These are the slides from our DSES Science Meeting, held online on November 23, 2020. The science meeting was led by Rich Russel, and moderated by Bill Miller.
We plan to upload the agenda and notes for the meeting soon also.
These are the slides from our DSES Science Meeting, held online on November 23, 2020. The science meeting was led by Rich Russel, and moderated by Bill Miller.
We plan to upload the agenda and notes for the meeting soon also.
Written summary and photos by Bill Miller.
Ray Uberecken and Bill Miller went to the Plishner site on Sat. October 31.
Ray brought back his EME 200 Watt amplifier box that he had removed on the previous weeks trip. The unit had blown a relay control FET that kept the unit in the transmit position so it would not connect the feed to the receiver. Ray and Bill donned climbing harnesses, scaled the scaffold, and installed the amplifier before the wind could start blowing about 11:00 AM at the site.
Ray also brought back the FT 736 Transceiver after repairing the seized tuning knob. He brought in a computer and an audio interface with JT-65 HF software loaded. This will enable digital mode EME on the next contest EME 50-1296 MHz — November 28-29, 2020. In addition, he installed an extra 1296 MHz 18 Watt auxiliary amplifier between the FT736 10W max output and the Amplifier at the feed point. This extra amplifier will enable the full power of the linear amp at the feed. Both the 18 watt amp and the 200 watt feed point amp are enabled with the Key circuit from the FT 736.
There is an extra power supply on the bench to power the 18 Watt amp and the key circuit to the feed amp is attached with the terminal block on the rack.
Ray also brought back the Electronic Keyer and Paddle for the FT736 moon bounce CW mode.
Once all this equipment was installed, we climbed the tower and replaced the bad swivel joint on the down feed coax with a short segment of very flexible RG8X cable to allow the cable wrap. Because this is the same impedance as the main hard line coax and very short it has insignificant loss to the signal.
We then called Myron Babcock to test the equipment. We pointed the dish at Colorado Springs and at first did not hear his signal. He swung his antenna around to point at Pike’s Peak and we did the same and established communication on 1296.1 MHz with clear copy. This proved the overall system viability.
Bill set up his phone app and computer program for aiming the Hughes Net dish for internet. After using the compass to point the dish to the apps specified Azimuth and Elevation and working the dish around for half an hour, we still couldn’t get the modem to lock up and receive the satellite. More research is needed to make sure we are trying for the correct satellite and have the right coordinates and tools to do the alignment on the next trip. Once we have the Hughes Net system working, we should have high speed internet capability for a number of uses.
Ray has been working on his new radio Astronomy receiver based on a medical signal preconditioner and a stable amplifier/integrator and A/D converter. The receiver will give a greater bandwidth than current SDRs with up to 100MHz of bandwidth.
A conversion program is needed to convert the comma delimited tabular output of the A/D to the .Fil file format for radio astronomy. Ray installed the receiver and checked its operation.
We stowed the dish, shut everything down, removed the trash and locked the site. Note that the new service position on the scaffold after the recalibration of the pointing system is 314.5 deg. All old bearings for Beacons and such should be adjusted by -2.5 deg.
You can read a PDF version of this report here: 2020-10-31-Plishner-site-trip-summary-v2-.pdf
Welcome to the DSES Science meeting 10-26-2020
2020-10-26 DSES Science Meeting Notes: by Bill Miller
We had 14 participants in the virtual science meeting today: Thanks everyone for joining.
Participants: Dr. Rich Russel, Ray Uberecken, Chad Carter N0ZMG, Don Lewis, Matt Mathews, Bob Haggart, Michael Nameika, Gary Agranat, Jonathan Ayers,Floyd Glick, Don Latham, Myron Babcock, Ted Cline on Phone, Bill Miller
Also see the Zoom Video Recording for more detail:
Agenda and notes:
By Gary Agranat, with Myron Babcock and Glenn Davis. Videos by Bill Miller.
On Saturday October 10, 2020 we succeeded in making our first Earth-Moon-Earth (EME) Moon Bounce communications. We succeeded at our first attempt. This accomplishment was several years in the making, thanks to the work of many members, past and present.
We did this participating in the annual ARRL EME contest held on the weekend of October 10-11, 2020 GMT. (That’s Friday 6 pm to Sunday 6 pm local time.) The frequencies available for this contest were in the ham radio bands from 50 to 1296 MHz. We used our 60-foot dish antenna at Haswell, CO, with a 1296 MHz feed with dual circular polarization, installed 2 weekends earlier.
EME Moon Bounce communications is directing a signal to the Moon. The Moon’s surface simply reflects the signal back to Earth. If the Moon is above your horizon, if you have suitable equipment, and if you know enough about what to do, it would be possible for you to receive the signal and communicate back. You could communicate to your neighbor or across continents. The signals, however, are extremely weak, having to travel back and forth the Earth-Moon distance, over 238,000 miles. EME generally requires efficient directional antennas to sufficiently increase the signal gain. Amplifiers can be used too. And the antennas have to point to the Moon. Also, radio signals sent through the ionosphere experience a rotation in their polarization. And there is some effective rotation from other causes, including from the changes in orientation from the Moon and from operating on different points of the Earth’s globe. Our solution is to circularly polarize our signals. And also, there is a Doppler shift between transmitted and received signal, mostly due to the Earth’s rotation, causing a difference in velocity between the Moon and our location on Earth. All of these are challenges to deal with.
Our team for the EME operation were Ray Uberecken AA0L, Myron Babcock KL7YY, Gary Agranat WA2JQZ, and Glenn Davis. Bill Miller KC0FHN also came on Saturday morning.
The team arrived Friday evening October 9, while we still had daylight, to set up and test. Testing included making pre-arranged tropospheric scatter contacts, which were successful. We also attempted to complete set-up of a Hughes Internet antenna, to give us Internet access, but that was not successful. We instead sometimes connected to the Internet using cellphones. Although the contest began at 6 PM local time, we had to wait for the moon to rise above the horizon. Moonrise for us was at about 11:30 PM local time, and the Moon was above our horizon until about 2 PM local time the next day Saturday. We chose to stay for just this one Moon pass, and not continue through Sunday, in order to not knock ourselves out on this first attempt.
After we completed our testing, we relaxed until we were ready to start. Looking outside, we had an exceptionally deep starry sky. We could see the Milky Way clearly arching overhead through Cygnus. Jupiter and Saturn were bright to the south, and Mars was very bright, rising in the east. Glenn Davis experimented with his camera and took some nice time exposure photos with the dish antenna, the stars, and the Milky Way.
I (Gary) meanwhile got some rest. This enabled the others to get some rest later in the morning while I continued.
Myron KL7YY wrote and emailed an update about our operations to the DSES membership on Saturday morning at around 4 AM. It provides a good narrative of how we were doing until that point, and his update follows next:
* * * * * * * * * * *
Summary of DSES first attempt at EME, Earth Moon Earth, contacts using the 60 foot dish:
On Friday evening, October 9 we started with a few nearby Tropospheric Scatter contacts around 7 PM with DSES member KL7IZW, Steve in Monument, CO, and W6OAL Dave in Parker. Around 9 PM we talked to N0YK in Scott City KS, These contacts ranged from 110 to 130 miles and confirmed that our system was working.
When the moon came over the horizon at midnight we tried to listen to the ON0EME moon beacon in Belgium but couldn’t hear it. About 45 minutes after moon rise we started to hear JT-65 digital signals. 10-15 minutes we started to hear CW signals. Glenn Davis made a few corrections to the tracking program and signals increased in strength. At times it sounded like a 20 meter CW contest pileup with all the loud signals bouncing off the moon all across 100 KHz of band (1296.0 to 1296.1 MHz). After about 90 minutes without hearing our own signal we rechecked the power to the amplifier at the feed horn and everything appeared to be normal. A few moments later we finally heard our own signal 2.5 seconds later on CW off the moon and the Belgium Moon Beacon. I made several calls on SSB and heard our echo really loud. We went back to CW and Gary proceeded to start making CW contacts. The first almost contact, a German station, abruptly dropped out so no official contact was completed. Our first official station worked on CW was with OH2DG in Finland. England was next followed by Italy, Poland, Denmark, Sweden and with DSES member Skip Macaulay, VE6BGT, in Alberta Canada.. Also made our first voice SSB contact with him as well. Seems that with every new contact we make it is with a new European country. In order to correct for Doppler shift and with no RIT we are changing VFO’s from Receive to Transmit by several KHz or more. Lots of CW signals being heard and we still have 12 more hours of moon to bounce signals off of… We are hearing our own echo and we have lots of hours to go. We plan on Digital mode later in the day but for now there are more than enough signals to hear on CW.
Our Moon bounce station consist of an older Yaesu FT-736R with 10 watts feeding almost 180 feet of half inch hardline into a 200 watt amplifier at the antenna feed horn. The receiver pre amplifier is a 30+db gain with a noise figure of minus .35. Our Effective Radiated Power (ERP) is over 6 million watts.
* * * * * * * * * * *
We operated with our club call sign K0PRT.
A short video of Myron KL7YY calling CQ. You can hear the echo of his signal coming back from the Moon a couple of seconds later. (Video length 35 seconds)
Because the signals are extremely weak, and there can be fading, there is a standard protocol for exchanging messages for EME contacts. This is intended to ensure as much of the message as possible can be copied and acknowledged on both sides. The basic format is simple, and one repeats a lot. One first exchanges call signs, then the signal reports, and then finally if that worked, an acknowledgement all that was copied correctly. If one only completes part of the contact, one should still log that, as that is an accomplishment. If using Morse Code, the standard is to send at 15 words per minute, but spacing out the characters longer than usual. The faster sending and spacing is to help one copy complete characters if there is fading. If one misses a character, one still has a high chance to get the character with the many repeats.
In order to have the proper frequency offset for the Doppler shift, we referenced the WSJT 10.0 software, at the suggestion of Steve KL7IZW. The software has an astronomical data section that calculates and displays the frequency offset. The higher the frequency, the more significant the offset. At 1296 MHz we had a difference of as much as 3 KHz between transmit and receive frequencies. The software also displays other useful data like local Moon rise and set times (based on Grid Square location).
The WSJT 10.0 software also can be used for JT65C digital EME communication. However, we didn’t figure out how to configure that in time with our setup, and so we didn’t do any digital contacts this time. We could tell we were hearing JT65 signals. They were present from 1296.05 to 1296.1 MHz, and we almost always could hear those signals while the Moon was up.
Glenn stayed up until about 3 AM, when we were sure our antenna azimuth alignment was correct and would continue to point accurately to the Moon. His work was invaluable in troubleshooting the azimuth offset, which turned out to be about 1.5 degrees, and honing in on the Moon once we heard CW signals.
Since the Moon rises in the east, our signal paths at first are to the east. That is to Europe and the North American east coast. As Myron mentions, once we started receiving the signals, we were hearing many European stations, and we were busy. Through the morning we made 14 contacts to Europe, to 8 European countries. We also made the contact to our DSES member Skip Macaulay VE6BGT in Alberta, Canada, on CW and then phone. W4OP in North Carolina, hearing us on SSB, then gave us a call on SSB too.
Ray AAOL brought a CW keyer that can send Morse Code with either a keyer paddle or a keyboard. It can store pre-programmed messages, like a CQ call. I (Gary) decided to use the keyer paddle, as that gave me more flexibility — I could quickly adjust for conditions — and I felt more comfortable as I am used to the key. Meanwhile, it seemed to me also that some of the CW contacts we made used software to send their messages. Those didn’t have good spacing between words or call signs. And that made copying slightly more challenging. A keyboard though can enable any of us to send, even if we don’t have practice sending Morse Code. Most of the contacts we made were with CW Morse Code.
This short video shows part of a Morse Code CW contact by Gary WA2JQZ. XE1XA in Mexico called CQ. We responded by sending our call sign K0PRT several times. Then K (the invitation to respond) several times. When we switch the VFO from the transmit to the receive frequency, you can hear the last part of our signal coming back, reflecting from the Moon, several seconds later. You then here the signal from XE1XA, also coming back reflecting from the Moon. He transmitted back our call sign as K0PRN, instead of K0PRT. We afterwards replied sending our callsign again, only, to give him the correction. That’s why we repeat a lot, and send sections of the message just one at a time. We completed the contact successfully. If you look carefully on the transceiver, you will see we switched about 2 KHz down from the transmit to receive frequency. (Video length 1:16)
At around 6 AM, when the Moon was high enough so that we no longer had a path to Europe, we took a break for breakfast and to rest.
In earlier discussions we thought we might have many more contacts across the Pacific and to the North American west coast, when the Moon was sufficiently to the west. But it turned out we had very few contacts that way. We made just two contacts to Japan. Our first was at about 9 AM local time, to JH1KRC. Our second was three hours later to JA6AHB. Instead we made a few more contacts to the US, a few to Canada, and one to Mexico. These other stations we heard were searching around too. That led me to believe that if there were any other signals out there, we likely would have heard them.
Our contacts included:
A video of Gary WA2JQZ responding to W6YX at Stanford University and having a 4 minute SSB QSO. (Video length 4:38)
We operated until about noon. We made 30 contacts in all. 25 contacts were CW (Morse Code) and 5 were SSB phone. 4 of the 5 phone contacts were with stations we also had CW QSOs with.
We submitted our contest log to ARRL the next day.
In the judgement of all of us, we had a very good EME operation. We are very pleased it worked so well on the first attempt. We clearly have a capable EME station.
Glenn and his team are continuing to follow up to investigate why we had a 1.5 degree azimuth offset.
It still takes my breath away to hear the echo of our signal coming back from the Moon, a couple of seconds later. The speed of light isn’t just a value in the books, it is something you experience viscerally first hand. It is real. EME is the longest signal path we have for communicating with others. This is fun.
These are the contacts we made. (CW = Morse Code, PH = SSB phone. Given also are the date and GMT times, the signal reports, and the other stations and their locations):
CW 10/10/2020 750 K0PRT 559 DL0SHF 559 Germany
CW 10/10/2020 756 K0PRT 559 OH2DG 579 Finland
CW 10/10/2020 805 K0PRT 559 G3LTF 579 England
CW 10/10/2020 814 K0PRT 549 I5MPK 569 Italy
CW 10/10/2020 846 K0PRT 569 SP6JLW 589 Poland
CW 10/10/2020 900 K0PRT 559 DL4DTU 559 Germany
CW 10/10/2020 912 K0PRT 579 SM4IVE 589 Sweden
CW 10/10/2020 919 K0PRT 549 DG5CST 569 Germany
CW 10/10/2020 934 K0PRT 559 VE6BGT 579 Alberta, Canada
PH 10/10/2020 947 K0PRT 57 VE6BGT 56 Alberta, Canada
PH 10/10/2020 947 K0PRT 55 W4OP 57 North Carolina, USA
CW 10/10/2020 1034 K0PRT 549 OK1KKD 569 Czech Republic
CW 10/10/2020 1043 K0PRT 599 OE5JFL 599 Austria
CW 10/10/2020 1049 K0PRT 579 W6YX 589 California, USA
CW 10/10/2020 1103 K0PRT 569 IK2MMB 569 Italy
CW 10/10/2020 1111 K0PRT 579 OZ4MM 599 Denmark
CW 10/10/2020 1149 K0PRT 549 OK1CS 579 Czech Republic
CW 10/10/2020 1153 K0PRT 569 OK2DL 479 Czech Republic
CW 10/10/2020 1201 K0PRT 559 VE6TA 579 Alberta, Canada
CW 10/10/2020 1503 K0PRT 559 JH1KRC 569 Japan
CW 10/10/2020 1526 K0PRT 549 AA4MD 559 Florida, USA
CW 10/10/2020 1533 K0PRT 569 WA9FWD 559 Wisconsin, USA
CW 10/10/2020 1540 K0PRT 569 W5LUA 579 Texas, USA
PH 10/10/2020 1547 K0PRT 569 W5LUA 579 Texas, USA
CW 10/10/2020 1652 K0PRT 539 VA7MM 559 British Columbia, Canada
CW 10/10/2020 1703 K0PRT 559 XE1XA 559 Mexico
PH 10/10/2020 1731 K0PRT 55 VE6TA 55 Alberta, Canada
CW 10/10/2020 1740 K0PRT 569 K2UYH 559 New Jersey, USA
CW 10/10/2020 1806 K0PRT 549 JA6AHB 569 Japan
PH 10/10/2020 1826 K0PRT 54 W6YX 55 California, USA
And these are summaries of our contacts from the logging program:
K0PRT’s Contest Summary Report
Total Contacts = 30
Operating Period: 2020/10/10 07:50 – 2020/10/10 18:26
Total Contacts by State \ Province: AB 4, CA 2, TX 2, BC 1, FL 1, NC 1, NJ 1, WI 1. 8 total.
Total Contacts by Country: USA 8, Canada 5, Czech Republic 3, Federal Republic of Germany 3, Italy 2, Japan, 2, Austria 1, Denmark 1, England 1, Finland 1, Mexico 1, Poland 1, Sweden 1. Total countries 13.
Total Contacts by Continent: Europe 14, North America 14, Asia 2. Total continents 3.
-72/73 Gary WA2JQZ
Addendum: QSL confirmations we received:
Cool Science Festival Presentation on Saturday October 11, 2020
Rich Russel made an online presentation at the Cool Science Festival. The presentation covered the science of radio astronomy and the accomplishments of the Deep Space Exploration Society. The presentation was streamed live on Facebook and Youtube. You can watch the presentation here:
This 8-day regional event, designed to ignite wonder and inspire curiosity about the world around us, attracts between 10,000 and 20,000 attendees each year. For more information about the Cool Science Festival go to:
Text and photos by Gary Agranat.
A DSES team worked at the Plishner Radio Telescope site in Haswell on Sunday September 27, 2o2o. Team members were Ray Uberecken, Floyd Glick, and Gary Agranat. We accomplished the main objective, to install a new 1296 MHz feed at the focus of the 60 dish antenna. We also installed a mast in the ground, on which will later be added a Hughes Internet satellite antenna. Two friends of Ray’s came out and did an immense service by using metal detectors and magnetic rollers to clear nails and other metallic debris on the site. We changed out two of the locks. And we inspected the bunker.
Ray and I met at the Plishner site at 0930 in the morning.
We first installed a sturdy pipe mast behind the operations trailer, on which will be mounted a small satellite antenna to access the Hughes network geosynchronous satellite for Internet access. Ray chose a spot that will not be blocked by the trailer or the 60-foot antenna. We mixed cement and set the pole in its hole with the cement, using a level to check that the mast is vertical.
After that we manually rotated the 60-foot dish antenna to the service platform. I figured out, with Ray’s help and the checklists, how to use the software to monitor the antenna pointing. (Note: we might want to add a checklist just for this type of procedure, for using the software for just manual antenna pointing, as when we service the antenna.)
Floyd came out to the site by 1030. Ray and Floyd climbed the service platform. I worked on the ground to move feeds and tools up and down to them. We replaced the 408 MHz feed at the antenna focus with the newly built 1296 MHz feed. The 1296 MHz feed was built by KL6M, to specifications provided by Steve Plock (KL7IZW). The feed mount at the dish focus was designed by Ray, to enable the feed to more easily rotate out and be changed.
Conditions were somewhat windy, with a cold front coming, but still manageable. By the afternoon the winds had picked up enough that we postponed any further work at the feed. Work that still needs completion is installation of a 200 Watt amplifier at the feed. Since we are planning to operate at 1296 MHz from the Operations Trailer, which has a long coax hard line path to the pedestal and antenna feed, we expect significant power loss from the long path. We therefore need to boost the power again at the feed. We plan to install the amplifier the next weekend. We then also intend to test our setup by trying tropospheric scatter communications to the north.
We are planning to use this configuration to operate EME (Earth Moon Earth) Moon Bounce communications. And specifically we plan to participate in the ARRL EME contests on October 10-11, 2020 and on November 28-29, 2020 (UTC).
We discussed our plans for the upcoming contest in 2 weekends. The Moon then will be at last quarter phase. What that means is that it will rise on Friday night a little before midnight (about 1130 PM), and set Saturday a little after 2 PM. That means we will prepare to do overnight and morning operations. After the Moon rises we will try to pick up the ON0EME beacon in Belgium. We can try to contact across the Atlantic Ocean. The US East Coast will be in night time conditions, and so we anticipate less contacts to there. Daytime conditions, when more hams would be awake, are more favorable for the US West Coast, and across the Pacific Ocean to Oceana, Asia, and Australia.
Note that the 60-foot antenna will be configured with the 1296 MHz feed through the end of November. This will be an opportunity to try using it for other 1296 MHz communications, including troposphere scatter.
A friend of Ray’s who works at Planet Granite Ryan, and his brother, Rob, came out to the site also. They have ground metal detectors and magnets on rollers, and systematically paced across the site to pick up nails and other small metallic debris. They did pick up lots of nails, including along the roadway. They spent a few hours with us, and left after lunch. They did us a great service by helping remove a lot of this debris.
We attempted to open the combination locks at the gate, the bunker, and the generator shack. After still having difficulty, we replaced the locks at the gate and bunker, with the locks Myron Babcock obtained for us. These are similar model locks, and the combinations were kept the same.
We had a report that the bunker had been flooded by two successive rain storms in July. We opened and inspected the bunker. The bunker was dry, though the floor had more-than-normal dust and dirt, and some tiny debris was spread here and there. It will require a fresh cleanup before normal use. We saw no indication of mold from dampness.
Tumbleweeds were accumulated again at the ramp entrance.
We completed our activities by early afternoon, about 3 PM.
For the team, – Gary
Text and photos by Gary Agranat. Analysis pdf by Rich Russel.
On Saturday September 12, 2020 an observing team of Rich Russel, Bob Haggart, Bill Miller, and Gary Agranat spent the day observing pulsars. This is the first observing session since we recalibrated the 60-foot antenna azimuth pointing the weekend before. The team observed 3 pulsars we had not seen before. Plus several other pulsars were attempted. The team spent the whole day at the site, from about 9 AM to 7 PM.
The pulsar signals are so faint that we cannot detect them directly. To observe them, we have to point to the correct celestial coordinates and then track that point as the Earth rotates. While we are pointed, our computer accumulates the signal data. We need at least a half hour continuously tracking the position. At this session some of our observing runs lasted 2 hours, for the fainter objects. At previous sessions we have tracked for as long as 4 hours.
After the observing track, we have our software process the data. The random background noise should cancel itself out. But the pulse signals should build up with time. If we have the correct timing interval of the pulses, and if everything else is working, the computer display will show the pulses, and several other parameters.
Pulsars are very unusual objects. These are what remain of massive stars (greater than 5 solar masses) after they use up all their fuel for nuclear burning. These more massive stars fuse heavier and heavier elements at their cores until they start to fuse iron from silicon. Unlike the fusion of other elements, iron requires energy to fuse, rather than produce energy. The sudden reduction of energy at the core drops the temperature and pressure there. The pressure at the core is no longer enough to counter the weight of the star’s material above it. Gravity is now the stronger force, and the material above collapses in on the center. The pressure and temperature at the core then becomes even higher, which starts new reactions that fuse the matter at the center to neutrons, and and which also generates neutrinos. The outer layers falling in at great speed bounces back out. The result is a supernova explosion. What remains is the neutron star at the center. It is extremely massive and compact. And like an ice skater rotating faster as the arms are brought in, the star’s rotation speeds up immensely. The star’s magnetic field also has become compressed and much more intense. Charged particles will rotate around the magnetic field lines, with very high energy. Whenever charged particles are forced to deviate their paths from a straight line they emit electromagnetic energy, like visible light and radio. At the neutron star’s poles, this energy is channeled out, with immense energy. Because the magnetic poles are generally not at the same spots as the rotational poles, the beam of this light and radio is spun around like a light house. If Earth happens to be in the path of such a beam, we detect that as a pulsar. So that’s what we’re observing. These neutron stars are hundreds and thousands of light years away.
Pulsars were first discovered by accident in 1967, by Jocelyn Bell (now Jocelyn Bell Burnell) who was then a graduate student at Cambridge University. Bob contributed a recent photograph of her, posed by some radio telescopes. We now proudly have that displayed on the wall above our computer displays.
Because the observing runs take a while, for this session we decided to try watching some videos. Bob brought a DVD player and a large monitor. Gary brought some educational videos, including one about the Crab Nebula and pulsars. Rich brought some movies.
This is a summary of our observing results: http://dses.science/wp-content/uploads/2020/09/11-Pulsars-Observed-so-Far-9-12-20.pdf.
On this work trip the team also inspected damage to our ham radio antennas, damage probably from the storm weather over the past months. 7 radials at the base of the vertical antenna were damaged. And the 3 element Yagi antenna on tower was slightly tilted along its longitudinal boom.
Tumbleweeds also had accumulated again at the bunker ramp. Some of the surrounding fence had also been damaged from the weather. Rich Russel brought some fencing to use in the future, to place over the immediate entrance path to the bunker door.
Repair of the ham antennas and ramp clearing will be planned for a future work trip.
Below is a photo narrative of the day’s work.
It was an excellent day’s work.
Bob Haggart and Rich Russel did an observation all nighter on Friday/Saturday (September 19, 2020, GMT) and observed 2 pulsars.
VELA (B0833-45) is one of the strongest pulsars at 5 JY while B1946+35 is at 0.145 JY.
DSES is one of the most northern amateur stations to detect VELA. We detected it in 15 minutes at 5 to 6 degrees elevation.
This make 13 pulsars and puts us 5th on the international amateur pulsar hunter list. http://www.neutronstar.joataman.net/
The DSES team of Rich Russel, Ray Uberecken, and Glenn Davis observed for pulsars on Saturday September 5, 2020 at the DSES 60-foot dish antenna at Haswell, CO.
The team successfully observed 5 pulsars which we hadn’t been able to detect before.
The success is attributed to the calibration of the antenna pointing system and the new automatic tracking system developed by the System 1 team.
We started with calibrating the azimuth of the antenna (it was 2.5 degrees off!) Elevation was good. Glenn put the offset in the auto tracking system and we were able to detect the B0329+54 pulsar within 30 minutes. (We use the B0329+54 pulsar, the first one we successfully saw last May, as a starting reference. If we can observe this, we know our system is working.) Every pulsar we looked at after that was detected – we just ran out of time for more!
It is possible we missed observing previous pulsars because our pointing accuracy was off.
See the slide set for our observation summary.
We are pretty sure we observed the Crab pulsar. The last slide shows an analysis of the time between pulses we measured for the Crab pulsar, compared to the standard reference database.
More detail to come at the next science meeting
Our total pulsar count is now 8!
These are the slides from our online Science meeting, on August 24, 2020. The meeting was hosted by our DSES Science Lead, Rich Russel,
You can watch the video of our meeting: