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Post by sage on Jan 20, 2024 1:02:05 GMT
I got the tables done, but have to see how bandwidth would affect the system, as those with the lowest bandwidth have the lowest noise. And I have to figure out how I would do some other problems that I found on the way. I should be able to post the tables soon after I solve these new problems.
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Post by sage on Jan 24, 2024 0:29:37 GMT
Table of Noise Equivalent Powerin watts MIR Detector Switchable Gain Wavelength range | Sensor | dB 0 | dB 5 | dB 10 | dB 15 | dB 20 | dB 25 | dB 30 | dB 35
| dB 40 | dB 50 | dB 60 | dB 70 | 900-2570 nm | PDA10DT |
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| 2.11E-9 | 1000-5800 nm | PDA10PT |
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| 1.885E-7 |
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| 600-16000nm | PDA13L2 | 3.248E-6 | 3.388E-6 | 3.138E-6
| 3.178E-6
| 3.208E-6
| 2.829E-6
| 2.639E-6
| 2.259E-6
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NIR Detector Switchable Gain Wavelength range | Sensor | dB 0 | dB 5 | dB 10 | dB 15 | dB 20 | dB 25 | dB 30 | dB 35 | dB 40 | dB 50 | dB 60 | dB 70
| 800-1700nm | PDA20CS2 | 2.023E-7 |
| 6.981E-9 |
| 2.93E-9 |
| 1.117E-9 |
| 5.85E-10 | 3.748E-10 | 2.135E-10 | 1.249E-10 | 900-1700nm | PDA10CS2
| 1.659E-7 |
| 4.824E-9 |
| 2.255E-9 |
| 1.068E-9 |
| 5.73E-10 | 3.631E-10 | 2.182E-10 | 1.227E-10 | 320-110nm | PDA100A2 | 2.378E-7 |
| 7.987E-9 |
| 3.005E-9 |
| 1.443E-9 |
| 8.01E-10 | 7.028E-10 | 5.92E-10 | 4.316E-10 | 350-1100nm | PDA36A2 | 2.622E-7 |
| 7.336E-9 |
| 3.4E-9 |
| 1.734E-9 |
| 9.75E-10 | 6.175E-10 | 3.795E-10 | 2.35E-10 |
MIR Detector with Fixed gains Wavelength range | Sensor | Noise Equivalent Power | 900-2600nm | PDA10D2 | 5.05E-8 | 2700-5300nm | PDA07P2 | 3.00E-7 | 2000-8000nm | PDAVJ8 | 1.70E-6 | 2000-10600nm | PDAVJ10 | 2.10E-6 | 2700-5000nm | PDAVJ5 | 1.40E-8 |
NIR Detector with Fixed gains Wavelength range | Sensor | Noise Equivalent Power | 800-1700nm | PDA015C2 | 3.899E-7 | 800-1700nm | PDA05CF2 | 1.543E-7 | 800-1700nm | PDF10C2 | 3.354E-14 | 800-1700nm | PDA20C2 | 4.919E-8 | 200-1100nm | PDA10A2 | 3.576E-7 | 320-1000nm | PDA8A2 | 5.515E-8 | 320-1100nm | PDF10A2 | 1.34E-14 | 400-1000nm | PDA015A2 | 7.018E-7
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Post by sage on Jan 31, 2024 23:25:49 GMT
Ok, right now I'm looking into Dichroic Mirrors and calibrated Thermal position sensor as they give position of the target.
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Post by sage on Feb 12, 2024 23:19:13 GMT
Space Infrared Interferometric Telescope (Spirit) used as Bolometer base line for main detection sensor. Band | 25-50 um | Detector NEP | 1.9E-19 W/sqrt(Hz) |
Superconducting Quantum Interference Device (Squid) used as base line for Hz Form this info we can get the Bandwidth factor and NEP Temp | Bandwidth factor | 293 k | 0.141026132 | 500 k | 0.041713463 | 1000 k | 0.006732099 | 1500 k | 0.002164611 | 2000 k | 0.000950628 | 2500 k | 0.00049851 | 3000 k | 0.000293096 |
Signal-to-noise ratio for an automatic system | 40:1 |
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Post by sage on Mar 11, 2024 20:53:19 GMT
Ok for some time now I have been learning the difference between interferometer and Grating Spectrometer. The problem is the diffraction limit, turns far away objects into a dot. The only way to get any information form a dot, is to find characteristics of the dots light. From this you can tell some important piece of information.
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Post by sage on Apr 24, 2024 17:54:48 GMT
Ok for some time, I have been talking with optical experts in the field. Double checking my work, and check out all the sensor types. I will do a final new post with all the updated, and finished work when I'm done talking to them.
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Post by sage on May 1, 2024 21:02:44 GMT
The last part I need is how to use a Stellar Parallax or just a Parallax to find the distance to the target.
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