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<p align="justify">Digital astronomical data acquisition system is a system to retrieve, collect and prepare data and process it to get the desired digital astronomical data. In obtaining digital astronomical data, an optimization of the entire acquisition system is needed. One of th...
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| Format: | Final Project |
| Language: | Indonesia |
| Online Access: | https://digilib.itb.ac.id/gdl/view/31202 |
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| Institution: | Institut Teknologi Bandung |
| Language: | Indonesia |
| Summary: | <p align="justify">Digital astronomical data acquisition system is a system to retrieve, collect and prepare data and process it to get the desired digital astronomical data. In obtaining digital astronomical data, an optimization of the entire acquisition system is needed. One of them is in the process of astronomical observation involving instruments in the form of collectors, analyzers, and detectors. Characterization is carried out to determine the performance of the instruments used to support the achievement of optimal digital astronomical data. Characterization by the in situ test method developed by Abbott (1995) produces physical parameters derived in the form of magnitudes: (1) gain of 0.514, (2) readout noise of 20.896 e- / pixels, (3) full well capacity of 33659,253 e-, (4) the shutter error is 0.01 seconds, (5) dark current is 0.047 e- / s / pixel, and (6) the charge transfer efficiency is 0.995. Astronomical tests on astronomical imaging systems empirically model signals to existing disturbances (signal to noise ratio or SNR) resulting in a trend along with increasing B-V values, SNR values for filter B decrease, while for R and I filters increase. The Detective Quantum Efficiency curve constructed shows that the ideal value of 0.5 can be achieved at a visual magnitude of about 13.<p align="justify"> |
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