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Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ
îðèãèíàëüíîãî äîêóìåíòà
: http://www.atnf.csiro.au/whats_on/workshops/synthesis2003/talks/sensitivity/tant.html
Äàòà èçìåíåíèÿ: Tue Apr 12 03:22:45 2016 Äàòà èíäåêñèðîâàíèÿ: Tue Apr 12 03:22:45 2016 Êîäèðîâêà: Ïîèñêîâûå ñëîâà: ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï |
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Definition of the antenna temperature |
| | Let us assume now that our telescope observes over a limited frequency range, |
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| | Similarly, the power of an astronomical source can be expressed as |
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| | where |
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, (the so-called "passband") with constant response over that range. When pointing at a blank portion of the sky, there are only contributions from what one would call "background" or "noise". The power of this component can be expressed as 
is the so-called "antenna temperature", which is a measure of the temperature equivalent of the power received from an astronomical source.