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Allow auto-seq in QRA64 mode; updates to User Guide.

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git-svn-id: svn+ssh://svn.code.sf.net/p/wsjt/wsjt/branches/wsjtx@7989 ab8295b8-cf94-4d9e-aec4-7959e3be5d79
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Joe Taylor 2017-08-02 20:43:06 +00:00
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103
doc/user_guide/en/astro_data.adoc
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@ -1,46 +1,57 @@
A text box entitled Astronomical Data provides information needed for
tracking the sun or moon, compensating for EME Doppler shift, and
estimating EME Doppler spread and path degradation. Toggle the
*Astronomical data* on the *View* menu to display or hide this window.
image::AstroData_2.png[align="center",alt="Astronomical Data"]
Available information includes the current UTC *Date* and time; *Az*
and *El*, azimuth and elevation of the moon at your own location, in
degrees; *SelfDop*, *Width*, and *Delay*, the Doppler shift, full
limb-to-limb Doppler spread in Hz, and delay of your own EME echoes in
seconds; and *DxAz* and *DxEl*, *DxDop*, and *DxWid*, corresponding
parameters for a station located at the *DX Grid* entered on the main
window. These numbers are followed by *Dec*, the declination of the
moon; *SunAz* and *SunEl*, the azimuth and elevation of the Sun;
*Freq*, your stated operating frequency in MHz; *Tsky*, the estimated
sky background temperature in the direction of the moon, scaled to the
operating frequency; *Dpol*, the spatial polarization offset in
degrees; *MNR*, the maximum non-reciprocity of the EME path in dB,
owing to a combination of Faraday rotation and spatial polarization;
and finally *Dgrd*, an estimate of the signal degradation in dB,
relative to the best possible time with the moon at perigee in a cold
part of the sky.
The state of the art for establishing three-dimensional locations of
the sun, moon, and planets at a specified time is embodied in a
numerical model of the solar system maintained at the Jet Propulsion
Laboratory. The model has been numerically integrated to produce
tabular data that can be interpolated with very high accuracy. For
example, the celestial coordinates of the moon or a planet can be
determined at a specified time to within about 0.0000003 degrees. The
JPL ephemeris tables and interpolation routines have been incorporated
into _WSJT-X_. Further details on accuracy, especially concerning
calculated EME Doppler shifts, are described in {lunarEchoes} for
November-December, 2016.
The sky background temperatures reported by _WSJT-X_ are derived from
the all-sky 408 MHz map of Haslam et al. (Astronomy and Astrophysics
Supplement Series, 47, 1, 1982), scaled by frequency to the -2.6
power. This map has angular resolution of about 1 degree, and of
course most amateur EME antennas have much broader beamwidths than
this. Your antenna will therefore smooth out the hot spots
considerably, and the observed extremes of sky temperature will be
less. Unless you understand your sidelobes and ground reflections
extremely well, it is unlikely that more accurate sky temperatures
would be of much practical use.
A text box entitled Astronomical Data provides information needed for
tracking the sun or moon, compensating for EME Doppler shift, and
estimating EME Doppler spread and path degradation. Toggle the
*Astronomical data* on the *View* menu to display or hide this window.
image::AstroData_2.png[align="center",alt="Astronomical Data"]
Available information includes the current UTC *Date* and time; *Az*
and *El*, azimuth and elevation of the moon at your own location, in
degrees; *SelfDop*, *Width*, and *Delay*, the Doppler shift, full
limb-to-limb Doppler spread in Hz, and delay of your own EME echoes in
seconds; and *DxAz* and *DxEl*, *DxDop*, and *DxWid*, corresponding
parameters for a station located at the *DX Grid* entered on the main
window. These numbers are followed by *Dec*, the declination of the
moon; *SunAz* and *SunEl*, the azimuth and elevation of the Sun;
*Freq*, your stated operating frequency in MHz; *Tsky*, the estimated
sky background temperature in the direction of the moon, scaled to the
operating frequency; *Dpol*, the spatial polarization offset in
degrees; *MNR*, the maximum non-reciprocity of the EME path in dB,
owing to a combination of Faraday rotation and spatial polarization;
and finally *Dgrd*, an estimate of the signal degradation in dB,
relative to the best possible time with the moon at perigee in a cold
part of the sky.
On the higher microwave bands, where Faraday rotation is minimal and
linear polarization is often used, spatial offset will reduce signal
levels. Some stations have implemented mechanical polarisation
adjustment to overcome this loss, and the amount of rotation needed is
predicted in real time by the value of *Dpol*. Positive Dpol means
that the antenna should be rotated in a clockwise direction looking
from behind the antenna towards the moon. For a dish antenna, the
feed should similarly be rotated clockwise looking into the mouth of
the feed. A negative value for Dpol means anticlockwise rotation.
The state of the art for establishing three-dimensional locations of
the sun, moon, and planets at a specified time is embodied in a
numerical model of the solar system maintained at the Jet Propulsion
Laboratory. The model has been numerically integrated to produce
tabular data that can be interpolated with very high accuracy. For
example, the celestial coordinates of the moon or a planet can be
determined at a specified time to within about 0.0000003 degrees. The
JPL ephemeris tables and interpolation routines have been incorporated
into _WSJT-X_. Further details on accuracy, especially concerning
calculated EME Doppler shifts, are described in {lunarEchoes} for
November-December, 2016.
The sky background temperatures reported by _WSJT-X_ are derived from
the all-sky 408 MHz map of Haslam et al. (Astronomy and Astrophysics
Supplement Series, 47, 1, 1982), scaled by frequency to the -2.6
power. This map has angular resolution of about 1 degree, and of
course most amateur EME antennas have much broader beamwidths than
this. Your antenna will therefore smooth out the hot spots
considerably, and the observed extremes of sky temperature will be
less. Unless you understand your sidelobes and ground reflections
extremely well, it is unlikely that more accurate sky temperatures
would be of much practical use.

41
doc/user_guide/en/vhf-features.adoc
View File

@ -108,7 +108,11 @@ is generally used for EME on the 5.7 and 10 GHz bands.
- For EME QSOs some operators use short-form JT4 messages consisting
of a single tone. To activate automatic generation of these messages,
check the box labeled *Sh*.
check the box labeled *Sh*. This also enables the generation of a
single tone at 1000Hz by selecting Tx6, to assist in finding signals
initially. The box labeled *Tx6* toggles the Tx6 message from 1000Hz
to 1250Hz to indicate to the other station that you are ready to
receive messages.
- Select *Deep* from the *Decode* menu. You may also choose to
*Enable averaging* over successive transmissions and/or *Enable deep
@ -151,15 +155,15 @@ image::JT65B.png[align="center",alt="JT65B"]
=== QRA64
QRA64 is an experimental mode in Version 1.7 of _WSJT-X_. The mode is
QRA64 is an experimental mode in Version 1.8 of _WSJT-X_. The mode is
designed especially for EME on VHF and higher bands; its operation is
generally similar to JT65. The following screen shot shows an example
of a QRA64C transmission from DL7YC recorded at G3WDG over the EME
path at 24 GHz. Doppler spread on the path was 78 Hz, so although the
signal is reasonably strong its tones are broadened enough to make
them hard to see on the waterfall. The red curve shows that the
decoder has achieved synchronization with a signal at approximately
967 Hz.
generally similar to JT4 and JT65. The following screen shot shows an
example of a QRA64C transmission from DL7YC recorded at G3WDG over the
EME path at 24 GHz. Doppler spread on the path was 78 Hz, so although
the signal is reasonably strong its tones are broadened enough to make
them hard to see on the waterfall. The triangular red marker below
the frequency scale shows that the decoder has achieved
synchronization with a signal at approximately 967 Hz.
image::QRA64.png[align="center",alt="QRA64"]
@ -177,12 +181,19 @@ most likely value for each of the message's 12 six-bit information
symbols. A decode is declared only when the total probability for all
12 symbols has converged to an unambiguous value very close to 1.
TIP: In _WSJT-X_ Version 1.7 QRA64 is different from JT65 in that the
decoder attempts to find and decode only a single signal in the
receiver passband. If many signals are present you may be able to
decode them by double-clicking on the lowest tone of each one in the
waterfall. A multi-decoder like those for JT65 and JT9 has not
yet been written.
For EME QSOs some operators use short-form QRA64 messages consisting
of a single tone. To activate automatic generation of these messages,
check the box labeled *Sh*. This also enables the generation of a
single tone at 1000Hz by selecting Tx6, to assist in finding signals
initially, as the QRA64 tones are often not visible on the waterfall.
The box labeled *Tx6* switches the Tx6 message from 1000Hz to 1250Hz
to indicate to the other station that you are ready to receive messages.
TIP: QRA64 is different from JT65 in that the decoder attempts to find
and decode only a single signal in the receiver passband. If many
signals are present you may be able to decode them by double-clicking
on the lowest tone of each one in the waterfall.
=== ISCAT

6
mainwindow.cpp
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@ -2765,8 +2765,8 @@ void MainWindow::readFromStdout() //readFromStdout
}
m_QSOText=decodedtext;
}
if(m_mode=="FT8") auto_sequence (decodedtext.string(), 25, 50);
if(m_mode=="FT8" or m_mode=="QRA64") auto_sequence (decodedtext.string(), 25, 50);
postDecode (true, decodedtext.string ());
// find and extract any report for myCall
@ -4814,7 +4814,7 @@ void MainWindow::on_actionQRA64_triggered()
"Using old QRA64 sync pattern.");
m_bQRAsyncWarned=true;
}
displayWidgets(nWidgets("111110010010111110000000"));
displayWidgets(nWidgets("111110010110111110000000"));
statusChanged();
}