Abstract: Radio Frequency Interference (RFI) is a confounding problem in radio SETI, as false positives are introduced into receiver signals. Various methods exist to attempt to excise suspected RFI, with a possibility that true positives are rejected, and that un-excised RFI remain as false positives. Uncertain far side-lobe antenna patterns add to the uncertainty. To ameliorate the RFI problem, a system having geographically-spaced simultaneous and synchronized reception has been implemented. A radio telescope at the Green Bank Observatory in Green Bank, West Virginia has been combined with a radio telescope of the Deep Space Exploration Society, near Haswell, Colorado to implement a spatial filter having a thrice-Moon-distance transmitter rejection. Approximately 135 hours of simultaneous synchronized pulse observations have been captured from November 2017 through February 2019. This presentation describes the problem, observation system, observed results and a proposed hypothesis to be subjected to attempts at refutation through further experimentation and RFI and ETI transmitter signal model development.
Two wave audio files from the presentation, “Tones” and “Slow Tones”:
These are the presentations from our DSES Science Meeting on November 26, 2018.
Dr. Richard Russel reported on the latest results from the Milky Way galactic rotation rate observations of November 16. Also, he compiled all of the observations of individual radio sources done with the 60-foot antenna with the Spectracyber 1420 MHz receiver. He includes descriptions of the objects and photos, as well frequency plot observations.
Prepared for the Deep Space Exploration Society by Skip Crilly. Revised November 8, 2018.
This is an updated revision of Skip Crilly’s slide set, originally presented last summer. Skip points out that the revision includes a summary of the pulses of November 2017 through November 2018.. Two newer NRAO 5690 plots in the presentation show the very stable performance of the telescope, and the narrower Plishner beamwidth.
These are the slides from Dr. Richard Russel’s presentation about the radio astronomy observations conducted at the Plishner site during the previous Saturday, September 22. The observing period was chosen for Saturday afternoon, when the Milky Way around the galactic center was starting to rise high enough in the east. Observations were done using the Spectracyber at the 1420 MHZ neutral hydrogen I (HI) frequency.
Goals for the observing included 1) using our in-house Radio Astronomy Guide as an observing reference, 2) seeking strong enough sources listed in our guide that could serve as calibration references, 3) scanning perpendicularly across the plane of the Milky Way to observe changes in hydrogen signal while pointed inside and outside the galactic plane, 4) starting a series of doppler shift measurements along the plane of the Milky Way at galactic longitudes 10 degrees apart.
Some sources were found, but some were not. Among those found were Centarus A, Sagitarius A, and Virgo A. A number of peaks in the hydrogen signal were seen where we didn’t have any reference information that sources were present. The scan perpendicularly across the galactic plane showed the higher concentration of hydrogen in the galactic plane. We likely also detected the weaker signal of hydrogen known to be above and below the plane in certain regions. For this observing set, some sources like Sag-A were so strong that they oversaturated the voltage scale we had initially set. Doppler shifts were measured at 5 points, 10 degrees apart, along the galactic plane. Please see the slides for details.
Please click the link to see the power point slide show.
Participants: Steve Plock, Ed Corn, Rich Russel, Dave Molter, Gary Agranat.
Summary and photos by Gary Agranat.
We worked at the Plishner Radio Telescope site on Saturday August 25, 2018. One motivation was to proceed with needed infrastructure work before the cold of winter returns. Another motivation was to follow up on the observations we made during the Open House with the 60-foot antenna. In addition, the antenna tuner for the bunker ham radio station was still not running, and needed to be checked. Here is a summary of what we did, with some photos.
1. Ed and Steve replaced the outflow hose from the ramp sump with one more durable (including durable against mice). Ed tested that the outflow did drain away from the ramp area. We placed a new aluminum manhole cover on the sump access (vs the original steel one), fabricated by Steve.
2. Ed moved the Internet hotspot to the bunker. The hotspot was used by Gary while testing and operating the ham radio station.
3. Dave brought 20 x 60-pound bags of cement, and used all of them to continue to repair/rebuild the ramp retaining wall. He made considerable progress extending the base of the wall. The higher the base of the wall reaches up the ramp, the less rain sediment will clog the sump pump. Dave stayed until late in the evening, until around sunset. Gary stayed with him and gave some help.
4. Rich brought the SpectraCyber 1420 MHz Hydrogen Line Spectrometer, and used it to continue to test the functioning and ability of the SpectraCyber together with the System 1 pointing system on the 60-foot antenna. Rich later showed Gary how to steer the dish antenna, and how to measure and record neutral hydrogen data. By the end of the day we located and measured several radio sources in the Sagitarius region. And we made a systematic scan almost perpendicular to the Milky Way galactic plane, in order to measure neutral hydrogen while pointing away from and in the plane. A more detailed discussion follows later in this post.
5. Gary tested the setup of the newly installed auto tuner for the FT-897 in the bunker ham station. With some adjusting and checking of cable connections, the tuner was found to be functioning OK. Gary took the opportunity to operate K0PRT in the QSO Parties this weekend for Kansas, Ohio, Hawaii, and for the US & Canadian islands, making about 30 contacts, on SSB and CW, on 40, 20, and 15 meters. Signal reports were mostly good, which seemed to indicate the combined FT-897 + tuner system is working OK. Gary wrote some Guidance Notes for using the tuner, and left those next to the tuner.
6. We received 20 QSL cards in the mail from the Open House special event station. Myron passed them on through Ed to Gary. Gary responded to all of them, and sent in the mail our QSL card responses to all by Monday.
Next are some photos of our work. Then follows a more detailed discussion about the SpectraCyber observations with the 60-foot antenna.
SpectraCyber observations with the 60-foot antenna
Rich brought the SpectraCyber 1420 MHz Hydrogen Line Spectrometer, to follow up on the successful observations we started to make with the 60-foot antenna during our Open House 2 weeks before. We used the System 1 pointing system. I later joined him by mid afternoon, after I finished my other work, and this is a report of what we did.
We started by searching for several sources with flux density values higher than 200 Janskies. However, at first no sources were found. The plane of the Milky Way was at that time very low along the southern horizon. There were few strong sources on our list available to look for at that time.
A little later, we just about ran into the Milky Way without looking for it, when the galactic plane rose higher. The signal trace of the SpectraCyber indicated the change: pointed away from the galactic plane, the signal trace stayed near about 3 volts, varying probably with noise, but not by more than a volt. Once pointing at the galactic plane, the voltage trace increased from about 5 to 7 volts (up to about 4 volts above the noise floor). The signal consistently showed a peak at about the center of the trace, at about the frequency of neutral hydrogen. We have not calibrated the SpectraCyber, and so we don’t exactly what frequency we were peaking. (The actual spectral line frequency is 1420.40575 MHz. And we may be seeing some doppler shift in our measurement.)
We then looked for several strong sources in the Sagitarius region, which by then had risen. We successfully found several, including:
Sagitarius A, the center of our Milky Way galaxy. The radio emission is thought to be from the secondary effects of a black hole there.
CTB 37, a supernova remnant about 20,000 light years away (see https://www.nasa.gov/mission_pages/chandra/ctb-37a.html.) Our signal trace showed three peaks through most of our scans. Our interpretation is that the central peak is the original supernova remnant. The other peaks would be the doppler-shifted material outflowing away and towards us, following the supernova explosion.
The Sagitarius Star Cloud Messier 24, with a colder hydrogen cloud closer along the line of sight that absorbs some of the M24 hydrogen signal. This is the radio source Tony Bigbee pointed to during our Open House 2 weeks earlier. The signal trace has a distinctive dip, which had been identified in data from the Parkes Observatory in Australia. And as Tony has discussed, was used in the past by the RASDR2 team as an engineering detection test. The dip in signal is interpreted as a hydrogen cloud along the line of sight that is colder than the background source. It absorbs the background signal and then reradiates it out, but in all directions, hence the net signal to us is reduced. We used the RA & Dec location coordinates recorded during the Open House. We found the source again without difficulty.
We used the System 1 computer display to read the angles our 60-foot antenna was pointed to. The display showed coordinates in both azimuth & elevation (Earth ground reference), and Right Ascension & Declination (celestial sky coordinate reference). We turned the antenna with the manual steering controls. At this time we do not have automatic tracking ability. But we were able to reasonably stay on our targets with continual manual adjustments. What we more often did was we found our source, then allowed the antenna to scan at the set elevation as the Earth rotated, and as a result get a short scan along a line of Declination. We then moved the elevation up and down slightly, to see differences in the scans a little north and south. We used this technique also to hone in on targets.
We then manually scanned across the Milky Way galactic plane, to obtain a slice from 16 to 20 hours Right Ascension, along the declination of -05 degrees. We stopped at intervals of 30 minutes Right Ascension (e.g., 17h 00 min, 17h 30 min, 18h 00 min, …), to let the SpectraCyber take full scans.
Our scan cut a steep acute angle through the width of the galactic plane, going across the constellations of Ophiuchus, the north edge of Scutum, and the southern part of Aquila. We therefore started and ended at angles pointed “above” and “below” from the galactic plane, and scanned across the galactic plane in between.
Since we were pointing to the southeast (and not due south), if we moved azimuth while maintaining elevation, the declination still changed. And so to keep on the -05 degree declination line, we had to adjust azimuth and elevation together.
DSES Science Meeting August 27, 2018 Follow Up
On the following Monday we had our monthly DSES Science Meeting at the home of Rich Russel.
At the meeting we discussed the observations we made with the 60-foot antenna two days earlier.
Tony Bigbee then also presented deeper details about his RASDR4 (Radio Astronomy Software Defined Radio). And he gave us more background about the earlier RASDR2 observations of Messier 24, with the dip in frequency. And he showed how he researched the earlier Parkes observatory data to find useable results and plots for us to compare to.
Editor’s note: During the DSES Open House on the weekend of August 11, 2018, three receiver systems were tested on the 60-foot dish antenna. Dr. Richard Russel reports on their successful results, and he shows what we see in our data plots. Some highlights to point out:
The Spectracyber definitively observed the neutral hydrogen of the Milky Way as the beam width completely crossed the galactic plane.
The RASDR4 observed a known neutral hydrogen radio source, which has a closer cloud along the line of sight that absorbs some of the hydrogen signal. The distinctive signal feature is known from published data by the Parkes Radio Observatory in Australia.
The RASDR2 detected a 1296 MHz beacon set up at the home of a member about 80 miles away. This is our first definitive detection of a beacon at 1296 MHz.
-Gary Agranat, website editor.
Open House Observations using the 60-foot Dish Antenna
The DSES and Society of Amateur Radio Astronomers (SARA) teams installed three different receivers onto the 60-foot dish during the open house.
Successful Installation and Testing of the DSES Spectracyber Neutral Hydrogen Receiver.
The Spectracyber was installed on the 60-foot dish during the DSES Open House on August 11, 2018.
The Spectracyber measures 1420.406 MHz +- 600 KHz. The observation was taken while passing the galactic plane at RA: 19hr 5 Min, Dec: 6 degrees 0 Min.
The observation shows a significant signal to noise ratio as seen below.
Follow-on observations will allow for measurement of the rotation rate of the Milky Way and Solar System!
RASDR4 Receiver Successful Observation of Hydrogen Absorption Line
Tony Bigbee used his RASDR4 on the 60-foot dish to observe this hydrogen absorption line at RA: 18.15hrs, Dec:-20 deg.
This target is a hydrogen source with a cloud of material between the source and Earth that absorbs the hydrogen energy resulting in a drop off of signal as shown below.
1296 MHz Beacon Observation using a RASDR2
Bogdan Vacaliuc installed a RASDR2 onto the 60-foot dish and was able to observe the 1296 MHZ beacon at Ray Uberecken’s house, about 80 statute miles distance to the west-northwest. This observation helped verify the azimuth pointing accuracy of the 60-foot dish.
The following is a comparison of simultaneous observations made on August 15, 2018 of the astronomical radio source, NRAO 5690.
The first plot is an observation made by Skip Crilly at the 4o foot radio telescope at Greenbank Observatory in West Virginia. The second plot is an observation made by Steve Plock at the DSES Plishner 60-foot antenna in Haswell, Colorado.
NRAO 5690 is a catalogued supernova remnant (SNR), with the celestial coordinate location of 18 hours 35 minutes Right Ascension and -7 degrees 20 minutes Declination. It is known to have an apparent radio brightness of 90 Janskies at 1.4 GHz *(1).
Each observation was made by Drift Scan. Drift scan is fixing the azimuth (left-right) direction of the antenna, and scanning the sky as the Earth rotates. For each dish antenna, the elevation above the horizon is also fixed. As the Earth turns (at a quarter of a degree per minute), each antenna can detect radio source objects within its sensitivity, as the objects cross the beam width.
The observation at Haswell was done during a 42 hour drift scan at -7.6 degrees declination, in support of the joint SETI (Search for Extraterrestrial Intelligence) work between DSES and Skip Crilly *(2). The dual plots show we are observing the same astronomical object at known pointing angles, and is a good verification of the two systems observing together.
1. Reference: NRAO VLA 1.4 GHz survey.
2. Geographically-spaced Synchronized Signal Detection System” by Skip Crilly. Presentation on June 11, 2018 at the Society of Amateur Radio Astronomers Conference Green Bank Observatory, West Virginia, USA
The DSES Sudden Ionospheric Disturbance Monitor (SID) detected in September several major solar eruptions – M and X Class Flares. Below are shown graphs of the data from four particular days.
The DSES SID instrument is located in Colorado Springs. It works by listening for a US Navy beacon station in North Dakota, call sign NML, transmitting on the Very Low Frequency (VLF) of 25 KHz. During the day, the D Layer of the ionosphere forms at lower altitudes and attenuates the VLF signal. But during solar flares, VLF signals can more easily pass through the D Layer, and they then get bounced back to the ground from the higher F Layer. The more the solar flare activity affecting our ionosphere, the better the VLF signal from NML propagates to us.
Strong solar flare events show a characteristic spike, and then a “shark tail” as the ionosphere recovers.
At night, the D Layer dissipates, and then the signal from NML usually easily reaches the receiver. At local sunrise, at about 1200 UTC, you can see the effect of the D Layer forming with the sudden drop in reception.
You can see evidence that the F Layer is influenced by the solar flares as well. Notice during the X 8.2 Flare on September 10 that the incoming signal becomes even stronger than during normal propagation at night.
The bottom axis of each graph is Greenwich (UTC) Time. The vertical axis shows the received energy. Individual flare events are identified and annotated in green. Some events occurred during local night.
DSES President Dr. Richard Russel has been measuring signal strengths 0f stations in the Very Low Frequency (VLF) band for the past year, looking for changes in ionospheric propagation due to solar flares. He uses a Sudden Ionospheric Disturbance (SID) monitor small radio telescope. His SID detector is located in Colorado Springs, CO. The measurements are sensitive to the changes in radio propagation at sunrise and sunset.
With his baseline of historical data at sunrise and sunset, he then predicted what could be expected during the August 20, 2017 solar eclipse. He presented his prediction work at the 2017 Society of Amateur Radio Astronomers Annual Conference at NRAO Greenbank, WV on July 25, 2017. His paper was titled, “Ionospheric Reflection Variation During Sunrise and Sunset and Predictions for the 2017 Total Eclipse”.
During the eclipse he made measurements, and found the results matched closely with his predictions. The link presents a summary of his work. Plus it has YouTube links to this and another of his talks at the SARA conference. The second talk is titled, “The Use of Monte-Carlo Analysis to Evaluate Radio Astronomy Source Detection”.