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EME Doppler calculations now use JPL Planetary Ephemeris.

Browse Source 
Also new, simplified routines for Doppler spread.
Beware! Not yet fully tested ...



git-svn-id: svn+ssh://svn.code.sf.net/p/wsjt/wsjt/branches/wsjtx@5496 ab8295b8-cf94-4d9e-aec4-7959e3be5d79
This commit is contained in:
Joe Taylor 2015-06-02 16:43:40 +00:00
parent adebd2420a
commit e837b9209e
17 changed files with 4495 additions and 378 deletions
Show Stats Download Patch File Download Diff File Expand all files Collapse all files

24
CMakeLists.txt
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@ -268,11 +268,8 @@ set (wsjt_FSRCS
lib/chkss2.f90
lib/coord.f90
lib/db.f90
lib/dcoord.f90
lib/decode65a.f90
lib/decode65b.f90
lib/fftw3mod.f90
lib/jt9fano.f90
lib/decode4.f90
lib/decoder.f90
lib/decjt9.f90
@ -280,18 +277,17 @@ set (wsjt_FSRCS
lib/deg2grid.f90
lib/demod64a.f90
lib/determ.f90
lib/dot.f90
lib/downsam9.f90
lib/encode232.f90
lib/encode4.f90
lib/entail.f90
lib/ephem.f90
lib/extract.F90
lib/extract4.f90
lib/geocentric.f90
lib/getmet4.f90
lib/fano232.f90
lib/fchisq.f90
lib/fchisq65.f90
lib/fftw3mod.f90
lib/fil3.f90
lib/fil3c.f90
lib/fil4.f90
@ -311,6 +307,7 @@ set (wsjt_FSRCS
lib/genwspr.f90
lib/geodist.f90
lib/getlags.f90
lib/getmet4.f90
lib/graycode.f90
lib/graycode65.f90
lib/grayline.f90
@ -323,13 +320,15 @@ set (wsjt_FSRCS
lib/interleave63.f90
lib/interleave9.f90
lib/inter_wspr.f90
lib/jplsubs.f
lib/jt4.f90
lib/jt4a.f90
lib/jt65a.f90
lib/jt9fano.f90
lib/libration.f90
lib/lpf1.f90
lib/mixlpf.f90
lib/moon2.f90
lib/moondop.f90
lib/moondopjpl.f90
lib/morse.f90
lib/move.f90
lib/options.f90
@ -343,6 +342,7 @@ set (wsjt_FSRCS
lib/savec2.f90
lib/sec_midn.f90
lib/setup65.f90
lib/slasubs.f
lib/sleep_msec.f90
lib/slope.f90
lib/smo.f90
@ -358,8 +358,6 @@ set (wsjt_FSRCS
lib/sync9.f90
lib/timer.f90
lib/timf2.f90
lib/tm2.f90
lib/toxyz.f90
lib/twkfreq.f90
lib/twkfreq65.f90
lib/wav11.f90
@ -1002,6 +1000,12 @@ install (FILES
#COMPONENT runtime
)
install (FILES
contrib/Ephemeris/JPLEPH
DESTINATION ${WSJT_SHARE_DESTINATION}/${WSJT_DATA_DESTINATION}
#COMPONENT runtime
)
#
# Mac installer files
#

BIN
contrib/Ephemeris/JPLEPH Normal file
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Binary file not shown.

6
lib/astro.f90
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@ -42,11 +42,7 @@ subroutine astro(nyear,month,nday,uth,freq8,Mygrid, &
call sun(nyear,month,nday,uth,lon,lat,RASun,DecSun,LST, &
AzSun,ElSun,mjd,day)
! freq=nfreq*1.e6
! if(nfreq.eq.2) freq=1.8e6
! if(nfreq.eq.4) freq=3.5e6
call MoonDop(nyear,month,nday,uth,lon,lat,RAMoon,DecMoon, &
call MoonDopJPL(nyear,month,nday,uth,lon,lat,RAMoon,DecMoon, &
LST,HA,AzMoon,ElMoon,vr,dist)
! Compute spatial polarization offset

29
lib/astro0.f90
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@ -1,14 +1,16 @@
subroutine astro0(nyear,month,nday,uth8,freq8,mygrid,hisgrid, &
AzSun8,ElSun8,AzMoon8,ElMoon8,AzMoonB8,ElMoonB8,ntsky,ndop,ndop00, &
dbMoon8,RAMoon8,DecMoon8,HA8,Dgrd8,sd8,poloffset8,xnr8,dfdt,dfdt0, &
width1,width2,w501,w502,xlst8,techo8)
width1,width2,xlst8,techo8)
parameter (DEGS=57.2957795130823d0)
character*6 mygrid,hisgrid
real*8 AzSun8,ElSun8,AzMoon8,ElMoon8,AzMoonB8,ElMoonB8
real*8 dbMoon8,RAMoon8,DecMoon8,HA8,Dgrd8,xnr8,dfdt,dfdt0,dt
real*8 sd8,poloffset8,day8,width1,width2,w501,w502,xlst8
real*8 sd8,poloffset8,day8,width1,width2,xlst8
real*8 uth8,techo8,freq8
real*8 xl,b
common/librcom/xl(2),b(2)
data uth8z/0.d0/
save
@ -19,18 +21,19 @@ subroutine astro0(nyear,month,nday,uth8,freq8,mygrid,hisgrid, &
day,xlon2,xlat2,xlst,techo)
AzMoonB8=AzMoon
ElMoonB8=ElMoon
xl2=xl(1)
xl2a=xl(2)
b2=b(1)
b2a=b(2)
call astro(nyear,month,nday,uth,freq8,mygrid,1,1, &
AzSun,ElSun,AzMoon,ElMoon,ntsky,doppler00,doppler, &
dbMoon,RAMoon,DecMoon,HA,Dgrd,sd,poloffset,xnr, &
day,xlon1,xlat1,xlst,techo)
xl1=xl(1)
xl1a=xl(2)
b1=b(1)
b1a=b(2)
day8=day
xlst8=xlst
techo8=techo
call tm2(day8,xlat1,xlon1,xl1,b1)
call tm2(day8,xlat2,xlon2,xl2,b2)
call tm2(day8+1.d0/1440.0,xlat1,xlon1,xl1a,b1a)
call tm2(day8+1.d0/1440.0,xlat2,xlon2,xl2a,b2a)
fghz=1.d-9*freq8
dldt1=DEGS*(xl1a-xl1)
dbdt1=DEGS*(b1a-b1)
@ -41,14 +44,6 @@ subroutine astro0(nyear,month,nday,uth8,freq8,mygrid,hisgrid, &
rate2=sqrt((dldt1+dldt2)**2 + (dbdt1+dbdt2)**2)
width2=0.5*6741*fghz*rate2
fbend=0.7
a2=0.0045*log(fghz/fbend)/log(1.05)
if(fghz.lt.fbend) a2=0.0
f50=0.19 * (fghz/fbend)**a2
if(f50.gt.1.0) f50=1.0
w501=f50*width1
w502=f50*width2
AzSun8=AzSun
ElSun8=ElSun
AzMoon8=AzMoon

6
lib/astrosub.f90
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@ -6,12 +6,16 @@ subroutine astrosub(nyear,month,nday,uth8,freq8,mygrid,hisgrid, &
implicit real*8 (a-h,o-z)
character*6 mygrid,hisgrid,c1*1
character*6 AzElFileName*(*),jpleph*(*)
character*80 jpleph_file_name
logical*1 bTx
common/jplcom/jpleph_file_name
jpleph_file_name=jpleph
call astro0(nyear,month,nday,uth8,freq8,mygrid,hisgrid, &
AzSun8,ElSun8,AzMoon8,ElMoon8,AzMoonB8,ElMoonB8,ntsky,ndop,ndop00, &
dbMoon8,RAMoon8,DecMoon8,HA8,Dgrd8,sd8,poloffset8,xnr8,dfdt,dfdt0, &
width1,width2,w501,w502,xlst8,techo8)
width1,width2,xlst8,techo8)
imin=60*uth8
isec=3600*uth8

40
lib/dcoord.f90
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@ -1,40 +0,0 @@
SUBROUTINE DCOORD(A0,B0,AP,BP,A1,B1,A2,B2)
implicit real*8 (a-h,o-z)
! Examples:
! 1. From ha,dec to az,el:
! call coord(pi,pio2-lat,0.,lat,ha,dec,az,el)
! 2. From az,el to ha,dec:
! call coord(pi,pio2-lat,0.,lat,az,el,ha,dec)
! 3. From ra,dec to l,b
! call coord(4.635594495,-0.504691042,3.355395488,0.478220215,
! ra,dec,l,b)
! 4. From l,b to ra,dec
! call coord(1.705981071d0,-1.050357016d0,2.146800277d0,
! 0.478220215d0,l,b,ra,dec)
! 5. From ecliptic latitude (eb) and longitude (el) to ra, dec:
! call coord(0.d0,0.d0,-pio2,pio2-23.443*pi/180,ra,dec,el,eb)
SB0=sin(B0)
CB0=cos(B0)
SBP=sin(BP)
CBP=cos(BP)
SB1=sin(B1)
CB1=cos(B1)
SB2=SBP*SB1 + CBP*CB1*cos(AP-A1)
CB2=SQRT(1.D0-SB2**2)
B2=atan(SB2/CB2)
SAA=sin(AP-A1)*CB1/CB2
CAA=(SB1-SB2*SBP)/(CB2*CBP)
CBB=SB0/CBP
SBB=sin(AP-A0)*CB0
SA2=SAA*CBB-CAA*SBB
CA2=CAA*CBB+SAA*SBB
TA2O2=0.0 !Shut up compiler warnings. -db
IF(CA2.LE.0.D0) TA2O2=(1.D0-CA2)/SA2
IF(CA2.GT.0.D0) TA2O2=SA2/(1.D0+CA2)
A2=2.D0*atan(TA2O2)
IF(A2.LT.0.D0) A2=A2+6.2831853071795864D0
RETURN
END SUBROUTINE DCOORD

11
lib/dot.f90
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@ -1,11 +0,0 @@
real*8 function dot(x,y)
real*8 x(3),y(3)
dot=0.d0
do i=1,3
dot=dot+x(i)*y(i)
enddo
return
end function dot

87
lib/ephem.f90 Normal file
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@ -0,0 +1,87 @@
subroutine ephem(mjd0,dut,east_long,geodetic_lat,height,nspecial, &
RA,Dec,Az,El,techo,dop,fspread_1GHz,vr)
implicit real*8 (a-h,o-z)
real*8 jd !Time of observationa as a Julian Date
real*8 mjd,mjd0 !Modified Julian Date
real*8 prec(3,3) !Precession matrix, J2000 to Date
real*8 rmatn(3,3) !Nutation matrix
real*8 rme2000(6) !Vector from Earth center to Moon, JD2000
real*8 rmeDate(6) !Vector from Earth center to Moon at Date
real*8 rmeTrue(6) !Include nutation
real*8 raeTrue(6) !Vector from Earth center to Obs at Date
real*8 rmaTrue(6) !Vector from Obs to Moon at Date
logical km,bary,jplok !Set km=.true. to get km, km/s from ephemeris
common/stcomx/km,bary,pvsun(6) !Common used in JPL subroutines
common/librcom/xl(2),b(2)
twopi=8.d0*atan(1.d0) !Define some constants
rad=360.d0/twopi
clight=2.99792458d5
au2km=0.1495978706910000d9
pi=0.5d0*twopi
pio2=0.5d0*pi
km=.true.
freq=1000.0d6
do jj=1,2
mjd=mjd0
if(jj.eq.1) mjd=mjd - 1.d0/1440.d0
djutc=mjd
jd=2400000.5d0 + mjd
djtt=mjd + sla_DTT(jd)/86400.d0
ttjd=jd + sla_DTT(jd)/86400.d0
! inquire(file='JPLEPH',exist=jplok)
! if(jplok) then
if(nspecial.ne.8) then
call pleph(ttjd,10,3,rme2000) !RME (J2000) from JPL ephemeris
year=2000.d0 + (jd-2451545.d0)/365.25d0
call sla_PREC (2000.0d0, year, prec) !Get precession matrix
rmeDate(1:3)=matmul(prec,rme2000(1:3)) !Moon geocentric xyz at Date
rmeDate(4:6)=matmul(prec,rme2000(4:6)) !Moon geocentric vel at Date
else
call sla_DMOON(djtt,rmeDate) !No JPL ephemeris, use DMOON
rmeDate=rmeDate*au2km
endif
if(nspecial.eq.7) then
rmeTrue=rmeDate
else
!Nutation to true equinox of Date
call sla_NUT(djtt,rmatn)
call sla_DMXV(rmatn,rmeDate,rmeTrue)
call sla_DMXV(rmatn,rmeDate(4),rmeTrue(4))
endif
! Local Apparent Sidereal Time:
djut1=djutc + dut/86400.d0
if(nspecial.eq.6) djut1=djutc
xlast=sla_DRANRM(sla_GMST(djut1) + sla_EQEQX(djtt) + east_long)
call sla_PVOBS(geodetic_lat,height,xlast,raeTrue)
rmaTrue=rmeTrue - raeTrue*au2km
if(nspecial.ne.2) then
! Allow for planetary aberration
tl=499.004782D0*SQRT(rmaTrue(1)**2 + rmaTrue(2)**2 + rmaTrue(3)**2)
rmaTrue(1:3)=rmaTrue(1:3)-tl*rmaTrue(4:6)/au2km
endif
!Topocentric RA, Dec, dist, velocity
call sla_DC62S(rmaTrue,RA,Dec,dist,RAdot,DECdot,vr)
dop=-2.d0 * freq * vr/clight !EME doppler shift
techo=2.d0*dist/clight !Echo delay time (s)
call libration(jd,RA,Dec,xl(jj),b(jj))
enddo
fspread_1GHz=0.0d0
dldt=57.2957795131*(xl(2)-xl(1))
dbdt=57.2957795131*(b(2)-b(1))
rate=sqrt((2*dldt)**2 + (2*dbdt)**2)
fspread_1GHz=0.5*6741*rate
call sla_DE2H(xlast-RA,Dec,geodetic_lat,Az,El)
return
end subroutine ephem

17
lib/geocentric.f90
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@ -1,17 +0,0 @@
subroutine geocentric(alat,elev,hlt,erad)
implicit real*8 (a-h,o-z)
! IAU 1976 flattening f, equatorial radius a
f = 1.d0/298.257d0
a = 6378140.d0
c = 1.d0/sqrt(1.d0 + (-2.d0 + f)*f*sin(alat)*sin(alat))
arcf = (a*c + elev)*cos(alat)
arsf = (a*(1.d0 - f)*(1.d0 - f)*c + elev)*sin(alat)
hlt = datan2(arsf,arcf)
erad = sqrt(arcf*arcf + arsf*arsf)
erad = 0.001d0*erad
return
end subroutine geocentric

899
lib/jplsubs.f Normal file
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@ -0,0 +1,899 @@
C++++++++++++++++++++++++
C
SUBROUTINE FSIZER1(NRECL,KSIZE,NRFILE,NAMFIL)
C
C++++++++++++++++++++++++
C
C Version 1.0 uses the INQUIRE statement to find out the the record length
C of the direct access file before opening it. This procedure is non-standard,
C but seems to work for VAX machines.
C
C THE SUBROUTINE ALSO SETS THE VALUES OF NRECL, NRFILE, AND NAMFIL.
C *****************************************************************
C *****************************************************************
C
C THE PARAMETERS NAMFIL, NRECL, AND NRFILE ARE TO BE SET BY THE USER
C
C *****************************************************************
C NAMFIL IS THE EXTERNAL NAME OF THE BINARY EPHEMERIS FILE
CHARACTER*80 NAMFIL
c NAMFIL='JPLEPH'
C *****************************************************************
C NRECL=1 IF "RECL" IN THE OPEN STATEMENT IS THE RECORD LENGTH IN S.P. WORDS
C NRECL=4 IF "RECL" IN THE OPEN STATEMENT IS THE RECORD LENGTH IN BYTES
C (for a VAX, it is probably 1)
C
NRECL=4
C *****************************************************************
C NRFILE IS THE INTERNAL UNIT NUMBER USED FOR THE EPHEMERIS FILE
c NRFILE=12
C *****************************************************************
C FIND THE RECORD SIZE USING THE INQUIRE STATEMENT
c IRECSZ=0
INQUIRE(FILE=NAMFIL,RECL=IRECSZ)
C IF 'INQUIRE' DOES NOT WORK, USUALLY IRECSZ WILL BE LEFT AT 0
IF(IRECSZ .LE. 0) write(*,*)
. ' INQUIRE STATEMENT PROBABLY DID NOT WORK'
KSIZE=IRECSZ/NRECL
RETURN
END
C++++++++++++++++++++++++
C
SUBROUTINE FSIZER2(NRECL,KSIZE,NRFILE,NAMFIL)
C
C++++++++++++++++++++++++
C THIS SUBROUTINE OPENS THE FILE, 'NAMFIL', WITH A PHONY RECORD LENGTH, READS
C THE FIRST RECORD, AND USES THE INFO TO COMPUTE KSIZE, THE NUMBER OF SINGLE
C PRECISION WORDS IN A RECORD.
C
C THE SUBROUTINE ALSO SETS THE VALUES OF NRECL, NRFILE, AND NAMFIL.
IMPLICIT DOUBLE PRECISION(A-H,O-Z)
SAVE
INTEGER OLDMAX
PARAMETER (OLDMAX = 400)
INTEGER NMAX
PARAMETER (NMAX = 1000)
CHARACTER*6 TTL(14,3),CNAM(NMAX)
CHARACTER*80 NAMFIL,jpleph_file_name
DIMENSION SS(3)
INTEGER IPT(3,13)
common/jplcom/jpleph_file_name
C *****************************************************************
C *****************************************************************
C
C THE PARAMETERS NRECL, NRFILE, AND NAMFIL ARE TO BE SET BY THE USER
C
C *****************************************************************
C NRECL=1 IF "RECL" IN THE OPEN STATEMENT IS THE RECORD LENGTH IN S.P. WORDS
C NRECL=4 IF "RECL" IN THE OPEN STATEMENT IS THE RECORD LENGTH IN BYTES
C (for UNIX, it is probably 4)
C
NRECL=4
C NRFILE IS THE INTERNAL UNIT NUMBER USED FOR THE EPHEMERIS FILE
NRFILE=12
C NAMFIL IS THE EXTERNAL NAME OF THE BINARY EPHEMERIS FILE
! NAMFIL='JPLEPH'
NAMFIL=jpleph_file_name
C *****************************************************************
C *****************************************************************
C ** OPEN THE DIRECT-ACCESS FILE AND GET THE POINTERS IN ORDER TO
C ** DETERMINE THE SIZE OF THE EPHEMERIS RECORD
MRECL=NRECL*1000
OPEN(NRFILE,
* FILE=NAMFIL,
* ACCESS='DIRECT',
* FORM='UNFORMATTED',
* RECL=MRECL,
* STATUS='OLD')
READ(NRFILE,REC=1)TTL,(CNAM(K),K=1,OLDMAX),SS,NCON,AU,EMRAT,
& ((IPT(I,J),I=1,3),J=1,12),NUMDE,(IPT(I,13),I=1,3)
CLOSE(NRFILE)
C FIND THE NUMBER OF EPHEMERIS COEFFICIENTS FROM THE POINTERS
KMX = 0
KHI = 0
DO I = 1,13
IF (IPT(1,I) .GT. KMX) THEN
KMX = IPT(1,I)
KHI = I
ENDIF
ENDDO
ND = 3
IF (KHI .EQ. 12) ND=2
KSIZE = 2*(IPT(1,KHI)+ND*IPT(2,KHI)*IPT(3,KHI)-1)
RETURN
END
C++++++++++++++++++++++++
C
SUBROUTINE FSIZER3(NRECL,KSIZE,NRFILE,NAMFIL)
C
C++++++++++++++++++++++++
C
C THE SUBROUTINE SETS THE VALUES OF NRECL, KSIZE, NRFILE, AND NAMFIL.
SAVE
CHARACTER*80 NAMFIL,jpleph_file_name
common/jplcom/jpleph_file_name
C *****************************************************************
C *****************************************************************
C
C THE PARAMETERS NRECL, NRFILE, AND NAMFIL ARE TO BE SET BY THE USER
C *****************************************************************
C NRECL=1 IF "RECL" IN THE OPEN STATEMENT IS THE RECORD LENGTH IN S.P. WORDS
C NRECL=4 IF "RECL" IN THE OPEN STATEMENT IS THE RECORD LENGTH IN BYTES
NRECL=4
C *****************************************************************
C NRFILE IS THE INTERNAL UNIT NUMBER USED FOR THE EPHEMERIS FILE (DEFAULT: 12)
NRFILE=12
C *****************************************************************
C NAMFIL IS THE EXTERNAL NAME OF THE BINARY EPHEMERIS FILE
! NAMFIL='JPLEPH'
NAMFIL=jpleph_file_name
C *****************************************************************
C KSIZE must be set by the user according to the ephemeris to be read
C For de200, set KSIZE to 1652
C For de405, set KSIZE to 2036
C For de406, set KSIZE to 1456
C For de414, set KSIZE to 2036
C For de418, set KSIZE to 2036
C For de421, set KSIZE to 2036
C For de422, set KSIZE to 2036
C For de423, set KSIZE to 2036
C For de424, set KSIZE to 2036
C For de430, set KSIZE to 2036
KSIZE = 2036
C *******************************************************************
RETURN
END
C++++++++++++++++++++++++++
C
SUBROUTINE PLEPH ( ET, NTARG, NCENT, RRD )
C
C++++++++++++++++++++++++++
C NOTE : Over the years, different versions of PLEPH have had a fifth argument:
C sometimes, an error return statement number; sometimes, a logical denoting
C whether or not the requested date is covered by the ephemeris. We apologize
C for this inconsistency; in this present version, we use only the four necessary
C arguments and do the testing outside of the subroutine.
C
C THIS SUBROUTINE READS THE JPL PLANETARY EPHEMERIS
C AND GIVES THE POSITION AND VELOCITY OF THE POINT 'NTARG'
C WITH RESPECT TO 'NCENT'.
C
C CALLING SEQUENCE PARAMETERS:
C
C ET = D.P. JULIAN EPHEMERIS DATE AT WHICH INTERPOLATION
C IS WANTED.
C
C ** NOTE THE ENTRY DPLEPH FOR A DOUBLY-DIMENSIONED TIME **
C THE REASON FOR THIS OPTION IS DISCUSSED IN THE
C SUBROUTINE STATE
C
C NTARG = INTEGER NUMBER OF 'TARGET' POINT.
C
C NCENT = INTEGER NUMBER OF CENTER POINT.
C
C THE NUMBERING CONVENTION FOR 'NTARG' AND 'NCENT' IS:
C
C 1 = MERCURY 8 = NEPTUNE
C 2 = VENUS 9 = PLUTO
C 3 = EARTH 10 = MOON
C 4 = MARS 11 = SUN
C 5 = JUPITER 12 = SOLAR-SYSTEM BARYCENTER
C 6 = SATURN 13 = EARTH-MOON BARYCENTER
C 7 = URANUS 14 = NUTATIONS (LONGITUDE AND OBLIQ)
C 15 = LIBRATIONS, IF ON EPH FILE
C
C (IF NUTATIONS ARE WANTED, SET NTARG = 14. FOR LIBRATIONS,
C SET NTARG = 15. SET NCENT=0.)
C
C RRD = OUTPUT 6-WORD D.P. ARRAY CONTAINING POSITION AND VELOCITY
C OF POINT 'NTARG' RELATIVE TO 'NCENT'. THE UNITS ARE AU AND
C AU/DAY. FOR LIBRATIONS THE UNITS ARE RADIANS AND RADIANS
C PER DAY. IN THE CASE OF NUTATIONS THE FIRST FOUR WORDS OF
C RRD WILL BE SET TO NUTATIONS AND RATES, HAVING UNITS OF
C RADIANS AND RADIANS/DAY.
C
C The option is available to have the units in km and km/sec.
C For this, set km=.true. in the STCOMX common block.
C
IMPLICIT DOUBLE PRECISION (A-H,O-Z)
INTEGER NMAX
PARAMETER (NMAX = 1000)
DIMENSION RRD(6),ET2Z(2),ET2(2),PV(6,13)
DIMENSION PVST(6,11),PNUT(4)
DIMENSION SS(3),CVAL(NMAX),PVSUN(6),ZIPS(2)
DATA ZIPS/2*0.d0/
LOGICAL BSAVE,KM,BARY
LOGICAL FIRST
DATA FIRST/.TRUE./
INTEGER LIST(12),IPT(39),DENUM
COMMON/EPHHDR/CVAL,SS,AU,EMRAT,DENUM,NCON,IPT
COMMON/STCOMX/KM,BARY,PVSUN
common/jplcom/jpleph_file_name
C INITIALIZE ET2 FOR 'STATE' AND SET UP COMPONENT COUNT
C
ET2(1)=ET
ET2(2)=0.D0
GO TO 11
C ENTRY POINT 'DPLEPH' FOR DOUBLY-DIMENSIONED TIME ARGUMENT
C (SEE THE DISCUSSION IN THE SUBROUTINE STATE)
ENTRY DPLEPH(ET2Z,NTARG,NCENT,RRD)
ET2(1)=ET2Z(1)
ET2(2)=ET2Z(2)
11 IF(FIRST) CALL STATE(ZIPS,LIST,PVST,PNUT)
FIRST=.FALSE.
96 IF(NTARG .EQ. NCENT) RETURN
DO I=1,12
LIST(I)=0
ENDDO
C CHECK FOR NUTATION CALL
IF(NTARG.NE.14) GO TO 97
IF(IPT(35).GT.0) THEN
LIST(11)=2
CALL STATE(ET2,LIST,PVST,PNUT)
DO I=1,4
RRD(I)=PNUT(I)
ENDDO
RRD(5) = 0.d0
RRD(6) = 0.d0
RETURN
ELSE
DO I=1,4
RRD(I)=0.d0
ENDDO
WRITE(6,297)
297 FORMAT(' ***** NO NUTATIONS ON THE EPHEMERIS FILE *****')
STOP
ENDIF
C CHECK FOR LIBRATIONS
97 CONTINUE
DO I=1,6
RRD(I)=0.d0
ENDDO
IF(NTARG.NE.15) GO TO 98
IF(IPT(38).GT.0) THEN
LIST(12)=2
CALL STATE(ET2,LIST,PVST,PNUT)
DO I=1,6
RRD(I)=PVST(I,11)
ENDDO
RETURN
ELSE
WRITE(6,298)
298 FORMAT(' ***** NO LIBRATIONS ON THE EPHEMERIS FILE *****')
STOP
ENDIF
C FORCE BARYCENTRIC OUTPUT BY 'STATE'
98 BSAVE=BARY
BARY=.TRUE.
C SET UP PROPER ENTRIES IN 'LIST' ARRAY FOR STATE CALL
DO I=1,2
K=NTARG
IF(I .EQ. 2) K=NCENT
IF(K .LE. 10) LIST(K)=2
IF(K .EQ. 10) LIST(3)=2
IF(K .EQ. 3) LIST(10)=2
IF(K .EQ. 13) LIST(3)=2
ENDDO
C MAKE CALL TO STATE
CALL STATE(ET2,LIST,PVST,PNUT)
DO I=1,10
DO J = 1,6
PV(J,I) = PVST(J,I)
ENDDO
ENDDO
IF(NTARG .EQ. 11 .OR. NCENT .EQ. 11) THEN
DO I=1,6
PV(I,11)=PVSUN(I)
ENDDO
ENDIF
IF(NTARG .EQ. 12 .OR. NCENT .EQ. 12) THEN
DO I=1,6
PV(I,12)=0.D0
ENDDO
ENDIF
IF(NTARG .EQ. 13 .OR. NCENT .EQ. 13) THEN
DO I=1,6
PV(I,13) = PVST(I,3)
ENDDO
ENDIF
IF(NTARG*NCENT .EQ. 30 .AND. NTARG+NCENT .EQ. 13) THEN
DO I=1,6
PV(I,3)=0.D0
ENDDO
GO TO 99
ENDIF
IF(LIST(3) .EQ. 2) THEN
DO I=1,6
PV(I,3)=PVST(I,3)-PVST(I,10)/(1.D0+EMRAT)
ENDDO
ENDIF
IF(LIST(10) .EQ. 2) THEN
DO I=1,6
PV(I,10) = PV(I,3)+PVST(I,10)
ENDDO
ENDIF
99 DO I=1,6
RRD(I)=PV(I,NTARG)-PV(I,NCENT)
ENDDO
BARY=BSAVE
RETURN
END
C+++++++++++++++++++++++++++++++++
C
SUBROUTINE INTERP(BUF,T,NCF,NCM,NA,IFL,PV)
C
C+++++++++++++++++++++++++++++++++
C
C THIS SUBROUTINE DIFFERENTIATES AND INTERPOLATES A
C SET OF CHEBYSHEV COEFFICIENTS TO GIVE POSITION AND VELOCITY
C
C CALLING SEQUENCE PARAMETERS:
C
C INPUT:
C
C BUF 1ST LOCATION OF ARRAY OF D.P. CHEBYSHEV COEFFICIENTS OF POSITION
C
C T T(1) IS DP FRACTIONAL TIME IN INTERVAL COVERED BY
C COEFFICIENTS AT WHICH INTERPOLATION IS WANTED
C (0 .LE. T(1) .LE. 1). T(2) IS DP LENGTH OF WHOLE
C INTERVAL IN INPUT TIME UNITS.
C
C NCF # OF COEFFICIENTS PER COMPONENT
C
C NCM # OF COMPONENTS PER SET OF COEFFICIENTS
C
C NA # OF SETS OF COEFFICIENTS IN FULL ARRAY
C (I.E., # OF SUB-INTERVALS IN FULL INTERVAL)
C
C IFL INTEGER FLAG: =1 FOR POSITIONS ONLY
C =2 FOR POS AND VEL
C
C
C OUTPUT:
C
C PV INTERPOLATED QUANTITIES REQUESTED. DIMENSION
C EXPECTED IS PV(NCM,IFL), DP.
C
C
IMPLICIT DOUBLE PRECISION (A-H,O-Z)
C
SAVE
C
DOUBLE PRECISION BUF(NCF,NCM,*),T(2),PV(NCM,*),PC(18),VC(18)
C
DATA NP/2/
DATA NV/3/
DATA TWOT/0.D0/
DATA PC(1),PC(2)/1.D0,0.D0/
DATA VC(2)/1.D0/
C
C ENTRY POINT. GET CORRECT SUB-INTERVAL NUMBER FOR THIS SET
C OF COEFFICIENTS AND THEN GET NORMALIZED CHEBYSHEV TIME
C WITHIN THAT SUBINTERVAL.
C
DNA=DBLE(NA)
DT1=DINT(T(1))
TEMP=DNA*T(1)
L=IDINT(TEMP-DT1)+1
C TC IS THE NORMALIZED CHEBYSHEV TIME (-1 .LE. TC .LE. 1)
TC=2.D0*(DMOD(TEMP,1.D0)+DT1)-1.D0
C CHECK TO SEE WHETHER CHEBYSHEV TIME HAS CHANGED,
C AND COMPUTE NEW POLYNOMIAL VALUES IF IT HAS.
C (THE ELEMENT PC(2) IS THE VALUE OF T1(TC) AND HENCE
C CONTAINS THE VALUE OF TC ON THE PREVIOUS CALL.)
IF(TC.NE.PC(2)) THEN
NP=2
NV=3
PC(2)=TC
TWOT=TC+TC
ENDIF
C
C BE SURE THAT AT LEAST 'NCF' POLYNOMIALS HAVE BEEN EVALUATED
C AND ARE STORED IN THE ARRAY 'PC'.
C
IF(NP.LT.NCF) THEN
DO 1 I=NP+1,NCF
PC(I)=TWOT*PC(I-1)-PC(I-2)
1 CONTINUE
NP=NCF
ENDIF
C
C INTERPOLATE TO GET POSITION FOR EACH COMPONENT
C
DO 2 I=1,NCM
PV(I,1)=0.D0
DO 3 J=NCF,1,-1
PV(I,1)=PV(I,1)+PC(J)*BUF(J,I,L)
3 CONTINUE
2 CONTINUE
IF(IFL.LE.1) RETURN
C
C IF VELOCITY INTERPOLATION IS WANTED, BE SURE ENOUGH
C DERIVATIVE POLYNOMIALS HAVE BEEN GENERATED AND STORED.
C
VFAC=(DNA+DNA)/T(2)
VC(3)=TWOT+TWOT
IF(NV.LT.NCF) THEN
DO 4 I=NV+1,NCF
VC(I)=TWOT*VC(I-1)+PC(I-1)+PC(I-1)-VC(I-2)
4 CONTINUE
NV=NCF
ENDIF
C
C INTERPOLATE TO GET VELOCITY FOR EACH COMPONENT
C
DO 5 I=1,NCM
PV(I,2)=0.D0
DO 6 J=NCF,2,-1
PV(I,2)=PV(I,2)+VC(J)*BUF(J,I,L)
6 CONTINUE
PV(I,2)=PV(I,2)*VFAC
5 CONTINUE
C
RETURN
C
END
C+++++++++++++++++++++++++
C
SUBROUTINE SPLIT(TT,FR)
C
C+++++++++++++++++++++++++
C
C THIS SUBROUTINE BREAKS A D.P. NUMBER INTO A D.P. INTEGER
C AND A D.P. FRACTIONAL PART.
C
C CALLING SEQUENCE PARAMETERS:
C
C TT = D.P. INPUT NUMBER
C
C FR = D.P. 2-WORD OUTPUT ARRAY.
C FR(1) CONTAINS INTEGER PART
C FR(2) CONTAINS FRACTIONAL PART
C
C FOR NEGATIVE INPUT NUMBERS, FR(1) CONTAINS THE NEXT
C MORE NEGATIVE INTEGER; FR(2) CONTAINS A POSITIVE FRACTION.
C
C CALLING SEQUENCE DECLARATIONS
C
IMPLICIT DOUBLE PRECISION (A-H,O-Z)
DIMENSION FR(2)
C MAIN ENTRY -- GET INTEGER AND FRACTIONAL PARTS
FR(1)=DINT(TT)
FR(2)=TT-FR(1)
IF(TT.GE.0.D0 .OR. FR(2).EQ.0.D0) RETURN
C MAKE ADJUSTMENTS FOR NEGATIVE INPUT NUMBER
FR(1)=FR(1)-1.D0
FR(2)=FR(2)+1.D0
RETURN
END
C++++++++++++++++++++++++++++++++
C
SUBROUTINE STATE(ET2,LIST,PV,PNUT)
C
C++++++++++++++++++++++++++++++++
C
C THIS SUBROUTINE READS AND INTERPOLATES THE JPL PLANETARY EPHEMERIS FILE
C
C CALLING SEQUENCE PARAMETERS:
C
C INPUT:
C
C ET2 DP 2-WORD JULIAN EPHEMERIS EPOCH AT WHICH INTERPOLATION
C IS WANTED. ANY COMBINATION OF ET2(1)+ET2(2) WHICH FALLS
C WITHIN THE TIME SPAN ON THE FILE IS A PERMISSIBLE EPOCH.
C
C A. FOR EASE IN PROGRAMMING, THE USER MAY PUT THE
C ENTIRE EPOCH IN ET2(1) AND SET ET2(2)=0.
C
C B. FOR MAXIMUM INTERPOLATION ACCURACY, SET ET2(1) =
C THE MOST RECENT MIDNIGHT AT OR BEFORE INTERPOLATION
C EPOCH AND SET ET2(2) = FRACTIONAL PART OF A DAY
C ELAPSED BETWEEN ET2(1) AND EPOCH.
C
C C. AS AN ALTERNATIVE, IT MAY PROVE CONVENIENT TO SET
C ET2(1) = SOME FIXED EPOCH, SUCH AS START OF INTEGRATION,
C AND ET2(2) = ELAPSED INTERVAL BETWEEN THEN AND EPOCH.
C
C LIST 12-WORD INTEGER ARRAY SPECIFYING WHAT INTERPOLATION
C IS WANTED FOR EACH OF THE BODIES ON THE FILE.
C
C LIST(I)=0, NO INTERPOLATION FOR BODY I
C =1, POSITION ONLY
C =2, POSITION AND VELOCITY
C
C THE DESIGNATION OF THE ASTRONOMICAL BODIES BY I IS:
C
C I = 1: MERCURY
C = 2: VENUS
C = 3: EARTH-MOON BARYCENTER
C = 4: MARS
C = 5: JUPITER
C = 6: SATURN
C = 7: URANUS
C = 8: NEPTUNE
C = 9: PLUTO
C =10: GEOCENTRIC MOON
C =11: NUTATIONS IN LONGITUDE AND OBLIQUITY
C =12: LUNAR LIBRATIONS (IF ON FILE)
C
C OUTPUT:
C
C PV DP 6 X 11 ARRAY THAT WILL CONTAIN REQUESTED INTERPOLATED
C QUANTITIES (OTHER THAN NUTATION, STOERD IN PNUT).
C THE BODY SPECIFIED BY LIST(I) WILL HAVE ITS
C STATE IN THE ARRAY STARTING AT PV(1,I).
C (ON ANY GIVEN CALL, ONLY THOSE WORDS IN 'PV' WHICH ARE
C AFFECTED BY THE FIRST 10 'LIST' ENTRIES, AND BY LIST(12)
C IF LIBRATIONS ARE ON THE FILE, ARE SET.
C THE REST OF THE 'PV' ARRAYIS UNTOUCHED.)
C THE ORDER OF COMPONENTS STARTING IN PV(1,I) IS: X,Y,Z,DX,DY,DZ.
C
C ALL OUTPUT VECTORS ARE REFERENCED TO THE EARTH MEAN
C EQUATOR AND EQUINOX OF J2000 IF THE DE NUMBER IS 200 OR
C GREATER; OF B1950 IF THE DE NUMBER IS LESS THAN 200.
C
C THE MOON STATE IS ALWAYS GEOCENTRIC; THE OTHER NINE STATES
C ARE EITHER HELIOCENTRIC OR SOLAR-SYSTEM BARYCENTRIC,
C DEPENDING ON THE SETTING OF COMMON FLAGS (SEE BELOW).
C
C LUNAR LIBRATIONS, IF ON FILE, ARE PUT INTO PV(K,11) IF
C LIST(12) IS 1 OR 2.
C
C NUT DP 4-WORD ARRAY THAT WILL CONTAIN NUTATIONS AND RATES,
C DEPENDING ON THE SETTING OF LIST(11). THE ORDER OF
C QUANTITIES IN NUT IS:
C
C D PSI (NUTATION IN LONGITUDE)
C D EPSILON (NUTATION IN OBLIQUITY)
C D PSI DOT
C D EPSILON DOT
C
C * STATEMENT # FOR ERROR RETURN, IN CASE OF EPOCH OUT OF
C RANGE OR I/O ERRORS.
C
C COMMON AREA STCOMX:
C
C KM LOGICAL FLAG DEFINING PHYSICAL UNITS OF THE OUTPUT
C STATES. KM = .TRUE., KM AND KM/SEC
C = .FALSE., AU AND AU/DAY
C DEFAULT VALUE = .FALSE. (KM DETERMINES TIME UNIT
C FOR NUTATIONS AND LIBRATIONS. ANGLE UNIT IS ALWAYS RADIANS.)
C
C BARY LOGICAL FLAG DEFINING OUTPUT CENTER.
C ONLY THE 9 PLANETS ARE AFFECTED.
C BARY = .TRUE. =\ CENTER IS SOLAR-SYSTEM BARYCENTER
C = .FALSE. =\ CENTER IS SUN
C DEFAULT VALUE = .FALSE.
C
C PVSUN DP 6-WORD ARRAY CONTAINING THE BARYCENTRIC POSITION AND
C VELOCITY OF THE SUN.
C
C
IMPLICIT DOUBLE PRECISION (A-H,O-Z)
SAVE
INTEGER OLDMAX
PARAMETER ( OLDMAX = 400)
INTEGER NMAX
PARAMETER ( NMAX = 1000)
DIMENSION ET2(2),PV(6,11),PNUT(4),T(2),PJD(4),BUF(1500),
. SS(3),CVAL(NMAX),PVSUN(6)
INTEGER LIST(12),IPT(3,13)
LOGICAL FIRST
DATA FIRST/.TRUE./
CHARACTER*6 TTL(14,3),CNAM(NMAX)
CHARACTER*80 NAMFIL
LOGICAL KM,BARY
COMMON/EPHHDR/CVAL,SS,AU,EMRAT,NUMDE,NCON,IPT
COMMON/CHRHDR/CNAM,TTL
COMMON/STCOMX/KM,BARY,PVSUN
C
C ENTRY POINT - 1ST TIME IN, GET POINTER DATA, ETC., FROM EPH FILE
C
IF(FIRST) THEN
FIRST=.FALSE.
C ************************************************************************
C ************************************************************************
C THE USER MUST SELECT ONE OF THE FOLLOWING BY DELETING THE 'C' IN COLUMN 1
C ************************************************************************
C CALL FSIZER1(NRECL,KSIZE,NRFILE,NAMFIL)
C CALL FSIZER2(NRECL,KSIZE,NRFILE,NAMFIL)
CALL FSIZER3(NRECL,KSIZE,NRFILE,NAMFIL)
IF(NRECL .EQ. 0) WRITE(*,*)' ***** FSIZER IS NOT WORKING *****'
C ************************************************************************
C ************************************************************************
IRECSZ=NRECL*KSIZE
NCOEFFS=KSIZE/2
OPEN(NRFILE,
* FILE=NAMFIL,
* ACCESS='DIRECT',
* FORM='UNFORMATTED',
* RECL=IRECSZ,
* STATUS='OLD')
READ(NRFILE,REC=1)TTL,(CNAM(K),K=1,OLDMAX),SS,NCON,AU,EMRAT,
& ((IPT(I,J),I=1,3),J=1,12),NUMDE,(IPT(I,13),I=1,3)
& ,(CNAM(L),L=OLDMAX+1,NCON)
IF(NCON .LE. OLDMAX)THEN
READ(NRFILE,REC=2)(CVAL(I),I=1,OLDMAX)
ELSE
READ(NRFILE,REC=2)(CVAL(I),I=1,NCON)
ENDIF
NRL=0
ENDIF
C ********** MAIN ENTRY POINT **********
IF(ET2(1) .EQ. 0.D0) RETURN
S=ET2(1)-.5D0
CALL SPLIT(S,PJD(1))
CALL SPLIT(ET2(2),PJD(3))
PJD(1)=PJD(1)+PJD(3)+.5D0
PJD(2)=PJD(2)+PJD(4)
CALL SPLIT(PJD(2),PJD(3))
PJD(1)=PJD(1)+PJD(3)
C ERROR RETURN FOR EPOCH OUT OF RANGE
IF(PJD(1)+PJD(4).LT.SS(1) .OR. PJD(1)+PJD(4).GT.SS(2)) GO TO 98
C CALCULATE RECORD # AND RELATIVE TIME IN INTERVAL
NR=IDINT((PJD(1)-SS(1))/SS(3))+3
IF(PJD(1).EQ.SS(2)) NR=NR-1
tmp1 = DBLE(NR-3)*SS(3) + SS(1)
tmp2 = PJD(1) - tmp1
T(1) = (tmp2 + PJD(4))/SS(3)
C READ CORRECT RECORD IF NOT IN CORE
IF(NR.NE.NRL) THEN
NRL=NR
READ(NRFILE,REC=NR,ERR=99)(BUF(K),K=1,NCOEFFS)
ENDIF
IF(KM) THEN
T(2)=SS(3)*86400.D0
AUFAC=1.D0
ELSE
T(2)=SS(3)
AUFAC=1.D0/AU
ENDIF
C INTERPOLATE SSBARY SUN
CALL INTERP(BUF(IPT(1,11)),T,IPT(2,11),3,IPT(3,11),2,PVSUN)
DO I=1,6
PVSUN(I)=PVSUN(I)*AUFAC
ENDDO
C CHECK AND INTERPOLATE WHICHEVER BODIES ARE REQUESTED
DO 4 I=1,10
IF(LIST(I).EQ.0) GO TO 4
CALL INTERP(BUF(IPT(1,I)),T,IPT(2,I),3,IPT(3,I),
& LIST(I),PV(1,I))
DO J=1,6
IF(I.LE.9 .AND. .NOT.BARY) THEN
PV(J,I)=PV(J,I)*AUFAC-PVSUN(J)
ELSE
PV(J,I)=PV(J,I)*AUFAC
ENDIF
ENDDO
4 CONTINUE
C DO NUTATIONS IF REQUESTED (AND IF ON FILE)
IF(LIST(11).GT.0 .AND. IPT(2,12).GT.0)
* CALL INTERP(BUF(IPT(1,12)),T,IPT(2,12),2,IPT(3,12),
* LIST(11),PNUT)
C GET LIBRATIONS IF REQUESTED (AND IF ON FILE)
IF(LIST(12).GT.0 .AND. IPT(2,13).GT.0)
* CALL INTERP(BUF(IPT(1,13)),T,IPT(2,13),3,IPT(3,13),
* LIST(12),PV(1,11))
RETURN
98 WRITE(*,198)ET2(1)+ET2(2),SS(1),SS(2)
198 FORMAT(' *** Requested JED,',f12.2,
* ' not within ephemeris limits,',2f12.2,' ***')
STOP
99 WRITE(*,'(2F12.2,A80)')ET2,'ERROR RETURN IN STATE'
STOP
END
C+++++++++++++++++++++++++++++
C
SUBROUTINE CONST(NAM,VAL,SSS,N)
C
C+++++++++++++++++++++++++++++
C
C THIS ENTRY OBTAINS THE CONSTANTS FROM THE EPHEMERIS FILE
C
C CALLING SEQEUNCE PARAMETERS (ALL OUTPUT):
C
C NAM = CHARACTER*6 ARRAY OF CONSTANT NAMES
C
C VAL = D.P. ARRAY OF VALUES OF CONSTANTS
C
C SSS = D.P. JD START, JD STOP, STEP OF EPHEMERIS
C
C N = INTEGER NUMBER OF ENTRIES IN 'NAM' AND 'VAL' ARRAYS
C
IMPLICIT DOUBLE PRECISION (A-H,O-Z)
SAVE
INTEGER NMAX
PARAMETER (NMAX = 1000)
CHARACTER*6 NAM(*),TTL(14,3),CNAM(NMAX)
DOUBLE PRECISION VAL(*),SSS(3),SS(3),CVAL(NMAX),ZIPS(2)
DOUBLE PRECISION PVST(6,11),PNUT(4)
DATA ZIPS/2*0.d0/
INTEGER IPT(3,13),DENUM,LIST(12)
logical first
data first/.true./
COMMON/EPHHDR/CVAL,SS,AU,EMRAT,DENUM,NCON,IPT
COMMON/CHRHDR/CNAM,TTL
C CALL STATE TO INITIALIZE THE EPHEMERIS AND READ IN THE CONSTANTS
IF(FIRST) CALL STATE(ZIPS,LIST,PVST,PNUT)
first=.false.
N=NCON
DO I=1,3
SSS(I)=SS(I)
ENDDO
DO I=1,N
NAM(I)=CNAM(I)
VAL(I)=CVAL(I)
ENDDO
RETURN
END

38
lib/libration.f90 Normal file
View File

@ -0,0 +1,38 @@
subroutine libration(jd,RA,Dec,xl,b)
! Compute optical libration of moon at jd: that is, the sub-observer
! point (xl,b) in selenographic coordinates. RA and Dec are
! topocentric values.
implicit real*8 (a-h,o-z)
parameter (RADS=0.0174532925199433d0)
parameter (TWOPI=6.28318530717959d0)
real*8 jd,j2000,mjd,lambda
j2000=2451545.0d0
RA2000=RA
Dec2000=Dec
year=2000.0d0 + (jd-j2000)/365.25d0
mjd=jd-2400000.d0
call sla_PRECES('FK5',year,2000.d0,RA2000,Dec2000)
call sla_EQECL(RA2000,Dec2000,mjd,lambda,beta)
day=jd - j2000
t = day / 36525.d0
xi = 1.54242 * RADS
ft = 93.2720993 + 483202.0175273 * t - .0034029 * t * t
b= ft / 360
a = 360 * (b - floor(b))
if (a.lt.0.d0) a = 360 + a;
f=a/57.2957795131d0
omega=sla_dranrm(2.182439196d0 - t*33.7570446085d0 + t*t*3.6236526d-5)
w = lambda - omega
y = sin(w) * cos(beta) * cos(xi) - sin(beta) * sin(xi)
x = cos(w) * cos(beta)
a = sla_dranrm(atan2(y, x))
xl = a - f
if(xl.lt.-0.25*TWOPI) xl=xl+TWOPI !Fix 'round the back' angles
if(xl.gt.0.25*TWOPI) xl=xl-TWOPI
b = asin(-sin(w) * cos(beta) * sin(xi) - sin(beta) * cos(xi))
return
end subroutine libration

166
lib/moon2.f90
View File

@ -1,166 +0,0 @@
subroutine moon2(y,m,Day,UT,lon,lat,RA,Dec,topRA,topDec, &
LST,HA,Az,El,dist)
implicit none
integer y !Year
integer m !Month
integer Day !Day
real*8 UT !UTC in hours
real*8 RA,Dec !RA and Dec of moon
! NB: Double caps are single caps in the writeup.
real*8 NN !Longitude of ascending node
real*8 i !Inclination to the ecliptic
real*8 w !Argument of perigee
real*8 a !Semi-major axis
real*8 e !Eccentricity
real*8 MM !Mean anomaly
real*8 v !True anomaly
real*8 EE !Eccentric anomaly
real*8 ecl !Obliquity of the ecliptic
real*8 d !Ephemeris time argument in days
real*8 r !Distance to sun, AU
real*8 xv,yv !x and y coords in ecliptic
real*8 lonecl,latecl !Ecliptic long and lat of moon
real*8 xg,yg,zg !Ecliptic rectangular coords
real*8 Ms !Mean anomaly of sun
real*8 ws !Argument of perihelion of sun
real*8 Ls !Mean longitude of sun (Ns=0)
real*8 Lm !Mean longitude of moon
real*8 DD !Mean elongation of moon
real*8 FF !Argument of latitude for moon
real*8 xe,ye,ze !Equatorial geocentric coords of moon
real*8 mpar !Parallax of moon (r_E / d)
real*8 lat,lon !Station coordinates on earth
real*8 gclat !Geocentric latitude
real*8 rho !Earth radius factor
real*8 GMST0,LST,HA
real*8 g
real*8 topRA,topDec !Topocentric coordinates of Moon
real*8 Az,El
real*8 dist
real*8 rad,twopi,pi,pio2
data rad/57.2957795131d0/,twopi/6.283185307d0/
d=367*y - 7*(y+(m+9)/12)/4 + 275*m/9 + Day - 730530 + UT/24.d0
ecl = 23.4393d0 - 3.563d-7 * d
! Orbital elements for Moon:
NN = 125.1228d0 - 0.0529538083d0 * d
i = 5.1454d0
w = mod(318.0634d0 + 0.1643573223d0 * d + 360000.d0,360.d0)
a = 60.2666d0
e = 0.054900d0
MM = mod(115.3654d0 + 13.0649929509d0 * d + 360000.d0,360.d0)
EE = MM + e*rad*sin(MM/rad) * (1.d0 + e*cos(MM/rad))
EE = EE - (EE - e*rad*sin(EE/rad)-MM) / (1.d0 - e*cos(EE/rad))
EE = EE - (EE - e*rad*sin(EE/rad)-MM) / (1.d0 - e*cos(EE/rad))
xv = a * (cos(EE/rad) - e)
yv = a * (sqrt(1.d0-e*e) * sin(EE/rad))
v = mod(rad*atan2(yv,xv)+720.d0,360.d0)
r = sqrt(xv*xv + yv*yv)
! Get geocentric position in ecliptic rectangular coordinates:
xg = r * (cos(NN/rad)*cos((v+w)/rad) - &
sin(NN/rad)*sin((v+w)/rad)*cos(i/rad))
yg = r * (sin(NN/rad)*cos((v+w)/rad) + &
cos(NN/rad)*sin((v+w)/rad)*cos(i/rad))
zg = r * (sin((v+w)/rad)*sin(i/rad))
! Ecliptic longitude and latitude of moon:
lonecl = mod(rad*atan2(yg/rad,xg/rad)+720.d0,360.d0)
latecl = rad*atan2(zg/rad,sqrt(xg*xg + yg*yg)/rad)
! Now include orbital perturbations:
Ms = mod(356.0470d0 + 0.9856002585d0 * d + 3600000.d0,360.d0)
ws = 282.9404d0 + 4.70935d-5*d
Ls = mod(Ms + ws + 720.d0,360.d0)
Lm = mod(MM + w + NN+720.d0,360.d0)
DD = mod(Lm - Ls + 360.d0,360.d0)
FF = mod(Lm - NN + 360.d0,360.d0)
lonecl = lonecl &
-1.274d0 * sin((MM-2.d0*DD)/rad) &
+0.658d0 * sin(2.d0*DD/rad) &
-0.186d0 * sin(Ms/rad) &
-0.059d0 * sin((2.d0*MM-2.d0*DD)/rad) &
-0.057d0 * sin((MM-2.d0*DD+Ms)/rad) &
+0.053d0 * sin((MM+2.d0*DD)/rad) &
+0.046d0 * sin((2.d0*DD-Ms)/rad) &
+0.041d0 * sin((MM-Ms)/rad) &
-0.035d0 * sin(DD/rad) &
-0.031d0 * sin((MM+Ms)/rad) &
-0.015d0 * sin((2.d0*FF-2.d0*DD)/rad) &
+0.011d0 * sin((MM-4.d0*DD)/rad)
latecl = latecl &
-0.173d0 * sin((FF-2.d0*DD)/rad) &
-0.055d0 * sin((MM-FF-2.d0*DD)/rad) &
-0.046d0 * sin((MM+FF-2.d0*DD)/rad) &
+0.033d0 * sin((FF+2.d0*DD)/rad) &
+0.017d0 * sin((2.d0*MM+FF)/rad)
r = 60.36298d0 &
- 3.27746d0*cos(MM/rad) &
- 0.57994d0*cos((MM-2.d0*DD)/rad) &
- 0.46357d0*cos(2.d0*DD/rad) &
- 0.08904d0*cos(2.d0*MM/rad) &
+ 0.03865d0*cos((2.d0*MM-2.d0*DD)/rad) &
- 0.03237d0*cos((2.d0*DD-Ms)/rad) &
- 0.02688d0*cos((MM+2.d0*DD)/rad) &
- 0.02358d0*cos((MM-2.d0*DD+Ms)/rad) &
- 0.02030d0*cos((MM-Ms)/rad) &
+ 0.01719d0*cos(DD/rad) &
+ 0.01671d0*cos((MM+Ms)/rad)
dist=r*6378.140d0
! Geocentric coordinates:
! Rectangular ecliptic coordinates of the moon:
xg = r * cos(lonecl/rad)*cos(latecl/rad)
yg = r * sin(lonecl/rad)*cos(latecl/rad)
zg = r * sin(latecl/rad)
! Rectangular equatorial coordinates of the moon:
xe = xg
ye = yg*cos(ecl/rad) - zg*sin(ecl/rad)
ze = yg*sin(ecl/rad) + zg*cos(ecl/rad)
! Right Ascension, Declination:
RA = mod(rad*atan2(ye,xe)+360.d0,360.d0)
Dec = rad*atan2(ze,sqrt(xe*xe + ye*ye))
! Now convert to topocentric system:
mpar=rad*asin(1.d0/r)
! alt_topoc = alt_geoc - mpar*cos(alt_geoc)
gclat = lat - 0.1924d0*sin(2.d0*lat/rad)
rho = 0.99883d0 + 0.00167d0*cos(2.d0*lat/rad)
GMST0 = (Ls + 180.d0)/15.d0
LST = mod(GMST0+UT+lon/15.d0+48.d0,24.d0) !LST in hours
HA = 15.d0*LST - RA !HA in degrees
g = rad*atan(tan(gclat/rad)/cos(HA/rad))
topRA = RA - mpar*rho*cos(gclat/rad)*sin(HA/rad)/cos(Dec/rad)
topDec = Dec - mpar*rho*sin(gclat/rad)*sin((g-Dec)/rad)/sin(g/rad)
HA = 15.d0*LST - topRA !HA in degrees
if(HA.gt.180.d0) HA=HA-360.d0
if(HA.lt.-180.d0) HA=HA+360.d0
pi=0.5d0*twopi
pio2=0.5d0*pi
call dcoord(pi,pio2-lat/rad,0.d0,lat/rad,ha*twopi/360,topDec/rad,az,el)
Az=az*rad
El=El*rad
return
end subroutine moon2

72
lib/moondop.f90
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@ -1,72 +0,0 @@
subroutine MoonDop(nyear,month,nday,uth4,lon4,lat4,RAMoon4, &
DecMoon4,LST4,HA4,AzMoon4,ElMoon4,vr4,dist4)
implicit real*8 (a-h,o-z)
real*4 uth4 !UT in hours
real*4 lon4 !West longitude, degrees
real*4 lat4 !Latitude, degrees
real*4 RAMoon4 !Topocentric RA of moon, hours
real*4 DecMoon4 !Topocentric Dec of Moon, degrees
real*4 LST4 !Locat sidereal time, hours
real*4 HA4 !Local Hour angle, degrees
real*4 AzMoon4 !Topocentric Azimuth of moon, degrees
real*4 ElMoon4 !Topocentric Elevation of moon, degrees
real*4 vr4 !Radial velocity of moon wrt obs, km/s
real*4 dist4 !Echo time, seconds
real*8 LST
real*8 RME(6) !Vector from Earth center to Moon
real*8 RAE(6) !Vector from Earth center to Obs
real*8 RMA(6) !Vector from Obs to Moon
real*8 rme0(6)
logical km
data rad/57.2957795130823d0/,twopi/6.28310530717959d0/
km=.true.
dlat=lat4/rad
dlong1=lon4/rad
elev1=200.d0
call geocentric(dlat,elev1,dlat1,erad1)
dt=100.d0 !For numerical derivative, in seconds
UT=uth4
! NB: geodetic latitude used here, but geocentric latitude used when
! determining Earth-rotation contribution to Doppler.
call moon2(nyear,month,nDay,UT-dt/3600.d0,dlong1*rad,dlat*rad, &
RA,Dec,topRA,topDec,LST,HA,Az0,El0,dist)
call toxyz(RA/rad,Dec/rad,dist,rme0) !Convert to rectangular coords
call moon2(nyear,month,nDay,UT,dlong1*rad,dlat*rad, &
RA,Dec,topRA,topDec,LST,HA,Az,El,dist)
call toxyz(RA/rad,Dec/rad,dist,rme) !Convert to rectangular coords
phi=LST*twopi/24.d0
call toxyz(phi,dlat1,erad1,rae) !Gencentric numbers used here!
radps=twopi/(86400.d0/1.002737909d0)
rae(4)=-rae(2)*radps !Vel of Obs wrt Earth center
rae(5)=rae(1)*radps
rae(6)=0.d0
do i=1,3
rme(i+3)=(rme(i)-rme0(i))/dt
rma(i)=rme(i)-rae(i)
rma(i+3)=rme(i+3)-rae(i+3)
enddo
call fromxyz(rma,alpha1,delta1,dtopo0) !Get topocentric coords
vr=dot(rma(4),rma)/dtopo0
RAMoon4=topRA
DecMoon4=topDec
LST4=LST
HA4=HA
AzMoon4=Az
ElMoon4=El
vr4=vr
dist4=dist
return
end subroutine MoonDop

43
lib/moondopjpl.f90 Normal file
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@ -0,0 +1,43 @@
subroutine MoonDopJPL(nyear,month,nday,uth4,lon4,lat4,RAMoon4, &
DecMoon4,LST4,HA4,AzMoon4,ElMoon4,vr4,dist4)
implicit real*8 (a-h,o-z)
real*4 uth4 !UT in hours
real*4 lon4 !East longitude, degrees
real*4 lat4 !Latitude, degrees
real*4 RAMoon4 !Topocentric RA of moon, hours
real*4 DecMoon4 !Topocentric Dec of Moon, degrees
real*4 LST4 !Locat sidereal time, hours
real*4 HA4 !Local Hour angle, degrees
real*4 AzMoon4 !Topocentric Azimuth of moon, degrees
real*4 ElMoon4 !Topocentric Elevation of moon, degrees
real*4 vr4 !Radial velocity of moon wrt obs, km/s
real*4 dist4 !Echo time, seconds
twopi=8.d0*atan(1.d0) !Define some constants
rad=360.d0/twopi
clight=2.99792458d5
call sla_CLDJ(nyear,month,nday,djutc,j)
djutc=djutc + uth4/24.d0
dut=-0.460d0
east_long=lon4/rad
geodetic_lat=lat4/rad
height=40.
nspecial=0
call ephem(djutc,dut,east_long,geodetic_lat,height,nspecial, &
RA,Dec,Az,El,techo,dop,fspread_1GHz,vr)
RAMoon4=RA
DecMoon4=Dec
LST4=LST
HA4=HA
AzMoon4=Az*rad
ElMoon4=El*rad
vr4=vr
dist4=techo
return
end subroutine MoonDopJPL

3396
lib/slasubs.f Normal file
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File diff suppressed because it is too large Load Diff

14
lib/tm2.f90
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@ -1,14 +0,0 @@
subroutine tm2(day,xlat4,xlon4,xl4,b4)
implicit real*8 (a-h,o-z)
parameter (RADS=0.0174532925199433d0)
real*4 xlat4,xlon4,xl4,b4
glat=xlat4*RADS
glong=xlon4*RADS
call tmoonsub(day,glat,glong,el,rv,xl,b,pax)
xl4=xl
b4=b
end subroutine tm2

25
lib/toxyz.f90
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@ -1,25 +0,0 @@
subroutine toxyz(alpha,delta,r,vec)
implicit real*8 (a-h,o-z)
real*8 vec(3)
vec(1)=r*cos(delta)*cos(alpha)
vec(2)=r*cos(delta)*sin(alpha)
vec(3)=r*sin(delta)
return
end subroutine toxyz
subroutine fromxyz(vec,alpha,delta,r)
implicit real*8 (a-h,o-z)
real*8 vec(3)
data twopi/6.283185307d0/
r=sqrt(vec(1)**2 + vec(2)**2 + vec(3)**2)
alpha=atan2(vec(2),vec(1))
if(alpha.lt.0.d0) alpha=alpha+twopi
delta=asin(vec(3)/r)
return
end subroutine fromxyz