Performance for a 10-meter aperture receiving telescope, and an ETI transmitter around a solar-type star at 10 light years. |
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Mean Power |
Peak Power | Pulse Duration | M-ary PPM | Bits Per Pulse | Data Rate bps | Peak EIRP W | Mag | Peak Signal dBW | Photons Per Pulse | Post-Detection SNR, dB | ||||
| 1 Hz | 1 kHz | 1 MHz | 1 GHz | |||||||||||
| a | 1 kW | 1 kW | NA | NA | NA | NA | 2.3 X 1018 | +23 | -157 | NA | -22 | -8 | -38 | -68 |
| b | 1 MW | 1 MW | NA | NA | NA | NA | 2.3 X 1021 | +15 | -126 | NA | 53 | 23 | -8 | -38 |
| c | 1 GW | 1 GW | NA | NA | NA | NA | 2.3 X 1024 | +8 | -96 | NA | 83 | 53 | 23 | -7 |
| d | 1 MW | 103 TW | 1 ns | NA | 1 | 1 | 2.3 X 1030 | NA | -36 | 7.4 X 105 | IB | IB | IB | 56 |
| e | 1 GW | 106 TW | 1 ns | NA | 1 | 1 | 2.3 X 1033 | NA | -6 | 7.4 X 108 | IB | IB | IB | 86 |
| f | 1 GW | 2 GW | 1 ns | 2 | 1 | 500 M | 4.6 X 1024 | NA | -93 | 1.5 X 100 | IB | IB | IB | -1 |
| g | 1 GW | 8 GW | 1 ns | 8 | 3 | 380 M | 1.8 X 1025 | NA | -87 | 5.9 X 100 | IB | IB | IB | 5 |
| h | 1 GW | 128 GW | 1 ns | 128 | 7 | 55 M | 2.9 X 1026 | NA | -75 | 9.5 X 101 | IB | IB | IB | 17 |
| i | 1 GW | 1 TW | 1 ns | 1024 | 10 | 10 M | 2.3 X 1027 | NA | -66 | 7.6 X 102 | IB | IB | IB | 26 |
| j | 1 GW | 8 TW | 1 ns | 8192 | 13 | 1.6 M | 1.9 X 1028 | NA | -57 | 6.1 X 103 | IB | IB | IB | 35 |
| k | 1 MW | 52 GW | 1 ns | 524288 | 19 | 36 k | 1.2 X 1027 | NA | -69 | 3.9 X 102 | IB | IB | IB | 23 |
| l | 1 GW | 520 TW | 1 ns | 524288 | 19 | 36 k | 1.2 X 1030 | NA | -39 | 3.9 X 105 | IB | IB | IB | 53 |
Wavelength = 656 nm
ETI Transmitting (Uplink) Telescope Diameter = 10.0 m
Earth Receiving Station (Downlink) Telescope Diameter = 10.0 m
Atmospheric Transmission = 0.40
Telescope Efficiency = 0.70
Monochromator Efficiency = 0.50
Quantum Efficiency = 0.50
NEP For Incoherent Receiver 10-4 pW/Hz
Dark Current < 3.2 X 10-6 pA (< 20 cps or 2 X 10-8 counts/ns).
Fraunhofer Suppression = 0 dB
CW Optical Bandwidth = 100 GHz (0.14 nm), Pulse Optical Bandwidth >> 100 GHz.
Unpolarized Detected Stellar Background -112 dBW = 6.3 X 10-12 W = 2.1 X 107 photons/s = 2.1 X 10-2 photons/ns (1.0 X 10-2 counts/ns).
Solar EIRP = 3.9 X 1026 W.
Shaded areas denote undetectable signals, i.e., negative SNRs or insufficient bandwidth (IB).
Results assume that star and transmitter are not separately resolved.
For the digital modulation systems, the pulse SNR for Poisson counting is the photon detection rate per pulse.
For pulsed SNRs > 20 dB, the Bit Error Rate (BER) < 10-8.
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