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JPLEPHINTERP

JPLEPHINTERP

Name


  JPLEPHINTERP

Author


  Craig B. Markwardt, NASA/GSFC Code 662, Greenbelt, MD 20770
  craigm@lheamail.gsfc.nasa.gov
  UPDATED VERSIONs can be found on my WEB PAGE:
      http://cow.physics.wisc.edu/~craigm/idl/idl.html

Purpose


  Interpolate position and motion of planetary bodies (JPL Ephemeris)

Major Topics


  Planetary Orbits, Interpolation

Calling Sequence


  JPLEPHINTERP, INFO, RAWDATA, T, X, Y, Z, [VX, VY, VZ, /EARTH, /SUN,
        OBJECTNAME=, CENTER=, TBASE=, POSUNITS=, VELUNITS= ]

Description



  JPLEPHINTERP interpolates the JPL DE200 or DE405 planetary
  ephemeris to find the positions and motions of planetary bodies.
  This routine is the second stage of a two-stage process to
  interpolate the JPL ephemeris. In this first stage, the file is
  opened using JPLEPHREAD, and the relevant portions of the table
  are read and stored into the two variables INFO and RAWDATA. In
  the second stage, the user actually interpolates the ephemeris for
  the desired bodies and to the desired ephemeris time using
  JPLEPHINTERP.
  The only independent variable which must be specified is T, the
  ephemeris time. For low to moderate accuracy applications, T is
  simply the conventional calendar date, expressed in Julian days.
  See below for high precision applications.
  Upon output, the position components of the desired body are
  returned in parameters X, Y and Z, and if requested velocity
  components are returned in parameters VX, VY and VZ. Coordinates
  are referred to the ephemeris's coordinate system: FK5 for
  JPL-DE200 and ICRS for JPL-DE405. By default, the origin of
  coordinates is the solar system barycenter (SSB), unless another
  origin is selected using the CENTER keyword.
  Users must set the VELOCITY keyword to generate body velocities.
  By default they are not generated.
  Users can select the desired body by using either the EARTH or SUN
  keywords, or the OBJECTNAME keyword.
  By default, positions are returned in units of KM and velocities
  in units of KM/DAY. However, the output units are selectable by
  setting the POSUNITS and VELUNITS keywords.
  High Precision Applications
  If the required precision is finer than a few hundred meters, the
  user must be aware that the formal definition of the ephemeris
  time is the coordinate time of a clock placed at the solar system
  barycenter (SSB). If the user's time is measured by a clock
  positioned elsewhere, then various corrections must be applied.
  Usually, the most significant correction is that from the
  geocenter to the SSB (see Fairhead & Bretagnon 1990; Fukushima
  1995). Not applying this correction creates an error with
  amplitude ~170 nano-light-seconds ( = 50 m) on the earth's
  position. (see TDB2TDT)
  For high precision, the user should also specify the TBASE
  keyword. TBASE should be considered a fixed epoch with respect to
  which T is measured; T should be small compared to TBASE.
  Internally, subtraction of large numbers occurs with TBASE first,
  so truncation error is minimized by specifying TBASE.
  Nutations and Librations
  This routine also provides information about earth nutations and
  lunar librations, which are stored in the JPL ephemeris tables.
  The POSUNITS and VELUNITS keywords do not affect these
  computations.
  Lunar librations in the form of three Euler angles are returned in
  X, Y, Z, in units of radians, and their time derivatives are
  returned in VX, VY, and VZ in units of radians per day.
  The earth nutation angles psi (nutation in longitude) and epsilon
  (nutation in obliquity) are returned in X and Y, in units of
  radians. Their time derivatives are returned in VX and VY
  respectively. The quantities returned in Z and VZ are undefined.
  Verification
  The precision routine has been verified using JPLEPHTEST, which is
  similar to the original JPL program EPHTEST. For years 1950 to
  2050, JPLEPHINTERP reproduces the original JPL ephemeris to within
  1 centimeter.
  Custom Ephemerides
  It is possible to make custom ephemerides using JPLEPHMAKE, or to
  augmented an existing ephemeris with additional data. In the
  former case JPLEPHINTERP should automatically choose the correct
  object from the table and interpolate it appropriately.
  For augmented ephemerides, the object can be specified by name,
  which works as expected, or by number, which has a special
  behavior. For augmented files only, the new objects begin at
  number 100.

Parameters



  INFO - structure returned by JPLEPHREAD. Users should not modify
          this structure.
  RAWDATA - raw data array returned by JPLEPHREAD. Users should not
            modify this data array.
  T - ephemeris time(s) of interest, relative to TBASE (i.e. the
      actual interpolation time is (T+TBASE)). May be a scalar or
      vector.
  X, Y, Z - upon return, the x-, y- and z-components of the body
            position are returned in these parameters. For
            nutations and librations see above.
  VX, VY, VZ - upon return, the x-, y- and z-components of the body
                velocity are returned in these parameters, if the
                VELOCITY keyword is set. For nutations and
                librations see above.

Keyword Parameters



  EARTH, SUN - set one of these keywords if the desired body is the
                earth or the sun. One of EARTH, SUN or OBJECTNAME
                must be specified.
  OBJECTNAME - a scalar string or integer, specifies the planetary
                body of interest. May take any one of the following
                integer or string values.
                  1 - 'MERCURY' 9 - 'PLUTO'
                  2 - 'VENUS' 10 - 'MOON' (earth's moon)
                  3 - 'EARTH' 11 - 'SUN'
                  4 - 'MARS' 12 - 'SOLARBARY' or 'SSB' (solar system barycenter)
                  5 - 'JUPITER' 13 - 'EARTHBARY' or 'EMB' (earth-moon barycenter)
                  6 - 'SATURN' 14 - 'NUTATIONS' (see above)
                  7 - 'URANUS' 15 - 'LIBRATIONS' (see above)
                  8 - 'NEPTUNE'
                For custom ephemerides, the user should specify the
                object name or number.
                For augmented ephemerides, the user should specify
                the name. If the number is specified, then numbers
                1-15 have the above meanings, and new objects are
                numbered starting at 100.
  CENTER - a scalar string or integer, specifies the origin of
            coordinates. See OBJECTNAME for allowed values.
            Default: 12 (Solar system barycenter)
  VELOCITY - if set, body velocities are generated and returned in
              VX, VY and VZ.
              Default: unset (no velocities)
  POSUNITS - a scalar string specifying the desired units for X, Y,
              and Z. Allowed values:
                'KM' - kilometers (default)
                'CM' - centimeters
                'AU' - astronomical units
                'LT-S' - light seconds
              If angles are requested, this keyword is ignored and
              the units are always 'RADIANS'.
  VELUNITS - a scalar string specifying the desired units for VX, VY
              and VZ. Allowed values:
                'KM/DAY' - kilometers per day (default)
                'KM/S' - kilometers per second
                'CM/S' - centimeters per second
                'LT-S/S' or 'V/C' - light seconds per second or
                    unitless ratio with speed of light, V/C
                'AU/DAY' - astronomical units per day
  TBASE - a scalar or vector, specifies a fixed epoch against wich T
          is measured. The ephemeris time will be (T+TBASE). Use
          this keyword for maximum precision.

Example



  Find position of earth at ephemeris time 2451544.5 JD. Units are
  in Astronomical Units.
  JPLEPHREAD, 'JPLEPH.200', pinfo, pdata, [2451544D, 2451545D]
  JPLEPHINTERP, pinfo, pdata, 2451544.5D, xearth, yearth, zearth, $
                /EARTH, posunits='AU'
   

References



  AXBARY, Arnold Rots.
      ftp://heasarc.gsfc.nasa.gov/xte/calib_data/clock/bary/
  HORIZONS, JPL Web-based ephermis calculator (Ephemeris DE406)
      http://ssd.jpl.nasa.gov/horizons.html
 
  Fairhead, L. & Bretagnon, P. 1990, A&A, 229, 240
  Fukushima, T. 1995, A&A, 294, 895
  Standish, E.M. 1982, "Orientation of the JPL Ephemerides,
      DE200/LE200, to the Dynamical Equinox of J2000", Astronomy &
      Astrophysics, vol. 114, pp. 297-302.
  Standish, E.M.: 1990, "The Observational Basis for JPL's DE200,
      the planetary ephemeris of the Astronomical Almanac", Astronomy
      & Astrophysics, vol. 233, pp. 252-271.

See Also


  JPLEPHREAD, JPLEPHINTERP, JPLEPHTEST, TDB2TDT, JPLEPHMAKE
 

Modification History


  Written and Documented, CM, Jun 2001
  Corrected bug in name conversion of NUTATIONS and LIBRATIONS, 18
    Oct 2001, CM
  Added code to handle custom-built ephemerides, 04 Mar 2002, CM
  Fix bug in evaluation of velocity (only appears in highest order
    polynomial term); JPLEPHTEST verification tests still pass;
    change is of order < 0.5 cm in position, 22 Nov 2004, CM
  Perform more validity checking on inputs; and more informative
    outputs, 09 Oct 2008, CM
  Allow SSB and EMB as shortcuts for solar system and earth-moon
    bary center, 15 Oct 2008, CM
  TBASE now allowed to be a vector or scalar, 01 Jan 2009, CM
  VELFAC keyword gives scale factor between POSUNITS and VELUNITS,
    12 Jan 2009, CM
  Add option VELUNITS='V/C' for unitless ratio with speed of light,
    2012-10-02, CM;
  $Id: jplephinterp.pro,v 1.19 2012/10/02 11:32:59 cmarkwar Exp $



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