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Solid metal construction for mechanical and thermal stability.

Footprint: 144x133mm, height:55mm,weight: 800 g

         Ariel is a F3, astigmatism corrected, compact, fiberoptics spectrometer for industrial and R&D desktop applications. It uses unfolded Czerny-Turner system with 80mm optical bench, torroid mirror for astigmatism correction, SMA 905 fiberoptics input, Gigabit LAN and USB 2 connections and extensive auxilary port functions for communication with other devices. It is a rugged spectrometer using fixed optical bench without moving or adjusting parts.

Ariel spectrometer has low aberration design  for the full spectrum that results in clean symmetrical peaks. Improved sensitivity at short and near-infrared wavelengths. All this coupled with fast integration time, onboard signal conditioning and LAN connectivity make Ariel spectrometer well suited for industrial and R&D applications.

Czerny Turner unfolded design with torroid mirror reduces light scattering, corrects astigmatism and optimized for low abberation and flat field across all measured spectrum


Wavelength  range, nm

380nm -1000nm

Wavelength resolution                    (with 20µm slit)       


Dynamic range     


Minimum integration time      

10 µs

Onboard data conditioning   

Averaging, boxcar, nonlinearity correction, dark signal correction,  fixed pattern noise correction


CMOS, 2048 pixels

Optical system      

Unfolded Czerny-Turner, fixed

Optical bench      

80 mm

Diffraction grating      

400 g/mm, blazed at 500nm

Astigmatism correction   

Torroid mirror

Input fiber connector    

SMA 905




16 bits, 10 MHz


Gigabit LAN, USB 2

Auxiliary port    

4xGPIO, I2C, 2xSPI, 4xPWM, 4xDAC, trigger, strobe



Minimum integration time      

10 µs

Ariel Specification and communication interface pdf

Imaging (detector) plane of spectrometer with and without astignatism correction. A. Ariel spectrometer B. Same design w/o astigmatism correction. C. Design with 600 g/mm (typical for small spectrometers) w/o astigmatism correction

Astigmatism correction

Spherical mirrors spectrometers can have significant astigmatism that is not corrected by Czerny-Turner design. Astigmatism means that a point at the entrance slit becomes a line at the imaging plane (on the detector). This results in the loss of light and increased scattering potential. Essentially, in case of oblique incidence, spherical mirror has different focus in sagittal and tangential planes. Astigmatism can be corrected using a cylindrical lens or torroid mirror. Torroid mirror is a cleaner but more expensive solution. High dispersion diffraction gratings (> 600g/mm) cause higher astigmatism that is more difficult to correct.

NonLinearity correction

CMOS detector response  is fairly linear at the low signals (<50% of dynamic range). But becomes non-linear at higher signals. The non-linearity is caused by the source- follower and charge to voltage converting capacitor. Hence, nonlinearity is slightly different from pixel to pixel. It is accurately corrected by factory calibration

Dark signal correction

Dark signal depends on integration time and temperature. Temperature dependence is relatively weak – dark signal decrease ~ 100 counts for 5 deg. increase in temperature. Temperature stabilizes after 40 min of operation. For an active CMOS detector, each pixel has a bit different dark current with a different rate of change. Careful factory calibration removes dark current.

Typical nonlinearity of the detector pixel: original and corrected

Typical dark signal vs. integration time for detector pixel

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