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High power, low-noise, and multiply resonant photodetector for interferometric gravitational wave detectors
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10.1063/1.2735559
/content/aip/journal/rsi/78/5/10.1063/1.2735559
http://aip.metastore.ingenta.com/content/aip/journal/rsi/78/5/10.1063/1.2735559
View: Figures

Figures

Image of FIG. 1.
FIG. 1.

Principle layout of a photodiode circuit. Unit C1 serves as a current-to-voltage converter. A1 is a voltage amplifier.

Image of FIG. 2.
FIG. 2.

(Color online) The main noise sources as functions of the conversion factor , converting photocurrent to voltage.

Image of FIG. 3.
FIG. 3.

The GEO600 dark-port photodetector design used until the end of 2005. The european symbol for coils is used as shown in the legend.

Image of FIG. 4.
FIG. 4.

LIGO photodetector design.

Image of FIG. 5.
FIG. 5.

VIRGO photodetector design.

Image of FIG. 6.
FIG. 6.

GEO600 new photodetector design. The resonant circuits L1/C1 and L2/C2 and the signal extraction around them are just two examples. If the sequence of L and C is altered, the shape of the response changes at frequencies different from the resonant frequency. A transformer (as L2/L2a) can be used to provide an optimized signal size.

Image of FIG. 7.
FIG. 7.

(Color online) Measurement of signal sizes at three radio frequencies, for the old and new GEO600 photodetector designs. The signal sizes are measured as a function of the laser power.

Image of FIG. 8.
FIG. 8.

Measurement of transfer functions from a photodiode test input to different points of the new photodetector circuit.

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/content/aip/journal/rsi/78/5/10.1063/1.2735559
2007-05-08
2014-04-17
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752b84549af89a08dbdd7fdb8b9568b5 journal.articlezxybnytfddd
Scitation: High power, low-noise, and multiply resonant photodetector for interferometric gravitational wave detectors
http://aip.metastore.ingenta.com/content/aip/journal/rsi/78/5/10.1063/1.2735559
10.1063/1.2735559
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