/High-Sensitivity Compact Spectrometer SC125
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High-Sensitivity Compact Spectrometer SC125
The compact high-sensitivity spectrometer SC125 is developed for low light applications such as measurements of Raman scattering, fluorescence, etc., that require especially high sensitivity or enhanced specifications in the UV spectral range.
  • Up-to-date model based on back-thinned arrays for operation with low signals
  • Enhanced UV sensitivity
  • Monolithic housing for optimum stability
  • Internal light traps to reduce stray light
  • Flexible configuration, including a choice of Diffraction gratings, spectral ranges and resolutions tailored to your requirement
  • User-friendly interface compatible with Windows XP, Windows 7, 8 and 10
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/ Description
/ Specifications
/ Options & Accessories

The high-aperture optical bench of the SC125 has no moving parts and minimizes the number of reflective surfaces. The SC125 features a monolithic housing, thus ensuring long-time measurement stability. The case has internal fins (light traps) that allow reducing stray light – a typical problem of compact short-focal length instruments.


The SC125 may contain as a detector either one of two non-cooled Hamamatsu back-thinned CCD-arrays without a charge-storage section (back-thinned FFT CCD), operating in the binning mode. Both arrays have wide spectral range and excellent sensitivity in the UV (see below for the curves of each detector spectral sensitivity and their specifications). These two arrays differ in quantum efficiency, data reading rate, dynamic range, and in pixel active area size.




The detector based on the S7030-1006 CCD-array is more sensitive, has lower noise, better values of dynamic range and uniformity. The detector based on the S10420-1106 CCD array is faster, has anti-blooming and, since it has a greater number of pixels and smaller pixel size, ensures better spectral resolution than the S7030-1006. The IMAGING Version (Optional) features an astigmatism compensator – cylindrical lens – installed after the entrance slit. This further enhances of system sensitivity.




Spectral curve of sensitivity of the back-thinned CCD detector model S10420-1106




Spectral curve of sensitivity of the back-thinned FFT-CCD detector model S7030-1006 in comparison with front-illuminated CCD with and without UV-coating

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Download specification


SPECTROMETER MODEL SC125- S10420 SC125- S11510 SC125- S7030
Spectral range, nm 200 — 1100
Focal length, mm 125
F/number 1 : 3,9
Entrance slit (one to choose) fixed width: 14μm, 30μm and 50 μm
Spectral resolution depends on selected diffraction grating (see table below)
CCD-detector model S10420-1106
Hamamatsu 		S11510-1106
Hamamatsu 		S7030-1006
Hamamatsu
Number of pixels 2068 × 70 1024 × 64
Number of active pixels 2048 × 64 1024 × 58
Pixel size, μm 14 × 14 24 × 24
Active area size, mm 28,672 × 0,896 24,6 × 1,4
Maximum spectral sensitivity, nm 500 700 650
Maximum quantum efficiency? % >75 >90
Non-uniformity of sensitivity(1),% ±3 ±3
Anti-blooming(2) Yes No
ADC Resolution 16bit, 250 kHz 16bit, 125 kHz
Mean-square reading noise, ADC counts <4 <2
Dynamic range in the binning mode ~ 16000 : 1 ~ 33 000 : 1
Exposure time 8,3 ms — 5 s (3) 8,2 ms — 2 s (3)
Frame processing time in the binning mode 9,39 ms 9,12 ms
Thermoelectric cooling No
Operating temperature 10 – 30 °С
Computer interface Full Speed USB
Triggering internal / external
Optical input — direct input through the SC125 input slit
— Optical Fiber : 0.6 (0.4)mm diameter, 1m length, SMA-905 connector
Dimensions, weight 158 × 182 × 74 мм; 2,2 кг


* Specifications are subject to change without notice.

1) Signal level — 50% of saturation.

2) anti-blooming – sensor’s feature eliminating overflow of charges from over-exposed pixels to the neighboring ones.

3) maximum storage time is deemed to be the time at which dark signal reaches 10% of the dynamic range at the ambient temperature +25°С


At the time of placing your order you should choose a grating lines density (i.e. spectral resolution of your instrument), as well as the spectral range for operation. For your convenience the table below lists the average values of grating dispersion, spectral resolution and multichannel array bandpass.



Diffraction gratings, lines/mm 1800 1200 900 600 400 300 200
— possible spectral range of grating operation, nm 180-600 180-900 180-1100 180-1100 190-1100 200-1100 200-1100
— multichannel array bandpass (average), nm1) 1052)923) 1702)1453) 2302)2003) 3502)3003) 5402)4603) 7202)6203) 10002)9203)
— reciprocal linear dispersion (average), nm/mm1) 3.8 6.0 8.2 12.5 19.0 25.4 38.0
— spectral resolution (average), nm 0.162)0.223) 0.252)0.363) 0.342)0.53) 0.52)0.753) 0.82)1.13) 1.02)1.53) 1.62)2.33)


1) for 300nm wavelength.

2) for the SC125- S10420 model.

3) for the SC125- S7030 model.


EXAMPLE: If you are interested in the1200 lines/mm grating and the S10420-1106 detector (spectral resolution of 0.25nm), then you should choose the location of 170nm multichannel array bandpass within the possible 180-900nm spectral range of the grating. For instance, the SC125- S10420 spectrometer operating in the range of 250-420nm with 0.25nm resolution.


The values indicated in the table are calculated for 300nm wavelength. With increased wavelength, dispersion of a specific grating and multichannel array bandpass are slightly decreased and resolution is improved. Contact a SOLAR LS specialist for more precise calculation of parameters for your instrument.


At your request the SC125 spectrometer can be equipped with optional calibration of spectral sensitivity.


Spectral ranges of calibration:

  • Cal-UV: within 220-400nm.
  • Cal-VIS: within 300-1050nm.
  • Calibration is performed with certified light sources (a deuterium lamp for the 220-400nm spectral range and a halogen lamp for the 300-1050nm range). It is made using a fiber input and is valid for 1 year provided that the optical fiber is not removed from the spectrometer. Calibration accuracy is +/-10%.


WHAT POSSIBILITIES ARE OFFERED BY SPECTRAL SENSITIVITY CALIBRATION


Whereas in the past the spectrum of your light source was superimposed by spectral curves of diffraction grating efficiency, detector sensitivity, reflective index of mirrors, now you have the opportunity to restore true spectra of the analysed source. You will be able to:

  • record true spectra
  • mathematically decompose complex lines of the spectrum into its components*
  • determine the tristimulus values and colour-rendering index of light sources*
  • determine the light power density in the UV ranges A, B, and C*.


* Features marked with an asterisk are not included into the software of your spectrometer; they are implemented by exporting to external programs.


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