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Figure 4 for example shows a result obtained in a narrowband SETI search near
the PiHI frequency (the number π times the HI observing line of 1420.4 MHz). This (extremely
powerful) ~10 second pulse of narrowband radiation appeared in one 50 second observation
period but was never re-observed. This pulse has interesting features: It is observed at a magic
frequency in the direction of a nearby and potentially habitable star. Yet we cannot be sure this
signal was created intentionally or unintentionally by some transmitter on Earth. Hence after
multiple observations over 2 weeks and no re-detection, we gave up (although this direction is
added to a catalogue of directions to re-observe as time permits).
Figure 4: A pulse with maximum power >300σ above the noise background was observed on a nearby
star (~100 LY, (J2000 RA, Dec) = (32.211809⁰, 22.441734⁰)) in the HabCat Catalog (Turnbull, 2003).
This pulse is interesting since it appears to arrive from the direction of a potentially habitable star and
because it appears very close (within the expected Doppler shift tolerance caused by relative motion)
to the “magic” PiHI frequency of 4462.3 MHz, this signal appeared in only one observation and never
thereafter. Given the proximity of this source, we do not expect substantial fading in the ISM; hence the
signal is really not present, most of the time.
JadeStar
My theory is that if this signal was in fact from a transmitter 100 light years away, that transmitter was not being used as a beacon for us but rather was being used in a similar way as we use the Arecibo planetary radar, which by the way, can also be detected 100 light years away.
We use Arecibo and other such radars take pictures of near Earth asteroids.
When we do this we are not intending to signal anyone and the transmissions are typically a one time affair as different asteroids have different trajectories so we aren't repeating these transmissions to the same areas of sky.
LABTECH767
reply to post by JadeStar
You never fail to impress, this is a terrific thread you have started, Do you by any chance remember the other signal from the 1970's when the noise was regared as nothing but random static but an absent minced intern sat there with his pen Joining the dot's litterally on the binary print out and ended up with an image of a stick man with a triangular head and in and three fingered hands standing in front of what looked like a radio satellite dish, it was one of those which used to be fairly well known but I can find nothing on it on the net.
Anyway The real difficulty is attenuation as you know and even a hundred arecibo sized dishes would be luck to pick anything more than a few light years away.
Performs range analysis of an electromagnetic communications system, assuming identical antennas at both ends. The example shows that the range over which a 1 MW hydrogen-line signal can be detected with existing receivers, assuming 100 meter dishes at both ends of the path, is on the order of 9 parsecs (28 LY). This spreadsheet may be used for range comparison of various systems.
Determines the sensitivity (in Janskys for continuum measurements, and Watts per square meter for narrow-band signal detection) of any radio telescope, given its pertinent receiver and antenna parameters. Also shows the flux density of any received signal as a function of observed Signal-to-Noise Ratio (SNR). The sample calculations seen in this spreadsheet show the sensitivity of the Ohio State University "Big Ear" radio telescope at the time the "Wow!" signal was detected. See this article for an example of sensitivity analysis.
Determines the Signal-to-Noise Ratio (SNR) for any communications system, given the operating characteristics of the transmitter, receiver, and the intervening free-space propagation path. The sample spreadsheet calculations show that the typical Project Argus station could easily receive a 1 MW hydrogen-line signal into a 100 meter dish, at a range of 1 parsec (3.26 LY), with just 10 seconds of integration. These normalized values may be used for comparison of various systems. See this article for more examples of link analysis.
lostbook
reply to post by JadeStar
Excellent thread, Jade...! Have there been any other signals besides the WOW signal and this one? I seem to remember that there were other signals.
DupontDeux
reply to post by JadeStar
How very well written - thank you!
I would love to hear more about the "thousands of interesting eading" captured each day. Do you know anything about what constitutes "interesting" and what makes them not-mentionable?
Ross 54
I've heard of the incident, but not the details. Somehow this leaked out to the news media, though they don't seem to have made too much of it. Apparently only after this did the SETI Instituter make a brief statement about it
The usual statement about one-off detections like this is that they are inconclusive. A 24/7 observation program would be a good idea, of course, it if could be managed.
How large would a single dish antenna need to be to detect a 300 sigma signal like this, with an appropriate integration time to detect 10 second pulses?
Thus, any radiotelescope with an overall sensitivity of -204 dBm would, in theory, be able to detect a "Wow!" type signal, if tuned to the right frequency, and pointed in the right direction, at the right time.
There is another way, and it has been described above. Consider that at the 21 cm neutral hydrogen line, a three- to five-meter diameter parabolic antenna (such as is commonly used for satellite TV reception) will have a power gain perhaps 200 times less than that of a "real" radio telescope such as Big Ear. The reduced capture area would also imply that such an antenna would enjoy 200 times the sky coverage, so a mere 5,000 such antennas could, if properly situated, "see" the whole sky at once. And such a global array of small telescopes could be constructed at a cost far less than that of a single Big Ear.
Unfortunately, this increase in angular coverage afforded by smaller antennas was accomplished by a reduction in their capture area, hence gain. Thus, as compared to our Big Ear example, these smaller antennas will experience a reduction in their effective communications range by that same factor of 200, all else being equal. A signal which could be detected by Big Ear at a range of, say, 20,000 LY, would be detectable to our smaller antennas at a distance of only 100 LY. Since for uniform distribution of candidate stars, the number of targets varies roughly with the cube of distance, this sacrifice in sensitivity significantly reduces (perhaps by a factor of several million) the number of suitable stars which might be within range of our sky survey.
I looked for, but didn't find any radial velocity measurements for this star. If we had this figure we could confirm that the signal really was accurately placed on the Pi*HI frequency, by correcting for the doppler shift. Since the reception frequency was around 1.5 MHz higher than the pi*HI frequency, the star would need to be moving toward us for this to work out.
LABTECH767
reply to post by JadeStar
www.nsa.gov...
galacticconnection.com...
While lecturing at an IEEE Conference on Military Electronics held in Washington, D.C. on 23 September 1965, Dr. Lambros Callimahos, a famous NSA cryptology expert who had authored a number of innovative studies on deciphering coded messages around the same time, seems to have made references to the very same series of “ET” communications as follows:
“As an illustration of how much information could be conveyed with a minimum of material, and as an example of facile inverse cryptography, let us consider a message I have devised to be typical of what we might expect of an initial communication from outer space.”
Indeed, it seems obvious here that Callimahos not only knew of a series of alleged “ET messages,” but admits to having designed them himself as an exercise! Furthermore, looking back at the roundup of articles released at the NSA’s website, among them one will also find the appropriately titled, “Communication With Extraterrestrial Intelligence” by none other than Lambros D. Callimahos.
While it seems obvious to us, looking at the series of documents in this order, what the intentions and goals of the two men were, we are left with a number of websites that do make the assertion that Campaigne’s lone documents were, in fact, addressing actual signals collected from outer space.
solargeddon
I may have missed it in the plethora of this wonderful thread....why has is this the first time we have heard of this second WOW?
I'm surprised it hasn't been media hyped, it does seem as though these days there is some push to desensitise us to all things alien.
Apologies if you have already covered this.
I looked for, but didn't find any radial velocity measurements for this star. If we had this figure we could confirm that the signal really was accurately placed on the Pi*HI frequency, by correcting for the doppler shift. Since the reception frequency was around 1.5 MHz higher than the pi*HI frequency, the star would need to be moving toward us for this to work out.