.help polmo Jun99 "Slalib Package"
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      SUBROUTINE slPLMO ( ELONGM, PHIM, XP, YP, ELONG, PHI, DAZ )

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      P L M O
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  Polar motion:  correct site longitude and latitude for polar
  motion and calculate azimuth difference between celestial and
  terrestrial poles.

  Given:
     ELONGM   d      mean longitude of the observer (radians, east +ve)
     PHIM     d      mean geodetic latitude of the observer (radians)
     XP       d      polar motion x-coordinate (radians)
     YP       d      polar motion y-coordinate (radians)

  Returned:
     ELONG    d      true longitude of the observer (radians, east +ve)
     PHI      d      true geodetic latitude of the observer (radians)
     DAZ      d      azimuth correction (terrestrial-celestial, radians)

  Notes:

   1)  "Mean" longitude and latitude are the (fixed) values for the
       site's location with respect to the IERS terrestrial reference
       frame;  the latitude is geodetic.  TAKE CARE WITH THE LONGITUDE
       SIGN CONVENTION.  The longitudes used by the present routine
       are east-positive, in accordance with geographical convention
       (and right-handed).  In particular, note that the longitudes
       returned by the slOBS routine are west-positive, following
       astronomical usage, and must be reversed in sign before use in
       the present routine.

   2)  XP and YP are the (changing) coordinates of the Celestial
       Ephemeris Pole with respect to the IERS Reference Pole.
       XP is positive along the meridian at longitude 0 degrees,
       and YP is positive along the meridian at longitude
       270 degrees (i.e. 90 degrees west).  Values for XP,YP can
       be obtained from IERS circulars and equivalent publications;
       the maximum amplitude observed so far is about 0.3 arcseconds.

   3)  "True" longitude and latitude are the (moving) values for
       the site's location with respect to the celestial ephemeris
       pole and the meridian which corresponds to the Greenwich
       apparent sidereal time.  The true longitude and latitude
       link the terrestrial coordinates with the standard celestial
       models (for precession, nutation, sidereal time etc).

   4)  The azimuths produced by slAOP and slAOPQ are with
       respect to due north as defined by the Celestial Ephemeris
       Pole, and can therefore be called "celestial azimuths".
       However, a telescope fixed to the Earth measures azimuth
       essentially with respect to due north as defined by the
       IERS Reference Pole, and can therefore be called "terrestrial
       azimuth".  Uncorrected, this would manifest itself as a
       changing "azimuth zero-point error".  The value DAZ is the
       correction to be added to a celestial azimuth to produce
       a terrestrial azimuth.

   5)  The present routine is rigorous.  For most practical
       purposes, the following simplified formulae provide an
       adequate approximation:

       ELONG = ELONGM+XP*COS(ELONGM)-YP*SIN(ELONGM)
       PHI   = PHIM+(XP*SIN(ELONGM)+YP*COS(ELONGM))*TAN(PHIM)
       DAZ   = -SQRT(XP*XP+YP*YP)*COS(ELONGM-ATAN2(XP,YP))/COS(PHIM)

       An alternative formulation for DAZ is:

       X = COS(ELONGM)*COS(PHIM)
       Y = SIN(ELONGM)*COS(PHIM)
       DAZ = ATAN2(-X*YP-Y*XP,X*X+Y*Y)

   Reference:  Seidelmann, P.K. (ed), 1992.  "Explanatory Supplement
               to the Astronomical Almanac", ISBN 0-935702-68-7,
               sections 3.27, 4.25, 4.52.

  P.T.Wallace   Starlink   22 February 1996

  Copyright (C) 1995 Rutherford Appleton Laboratory
  Copyright (C) 1995 Association of Universities for Research in Astronomy Inc.

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