Es’hail 2 is the second communications satellite operated by the Qatari company Es’hailSat. It was built by Mitsubishi Electric Corporation (MELCO). It carries several Ku and Ka band transponders intended for digital television, Internet access and other data services. It also carries an Amateur radio payload designed by AMSAT-DL, in collaboration with the Qatar Amateur Radio Society. The payload has two transponders, with S-band uplink and X-band downlink. One of the transponders is 250kHz wide and intended for narrowband modes, and the other one is 8MHz wide and intended for DVB-S and other wideband data modes.
SpaceX live-streamed the launch, and the recording can be seen in YouTube. Today, Space-Track has published the first TLEs for Es’hail 2 and the second stage of the Falcon 9 rocket. Here I look at these TLEs using GMAT.
Lately, I have been testing the GPSDO that I will use to discipline my Es’hail 2 groundstation. One of the tests I have done is to measure the frequency of the TCXO that I use in my Hermes-Lite 2.0beta2 over a few days. Here I show the details of the measurement process and how to process the data in Python.
The planning for the activations of the Amateur payload made by Wei Mingchuan BG2BHC was as follows.
7 Nov 2018 08:13 to 7 Nov 2018 10:13 8 Nov 2018 09:40 to 8 Nov 2018 11:40 9 Nov 2018 12:00 to 9 Nov 2018 14:00 10 Nov 2018 14:00 to 10 Nov 2018 16:00 11 Nov 2018 13:30 to 11 Nov 2018 15:30
On November 7, from 8:13 to 9:33 UTC, a total of 9 images with 10 minutes of spacing between each would be taken. These images would be downloaded during the activations on the next days. As usual, an image would also be taken when the Amateur payload powered up on November 8 to 11, but the main focus was on downloading the sequence of images taken on November 7. This is a complete report of the images taken and downloaded.
Now that the planned dates are closer, it is good to rerun the calculations with a newer orbital state. It turns out that there has been an important change in the mean anomaly, which shifts all the predictions by a few hours.
I have spoken in other occasions about planning the appropriate times to take pictures with the DSLWP-B Inory eye camera. In the beginning of October there was a window that allowed us to take images of the Moon and Earth. A lunar month after this we have new Moon again, so it is an appropriate time to take images with the camera.
This time, the Moon will pass nearer to the centre of the image than on October, and at certain times the Earth will hide behind the Moon, as seen from the camera. This opens up the possibility for taking Earthrise pictures such as the famous image taken during the Apollo 8 mission.
I have updated my camera planning Jupyter notebook to compute the appropriate moments to take images. The image below shows my usual camera field of view diagram.
The vertical axis represents the angular distance in degrees between each object and the centre of the image (Assuming the camera is pointing perfectly away from the Sun. In real life we can have a couple degrees of offset). The red lines represent the limits of the camera field of view, which are measured between the centre and the nearest edge, and between the centre and one corner. Everything between these two lines will only appear if the camera rotation is adequate. Everything below the lower line is guaranteed to appear, regardless of rotation.
We see that between November 6th and November 9th there are four times when the camera will be able to image the Earth and the Moon simultaneously. On the 6th it is almost guaranteed that the Earth will appear inside the image, and on the 9th it depends on the orientation of the camera. On the 7th and 8th it is guaranteed that the Earth will be in the image.
To compute appropriate times for taking an Earthrise picture, I have made the graph below. This shows the angular distance between the Earth and the rim of the Moon. If the distance is negative, the Earth is hidden by the Moon. We see that the Earth hides behind the lunar disc on each of the four days mentioned above.
In the figures below, we zoom in each of the events. In this level of zoom we can plot the “inner” and “outer” Earth rim, so we can see when the Earth is partially hidden by the Moon.
On November 6th the situation is the most interesting in my opinion. It turns out the the Earth will not even hide completely between the Moon. In theory, a tiny sliver will remain visible. Also, it will take more time for the Earth to hide behind the Moon and then reappear. As we will see, the next days this will happen faster. Here, it takes 15 minutes for the Earth to hide, and another 15 minutes to reappear. It spends 10 minutes almost hidden.
It can be a good idea to take a series of 10 images with an interval of 5 minutes between each image, and spanning from 12:40 UTC to 13:30 UTC, to get a good coverage for this event.
On November 7th the Earth goes deeper into the lunar disc, taking 5 minutes to hide, spending 70 minutes hidden, and taking 10 minutes to reappear.
On November 8th the Earth goes even deeper into the lunar disc. It takes around 7 minutes to hide, spends 105 minutes hidden and takes 10 minutes to reappear.
On November 9th the configuration is quite similar to November 7th, but the hiding speed is slower. It takes 15 minutes to hide, spends 100 minutes hidden and takes 15 minutes to reappear.
Overall, I think that the best would be to take a good series of images on November 6th, since this shallow occultation is a rarer event. The challenge will be perhaps to download all the images taken during these days. On average, I think we are downloading around 2 new images per 2 hour activation, taking into account repeats due to lost blocks and dead times. DSLWP-B is able to store 16 images onboard, and every time the UHF transmitter comes on, a new image is taken, overwriting an old image (more information in this post). Thus, if we take many images during these days, we have the danger of overwriting some when trying to download them over the next few days.
Perhaps a good strategy is to arrange for a series of 10 images to be taken on the 6th, and then programming the UHF transmitter to take an image as the Earth comes out of its occultation on the 7th, 8th and 9th. In this way, the 2 hour periods of these three days can be used to download some of the images taken on the 6th, and there are still 3 images of margin in the buffer in case something goes wrong during the downloads over the next few days.
In my previous post I showed that during the DSLWP-B observation on 2018-10-27 17:20 UTC, the orbit of DSLWP-B would take it behind the Moon. This doesn’t happen every orbit (read as every day, since the orbit period is around 22 hours). It depends on the angle from which the orbit is viewed from Earth, and hence on the lunar phase.
Knowing beforehand when DSLWP-B will hide behind the Moon allows to perform radio occultation studies. These consist in measuring the RF signal from DSLWP-B as it gets blocked by the lunar disc. Interesting phenomena such as diffraction can be observed.
I have calculated the occultations that will be visible from the Dwingeloo radiotelescope in the remaining part of this year.
I have made a Python script to plot the Doppler and geometry for a DSLWP-B observation. This can be useful for several things: predicting the downlink and uplink Doppler corrections, checking for the Doppler of the Moonbounce signal, checking the position of DSLWP-B in the sky, and studying Moonbounce geometry.
I have already spoken about the Moonbounce signal from DSLWP-B in several posts. To sum up, DSLWP-B is a Chinese satellite that is orbiting the Moon since May 25. The satellite has an Amateur payload that transmits GMSK and JT4G telemetry in the 70cm Amateur satellite band. This signal can be received by well equipped groundstations on Earth, including the 25m radiotelescope at Dwingeloo, in the Netherlands (and also by much smaller stations).
The people at Dwingeloo publish the recordings that they make of the RF signal. In two of these recordings, the signal from DSLWP-B is received not only via the direct path, but also through a reflection off the Moon’s surface. The reflected signal is around 25dB weaker, usually has a different Doppler shift, and has a Doppler spread of around 50 to 200Hz.
What I find most interesting about this is that of all the days that Dwingeloo has observed DSLWP-B, in only two of them (on 2018-10-07 and 2018-10-19) the Moonbounce signal has been visible. Mathematically, using a specular reflection on a sphere model, whenever the satellite is visible directly, there is also a ray from the spacecraft that reflects off the lunar surface and arrives at the groundstation (see the proof here). Therefore, I think that there must be something about the particular geometry of the days 7th and 19th that made the Moon reflections relatively stronger and hence detectable. Here I use GMAT to study the orbital geometry when the reflections were received.
On the other hand, JT4G is a digital mode designed for Earth-Moon-Earth microwave communications, so it is tolerant to high Doppler spreads. However, the reflections of the B0 transmitter at 435.4MHz, which contained the JT4G transmissions, were very weak, so I had not attempted to decode the JT4G Moonbounce signal.
On 2018-10-19, the Moonbounce signal from DSLWP-B was again visible in Dwingeloo’s recordings. I have used the 2018-10-19T17:53:35 435.4MHz recording and managed to decode the Moonbounce signal of one out of the five JT4G transmissions that appear in the recording.
To extract the data from the recording to WAV files that can be read by WSJT-X, I have used the following Jupyter notebook. Then I have used WSJT-X version 2.0.0-rc3 to try to decode the Moonbounce signal. Since the JT4 decoder only decodes a single signal at the selected frequency, it is enough to select the frequency of the Moonbounce signal in WSJT-X. The direct signal will not be decoded, even though it is also present in the WAV file.
The only transmission that I have managed to decode was made at 18:11 UTC. The two screenshots below show WSJT-X decoding the WAV file extracted from the recording.
Note the direct signal with a lowest tone at 1800Hz. The reflected signal is very faint, with a lowest tone at 700Hz. The Doppler spread of the reflected signal is large, approximately 200Hz, although it is difficult to judge from the spectrum.
When the WAV file is created, I also compensate for a linear frequency drift of 25Hz per minute due to Doppler, but this is not essential to obtain a valid decode.
The WAV file that produces a decode can be downloaded here. This file can be opened directly by WSJT-X.