According to our team “The frequency offset is ~18025 Hz on Spectravue, so it looks likely. He’s tuned to XB, so just seeing the very tip of the PM carrier.”
Phil Karn KA9Q
Thank you for the timestamp, qth etc, and the info about the Spectravue
I examined the file anyway and worked out that a “stereo” signal was I and Q,
16-bits each, LSB first.
I confirm the signal as you found. I averaged small and large numbers of
FFTs. This showed that the signal strength varied, between approximately
11 to 16 dB-Hz. The spacecraft is spinning at about 3 rpm, so this may be
Attached is a typical plot from my my own software. This is not the strongest
signal display; the largest I found was a signal = -45.7 dB over the
noisefloor = -53.8 dB, or SNR = 8.1 dB.
With a bin bandwidth of 0.124 Hz, this equates to a CNR of 16.4 dB-Hz.
73 de James G3RUH
ISEE-3 signal processed by G3RUH
Finally after four days of attempts I detected the ISEE-3 / ICE space probe
I used the LHCP channel that is at 2217.5MHz becuse I have a lot of noise in the RHCP channel. I used a can feddhorn and a plexiglas depolarizer.
The signal is very weak and impossible to see without time integration. The offset reported by the Arecibo guys of 7202Hz has been very important to locate the probe. In my case I’m getting the probe with a carrier offset of 6035Hz from 2217.5MHz.
Here the first detection:
ISEE-3 / ICE Dection
After the detction, to confirm that I moved the dish 18deg, and the signal disappears:
ISEE-3 / ICE off center
To confirm again the signal I stoped the doppler compensation:
ISEE-3 / ICE no signal without the doppler compensation
Finally I started to compensate the doppler again and the signal is acquired again:
ISEE-3 / ICE with doppler corrected
To finally confirm at 100% a offline signal process without doppler compensation to see doppler signature. I used the amazing baudline autodrift option, it is a great feature to see signals with doppler:
ISEE-3 / ICE baudline autodrift
Here the IQ recording from Spectravue without the doppler compensation used in the baudline analysis. The sample rate is 8138 samples/sec:
Detected the GAIA spacecraft travelling to the L2 point.
ESA GAIA Mission
The frequency is 8465 MHz and for the moment don’t have ephemeris from the JPL/Horizons or spice kernels. For the moment using the ephems from GBOT getting a aprox RA and DEC and using my own tools for full tracking.
Integrating the Yutu using baudline the signals recorded during the seperation from the Chang’e 3 you can see two signal variations. At the 20:27:31 UTC during two minutes aprox the signal was more weak and scince the 20:35:40 UTC the signal was boosted. Then the separation was before of the 20:40 UTC ?
Signal integration from the Yutu landing
Yesterday the Chang’e3 spacecraft andt the Yutu rover was landing successfuly. I was start to track the moon since the 18:30 to the 22:30 UTC. And I was listen Yutu from the start of my window and the signal was over 15dB of SN at 1Hz of BW. The frequency of the rover is 8462.08000MHz with the moon doppler of -0.6Hz/s of aprox. The signal was easy to listen in the earphones, and sounds like a some kind of morse.
For this event I was setup two receivers, as main a AOR AR5000 and Rfspace SDR14. As second receiver a rtl-sdr doongle with r820t tuner and baudline.
Yutu rover, using AR5000 + SDR14
Yutu rover using rtl-sdr + baudline
The command line to use rtlsdr with baudline was:
rtl_fm -g 44 -d0 -f$1 -s 250000 -F -U | ./baudline.static -stdin -samplerate 250000 -channels 1 -session rtlsdr1chUSB0 -basefrequency $1
Yutu rover using rtlsdr + baudline
Now you can listen how sounds the data stream from Yutu. A short audio record of the signal demodulated:
Another full orbit of Chang’e 3 centered ar 8470MHz with a 100KHz span. This time with locking to ground station included:
Chang’e 3 full orbit
Zoom of one of the frequency lock to some tracking Ground Station:
Chang’e 3 Grond Station locking
Yesterday the Chang’e3 spacecraft finished the orbital insertion into polar orbit around the moon. The signal is strong and easy to listen in the receiver speaker. Today I get a full orbit of the probe. Every pixel are 10secs and the receiver was tuned at 8479.749200MHz
Chang’e3 full orbit
More info of Chang’e3 in Spaceflight101.
This week he the enthusiasts os the space probes and the amateur-DSN are living a nice week dued the flyby of the Juno spacecraft. The flyby will be in the next October 9th.
When the spaceprobes are very near to the Earth to do a flyby, the low gain (LGA)and medium gain (MGA) antennas are used. As this antennas not are in the central axis of the probe and it is rotating continuosly, you can see the rotational movement in the screenshoot:
Juno received from EB3FRN station
The next images, I’m comparing the data using my ephemeris in the upper side and Horizons ephemeris in the lower side. Remember that Horizons dont give data for planetary probes, and are using the data of the planet that is orbiting the planet.
Data for Mars Express
As you can apreciate, in the upper side, the range calculated using SPICE and the mission kernels is smaller than the range of the MARS calculated by Horizons. Then the MEX space probe not is eclipsed by the planet and then detectatble for our stations in the earth! Check the difference of 60 KHz in the predicted frecuency and doppler too.
Data for Mars Reconnaissance Orbiter
Now the inverse case, the MRO probe is more away from the earth, then the probe is eclipsed by the planet.
Another issue observed is a small position difference from JPL/Horizons to my ephemerris using SPICE. It happend, because JPL/Horizons uses TDB as time reference and I’m using UTC. Then, exists a difference of few secconds produced by the leap seconds.
As I was write in my last post, one of the challenges of the amateur-DSN stations is get the ephemeris of the space probes to get the position and deldot for the doppler. JPL Horizons helps, but dont give info about the planetary space probes. How solve it? The solution is use the same data and tools that are using the mission control Every mission, have a dataset called kernel that contains info about position, instruments and clock onboard, mission operations, etc… this data is public and is controlled by NASA / NAIF and can be obtenied from here.
JPL / NAIF website
The Nasa NAIF, proces a toolkit called SPICE to use this data. This toolkit is available in a lot of programming languages and have a good documentation. Using a small piece of code from Achim Vollhardt DH2VA that he was send-me in 2006 and after some years googling a lot, finally I build my own planetary probes ephemeris generator.
Spice tookit code
In the next post the results…
One of the challenges of the amateur-DSN stations to track planetary and solar system space-probes is the position and frecuency accuracy. Currently all the stations are using the ephemeris provided by the JPL Horizons system. This is a cool system and can be used online using telnet, using a web interface or via email and provide-us the position, range and deldot of the select target, then using this data can track easy the probes and calculate the doppler.
Due that the JPL Horizons is a service for the main public basically for amateurs and space anthussiastas, they can not provide ephemeris for probes or missions that are orbiting a planet because this kind of missions not are static and depends of the stage of the mission.
The solution provided by Horizons is track the planet is orbiting the probe, for example to track MRO, MEX and MO have to track Mars. It works because the position difference is minimal, a typical difference of less of 0.05 deg and it not makes a sense in our small dishes. The amateur-DSN members are detecting space propbes that are orbiting a planet during years with good results, but we have some troubles like taht we dont know when the probe is eclipsed by the planet and, and we dont know the exact frequency where is the probe, because the probe and planet have a differnt deldot. Now I’m working in generate my own ephemeris, to get the data of the probes that are orbiting planets.
A interesting issue about Horizons that I discovered recently is that dont give the data in UTC time, it gives the data in Barycentric Dynamical Time.
Today I continued updating the downconverter for X-band deep space probes. Having the local oscillator selected, today was the mixer selection. Up today I was using a RHG mixer purchased in 2006, but from the 2006 up today I purchased another units, but not tested up today.
RF Mixer testing, test setup
After test the 5 units, looks that I have a unit perfect for 8.4 GHz it is a Aertech 8500 this mixer look more of 4 dB better that the RHG mixer used up today.
RF Mixer comparation
Now only need check the low noise amplifier to see the performance and decide if I build a new one. I’m very anxious to receive space probes again!
After the dish controller rebuild, now I’m updating the X-Band downconverter.
One question that rounds over my mind some times is how good is the phase noise of the Ma/Com brick that I’m using in the downconverter as local oscillator. The last year I was puchase in eBay a nice Ferranti brick oscillator.
Phase noise test
The two units are locked to a 10MHz rubidium reference. After some tests and tuning, the Ferranti beats the Ma/Com, it is much clear:
Macom vs Ferranti PN