I've not done the calculation, but I wonder how the practical limits of concentrating a singnal compare to the number of arc seconds a star travels in several years.
Diffraction makes it spread out, and is related to aperture. I don't know if diffraction affects signal quality.
Would using the frequency of hydrogen mean there is a lot of background hydrogen noise? I read that microwaves at 1-10mhz is best.
The problem is that even the largest steerable radio telescope is only about 100 meters diameter. 1.42 GHz is about 21cm (actually nicknamed 21cm line by radioastronomers), so in terms of wavelength, the dish is less than 500 wavelengths -- the half power beamwidth is about 12 arc minutes. "Diffraction" (wave nature) causes sidelobes that are identical to what we see in Airy rings. Not a huge problem for transmitting power loss, but a bigger problem for receiving, since the sidelobes at the feed antenna picks up noise from the warm ground (compared to the detectors, which are cooled to near absolute 0 K), but you can control that by designing a feed antenna that does not illuminate the ground, at a small loss to aperture.
Although the sky coverage is more limited, the Arecibo (Puerto Rico) antenna was much larger, but that radiotelescope is no more -- in spite of that, lots of SETI search was done at Arecibo, both by piggy backing on other experiments, or alone. The first SETI attempt was done by Frank Drake (Project Ozma) with just a 26m dish :-).
The usual reason for picking the microwave region near 1.4 GHz is that for earthbound telescopes, it has the best SNR. The "romantic" reason, attributed to Barney Oliver, is that it is at the "water hole" region -- Hydrogen spin flip radiation is at 1420.404 MHz, and there are four lines that are associated with Hydroxyl radical (OH) around 1667 MHz -- ergo H2O :-).
https://www.seti.net...e/waterhole.php for example, shows the water hole inside the best SNR region between 1000 MHz and 10000 MHz.
And other rationales include that is a natural place to transmit if the transmitter and the receiver are trying to meet up blindy. But I have also read of searches at 2x Hydrogen spin flip, to avoid the background noise from H. I heard of suggestions at pi times Hydrogen, but I am not sure anyone actually did it :-).
I think the 1.420 GHz Hydrogen spin flip was either predicted or discovered during or just after WWII. It was not until the early 1960s that the Hydroxyl radical lines were observed by Sandy Weinreb, using the autocorrelation receiver that he created for his Ph.D thesis. (Sandy was my supervisor when I was a summer intern during my Junior and Senior years at Green Bank in the late 1960s :-).
Chen
Edited by w7ay, 28 March 2025 - 02:33 AM.