This autumn Dr. Richard Russel attended the Very Large Array (VLA) Imaging course in Socorro, New Mexico. The course taught how to take the data sets from multiple large interferometer antenna systems and produce images and science statistics.. This post presents the slides from the DSES Science Meeting on November 25, 2019. This is an update from Dr. Russel’s posts on the topic from October 19 and 31.
Dr. Russel also presents his September 2019 results of Hydrogen 21 cm (HI) drift scan measurements at his newly installed 9-foot dish antenna at his home in Colorado Springs.
Please click the link to view the illustrated pdf file:
Recently Dr. Richard Russel attended the Very Large Array (VLA) Imaging course in Socorro, New Mexico. The course taught how to take the data sets from multiple large interferometer antenna systems and produce images and science statistics.. This post is an update from Dr. Russel’s post on this topic on October 19.
In this post, Dr. Russel also presents initial results of Hydrogen 21 cm (HI) drift scan measurements at his newly installed 9-foot dish antenna at his home in Colorado Springs.
Please click the link to view the illustrated post:
Recently Dr. Richard Russel attended the Very Large Array (VLA) Imaging course in Socorro, New Mexico. This course taught how to take the data sets from the VLA archive and produce images. The following is the first set of images reduced from the VLA archive by Dr. Russel.
Images were made of these astronomical objects:
3C75 Binary Black Hole System
3C391 Supernova Remnant
Asymptotic Giant Branch (AGB) Star IRC+10216
MG0414+0534 Gravitational Lens HI Absorption Line
Each image takes about 1 day to produce from the raw observation.
The DSES 9-foot dish is operational at Dr. Russel’s house in Colorado Springs. It is outfitted with a 1420 MHz feed with 2 low-noise amplifiers with over 40 dBi of gain and a noise figure of 0.35. The receiving system is a Spectracyber 1.
The output of the Spectracyber shows the relative peaks of hydrogen with a corresponding Doppler measurement.
Dr. Russel performed a drift scan of the visible sky and plotted the relative peak hydrogen signals.
The hydrogen maps very well
to the visible Milky Way. The plot below converts the Celestial Coordinates
into Galactic Coordinates. Note that the peak hydrogen is concentrated near the
0 Galactic Latitude.
Thanks to Ray Uberecken and Steve Plock for helping to set up the system.
Ray Uberecken came over today with another LNA, which we put in series with the first LNA. This did the trick and overcame our cable loss problem. I conducted a small drift scan across the galactic center at -32 Declination. Here is a quick result.
I will spend the next couple of days fine tuning the azimuth pointing and weatherizing the LNAs.
I will forward information to allow certain members teamviewer access if they want.
Thanks Ray and Steve Plock for their technical support!!
Part 2 – September 4, 2019
The 9 ft dish at Dr. Russel’s house is operational! It is set up to collect neutral hydrogen frequencies at 1420.406MHz. Today the dish azimuth was aligned using the Sun and a level.
The receiver is a Spectracyber 1 from Radio Astronomy Supplies. Below is the measurement of the hydrogen spectrum near the galactic center. RA 17hr 58min DEC -32 degrees
Training on the use of the system will be conducted at the science meetings.
This is Skip Crilly‘s updated paper/presentation, “Radio Search for Extraterrestrial Intelligence SETI is fun ! Geographically-spaced Synchronized Signal Detection System“, updated July 2019. Skip presented it at the Society of Amateur Radio Astronomers conference at Greenbank, WV on August 4, 2019. The link will open as a pdf file.
During the past year, Dr. Russel led us in measuring the Doppler shifts of galactic neutral hydrogen (HI). Building on his experience from navigation, he then developed his ideas on how to use HI Doppler shift measurements to navigate from star to star across galactic space.
This year we are undertaking measuring the pulse time of pulsars. Pulsars are understood to be the star remnants of supernova explosions. They become what are called neutron stars. The supernovas compress the stars tightly into enormous densities so that their matter become neutrons, and the stars are only about 7 miles in diameter. Due to the conservation of angular momentum, their spin increases very rapidly. The youngest rotate with periods of miliseconds. Their magnetic poles are often offset from their spin axes. Electrons spin rapidly along the outgoing magnetic field lines of the poles, producing synchrotron radiation, which in turn produce broad band radio signals. If a magnetic pole is oriented so that it points at Earth during the rotation, we receive a radio pulse, and maybe pulses at other wavelengths too. (That is how pulsars were first discovered during the late 1960s.)
The pulses are very regular. But the spin of the pulsars gradually lose energy and slow down over time too.
Dr. Russel took his ideas for navigation, and now he has developed a concept for doing interstellar navigation using pulsars as references. That’s what this slide set is about. He just submitted a paper on the topic to the journal of the Society of Amateur Radio Astronomers.
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.