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SUBROUTINE slPLMO ( ELONGM, PHIM, XP, YP, ELONG, PHI, DAZ )
*+
* - - - - - -
* P L M O
* - - - - - -
*
* 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 30 November 2000
*
* Copyright (C) 2000 Rutherford Appleton Laboratory
*
* License:
* This program is free software; you can redistribute it and/or modify
* it under the terms of the GNU General Public License as published by
* the Free Software Foundation; either version 2 of the License, or
* (at your option) any later version.
*
* This program is distributed in the hope that it will be useful,
* but WITHOUT ANY WARRANTY; without even the implied warranty of
* MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the
* GNU General Public License for more details.
*
* You should have received a copy of the GNU General Public License
* along with this program (see SLA_CONDITIONS); if not, write to the
* Free Software Foundation, Inc., 51 Franklin Street, Fifth Floor,
* Boston, MA 02110-1301 USA
*
* Copyright (C) 1995 Association of Universities for Research in Astronomy Inc.
*-
IMPLICIT NONE
DOUBLE PRECISION ELONGM,PHIM,XP,YP,ELONG,PHI,DAZ
DOUBLE PRECISION SEL,CEL,SPH,CPH,XM,YM,ZM,XNM,YNM,ZNM,
: SXP,CXP,SYP,CYP,ZW,XT,YT,ZT,XNT,YNT
* Site mean longitude and mean geodetic latitude as a Cartesian vector
SEL=SIN(ELONGM)
CEL=COS(ELONGM)
SPH=SIN(PHIM)
CPH=COS(PHIM)
XM=CEL*CPH
YM=SEL*CPH
ZM=SPH
* Rotate site vector by polar motion, Y-component then X-component
SXP=SIN(XP)
CXP=COS(XP)
SYP=SIN(YP)
CYP=COS(YP)
ZW=(-YM*SYP+ZM*CYP)
XT=XM*CXP-ZW*SXP
YT=YM*CYP+ZM*SYP
ZT=XM*SXP+ZW*CXP
* Rotate also the geocentric direction of the terrestrial pole (0,0,1)
XNM=-SXP*CYP
YNM=SYP
ZNM=CXP*CYP
CPH=SQRT(XT*XT+YT*YT)
IF (CPH.EQ.0D0) XT=1D0
SEL=YT/CPH
CEL=XT/CPH
* Return true longitude and true geodetic latitude of site
IF (XT.NE.0D0.OR.YT.NE.0D0) THEN
ELONG=ATAN2(YT,XT)
ELSE
ELONG=0D0
END IF
PHI=ATAN2(ZT,CPH)
* Return current azimuth of terrestrial pole seen from site position
XNT=(XNM*CEL+YNM*SEL)*ZT-ZNM*CPH
YNT=-XNM*SEL+YNM*CEL
IF (XNT.NE.0D0.OR.YNT.NE.0D0) THEN
DAZ=ATAN2(-YNT,-XNT)
ELSE
DAZ=0D0
END IF
END
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