subpnt_c |

## Procedurevoid subpnt_c ( ConstSpiceChar * method, ConstSpiceChar * target, SpiceDouble et, ConstSpiceChar * fixref, ConstSpiceChar * abcorr, ConstSpiceChar * obsrvr, SpiceDouble spoint [3], SpiceDouble * trgepc, SpiceDouble srfvec [3] ) ## AbstractCompute the rectangular coordinates of the sub-observer point on a target body at a specified epoch, optionally corrected for light time and stellar aberration. The surface of the target body may be represented by a triaxial ellipsoid or by topographic data provided by DSK files. This routine supersedes subpt_c. ## Required_ReadingDSK FRAMES NAIF_IDS PCK SPK TIME ## KeywordsGEOMETRY ## Brief_I/OVariable I/O Description -------- --- -------------------------------------------------- method I Computation method. target I Name of target body. et I Epoch in TDB seconds past J2000 TDB. fixref I Body-fixed, body-centered target body frame. abcorr I Aberration correction flag. obsrvr I Name of observing body. spoint O Sub-observer point on the target body. trgepc O Sub-observer point epoch. srfvec O Vector from observer to sub-observer point. ## Detailed_Inputmethod is a short string providing parameters defining the computation method to be used. In the syntax descriptions below, items delimited by brackets are optional. `method' may be assigned the following values: "NEAR POINT/ELLIPSOID" The sub-observer point computation uses a triaxial ellipsoid to model the surface of the target body. The sub-observer point is defined as the nearest point on the target relative to the observer. The word "NADIR" may be substituted for the phrase "NEAR POINT" in the string above. For backwards compatibility, the older syntax "Near point: ellipsoid" is accepted as well. "INTERCEPT/ELLIPSOID" The sub-observer point computation uses a triaxial ellipsoid to model the surface of the target body. The sub-observer point is defined as the target surface intercept of the line containing the observer and the target's center. For backwards compatibility, the older syntax "Intercept: ellipsoid" is accepted as well. "NADIR/DSK/UNPRIORITIZED[/SURFACES = <surface list>]" The sub-observer point computation uses DSK data to model the surface of the target body. The sub-observer point is defined as the intercept, on the surface represented by the DSK data, of the line containing the observer and the nearest point on the target's reference ellipsoid. If multiple such intercepts exist, the one closest to the observer is selected. Note that this definition of the sub-observer point is not equivalent to the "nearest point on the surface to the observer." The phrase "NEAR POINT" may NOT be substituted for "NADIR" in the string above. 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 escaped 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. "INTERCEPT/DSK/UNPRIORITIZED[/SURFACES = <surface list>]" The sub-observer point computation uses DSK data to model the surface of the target body. The sub-observer point is defined as the target surface intercept of the line containing the observer and the target's center. If multiple such intercepts exist, the one closest to the observer is selected. The surface list specification is optional. The syntax of the list is identical to that for the NADIR option described above. Neither case nor white space are significant in `method', except within double-quoted strings. For example, the string " eLLipsoid/nearpoint " is valid. Within double-quoted strings, 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 is the name of the target body. The target body is an ephemeris object (its trajectory is given by SPK data), and is an extended object. The string `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. When the target body's surface is represented by a tri-axial ellipsoid, this routine assumes that a kernel variable representing the ellipsoid's radii is present in the kernel pool. Normally the kernel variable would be defined by loading a PCK file. et is the epoch of participation of the observer, expressed as TDB seconds past J2000 TDB: `et' is the epoch at which the observer's state is computed. When aberration corrections are not used, `et' is also the epoch at which the position and orientation of the target body are computed. When aberration corrections are used, the position and orientation of the target body are computed at et-lt or et+lt, where `lt' is the one-way light time between the sub-observer point and the observer, and the sign applied to `lt' depends on the selected correction. See the description of `abcorr' below for details. fixref is the name of a body-fixed reference frame centered on the target body. `fixref' may be any such frame supported by the SPICE system, including built-in frames (documented in the Frames Required Reading) and frames defined by a loaded frame kernel (FK). The string `fixref' is case-insensitive, and leading and trailing blanks in `fixref' are not significant. The output sub-observer point `spoint' and the observer-to-sub-observer point vector `srfvec' will be expressed relative to this reference frame. abcorr indicates the aberration corrections to be applied when computing the target's position and orientation. For remote sensing applications, where the apparent sub-observer point seen by the observer is 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" Apply no correction. Return the geometric sub-observer point on the target body. Let `lt' represent the one-way light time between the observer and the sub-observer point (note: NOT between the observer and the target body's center). The following values of `abcorr' apply to the "reception" case in which photons depart from the sub-observer point'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 yields the location of sub-observer point at the moment it emitted photons arriving at the observer at `et'. The light time correction uses an iterative solution of the light time equation. The solution invoked by the "LT" option uses one iteration. Both the target position as seen by the observer, and rotation of the target body, are corrected for light time. "LT+S" Correct for one-way light time and stellar aberration using a Newtonian formulation. This option modifies the sub-observer point obtained with the "LT" option to account for the observer's velocity relative to the solar system barycenter. These corrections yield the apparent sub-observer point. "CN" Converged Newtonian light time correction. In solving the light time equation, the "CN" correction iterates until the solution converges. Both the position and rotation of the target body 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. The following values of `abcorr' apply to the "transmission" case in which photons *depart* from the observer's location at `et' and arrive at the sub-observer point at the light-time corrected epoch et+lt: "XLT" "Transmission" case: correct for one-way light time using a Newtonian formulation. This correction yields the sub-observer location at the moment it receives photons emitted from the observer's location at `et'. The light time correction uses an iterative solution of the light time equation. The solution invoked by the "LT" option uses one iteration. Both the target position as seen by the observer, and rotation of the target body, are corrected for light time. "XLT+S" "Transmission" case: correct for one-way light time and stellar aberration using a Newtonian formulation This option modifies the sub-observer point obtained with the "XLT" option to account for the observer's velocity relative to the solar system barycenter. "XCN" Converged Newtonian light time correction. This is the same as "XLT" correction but with further iterations to a converged Newtonian light time solution. "XCN+S" "Transmission" case: converged Newtonian light time and stellar aberration corrections. Neither case nor white space are significant in `abcorr'. For example, the string "Lt + s" is valid. obsrvr is the name of the observing body. The observing body is an ephemeris object: it typically is 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 "MOON" and "301" are legitimate strings that indicate the moon is the observer. ## Detailed_Outputspoint is the sub-observer point on the target body. For target shapes modeled by ellipsoids, the sub-observer point is defined either as the point on the target body that is closest to the observer, or the target surface intercept of the line from the observer to the target's center. For target shapes modeled by topographic data provided by DSK files, the sub-observer point is defined as the target surface intercept of the line from the observer to either the nearest point on the reference ellipsoid, or to the target's center. If multiple such intercepts exist, the one closest to the observer is selected. The input argument `method' selects the target shape model and sub-observer point definition to be used. `spoint' is expressed in Cartesian coordinates, relative to the body-fixed target frame designated by `fixref'. The body-fixed target frame is evaluated at the sub-observer epoch `trgepc' (see description below). When light time correction is used, the duration of light travel between `spoint' to the observer is considered to be the one way light time. When aberration corrections are used, `spoint' is computed using target body position and orientation that have been adjusted for the corrections applicable to `spoint' itself rather than to the target body's center. In particular, if the stellar aberration correction applicable to `spoint' is represented by a shift vector S, then the light-time corrected position of the target is shifted by S before the sub-observer point is computed. The components of `spoint' have units of km. trgepc is the "sub-observer point epoch." `trgepc' is defined as follows: letting `lt' be the one-way light time between the observer and the sub-observer point, `trgepc' is the epoch et-lt, et+lt, or `et' depending on whether the requested aberration correction is, respectively, for received radiation, transmitted radiation, or omitted. `lt' is computed using the method indicated by `abcorr'. `trgepc' is expressed as seconds past J2000 TDB. SRFVEC is the vector from the observer's position at `et' to the aberration-corrected (or optionally, geometric) position of `spoint', where the aberration corrections are specified by `abcorr'. `srfvec' is expressed in the target body-fixed reference frame designated by `fixref', evaluated at `trgepc'. The components of `srfvec' are given in units of km. One can use the CSPICE function vnorm_c to obtain the distance between the observer and `spoint': dist = vnorm_c ( 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 via the call: vsub_c ( spoint, srfvec, obspos ); 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 pxfrm2_c 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: pxfrm2_c ( fixref, ref, trgepc, et, xform ); mxv_c ( xform, srfvec, refvec ); The second example in the Examples header section below presents a complete program that demonstrates this procedure. ## ParametersNone. ## Exceptions1) If the specified aberration correction is unrecognized, the error will be diagnosed and signaled by a routine in the call tree of this routine. 2) If either the target or observer input strings cannot be converted to an integer ID code, the error SPICE(IDCODENOTFOUND) is signaled. 3) If `obsrvr' and `target' map to the same NAIF integer ID code, the error SPICE(BODIESNOTDISTINCT) is signaled. 4) If the input target body-fixed frame `fixref' is not recognized, the error SPICE(NOFRAME) is signaled. A frame name may fail to be recognized because a required frame specification kernel has not been loaded; another cause is a misspelling of the frame name. 5) If the input frame `fixref' is not centered at the target body, the error SPICE(INVALIDFRAME) is signaled. 6) If the input argument `method' is not recognized, the error SPICE(INVALIDMETHOD) is signaled by this routine, or the error is diagnosed by a routine in the call tree of this routine. If the sub-observer point type is not specified or is not recognized, the error SPICE(INVALIDSUBTYPE) is signaled. 7) If the target and observer have distinct identities but are at the same location (for example, the target is Mars and the observer is the Mars barycenter), the error SPICE(NOSEPARATION) is signaled. 8) If insufficient ephemeris data have been loaded prior to calling ## FilesAppropriate kernels must be loaded by the calling program before this routine is called. The following data are required: - SPK data: ephemeris data for target and observer 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. - Target body orientation data: these may be provided in a text or binary PCK file. In some cases, target body orientation may be provided by one more more CK files. In either case, data are made available by loading the files via furnsh_c. - Shape data for the target body: PCK data: If the target body shape is modeled as an ellipsoid, triaxial radii for the target body must be loaded into the kernel pool. Typically this is done by loading a text PCK file via furnsh_c. Triaxial radii are also needed if the target shape is modeled by DSK data, but the DSK NADIR method is selected. DSK data: If the target shape is modeled by DSK data, DSK files containing topographic data for the target body must be loaded. If a surface list is specified, data for at least one of the listed surfaces must be loaded. The following data may be required: - 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. - Surface name-ID associations: if surface names are specified in `method', the association of these names with their corresponding surface ID codes must be established by assignments of the kernel variables NAIF_SURFACE_NAME NAIF_SURFACE_CODE NAIF_SURFACE_BODY Normally these associations are made by loading a text kernel containing the necessary assignments. An example of such assignments is NAIF_SURFACE_NAME += 'Mars MEGDR 128 PIXEL/DEG' NAIF_SURFACE_CODE += 1 NAIF_SURFACE_BODY += 499 - SCLK data: if the target body's orientation is provided by CK files, an associated SCLK kernel must be loaded. In all cases, kernel data are normally loaded once per program run, NOT every time this routine is called. ## ParticularsFor ellipsoidal target bodies, there are two different popular ways to define the sub-observer point: "nearest point on the target to the observer" or "target surface intercept of the line containing observer and target." These coincide when the target is spherical and generally are distinct otherwise. For target body shapes modeled using topographic data provided by DSK files, the "surface intercept" notion is valid, but the "nearest point on the surface" computation is both inefficient to execute and may fail to yield a result that is "under" the observer in an intuitively clear way. The NADIR option for DSK shapes instead finds the surface intercept of a ray that passes through the nearest point on the target reference ellipsoid. For shapes modeled using topography, there may be multiple ray-surface intercepts; the closest one to the observer is selected. The NADIR definition makes sense only if the target shape is reasonably close to the target's reference ellipsoid. If the target is very different---the nucleus of comet Churyumov-Gerasimenko is an example---the intercept definition should be used. This routine computes light time corrections using light time between the observer and the sub-observer point, as opposed to the center of the target. Similarly, stellar aberration corrections done by this routine are based on the direction of the vector from the observer to the light-time corrected sub-observer point, not to the target center. This technique avoids errors due to the differential between aberration corrections across the target body. Therefore it's valid to use aberration corrections with this routine even when the observer is very close to the sub-observer point, in particular when the observer to sub-observer point distance is much less than the observer to target center distance. When comparing sub-observer point computations with results from sources other than SPICE, it's essential to make sure the same geometric definitions are used. Using DSK data ============== DSK loading and unloading ------------------------- DSK files providing data used by this routine are loaded by calling furnsh_c and can be unloaded by calling unload_c or kclear_c. See the documentation of furnsh_c 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 sets 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 "NADIR/DSK/UNPRIORITIZED/<surface list>" "DSK/NADIR/<surface list>/UNPRIORITIZED" "UNPRIORITIZED/<surface list>/DSK/NADIR" The simplest form of the `method' argument specifying use of DSK data is one that lacks a surface list, for example: "NADIR/DSK/UNPRIORITIZED" "INTERCEPT/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 strings suffice. 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\"" Escaped 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 "NADIR/DSK/UNPRIORITIZED/SURFACES= \"Mars MEGDR 64 PIXEL/DEG\",3" Aberration corrections ---------------------- 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 an 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. ## ExamplesThe numerical results shown for these examples 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 sub-Earth point on Mars for a specified time. Compute the sub-Earth points using both triaxial ellipsoid and topographic surface models. Topography data are provided by a DSK file. For the ellipsoid model, use both the "intercept" and "near point" sub-observer point definitions; for the DSK case, use both the "intercept" and "nadir" definitions. Display the locations of both the Earth and the sub-Earth point relative to the center of Mars, in the IAU_MARS body-fixed reference frame, using both planetocentric and planetographic coordinates. 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: subpnt_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 --------- -------- de430.bsp Planetary ephemeris mar097.bsp Mars satellite ephemeris pck00010.tpc Planet orientation and radii naif0011.tls Leapseconds 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', 'megr90n000cb_plate.bds' ) \begintext Example code begins here. /. Program subpnt_ex1 ./ #include <stdio.h> #include "SpiceUsr.h" int main() { /. Local parameters ./ #define META "subpnt_ex1.tm" #define MTHLEN 81 #define NMETH 4 /. Local variables ./ static SpiceChar * method[NMETH] = { "Intercept/ellipsoid", "Near point/ellipsoid", "Intercept/DSK/Unprioritized", "Nadir/DSK/Unprioritized" }; SpiceDouble et; SpiceDouble f; SpiceDouble obspos [3]; SpiceDouble odist; SpiceDouble opclat; SpiceDouble opclon; SpiceDouble opcrad; SpiceDouble opgalt; SpiceDouble opglat; SpiceDouble opglon; SpiceDouble radii [3]; SpiceDouble re; SpiceDouble rp; SpiceDouble spclat; SpiceDouble spclon; SpiceDouble spcrad; SpiceDouble spgalt; SpiceDouble spglat; SpiceDouble spglon; SpiceDouble spoint [3]; SpiceDouble srfvec [3]; SpiceDouble trgepc; SpiceInt i; SpiceInt n; /. Load kernel files via the meta-kernel. ./ furnsh_c ( META ); /. Convert the UTC request time string to seconds past J2000, TDB. ./ str2et_c ( "2008 aug 11 00:00:00", &et ); /. Look up the target body's radii. We'll use these to convert Cartesian to planetographic coordinates. Use the radii to compute the flattening coefficient of the reference ellipsoid. ./ bodvrd_c ( "MARS", "RADII", 3, &n, radii ); /. Let `re and `rp' be, respectively, the equatorial and polar radii of the target. ./ re = radii[0]; rp = radii[2]; f = ( re - rp ) / re; /. Compute sub-observer point using light time and stellar aberration corrections. Use both ellipsoid and DSK shape models, and use all of the "near point," "intercept," and "nadir" sub-observer point definitions. ./ for ( i = 0; i < NMETH; i++ ) { ## RestrictionsNone. ## Literature_ReferencesNone. ## Author_and_InstitutionN.J. Bachman (JPL) S.C. Krening (JPL) B.V. Semenov (JPL) ## Version-CSPICE Version 2.0.0, 05-APR-2017 (NJB) Fixed a few header comment typos. 14-OCT-2015 (NJB) Updated to support surfaces represented by DSK data. -CSPICE Version 1.0.2, 02-APR-2011 (NJB) (SCK) References to the new pxfrm2_c routine were added, which changed the Detailed Output section and the second example. Miscellaneous, minor header comment corrections were made. -CSPICE Version 1.0.1, 06-FEB-2009 (NJB) Incorrect frame name fixfrm was changed to fixref in documentation. In the header examples, meta-kernel names were updated to use the suffix ".tm" -CSPICE Version 1.0.0, 02-MAR-2008 (NJB) ## Index_Entriesfind sub-observer point on target body find sub-spacecraft point on target body find nearest point to observer on target body |

Wed Apr 5 17:54:45 2017