InGaAs Array - HORIBA Jobin Yvon - #2

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alists in Spectroscopy
Optical Spectroscopy Division
IGA-3000Array Detectors
IGA-3000 Detectors: Highest NIR Sensitivity with Ultra Low Noise
Wavelength Range (***)
800 - 1700 nm
Pixel formats
256x1 or 512x1
512x1
Pixel size
50x500 urn
25x500 um
Optical Fill Factor:
100%
Cooling options:
2-stage TE or LN2 (*)
Full well capacity (**)
130,000,000 e- (Typ) (HiD mode) 5,000,000 e- (Typ) (HiS mode)
Gain (Typ):
75 e-/count (HiS mode) 2000 e-/count (HiD mode)
Fixed Pattern Noise
250 e-/sec (Typ) Ln2 - 500 e-/sec (max) 900 e-/sec (Typ) HiS TE - 1000 e-/sec (max) 7500 e-/sec (Typ) HiD TE - 10,000 e-/sec (max)
Read noise
HiS mode
650 e-rms (Typ) LN2 1000 e-rms (Typ) TE
800 e- rms (Typ) LN2
HiD mode
6000 e- rms (Typ) LN2 10,000 e-rms (Typ) TE
10,000 e- rms (Typ) LN2
Controller
16 bits
Response non-linearity
% (Typ)
Response non-uniformity
+/- 5 % of mean (Typ), +/- 10 % of mean (max)
Pixel defects
Maximum of 2 black or hot spots for 256 pixel array Maximum of 5 black or hot spots for 512 pixel array
Jobin Yvon Noise expertise:
The InGaAs arrays used in spectroscopy are constructed from individual photodiodes arranged in a linear array with a silicon CMOS readout multiplexer circuit. In high precision low-light level spectroscopic applications it is important to understand the various noise sources which contribute to a measurement with an InGaAs array and thus affect the signal-to-noise ratio. Each individual InGaAs photodiode pixel in an array is connected to its own capacitive transimpedance preamplifier circuit. As a result, the bias voltages are often slightly different from pixel to pixel. These minute differences in the output of each element lead to a predictable and repeatable noise signal known as fixed pattern response. This source is a strong function of both the integration time and the array operating temperature, and can be reduced by thermoelectric or liquid nitrogen cooling. Fortunately, the fixed pattern response is highly repeatable and can be almost eliminated by subtracting a dark acquisition of the same integration time as the illuminated spectrum of interest. In order to accomplish the dark acquisition it is mandatory to block the signal to the detector using a mechanical shutter. Some InGaAs arrays have an electronic sink circuit that dumps the photocurrent and essentially flushes the detectors in an analogous manner to a CCD detector. This so-called "electronic shutter" does not permit a dark acquisition to be made but it does allow the user to set a fast integration time. Other sources of noise in an InGaAs array which contribute to the measurement include read noise, which is electronic noise
InGaAs linear array Specifications
Typical specifications based on manufacturer Information. Subject to change without notice.
(*) Adjustable temperature control (**) Dynamic Range = Full well capacity/Read noise
that occurs when the elements are read out, and dark signal, which is the un-illuminated response of the detector. The total noise contribution to the measurement contains contributions from all sources of dark, readout, fixed-pattern and shot noise. The shot noise is the intrinsic noise distribution in the photon signal and is equal to the square root of the total signal. A clear understanding of the noise process, the technical specifications of the detector and how these measurements are defined play a critical important role when comparing array detector performance.
Typical spectral response of Spectrum One InGaAs detectors at 25°C.
(***) Long wavelength cut-off is dependant on cooling temperature (Xmax = XRT - 1nm per degree).
l-877-JYHoriba
China: 86-10-68313388 Germany: 89/46.23.17-0 Italy: 2/57.60.30.50 Japan: (81)3-5823-0140 U.K.: 020-8204-8142
In the USA:
Jobin Yvon Inc
3880 Park Ave,
Edison, New Jersey,
08820 USA
Tel: (732)-494-8660
Fax: (732)-549-9309
Email: OSD@jyhoriba.com
In France:
Jobin Yvon SA 16-18 rue du Canal 91165 Longjumeau cedex France
Tel: (33) (0) 1 64.54.13.00 Fax: (33) (0) 1 69.09.93.19
P/N : OSD-0007 REV.B
HORIBA GROUP
wwwjyhoriba.com
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