void spkezp_c ( SpiceInt targ,
SpiceDouble et,
ConstSpiceChar * ref,
ConstSpiceChar * abcorr,
SpiceInt obs,
SpiceDouble ptarg[3],
SpiceDouble * lt )
/*
-Brief_I/O
Variable I/O Description
-------- --- --------------------------------------------------
targ I Target body NAIF ID code.
et I Observer epoch.
ref I Reference frame of output position vector.
abcorr I Aberration correction flag.
obs I Observing body NAIF ID code.
ptarg O Position of target.
lt O One way light time between observer and target.
-Detailed_Input
targ is the NAIF ID code for a target body. The target
and observer define a position vector which points
from the observer to the target.
et is the ephemeris time, expressed as seconds past
J2000 TDB, at which the position of the target body
relative to the observer is to be computed. 'et'
refers to time at the observer's location.
ref is the name of the reference frame relative to which
the output position vector should be expressed. This
may be any 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).
When 'ref' designates a non-inertial frame, the
orientation of the frame is evaluated at an epoch
dependent on the selected aberration correction. See
the description of the output position vector 'ptarg'
for details.
abcorr indicates the aberration corrections to be applied to
the position of the target body 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. Return the
geometric position of the target body
relative to the observer.
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
yields the position of the target 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 (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
position obtained with the "LT" option
to account for the observer's velocity
relative to the solar system
barycenter. The result is the apparent
position of the target---the position
as seen by the observer.
"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.
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
target's location 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
position of the target at the moment it
receives photons emitted from the
observer's location at 'et'.
"XLT+S" "Transmission" case: correct for one-way
light time and stellar aberration using a
Newtonian formulation. This option
modifies the position obtained with the
"XLT" option to account for the observer's
velocity relative to the solar system
barycenter. The computed target position
indicates the direction that photons
emitted from the observer's location must
be "aimed" to hit the target.
"XCN" "Transmission" case: converged
Newtonian light time correction.
"XCN+S" "Transmission" case: converged
Newtonian light time and stellar
aberration corrections.
Neither special nor general relativistic effects are
accounted for in the aberration corrections applied
by this routine.
Case and blanks are not significant in the string
abcorr.
obs is the NAIF ID code for an observing body.
-Detailed_Output
ptarg is a Cartesian 3-vector representing the position of
the target body relative to the specified observer.
'ptarg' is corrected for the specified aberrations, and
is expressed with respect to the reference frame
specified by 'ref'. The three components of 'ptarg'
represent the x-, y- and z-components of the target's
position.
Units are always km.
'ptarg' points from the observer's location at 'et' to
the aberration-corrected location of the target.
Note that the sense of this position vector is
independent of the direction of radiation travel
implied by the aberration correction.
Non-inertial frames are treated as follows: letting
ltcent be the one-way light time between the observer
and the central body associated with the frame, the
orientation of the frame is evaluated at et-ltcent,
et+ltcent, or 'et' depending on whether the requested
aberration correction is, respectively, for received
radiation, transmitted radiation, or is omitted. ltcent
is computed using the method indicated by abcorr.
lt is the one-way light time between the observer and
target in seconds. If the target position is corrected
for aberrations, then 'lt' is the one-way light time
between the observer and the light time corrected
target location.
-Parameters
None.
-Exceptions
1) If name of target or observer cannot be translated to its
NAIF ID code, the error SPICE(IDCODENOTFOUND) is signaled.
2) If the reference frame 'ref' is not a recognized reference
frame the error SPICE(UNKNOWNFRAME) is signaled.
3) If the loaded kernels provide insufficient data to
compute the requested position vector, the deficiency will
be diagnosed by a routine in the call tree of this routine.
4) If an error occurs while reading an SPK or other kernel file,
the error will be diagnosed by a routine in the call tree
of this routine.
-Files
This routine computes positions using SPK files that have been
loaded into the SPICE system, normally via the kernel loading
interface routine furnsh_c. See the routine furnsh_c and the SPK
and KERNEL Required Reading for further information on loading
(and unloading) kernels.
If the output position 'ptarg' is to be expressed relative to a
non-inertial frame, or if any of the ephemeris data used to
compute 'ptarg' are expressed relative to a non-inertial frame in
the SPK files providing those data, additional kernels may be
needed to enable the reference frame transformations required to
compute the position. These additional kernels may be C-kernels, PCK
files or frame kernels. Any such kernels must already be loaded
at the time this routine is called.
-Particulars
This routine is part of the user interface to the SPICE ephemeris
system. It allows you to retrieve position information for any
ephemeris object relative to any other in a reference frame that
is convenient for further computations.
Aberration corrections
======================
In space science or engineering applications one frequently
wishes to know where to point a remote sensing instrument, such
as an optical camera or radio antenna, in order to observe or
otherwise receive radiation from a target. This pointing problem
is complicated by the finite speed of light: one needs to point
to where the target appears to be as opposed to where it actually
is at the epoch of observation. We use the adjectives
"geometric," "uncorrected," or "true" to refer to an actual
position or state of a target at a specified epoch. When a
geometric position or state vector is modified to reflect how it
appears to an observer, we describe that vector by any of the
terms "apparent," "corrected," "aberration corrected," or "light
time and stellar aberration corrected." The SPICE Toolkit can
correct for two phenomena affecting the apparent location of an
object: one-way light time (also called "planetary aberration") and
stellar aberration.
One-way light time
------------------
Correcting for one-way light time is done by computing, given an
observer and observation epoch, where a target was when the observed
photons departed the target's location. The vector from the
observer to this computed target location is called a "light time
corrected" vector. The light time correction depends on the motion
of the target relative to the solar system barycenter, but it is
independent of the velocity of the observer relative to the solar
system barycenter. Relativistic effects such as light bending and
gravitational delay are not accounted for in the light time
correction performed by this routine.
Stellar aberration
------------------
The velocity of the observer also affects the apparent location
of a target: photons arriving at the observer are subject to a
"raindrop effect" whereby their velocity relative to the observer
is, using a Newtonian approximation, the photons' velocity
relative to the solar system barycenter minus the velocity of the
observer relative to the solar system barycenter. This effect is
called "stellar aberration." Stellar aberration is independent
of the velocity of the target. The stellar aberration formula
used by this routine does not include (the much smaller)
relativistic effects.
Stellar aberration corrections are applied after light time
corrections: the light time corrected target position vector is
used as an input to the stellar aberration correction.
When light time and stellar aberration corrections are both
applied to a geometric position vector, the resulting position
vector indicates where the target "appears to be" from the
observer's location.
As opposed to computing the apparent position of a target, one
may wish to compute the pointing direction required for
transmission of photons to the target. This also requires correction
of the geometric target position for the effects of light time
and stellar aberration, but in this case the corrections are
computed for radiation traveling *from* the observer to the target.
We will refer to this situation as the "transmission" case.
The "transmission" light time correction yields the target's
location as it will be when photons emitted from the observer's
location at `et' arrive at the target. The transmission stellar
aberration correction is the inverse of the traditional stellar
aberration correction: it indicates the direction in which
radiation should be emitted so that, using a Newtonian
approximation, the sum of the velocity of the radiation relative
to the observer and of the observer's velocity, relative to the
solar system barycenter, yields a velocity vector that points in
the direction of the light time corrected position of the target.
One may object to using the term "observer" in the transmission
case, in which radiation is emitted from the observer's location.
The terminology was retained for consistency with earlier
documentation.
Below, we indicate the aberration corrections to use for some
common applications:
1) Find the apparent direction of a target. This is
the most common case for a remote-sensing observation.
Use "LT+S": apply both light time and stellar
aberration corrections.
Note that using light time corrections alone ("LT") is
generally not a good way to obtain an approximation to an
apparent target vector: since light time and stellar
aberration corrections often partially cancel each other,
it may be more accurate to use no correction at all than to
use light time alone.
2) Find the corrected pointing direction to radiate a signal
to a target. This computation is often applicable for
implementing communications sessions.
Use "XLT+S": apply both light time and stellar
aberration corrections for transmission.
3) Compute the apparent position of a target body relative
to a star or other distant object.
Use "LT" or "LT+S" as needed to match the correction
applied to the position of the distant object. For
example, if a star position is obtained from a catalog,
the position vector may not be corrected for stellar
aberration. In this case, to find the angular
separation of the star and the limb of a planet, the
vector from the observer to the planet should be
corrected for light time but not stellar aberration.
4) Obtain an uncorrected position vector derived directly from
data in an SPK file.
Use "NONE".
5) Use a geometric position vector as a low-accuracy estimate
of the apparent position for an application where execution
speed is critical.
Use "NONE".
6) While this routine cannot perform the relativistic
aberration corrections required to compute positions
with the highest possible accuracy, it can supply the
geometric positions required as inputs to these computations.
Use "NONE", then apply relativistic aberration
corrections (not available in the SPICE Toolkit).
Below, we discuss in more detail how the aberration corrections
applied by this routine are computed.
Geometric case
==============
spkezp_c begins by computing the geometric position T(et) of the
target body relative to the solar system barycenter (SSB).
Subtracting the geometric position of the observer O(et) gives
the geometric position of the target body relative to the
observer. The one-way light time, 'lt', is given by
| T(et) - O(et) |
lt = -------------------
c
The geometric relationship between the observer, target, and
solar system barycenter is as shown:
SSB ---> O(et)
| /
| /
| /
| / T(et) - O(et)
V V
T(et)
The returned position is
T(et) - O(et)
Reception case
==============
When any of the options "LT", "CN", "LT+S", "CN+S" is selected
for `abcorr', spkezp_c computes the position of the target body at
epoch et-lt, where 'lt' is the one-way light time. Let T(t) and
O(t) represent the positions of the target and observer
relative to the solar system barycenter at time t; then 'lt' is
the solution of the light-time equation
| T(et-lt) - O(et) |
lt = ------------------------ (1)
c
The ratio
| T(et) - O(et) |
--------------------- (2)
c
is used as a first approximation to 'lt'; inserting (2) into the
right hand side of the light-time equation (1) yields the
"one-iteration" estimate of the one-way light time ("LT").
Repeating the process until the estimates of 'lt' converge yields
the "converged Newtonian" light time estimate ("CN").
Subtracting the geometric position of the observer O(et) gives
the position of the target body relative to the observer:
T(et-lt) - O(et).
SSB ---> O(et)
| \ |
| \ |
| \ | T(et-lt) - O(et)
| \ |
V V V
T(et) T(et-lt)
The light time corrected position vector is
T(et-lt) - O(et)
If correction for stellar aberration is requested, the target
position is rotated toward the solar system
barycenter-relative velocity vector of the observer. The
rotation is computed as follows:
Let r be the light time corrected vector from the observer
to the object, and v be the velocity of the observer with
respect to the solar system barycenter. Let w be the angle
between them. The aberration angle phi is given by
sin(phi) = v sin(w) / c
Let h be the vector given by the cross product
h = r X v
Rotate r by phi radians about h to obtain the apparent
position of the object.
Transmission case
==================
When any of the options "XLT", "XCN", "XLT+S", "XCN+S" is
selected, spkezp_c computes the position of the target body T at
epoch et+lt, where 'lt' is the one-way light time. 'lt' is the
solution of the light-time equation
| T(et+lt) - O(et) |
lt = ------------------------ (3)
c
Subtracting the geometric position of the observer, O(et),
gives the position of the target body relative to the
observer: T(et-lt) - O(et).
SSB --> O(et)
/ | *
/ | * T(et+lt) - O(et)
/ |*
/ *|
V V V
T(et+lt) T(et)
The position component of the light-time corrected position
is the vector
T(et+lt) - O(et)
If correction for stellar aberration is requested, the target
position is rotated away from the solar system barycenter-
relative velocity vector of the observer. The rotation is
computed as in the reception case, but the sign of the
rotation angle is negated.
Precision of light time corrections
===================================
Corrections using one iteration of the light time solution
----------------------------------------------------------
When the requested aberration correction is "LT", "LT+S",
"XLT", or "XLT+S", only one iteration is performed in the
algorithm used to compute 'lt'.
The relative error in this computation
| LT_ACTUAL - LT_COMPUTED | / LT_ACTUAL
is at most
(V/C)**2
----------
1 - (V/C)
which is well approximated by (V/C)**2, where V is the
velocity of the target relative to an inertial frame and C is
the speed of light.
For nearly all objects in the solar system V is less than 60
km/sec. The value of C is 300000 km/sec. Thus the one
iteration solution for 'lt' has a potential relative error of
not more than 4*10**-8. This is a potential light time error
of approximately 2*10**-5 seconds per astronomical unit of
distance separating the observer and target. Given the bound
on V cited above:
As long as the observer and target are
separated by less than 50 astronomical units,
the error in the light time returned using
the one-iteration light time corrections
is less than 1 millisecond.
Converged corrections
---------------------
When the requested aberration correction is "CN", "CN+S",
"XCN", or "XCN+S", three iterations are performed in the
computation of 'lt'. The relative error present in this
solution is at most
(V/C)**4
----------
1 - (V/C)
which is well approximated by (V/C)**4. Mathematically the
precision of this computation is better than a nanosecond for
any pair of objects in the solar system.
However, to model the actual light time between target and
observer one must take into account effects due to general
relativity. These may be as high as a few hundredths of a
millisecond for some objects.
When one considers the extra time required to compute the
converged Newtonian light time (the state of the target relative
to the solar system barycenter is looked up three times instead
of once) together with the real gain in accuracy, it seems
unlikely that you will want to request either the "CN" or "CN+S"
light time corrections. However, these corrections can be useful
for testing situations where high precision (as opposed to
accuracy) is required.
Relativistic Corrections
=========================
This routine does not attempt to perform either general or
special relativistic corrections in computing the various
aberration corrections. For many applications relativistic
corrections are not worth the expense of added computation
cycles. If however, your application requires these additional
corrections we suggest you consult the astronomical almanac (page
B36) for a discussion of how to carry out these corrections.
-Examples
1) Load a planetary ephemeris SPK, then look up a series of
geometric positions of the moon relative to the earth,
referenced to the J2000 frame.
#include <stdio.h>
#include "SpiceUsr.h"
void main()
{
#define ABCORR "NONE"
#define FRAME "J2000"
/.
The name of the SPK file shown here is fictitious;
you must supply the name of an SPK file available
on your own computer system.
./
#define SPK "planetary_spk.bsp"
/.
ET0 represents the date 2000 Jan 1 12:00:00 TDB.
./
#define ET0 0.0
/.
Use a time step of 1 hour; look up 100 states.
./
#define STEP 3600.0
#define MAXITR 100
/.
The NAIF IDs of the earth and moon are 399 and 301 respectively.
./
#define OBSERVER 399
#define TARGET 301
/.
Local variables
./
SpiceInt i;
SpiceDouble et;
SpiceDouble lt;
SpiceDouble pos [3];
/.
Load the spk file.
./
furnsh_c ( SPK );
/.
Step through a series of epochs, looking up a position vector
at each one.
./
for ( i = 0; i < MAXITR; i++ )
{
et = ET0 + i*STEP;
spkezp_c ( TARGET, et, FRAME, ABCORR,
OBSERVER, pos, < );
printf( "\net = %20.10f\n\n", et );
printf( "J2000 x-position (km): %20.10f\n", pos[0] );
printf( "J2000 y-position (km): %20.10f\n", pos[1] );
printf( "J2000 z-position (km): %20.10f\n", pos[2] );
}
}
-Restrictions
None.
-Literature_References
SPK Required Reading.
-Author_and_Institution
C.H. Acton (JPL)
B.V. Semenov (JPL)
N.J. Bachman (JPL)
W.L. Taber (JPL)
-Version
-CSPICE Version 2.0.5, 04-APR-2008 (NJB)
Corrected minor error in description of XLT+S aberration
correction.
-CSPICE Version 2.0.4, 17-APR-2005 (NJB)
Error was corrected in example program: variable name `state'
was changed to `pos' in printf calls.
-CSPICE Version 2.0.3, 12-DEC-2004 (NJB)
Minor header error was corrected.
-CSPICE Version 2.0.2, 13-OCT-2003 (EDW)
Various minor header changes were made to improve clarity.
Added mention that 'lt' returns a value in seconds.
-CSPICE Version 2.0.1, 29-JUL-2003 (NJB) (CHA)
Various minor header changes were made to improve clarity.
-CSPICE Version 2.0.0, 31-DEC-2001 (NJB)
Updated to handle aberration corrections for transmission
of radiation. Formerly, only the reception case was
supported. The header was revised and expanded to explain
the functionality of this routine in more detail.
-CSPICE Version 1.0.0, 29-MAY-1999 (NJB) (WLT)
-Index_Entries
get target position relative to an observer
get position relative observer corrected for aberrations
read ephemeris data
read trajectory data
-&
*/
{ /* Begin spkezp_c */
/*
Participate in error tracing.
*/
chkin_c ( "spkezp_c" );
/*
Check the input strings to make sure the pointers are non-null
and the string lengths are non-zero.
*/
CHKFSTR ( CHK_STANDARD, "spkezp_c", ref );
CHKFSTR ( CHK_STANDARD, "spkezp_c", abcorr );
/*
Call the f2c'd Fortran routine. Use explicit type casts for every
type defined by f2c.
*/
spkezp_ ( ( integer * ) &targ,
( doublereal * ) &et,
( char * ) ref,
( char * ) abcorr,
( integer * ) &obs,
( doublereal * ) ptarg,
( doublereal * ) lt,
( ftnlen ) strlen(ref),
( ftnlen ) strlen(abcorr) );
chkout_c ( "spkezp_c" );
} /* End spkezp_c */
/* $Procedure ZZGFDIQ ( GF, return distance between objects ) */
/* Subroutine */ int zzgfdiq_(integer *targid, doublereal *et, char *abcorr,
integer *obsid, doublereal *dist, ftnlen abcorr_len)
{
extern /* Subroutine */ int chkin_(char *, ftnlen);
extern doublereal vnorm_(doublereal *);
extern logical failed_(void);
doublereal lt;
extern /* Subroutine */ int chkout_(char *, ftnlen), spkezp_(integer *,
doublereal *, char *, char *, integer *, doublereal *, doublereal
*, ftnlen, ftnlen);
extern logical return_(void);
doublereal pos[3];
/* $ Abstract */
/* SPICE Private routine intended solely for the support of SPICE */
/* routines. Users should not call this routine directly due */
/* to the volatile nature of this routine. */
/* Return the distance between two ephemeris objects, optionally */
/* corrected for light time and stellar aberration. */
/* $ Disclaimer */
/* THIS SOFTWARE AND ANY RELATED MATERIALS WERE CREATED BY THE */
/* CALIFORNIA INSTITUTE OF TECHNOLOGY (CALTECH) UNDER A U.S. */
/* GOVERNMENT CONTRACT WITH THE NATIONAL AERONAUTICS AND SPACE */
/* ADMINISTRATION (NASA). THE SOFTWARE IS TECHNOLOGY AND SOFTWARE */
/* PUBLICLY AVAILABLE UNDER U.S. EXPORT LAWS AND IS PROVIDED "AS-IS" */
/* TO THE RECIPIENT WITHOUT WARRANTY OF ANY KIND, INCLUDING ANY */
/* WARRANTIES OF PERFORMANCE OR MERCHANTABILITY OR FITNESS FOR A */
/* PARTICULAR USE OR PURPOSE (AS SET FORTH IN UNITED STATES UCC */
/* SECTIONS 2312-2313) OR FOR ANY PURPOSE WHATSOEVER, FOR THE */
/* SOFTWARE AND RELATED MATERIALS, HOWEVER USED. */
/* IN NO EVENT SHALL CALTECH, ITS JET PROPULSION LABORATORY, OR NASA */
/* BE LIABLE FOR ANY DAMAGES AND/OR COSTS, INCLUDING, BUT NOT */
/* LIMITED TO, INCIDENTAL OR CONSEQUENTIAL DAMAGES OF ANY KIND, */
/* INCLUDING ECONOMIC DAMAGE OR INJURY TO PROPERTY AND LOST PROFITS, */
/* REGARDLESS OF WHETHER CALTECH, JPL, OR NASA BE ADVISED, HAVE */
/* REASON TO KNOW, OR, IN FACT, SHALL KNOW OF THE POSSIBILITY. */
/* RECIPIENT BEARS ALL RISK RELATING TO QUALITY AND PERFORMANCE OF */
/* THE SOFTWARE AND ANY RELATED MATERIALS, AND AGREES TO INDEMNIFY */
/* CALTECH AND NASA FOR ALL THIRD-PARTY CLAIMS RESULTING FROM THE */
/* ACTIONS OF RECIPIENT IN THE USE OF THE SOFTWARE. */
/* $ Required_Reading */
/* GF */
/* NAIF_IDS */
/* SPK */
/* TIME */
/* $ Keywords */
/* DISTANCE */
/* EPHEMERIS */
/* GEOMETRY */
/* SEARCH */
/* $ Declarations */
/* $ Brief_I/O */
/* VARIABLE I/O DESCRIPTION */
/* -------- --- -------------------------------------------------- */
/* TARGID I Target body. */
/* ET I Observer epoch. */
/* ABCORR I Aberration correction flag. */
/* OBSID I Observing body. */
/* DIST O Distance between target and observer. */
/* $ Detailed_Input */
/* TARGID is the NAIF ID code for a target body. The target and */
/* observer define a position vector that points from */
/* the observer to the target. */
/* ET is the ephemeris time, expressed as seconds past */
/* J2000 TDB, at which the position of the target body */
/* relative to the observer is to be computed. ET refers */
/* to time at the observer's location. */
/* ABCORR indicates the aberration corrections to be applied to */
/* the position of the target body to account for */
/* one-way light time and stellar aberration. Any */
/* aberration correction accepted by SPKEZR may be used. */
/* $ Detailed_Output */
/* DIST is the norm (magnitude) of the specified Cartesian */
/* 3-vector representing the position of the target body */
/* relative to the specified observer, where the */
/* position is corrected for the specified aberrations. */
/* The position vector points from the observer's */
/* location at ET to the aberration-corrected location */
/* of the target. */
/* Units are km. */
/* $ Parameters */
/* None. */
/* $ Exceptions */
/* 1) If an error occurs while reading an SPK or other kernel file, */
/* the error will be diagnosed by a routine in the call tree */
/* of this routine. */
/* $ Files */
/* Appropriate 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 for the */
/* input epoch 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. */
/* - If non-inertial reference frames are used, then PCK */
/* files, frame kernels, C-kernels, and SCLK kernels may be */
/* needed. */
/* In all cases, kernel data are normally loaded once per program */
/* run, NOT every time this routine is called. */
/* $ Particulars */
/* This routine centralizes distance computations performed by */
/* entry points in the GF distance utility package ZZGFDIU. */
/* $ Examples */
/* See the entry point ZZGFDIGQ in ZZGFDIU. */
/* $ Restrictions */
/* This is a SPICELIB private routine; it should not be called by */
/* user applications. */
/* $ Literature_References */
/* None. */
/* $ Author_and_Institution */
/* N.J. Bachman (JPL) */
/* L.S. Elson (JPL) */
/* W.L. Taber (JPL) */
/* I.M. Underwood (JPL) */
/* E.D. Wright (JPL) */
/* $ Version */
/* - SPICELIB Version 1.0.0 05-MAR-2009 (NJB) (LSE) (WLT) (IMU) (EDW) */
/* -& */
/* $ Index_Entries */
/* compute the apparent distance between two objects */
/* -& */
/* SPICELIB functions */
/* Local Variables */
/* Standard SPICE error handling. */
if (return_()) {
return 0;
}
chkin_("ZZGFDIQ", (ftnlen)7);
/* Get the position of the target relative to the observer. */
spkezp_(targid, et, "J2000", abcorr, obsid, pos, <, (ftnlen)5,
abcorr_len);
if (failed_()) {
chkout_("ZZGFDIQ", (ftnlen)7);
return 0;
}
*dist = vnorm_(pos);
chkout_("ZZGFDIQ", (ftnlen)7);
return 0;
} /* zzgfdiq_ */