25.4-cm Optical Receiver Performance
9301-005
Performance for the
10" (25.4 cm) Meade LX200 receiving telescope, and an ETI transmitter around a
solar-type star at 10 light years. |
|
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 |
-188 |
NA |
-29 |
-59 |
-89 |
-119 |
b |
1 MW |
1 MW |
NA |
NA |
NA |
NA |
2.3 X 1021 |
+15 |
-158 |
NA |
20 |
-10 |
-40 |
-80 |
c |
1 GW |
1 GW |
NA |
NA |
NA |
NA |
2.3 X 1024 |
+8 |
-128 |
NA |
51 |
21 |
-9 |
-39 |
d |
1 MW |
103 TW |
1 ns |
NA |
1 |
1 |
2.3 X 1030 |
NA |
-68 |
4.8 X 1002 |
IB |
IB |
IB |
24 |
e |
1 GW |
106 TW |
1 ns |
NA |
1 |
1 |
2.3 X 1033 |
NA |
-38 |
4.8 X 1005 |
IB |
IB |
IB |
54 |
f |
1 GW |
2 GW |
1 ns |
2 |
1 |
500 M |
4.6 X 1024 |
NA |
-125 |
9.5 X 10-4 |
IB |
IB |
IB |
-33 |
g |
1 GW |
8 GW |
1 ns |
8 |
3 |
380 M |
1.8 X 1025 |
NA |
-119 |
3.8 X 10-3 |
IB |
IB |
IB |
-27 |
h |
1 GW |
128 GW |
1 ns |
128 |
7 |
55 M |
2.9 X 1026 |
NA |
-107 |
6.1 X 10-2 |
IB |
IB |
IB |
-15 |
i |
1 GW |
1 TW |
1 ns |
1024 |
10 |
10 M |
2.3 X 1027 |
NA |
-98 |
4.9 X 10-1 |
IB |
IB |
IB |
-6 |
j |
1 GW |
8 TW |
1 ns |
8192 |
13 |
1.6 M |
1.9 X 1028 |
NA |
-89 |
3.9 X 1000 |
IB |
IB |
IB |
3 |
k |
1 MW |
52 GW |
1 ns |
524288 |
19 |
36 k |
1.2 X 1027 |
NA |
-101 |
2.5 X 10-1 |
IB |
IB |
IB |
-9 |
l |
1 GW |
524 TW |
1 ns |
524288 |
19 |
36 k |
1.2 X 1030 |
NA |
-71 |
2.5 X 1002 |
IB |
IB |
IB |
21 |
Wavelength = 656 nm
ETI Transmitting (Uplink) Telescope Diameter = 10.0 m
Earth Receiving Station (Downlink) Telescope Diameter = 25.4 cm
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 -144 dBW = 4.0 X 10-15
W = 1.3 X 104 photons/s = 1.3 X 10-5 photons/ns (6.6 X 10-4
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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