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ARIEL: COMPACT ASTIGMATISM-CORRECTED  SPECTROMETER

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 fiberoptics spectrometer has low aberration design for the full spectrum. The spectrum has  clean symmetrical peaks and  improved sensitivity at short and near-infrared wavelengths. All this coupled with fast integration time, onboard signal conditioning and LAN connectivity make Ariel spectrometer perfectly 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

ARIEL SPECTROMETER: BASIC SPECIFICATION

Parameter
VIS 
UVVIS

Wavelength  range, nm

380nm -1000nm

200nm -1000 nm

Wavelength resolution                    (with 20µm slit)       

1nm

1nm

Dynamic range     

>4000

>4000

Minimum integration time      

10 µs

.10 µs

Onboard data conditioning   

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

the same

Detector 

CMOS, 2048 pixels

CMOS, 2048 pixels 

Optical system      

Unfolded Czerny-Turner, fixed

Unfolded Czerny-Turner, fixed

Optical bench      

80 mm

80mm

Diffraction grating      

400 g/mm, blazed at 500nm

300 g/mm dual-blazed 

Astigmatism correction   

Torroid mirror

Torroid mirror 

Input fiber connector    

SMA 905

SMA 905

F#     

3

   3

ADC     

16 bits, 10 MHz

16 bits, 10 MHz

Connection   

Gigabit LAN, USB 2.0

Gigabit LAN, USB 2.0 

Auxiliary port    

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

the same 

Power     

24VDC

24VDC

Minimum integration time      

10 µs

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. This correction increases light collection 3x to 4x. It also  decrease the coma across the spectrum – this is important for clean symmetrical peaks in spectroscopic data. 

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. The residual non-linearity is < 0.2%

Dark signal correction

Dark signal depends on integration time and temperature. For an active CMOS detector, each pixel has a bit different dark current with a different rate of change. Each spectrometer is carefully calibrated on  per pixel basis and for range of operating temperatures. This calibration is stored on board and automatically loaded depending on temperature of the detector. This way, the dark is fully corrected.  

Typical nonlinearity of the detector pixel: original and corrected

Typical dark signal vs. integration time for detector pixel

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