SVN r8568
This commit is contained in:
Jordan Sherer
@@ -1,127 +0,0 @@
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subroutine sync8(dd,nfa,nfb,nfqso,s,candidate,ncand)
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include 'ft8_params.f90'
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parameter (JZ=31) !DT up to +/- 2.5 s
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complex cx(0:NH1)
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real s(NH1,NHSYM)
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real savg(NH1)
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real x(NFFT1)
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real sync2d(NH1,-JZ:JZ)
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real red(NH1)
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real candidate0(3,200)
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real candidate(3,200)
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real dd(NMAX)
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integer jpeak(NH1)
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integer indx(NH1)
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integer ii(1)
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integer icos7(0:6)
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data icos7/2,5,6,0,4,1,3/ !Costas 7x7 tone pattern
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equivalence (x,cx)
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! Compute symbol spectra at half-symbol steps.
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savg=0.
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istep=NSPS/2 !960
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tstep=istep/12000.0 !0.08 s
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df=12000.0/NFFT1 !3.125 Hz
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! Compute symbol spectra at half-symbol steps
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fac=1.0/300.0
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do j=1,NHSYM
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ia=(j-1)*istep + 1
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ib=ia+NSPS-1
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x(1:NSPS)=fac*dd(ia:ib)
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x(NSPS+1:)=0.
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call four2a(x,NFFT1,1,-1,0) !r2c FFT
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do i=1,NH1
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s(i,j)=real(cx(i))**2 + aimag(cx(i))**2
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enddo
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savg=savg + s(1:NH1,j) !Average spectrum
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enddo
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savg=savg/NHSYM
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! do i=1,NH1
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! write(51,3051) i*df,savg(i),db(savg(i))
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!3051 format(f10.3,e12.3,f12.3)
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! enddo
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ia=max(1,nint(nfa/df))
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ib=nint(nfb/df)
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do i=ia,ib
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do j=-JZ,JZ
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t=0.
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t0=0.
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do n=0,6
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k=j+2*n
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if(k.ge.1) then
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t=t + s(i+2*icos7(n),k)
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t0=t0 + sum(s(i:i+12:2,k))
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endif
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t=t + s(i+2*icos7(n),k+72)
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t0=t0 + sum(s(i:i+12:2,k+72))
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if(k+144.le.NHSYM) then
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t=t + s(i+2*icos7(n),k+144)
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t0=t0 + sum(s(i:i+12:2,k+144))
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endif
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enddo
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t0=(t0-t)/6.0
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sync2d(i,j)=t/t0
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enddo
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enddo
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red=0.
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do i=ia,ib
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ii=maxloc(sync2d(i,-JZ:JZ)) - 1 - JZ
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j0=ii(1)
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jpeak(i)=j0
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red(i)=sync2d(i,j0)
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! write(52,3052) i*df,red(i),db(red(i))
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!3052 format(3f12.3)
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enddo
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iz=ib-ia+1
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call indexx(red(ia:ib),iz,indx)
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ibase=indx(nint(0.40*iz)) - 1 + ia
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base=red(ibase)
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red=red/base
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candidate0=0.
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k=0
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syncmin=2.0
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do i=1,100
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n=ia + indx(iz+1-i) - 1
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if(red(n).lt.syncmin) exit
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if(k.lt.200) k=k+1
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candidate0(1,k)=n*df
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candidate0(2,k)=(jpeak(n)-1)*tstep
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candidate0(3,k)=red(n)
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enddo
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ncand=k
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! Put nfqso at top of list, and save only the best of near-dupe freqs.
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do i=1,ncand
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if(abs(candidate0(1,i)-nfqso).lt.10.0) candidate0(1,i)=-candidate0(1,i)
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if(i.ge.2) then
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do j=1,i-1
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fdiff=abs(candidate0(1,i))-abs(candidate0(1,j))
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if(abs(fdiff).lt.4.0) then
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if(candidate0(3,i).ge.candidate0(3,j)) candidate0(3,j)=0.
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if(candidate0(3,i).lt.candidate0(3,j)) candidate0(3,i)=0.
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endif
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enddo
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! write(*,3001) i,candidate0(1,i-1),candidate0(1,i),candidate0(3,i-1), &
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! candidate0(3,i)
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!3001 format(i2,4f8.1)
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endif
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enddo
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fac=20.0/maxval(s)
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s=fac*s
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call indexx(candidate0(1,1:ncand),ncand,indx)
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do i=1,ncand
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j=indx(i)
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candidate(1,i)=abs(candidate0(1,j))
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candidate(2,i)=candidate0(2,j)
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candidate(3,i)=candidate0(3,j)
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enddo
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return
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end subroutine sync8
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@@ -1,46 +0,0 @@
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A text box entitled Astronomical Data provides information needed for
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tracking the sun or moon, compensating for EME Doppler shift, and
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estimating EME Doppler spread and path degradation. Toggle the
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*Astronomical data* on the *View* menu to display or hide this window.
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image::AstroData_2.png[align="center",alt="Astronomical Data"]
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Available information includes the current UTC *Date* and time; *Az*
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and *El*, azimuth and elevation of the moon at your own location, in
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degrees; *SelfDop*, *Width*, and *Delay*, the Doppler shift, full
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limb-to-limb Doppler spread in Hz, and delay of your own EME echoes in
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seconds; and *DxAz* and *DxEl*, *DxDop*, and *DxWid*, corresponding
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parameters for a station located at the *DX Grid* entered on the main
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window. These numbers are followed by *Dec*, the declination of the
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moon; *SunAz* and *SunEl*, the azimuth and elevation of the Sun;
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*Freq*, your stated operating frequency in MHz; *Tsky*, the estimated
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sky background temperature in the direction of the moon, scaled to the
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operating frequency; *Dpol*, the spatial polarization offset in
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degrees; *MNR*, the maximum non-reciprocity of the EME path in dB,
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owing to a combination of Faraday rotation and spatial polarization;
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and finally *Dgrd*, an estimate of the signal degradation in dB,
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relative to the best possible time with the moon at perigee in a cold
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part of the sky.
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The state of the art for establishing three-dimensional locations of
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the sun, moon, and planets at a specified time is embodied in a
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numerical model of the solar system maintained at the Jet Propulsion
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Laboratory. The model has been numerically integrated to produce
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tabular data that can be interpolated with very high accuracy. For
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example, the celestial coordinates of the moon or a planet can be
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determined at a specified time to within about 0.0000003 degrees. The
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JPL ephemeris tables and interpolation routines have been incorporated
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into _WSJT-X_. Further details on accuracy, especially concerning
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calculated EME Doppler shifts, are described in {lunarEchoes} for
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November-December, 2016.
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The sky background temperatures reported by _WSJT-X_ are derived from
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the all-sky 408 MHz map of Haslam et al. (Astronomy and Astrophysics
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Supplement Series, 47, 1, 1982), scaled by frequency to the -2.6
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power. This map has angular resolution of about 1 degree, and of
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course most amateur EME antennas have much broader beamwidths than
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this. Your antenna will therefore smooth out the hot spots
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considerably, and the observed extremes of sky temperature will be
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less. Unless you understand your sidelobes and ground reflections
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extremely well, it is unlikely that more accurate sky temperatures
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would be of much practical use.
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