MLABlibrarysvnkaklikMLAB_E8magsvn

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/dokumenty/skolni/diplomka/diplomka.pdf
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/dokumenty/skolni/diplomka/diplomka.tex
61,7 → 61,7
\keywordsCZ { Radioastronomie, digitalizace signálu, A/D konverze
}
\thanks { % Use main language here
\thanks { Chtěl bych poděkovat Ing. Martinu Matouškovi, Ph.D. a Ing. Ondřeji Sychrovskému za věcné připomínky. Dále pak Fluktuacii a prof. Ing. Václavu Hlaváčovi, CSc. za jazykové korekce.
}
\declaration { % Use main language here

/dokumenty/skolni/diplomka/introduction.tex
36,10 → 36,10
Sensitivity and noise number are parameters that are tied together. However, the requirement for multi-antenna and multi-receiver arrays forces to keep the price of receiver at the minimal value. This implies that the sensitivity and noise number have to be at least so good in the detection (signal $/$ noise $>$ 1 ) of an observed object, that it would be detected on the majority of receivers connected to an observation network.
\secc Dynamic range
\label[dynamic-range-theory] \secc Dynamic range
\label[dynamic-range-theory]
The dynamic range represents a huge problem of current radioastronomical receivers. This parameter is enforced by humans present everywhere and creating electromagnetic inference (EMI\glos{EMI}{Electromagnetic interference}) radiation on radio frequency (RF\glos{RF}{Radio frequency}) band. The modern radioastronomy receiver must not be saturated by these high levels of signals but still needs to have enough sensitivity to see faint signals from natural sources. The dynamic range is limited either by the construction of the analog circuitry in the receiver or by the digitization unit.
The maximal theoretical dynamic range of analog-to-digital converter (ADC \glos{ADC}{analog-to-digital converter}) could be estimated from ADC bit depth using a following formula~\ref[dynamic-range]