lpetrich
Contributor
Eavesdropping Mode and Radio Leakage from Earth - WOODRUFF T. SULLIVAN III
Television channel frequencies
TV broadcasts are separated in frequency by 6 Mhz, meaning that that is the upper limit of their bandwith. However, their carrier signals have bandwidths of around 0.1 Hz, some 60 million times less. Since the interstellar background has an intensity proportional to the bandwidth, as is typical of "noisy" signals, that means that it's MUCH easier to detect carrier signals than TV signals in general. One needs to look at lots of *very* narrow frequency bands, and that's typically done in SETI efforts.
So WTS worked out what one would find if one only looked at the carrier signals.
Television channel frequencies - VHF: 41 to 224 MHz - UHF: 471 to 951 MHz - it varies from place to place, so I was trying to be inclusive. For instance, the US has 54 to 82 MHz (channels 2 to 6), 174 - 210 MHz (channels 7 to 13), 470 - 884 MHz (channels 14 - 83).
That means that TV carrier waves can be observed with a frequency resolution of 10-9 and in velocity terms, that is 30 cm/s, 1 foot per second. But for that high resolution, one needs to integrate over at least 10 seconds.
WTS then noted that TV broadcasts tend to be concentrated at around a few degrees around horizontal, so as not to waste transmission energy broadcasting in directions where there are no receivers. That means that as each TV station will be most visible around when it rises and sets. At station dawn, its signal jumps to its maximum, then more slowly declines to near zero. Then at station dusk, the signal rises to its maximum, then declines to zero.
From station rise and set times, one can find the location on the Earth of each one, and one will soon discover that many stations are clustered, with nearly the same location.
The Doppler shift over the year should be readily observable, 30 km/s or 10-4 when edge-on. The observers should find it easy to observe the Sun, and they can work out that it's a 4.5-billion-year-old main sequence star with a certain mass. With that mass value, they can then find out how far away the Earth is from the Sun, and from that, how much sunlight it received. Enough to make water liquid.
Television channel frequencies
TV broadcasts are separated in frequency by 6 Mhz, meaning that that is the upper limit of their bandwith. However, their carrier signals have bandwidths of around 0.1 Hz, some 60 million times less. Since the interstellar background has an intensity proportional to the bandwidth, as is typical of "noisy" signals, that means that it's MUCH easier to detect carrier signals than TV signals in general. One needs to look at lots of *very* narrow frequency bands, and that's typically done in SETI efforts.
So WTS worked out what one would find if one only looked at the carrier signals.
Television channel frequencies - VHF: 41 to 224 MHz - UHF: 471 to 951 MHz - it varies from place to place, so I was trying to be inclusive. For instance, the US has 54 to 82 MHz (channels 2 to 6), 174 - 210 MHz (channels 7 to 13), 470 - 884 MHz (channels 14 - 83).
That means that TV carrier waves can be observed with a frequency resolution of 10-9 and in velocity terms, that is 30 cm/s, 1 foot per second. But for that high resolution, one needs to integrate over at least 10 seconds.
WTS then noted that TV broadcasts tend to be concentrated at around a few degrees around horizontal, so as not to waste transmission energy broadcasting in directions where there are no receivers. That means that as each TV station will be most visible around when it rises and sets. At station dawn, its signal jumps to its maximum, then more slowly declines to near zero. Then at station dusk, the signal rises to its maximum, then declines to zero.
From station rise and set times, one can find the location on the Earth of each one, and one will soon discover that many stations are clustered, with nearly the same location.
The Doppler shift over the year should be readily observable, 30 km/s or 10-4 when edge-on. The observers should find it easy to observe the Sun, and they can work out that it's a 4.5-billion-year-old main sequence star with a certain mass. With that mass value, they can then find out how far away the Earth is from the Sun, and from that, how much sunlight it received. Enough to make water liquid.