apr  5 18:00:33 2017