RaySphere Solar Analysis System (RaySphere and RaySphere 1700) Installation and Operation Manual Document Number RAYSPHERE

Transcription

1 RaySphere Solar Analysis System (RaySphere and RaySphere 1700) Installation and Operation Manual Document Number RAYSPHERE Offices: Ocean Optics, Inc. World Headquarters 830 Douglas Ave., Dunedin, FL, USA Phone Fax a.m. 8 p.m. (Mon-Thu), 8 a.m. 6 p.m. (Fri) EST Info@OceanOptics.com (General sales inquiries) Orders@OceanOptics.com (Questions about orders) TechSupport@OceanOptics.com (Technical support)

2 Additional Offices: Ocean Optics Asia 137 Xianxia Road, Suite 1802, Changning District, Shanghai, PRC Phone Fax Ocean Optics EMEA Geograaf 24, 6921 EW DUIVEN, The Netherlands Phone 31-(0) Fax 31-(0) Regional Headquarters Maybachstrasse Ostfildern Phone Fax Copyright 2012 Ocean Optics, Inc. All rights reserved. No part of this publication may be reproduced, stored in a retrieval system, or transmitted, by any means, electronic, mechanical, photocopying, recording, or otherwise, without written permission from Ocean Optics, Inc. This manual is sold as part of an order and subject to the condition that it shall not, by way of trade or otherwise, be lent, re-sold, hired out or otherwise circulated without the prior consent of Ocean Optics, Inc. in any form of binding or cover other than that in which it is published. Trademarks All products and services herein are the trademarks, service marks, registered trademarks or registered service marks of their respective owners. Limit of Liability Ocean Optics has made every effort to make this manual as complete and as accurate as possible, but no warranty or fitness is implied. The information provided is on an as is basis. Ocean Optics, Inc. shall have neither liability nor responsibility to any person or entity with respect to any loss or damages arising from the information contained in this manual.

3 Important Safety Notices 1. Read the instructions first to avoid any damages. 2. Store your RaySphere system at above -10 C and below 50 C to avoid any damages. 3. This is a calibrated measurement device. Handle the system with care. The calibration precision may be lost if any dust or other pollutant enters the integrating sphere. When the system is not in use, store it with a dust protector. When removing the dust protector, be sure to keep pollutants from entering the integrating sphere aperture. 4. Recalibration is recommended after one year of use or sooner is the measurements do not seem to be accurate. More frequent recalibration may be needed of the RaySphere has suffered any heavy shocks or is being used in a dusty environment. 5. The RaySphere is heavy. Take care to keep it from falling. 6. If the seal on the screws is broken, then the calibration is no longer valid. 7. To ship the RaySphere, pack it in the Pelican case, which is optimized for transport. Hand carrying if the RaySphere is recommended for all traveling. 8. Contact your Ocean Optics regional headquarters for questions about RaySphere. 9. Be sure to follow all safety instructions for your solar simulator. 10. Do not cover vents. 11. Do not cover the holes at the top of the RaySphere main body. RAYSPHERE i

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5 Table of Contents About This Manual... v Document Purpose and Intended Audience... v Document Summary... v Product-Related Documentation... vi Upgrades... vi Chapter 1: Introduction... 1 Description... 1 Photocurrent Recording... 2 Calibration... 2 RaySphere Software... 2 Shipment Components... 2 Chapter 2: Installation and Set-up... 5 Overview... 5 RaySphere Components... 5 Installing Software... 6 Assembling RaySphere... 8 Chapter 3: Software Operation... 9 Overview... 9 Software Structure... 9 System Tab Photo Current/Trigger Settings Tab Spectrometer Tab Classification Tab Warnings and Status Information Chapter 4: File Types and Data Files Overview Calibration Files Parameter File RAYSPHERE i

6 Table of Contents Stray Light Correction Matrix Saved File Types Chapter 5: Operation Overview Triggering and Measurement Modes Optical Triggering External Triggering Manual Triggering Signal Path of Trigger Timing and Delays Chapter 6: Using Preconfigured Configuration Files Overview How to Use Configuration Files Contents of a Configuration File How to Create a Configuration File Chapter 7: Classifying the Solar Simulator and Displaying the Results Overview Saving Results Validating a Solar Simulator Using RaySphere with a Flash Solar Simulator Using RaySphere with a Continuous Solar Simulator Validating the Test Results Chapter 8: Test Report Overview Chapter 9: Nonlinearity Correction and Calibration Overview Nonlinearity Correction Wavelength Calibration Absolute Irradiance Calibration Uncertainties Calculation ii RAYSPHERE

7 Table of Contents Uncertainty for Spectral Match Test Uncertainty of Repeated Measurements Quantitative Uncertainties How to Estimate the Uncertainties for the Spectral Match Test Appendix A: Components Technical Notes Overview QE65000 Spectrometer NIRQuest Spectrometer Trigger Electronics USB-Hub Appendix B: Specifications and Mechanical Diagram Mounting Options for RaySphere Main Body Index RAYSPHERE iii

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9 About This Manual Document Purpose and Intended Audience This document provides you with a detailed description of the RaySphere and RaySphere 1700 systems, including installation and operating instructions. Quick start instructions are available for users who are just interested in testing a solar simulator with RaySphere. See Product-Related Documentation. What s New in this Document This version of the RaySphere Solar Analysis System Installation and Operation Manual updates specification information. Document Summary Chapter Chapter 1: Introduction Description Contains a description of the RaySphere system. Chapter 2: Installation and Set-up Chapter 3: Software Operation Provides installation instructions for RaySphere hardware and software. Provides software operation instructions for RaySphere. Chapter 4: File Types and Data Files Chapter 5: Operation Chapter 6: Using Preconfigured Configuration Files Chapter 7: Classifying the Solar Simulator and Displaying the Results Chapter 8: Test Report Provides information on the calibration files, the stray light correction matrix and the saved file types. Contains instructions for operating the RaySphere system using triggering. Provides information on using preconfigured configuration files, including how to create them. Provides procedures for using RaySphere with solar simulators and how to validate your results. Describes a typical test report. Chapter 9: Nonlinearity Correction and Calibration Appendix A: Components Technical Notes Contains nonlinearity correction and calibration information as they pertain to RaySphere. Lists technical notes for the RaySphere components. RAYSPHERE v

10 About This Manual Chapter Appendix B: Specifications Description Contains product specifications. Product-Related Documentation RaySphere Quick Start Instructions NIRQuest Near Infrared Spectrometer Installation and Operation Manual QE65000 Scientific-grade Fiber Optic Spectrometer Installation and Operation Manual SpectraSuite Spectrometer Operating Software Installation and Operation Manual External Triggering Options for Firmware Versions 3.0 and Above You can access documentation for Ocean Optics products by visiting our website at Select Technical Operating Instructions, then choose the appropriate document from the available drop-down lists. Or, use the Search by Model Number field at the bottom of the web page. You can also access operating instructions for Ocean Optics products on the Software and Technical Resources CD included with the system. Engineering-level documentation is located on our website at Technical Engineering Docs. Upgrades Occasionally, you may find that you need Ocean Optics to make a change or an upgrade to your system. To facilitate these changes, you must first contact Customer Support and obtain a Return Merchandise Authorization (RMA) number. Please contact Ocean Optics for specific instructions when returning a product. vi RAYSPHERE

11 Description Chapter 1 Introduction RaySphere is a calibrated high-performance measurement device. It is designed for testing the spectral distribution of all types of Solar Simulators and for validating the Simulator for the spectral match test in accordance with the international standard IEC : Solar Simulator Performance Requirements. The RaySphere series of products consists of RaySphere and RaySphere They provide the following features: Intuitive graphical interface Graphical and table display of classification results by wavelength bin Output of actual spectra in mw/cm 2 /nm Output of actual measurement and triggering timing with +/-44 µs resolution Printable classification report RAYSPHERE

12 1: Introduction RaySphere contains one QE65000 spectrometer, while RaySphere 1700 contains two spectrometers (QE65000 and NirQ512) and a trigger unit to control the measurement procedure and a hub. The trigger sources can be a flash from the solar simulator, an electrical trigger pulse (high level with +5 V or +24 V) or a measurement can be generated manually at any time. RaySphere software allows full control during the testing and generates a test report with the classification of the simulator. Photocurrent Recording A unique innovation for test control is the function photocurrent recording. A photodiode detects the integral light intensity of the environment. The sudden increase of intensity is interpreted by the electronics as a measurement event and the complete flash signal is recorded up to 160 ms flash duration. The time-dependent photocurrent is displayed and the time interval in which the spectrometer has recorded light from the solar simulator is indicated. The user can adjust delays to make sure that the recording time of the spectrometer was at the stable flash phase and maximum control for the testing procedure is given to minimize any kind of mismeasurement. Calibration The calibration is tested by an independent certificated optical calibration laboratory. The inaccuracy for the spectral match as described in IEC is typically on the order of 2 %. Uncertainty has been minimized to achieve highest precision. A detailed description about calibration and uncertainty is given in this document. RaySphere Software The RaySphere software allows intuitive operation of the system and automatically generates a test report with classification of the simulator. The software was especially designed for the requirements of the solar industry. Shipment Components The RaySphere package consists of the following items: Pelican case: The transport box for the complete RaySphere System RaySphere main body Power Supply Four Power Cables, one each for USA, Europe, UK, and Australia Power Supply Connection Cable [SubD-type, 3 meters length] USB cable (USB-CBL-1): Connects RaySphere to a computer s USB port, 3 meters length RaySphere CD: Contains RaySphere software and calibration files and manual 2 RAYSPHERE

13 1: Introduction Software and Technical Resources CD: Contains software, operating instructions, and product information for all Ocean Optics software, spectrometers, and spectroscopic accessories. You need Adobe Acrobat Reader version 6.0 or higher to view these files (version 7.0 is included on the CD). Documentation is also available on our website at Calibration documents RAYSPHERE

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15 Overview Chapter 2 Installation and Set-up This chapter contains information for assembling your RaySphere unit. RaySphere Components The following figures show the parts of the RaySphere main body. RaySphere Body RAYSPHERE

16 2: Installation and Setup RaySphere Components Installing Software Caution Install the software BEFORE connecting the spectrometer to your PC. The RaySphere software installs the drivers required for spectrometer installation. If you do not install RaySphere software first, the system will not properly recognize the spectrometer. RaySphere includes special software for operating your RaySphere system. This software is located on the Software & Technical Resources CD. The installation instructions are included below. In addition, if you have purchased and are using SpectraSuite with the RaySphere for controlling the spectrometers, follow the instructions in the SpectraSuite Spectrometer Operating Software Installation and Operation Manual for software installation instructions (see Product-Related Documentation). 6 RAYSPHERE

17 2: Installation and Setup Caution Do not run SpectraSuite and RaySphere software at the same time on the computer. Procedure To install RaySphere software from the RaySphere CD, 1. Close all other applications running on the computer. 2. Load the RaySphere CD. The CD contains the calibration data, fundamental settings and the software for operating the RaySphere on a 32-bit or 64-bit computer. 3. Select the Setup CD folder. 4. Select the installation file for either a 32- or 64-bit system. The setup process begins and the following screen appears: 5. Click the Install button. Then follow the prompts in the installation wizard. RAYSPHERE

18 2: Installation and Setup Note If the following screen appears during the installation, select Repair: 6. Click Close when the installation is completed. It is not necessary to restart your computer. Assembling RaySphere Follow the steps below to set up your RaySphere for use. Procedure 1. Connect the power cable to the power supply. 2. Connect the RaySphere unit to the power supply with the SubD cable. 3. Switch on the power supply. 4. Connect the RaySphere to your computer using a USB cable. Caution Be sure to switch on the power supply before connecting the RaySphere to your computer. Your RaySphere is now ready to use after 20 minutes of warm-up time. 8 RAYSPHERE

19 Overview Chapter 3 Software Operation The RaySphere software is designed for requirements of the solar industry and related applications. The operation and functions are as intuitive as possible and the functions are designed with the needs of the user in mind. Software Structure The software consists of four main functions tabs for controlling RaySphere settings and operation: System Photocurrent Trigger / Settings Spectrometer Classification RAYSPHERE

20 3: Software Operation The four functions appear in the upper command line of the main screen. Pressing one of the controls changes the background of the function name to green. The section becomes active and the page with the function details appears. System Tab The system tab allows you to load and save data. Load All Load All ( ) loads the following file types with the name you specify: Classification_Date_time_Name.txt Configuration_Date_Time_Name.cfg PDcurr_Date_Time_Name.cfg Report_Date_Time_Name.pdf Spec_merge_Date_Time_Name.txt Spec_NR_Date_Time_Name.txt Spec_QE_Date_Time_Name.txt Spectrum _Date_Time_Name.txt See File Types and Data Files for more information. Load Config Load Config ( ) loads a configuration file to operate RaySphere under conditions defined in the file. Save All Save All ( ) saves all data as one of the following file types: Classification_Date_time_Name.txt 10 RAYSPHERE

21 3: Software Operation Configuration_Date_Time_Name.cfg PDcurr_Date_Time_Name.cfg Report_Date_Time_Name.pdf Spec_merge_Date_Time_Name.txt Spec_NR_Date_Time_Name.txt Spec_QE_Date_Time_Name.txt Spectrum _Date_Time_Name.txt See File Types and Data Files for more information. Procedure To save data, 1. Click the Save All icon ( ). The Save Data dialog box opens. 2. Select or create the folder where the data is to be saved. 3. Assign a name to the file. It is recommended to use the serial number of the solar simulator or anything specific which clearly identifies the tested solar simulator. 4. The date and time is added from your computer settings. Ensure that your computer is using the correct date and time. Save Config Save Config ( ) saves the actual RaySphere confguration in one file. Photo Current/Trigger Settings Tab The Photo Current/ Trigger Settings tab enables you to control the settings for photo current and triggering of the RaySphere. The maximum sample time for the photocurrent is 160 ms. RAYSPHERE

22 3: Software Operation Connect Pd Connect Pd connects RaySphere photocurrent and trigger unit electronics to the computer when the Start ( ) button is pressed. Icon Meaning The computer has no connection to RaySphere s photocurrent and trigger unit. The computer is connected successfully to the RaySphere electronics. Sets the system to ready status for taking a measurement. Disables the ready status to allow changes to photocurrent and trigger settings. See Changing Photocurrent and Trigger Settings. Displays the Photocurrent/ Trigger Settings dialog box to allow changes to the photocurrent and trigger settings. Changing Photocurrent and Trigger Settings Procedure To change photocurrent and trigger settings, 1. Click the Setting button ( ). The Photocurrent/Trigger Settings dialog box appears. 12 RAYSPHERE

23 3: Software Operation Make the desired setting changes. Setting *Delay of QE/NQ Amplification Meaning Set the delay time for the QE65000 (QE) and/or NIRQuest (NQ) spectrometer in the RaySphere. The available range is ms. Sets the amplification of the photocurrent in two steps: Gain 1, Gain 2, Gain 3: amplify by a factor of 1, 10, 100, respectively Fine amplification by a factor of 1:10 The resulting overall amplification is: Amplification = GainX x fine amplification. [GainX = {1; 2; 3}] *Trigger Level Adjusts the trigger level values for the photocurrent from 500 to Trigger Source Changes the trigger source: External RaySphere reacts to an electrical trigger pulse which can be applied on the power supply Flash RaySphere triggers itself by flash if the trigger level is reached Manual Spectrum recording is done manually. RaySphere measures when the sample button on the Spectrometer page is pressed. Off no triggering RAYSPHERE

24 3: Software Operation Setting Operation Mode Meaning Changes the mode of operation: Continuous/ValueFind optimizes the values for trigger levels, delays and integration times Autotest/SingleSpec Used for single measurements of the solar simulator * The values for trigger level and delays are stored in RaySphere s electronics to ensure immediate response and minimize jitter. Photocurrent Graph The photocurrent is recorded by a photodiode, digitalized, and displayed in the graph on the Trigger Settings / Photo Current page as shown in the example below: The time evolution of a flash from a solar simulator is displayed on the graph. This graph contains the following components: X-axis time in ms. 14 RAYSPHERE

25 Y-axis -- the amplified photocurrent in arbitrary units 3: Software Operation Trigger level -- Marks the position when the trigger level was reached by the increasing light intensity All delays (set delay and spectrometer internal delay) are taken into account. This allows you to control the timing of the recording of the flash. You can change the delay values to ensure that RaySphere records the simulator s spectrum while the flash time is stable. The maximum sample time for the photocurrent is 160 ms. The graph also shows the time that expired before the trigger level was reached. Spectrometer Tab The Spectrometer tab enables you to perform a variety of functions related to the spectrometers contained by the RaySphere unit. Functions Control QE65000 Function Displays the Spectrum dialog box for changing the QE65000 settings. RAYSPHERE

26 3: Software Operation Control NIR Merge Sample Reconnect Zoom In/Zoom Out Select x-axis Function Displays the Spectrum dialog box for changing the NIRQuest512 settings (if the NIRQuest512 is installed in your RaySphere). Merges the spectral data from the QE65000 and NIRQuest512 spectrometers (if your RaySphere contains both spectrometers). There is an overlap in the spectral range from 950 nm to 1050 nm if both spectrometers are built into your RaySphere. The merge interval is limited to 1 nm in width. Records a spectrum the manual trigger mode is active. The exact function of Sample depends on the selected Trigger Source setting in the Photo Current/Trigger Settings Tab dialog box. When this button is pressed, the software tries to connect to the spectrometer(s). If the spectrometer(s) are not connected after pressing the button several times, restart the program and reapply power the RaySphere system. Changes the scaling in the graph with the absolute irradiance displayed. Use this button in conjunction with the mouse to select and zoom in on a specific area of the graph. The Select function does not affect the x-axis scaling. Changes the wavelength range on the graph s x-axis. Indicates the spectrometer saturation. Saturation Spectrum Graph The Graph displays the last recorded spectrum. The absolute irradiance data is represented by the y-axis in µw/cm^2/nm while the x-axis shows the wavelength in nm. Spectrum Dialog Box Press the or buttons to invoke the Spectrum dialog box. 16 RAYSPHERE

27 3: Software Operation Use this dialog box to set the following spectrometer functions: Control Integration Time Scans to average Function Set the spectrometer s integration time in ms starting from 8 ms. The preferred Delimiter to separate the digits is the. Symbol. Set the number of spectral recordings to use to average for the spectrum. It is recommended that a single spectrum be used. Use only one spectrum if a solar simulator is being used. The function is disabled. Boxcar width Set the number of pixels to use for a moving average. The recommend setting is 5. The bandwith of one pixel is ~ 0.7 nm for the QE65000 and ~ 1.6 nm for the NirQuest512. TEC set Save TEC settings Set the detector temperature in C. Use the specified temperature in the calibration documents or see the calibration label below the RaySphere s main body. The calibration has an increased uncertainty if a different TEC is chosen. See Nonlinearity Correction and Calibration for more detail. Saves the temperature setting. After changing the temperature, it is recommended to record a valid dark spectrum. RAYSPHERE

28 3: Software Operation Control Current temperature Dark Spectrum Calibration File Function The actual TEC (sensor tempertaure) is read out from the device. The status will be actualized every 5 seconds. The first value is dispalyed after 5 seconds. Press this button to record a spectrum the the current settings and display its graph in this dialog box. This spectrum is used as the dark and reference spectra. Be sure to record the dark and reference spectra using the identical spectrometer function settings. The dark spectrum has to be measured 20 minutes after switching on the software and before the measurement of the solar simulator is performed. Press the button in the Calibration File field to load the calibration file. Follow the wizard prompts. If the file being loaeded does not match the RaySphere s serial number, then a warning appears. A warning also appears in the calibration file date is older than one year. The calibration files for the spectrometers are in the folder calibrationdata on the RaySphere CD. The calibration files for the QE65000 spectrometers start with QE. The files for the NirQuest512 start with NQ. The file parameter.xmls contains fundamental settings and default settings such as names of the calibration files and default settings for the RaySphere software settings. The parameters (and the calibration files mentioned in there) are loaded automatically to the software if the RaySphere software is started. The settings in there can be changed by opening the parameter files as ASCII code. Stray light correction file Apply Cancel Load the stray light correction file you received from Ocean Optics. Press this button to apply the current settings. Any changes made since the last time the Apply button was pressed are no saved to the device. Classification Tab The RaySphere software analyzes the spectral data and calculates the classification of the simulator. This information is displayed in the Classification tab. The simulator is classified in accordance with the international standard for solar simulators IEC : Solar Simulator Performance Requirements. The test performed by RaySphere is the Spectral Match Test. The Classification Tab displays the results of the solar simulator test in four parts (clockwise from upper left corner): The spectrum in absolute irradiance over a wavelength range from 400 nm to 1100 nm. The physical unit of the absolute irradiance is µw/cm^2/nm. The upper scale refers to the definition of spectral bands as done in the international standard IEC The result from the spectral match test displayed in a diagram. The results from the spectral match test displayed in a table. 18 RAYSPHERE

29 3: Software Operation The recorded Photocurrent diagram, which shows the time evolution of the flash. The marks indicate at which times the spectrometer recording began and ended. For more information, see Classifying the Solar Simulator and Displaying the Results. Warnings and Status Information The RaySphere software controls several parameters which might affect the accuracy of the measurement. The indicators System, Recording and Measurement monitor several parameters. The indicator color changes from green to red if an important parameter is out of range or not acceptable. Click on the red item to display the warning message. Possible warning messages are listed below: Message Type Message Meaning System No spectrometer is connecting No spectrometer is connected to the RaySphere system Trigger is not connecting The ID Query failed. Please try again or unplug and replug the USB device and Restart RaySphere please. Failed to read data (error " + error type + ") No trigger device is connected to the RaySphere system Failure to connect to the trigger device Failure to read data from the trigger device RAYSPHERE

30 3: Software Operation Message Type Message Meaning Recording Failed to write to device [error " + error type + "Command:" + command content] The first [or second] spectrometer needs Record. Classification needs irradiance data Failure to write a command to the trigger device The spectrometer has no spectrum data Both of the spectrometers have no spectrum data Measurement [spectrometer name] needs calibration An absolute irradiance calibration has not been loaded [spectrometer name] the most recently acquired spectrum was saturated [spectrometer name] detector temperature is [degree] Celsius degree It will take [20 minutes minus the elapsed time] more minutes to warm up done The spectrum data is saturated The actual TEC degree is different from the target degree Warm-up time is not reached within 20 minutes Note You can perform tests and generate a certificate while a warning is present. However, the warnings are listed in the certificate and inaccuracies might increase if a warning was present during certification. 20 RAYSPHERE

31 Overview Chapter 4 File Types and Data Files You must load the following types of files into RaySphere to be able to operate the system: Calibration files for absolute irradiance Stray light correction matrix. The Ocean Optics CD that came with your system contains the calibration files and the stray light correction matrix. Calibration Files The calibration files have a name structure similar to the following: Serialnumber_of_the_Spectrometer_Datei.irradcal Serialnumber_of_the_Spectrometer_OOIIrrad.cal Both files load at the same time. Note These files contain the calibration information for each individual RaySphere system. Never make any changes in these files. The calibration files for the spectrometers are in the folder calibrationdata on the delivered RaySphere CD. RAYSPHERE

32 3: Software Operation Parameter File The file parameter.xmls contains fundamental settings and default settings such as names of the calibration files and default settings for the RaySphere software settings. The parameters (and the calibration files mentioned in there) are loaded automatically to the software if the RaySphere software is started. The settings there can be changed by opening the parameter files as ASCII code. Stray Light Correction Matrix The stray light correction matrix is on the CD that comes with your RaySphere system. These files have a name similar to the following: Serialnumber_of_the_Spectrometer_Datei _EasyCorr.txt Do not make any changes to this file. Saved File Types The RaySphere software creates several files when data is stored. The files are stored to guarantee the traceability to the original measured data listed in the created test report and to save the configuration of the measurement procedure. The files that are saved are as follows: Classification_Date_time_Name.txt. Contains the classification of the solar simulator in a table. An example is given below: Configuration_Date_Time_Name.cfg. Contains all relevant parameters of the measurement. A detailed description is given in File Types and Data Files. 22 RAYSPHERE

33 4: File Types and Data Files PDcurr_Date_Time_Name.cfg. Contains the photocurrent data. The first column represents the photocurrent intensity in arbitrary units. The following three columns have the values true and false and represent the status information of the RaySphere System. The first value changes from false to true if the intensity on the PD is higher than the set trigger level. The value true in the second and third column indicates when a trigger pulse was sent out to the spectrometers. The second column is for the QE and the third column is for the NirQuest512. The fourth column indicates that the trigger electronics are working properly. The data points have an intercept of 87 ms. Spec_merge_Date_Time_Name.txt Spec_NR_Date_Time_Name.txt and Spec_QE_Date_Time_Name.txt. Contains the raw data of the spectrum in two columns. The first column represents the wavelength in nm and the second one is the measured absolute intensity in µw/cm^2/nm. Spectrum _Date_Time_Name.txt. contains the data point for the spectrum which was used for solar simulator validation. The two columns represent wavelength in nm and absolute intensity in µw/cm^2/nm. Report_Date_time_Name.pdf. Contains the PDF of the test report measurement data. A detailed description of the report is in Test Report. The Name can be chosen by the user during the save procedure. The date and time are automatically implemented in the name by the software. Be sure that the date and time in the user s computer is correct. All files are in ASCII format. RAYSPHERE

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35 Overview Chapter 5 Operation The RaySphere software offers several operation modes. The simplest way to operate and validate a solar simulator is to use the configuration files. The complete settings are written in the file and can be loaded and used with minimum effort. This procedure ensures the best results. For details, see the section Using Preconfigured Configuration Files in this manual or take a view in the RaySphere Quick Start Instructions (see Product-Related Documentation). Some other procedures for testing may be required for scientists or for members of a development department. For those experts, a description for all measurement modes is provided in this chapter. Triggering and Measurement Modes RaySphere offers three modes to trigger the system. Optical trigger signal from a flashing Solar Simulator. Include Timing Diagram External trigger electrical trigger signal with 5 V or 24 V high level. Includes Timing Diagram. Manual trigger from the computer. Includes Timing Diagram, if activated. Maximum trigger frequency is 5 Hz. Maximum speed for spectrum recording and processing is 1 Hz. It is recommended to perform 3 spectrum recordings (and to excite 3 flashes) within 5 minutes and to use the data from the last flash for the validation and the certificate. Optical Triggering A photodiode records the incoming light passing through the small hole in the RaySphere s main body. The photocurrent amplification is set using the software (see Chapter 4: Software Operation, Changing Photocurrent and Trigger Settings. The amplified photocurrent runs through a comparator, which is part of the electronics. The comparator level can also be set using the software. The comparator level and trigger level are identical. As soon as the level is reached by the photocurrent, the electronics will interpret this as a triggering event and send out trigger signals to the spectrometers. The signal is delayed by the amount of time set for the delay. The timing is described in Timing and Delays. RAYSPHERE

36 5: Operation The photocurrent, which is proportional to the incoming light, is being digitized in data points that are separated into 44 µs intervals. Each data point represents the averaged value of light intensity for 44 µs. Each data point gets a time mark to ensure correct timing. The data points are stored in the trigger electronics until the software requests the data to transmit. Procedure To record a spectrum for a flash, 1. Click the Setting button ( ). The Photocurrent/Trigger Settings dialog box appears. 2. Set the Trigger Source to Flash and click OK. 3. To run the system, press button. Adjusting the Photocurrent Amplification and Trigger Level The photocurrent is amplified by an on board amplifier. Amplification is set in the Photocurrent / Trigger Settings dialog box (see Chapter 4: Software Operation, Changing Photocurrent and Trigger Settings). 26 RAYSPHERE

37 5: Operation Procedure To adjust the photocurrent amplification and trigger level, 1. Click the Setting button ( ). The Photocurrent/Trigger Settings dialog box appears. 2. Choose the Operation Mode Continuous/ValueFind. 3. Click the OK and the buttons to activate the settings. The actual digitalized photocurrent is continuously displayed in the graph. 4. Excite a flash and observe the photocurrent behavior on your computer screen. The flash appears and disappears quickly. Nevertheless, you can determine if the photocurrent is saturated (meaning the amplification is too high) or if the flash intensity is too low (meaning the Gain is too small). 5. The amplification works on a linear scale. Adjust the amplification until the flash intensity is greater than 700 arbitrary units on the y-axis of the graph. Set the trigger level value between 500 and the maximum of intensity. 6. Change the Operation mode to Autotest/SingleSpec. The photocurrent is not displayed continuously. RAYSPHERE

38 5: Operation 7. Press the button in the Spectrometer tab. 8. Excite a flash. RaySphere measures the flash and displays the time-resolved photocurrent of the flash in a graph that resembles the following (ideal case): The system measures the flash if the photocurrent is saturated as well. In this example, it is hard to decide if the flash intensity was constant during the spectrometer s exposure time. If you are using a tested and verified configuration file for this type of flasher, then the measurement is still valid. 9. Adjust the timing of RaySphere for your solar simulator in the next step. See the section Timing and Delays. External Triggering You can excite the measurement of a spectrum by using an external trigger signal. Some flashers provide a trigger output to control processes of external devices or a signal from a SPS is available. Check if the properties of the output match with requirements for RaySphere external triggering and the trigger is of level type and accepts levels from 5 V to 24 V. Do not apply higher voltages. The minimum high time is 500 ns. The signal cable can be applied at the BNC-connector located on the power supply. 28 RAYSPHERE

39 5: Operation Procedure To record a spectrum from a triggered pulse, 1. Press the Setting button ( ). The Photocurrent/Trigger Settings dialog box appears. 2. Set the Trigger Source to External. See Changing Photocurrent and Trigger Settings for more information. The chosen parameters for delay are still active. The Photocurrent data will also be displayed. 3. Press the button in the Spectrometer tab. A spectrum will be recorded when a trigger pulse is sent to RaySphere. Manual Triggering The software allows you to record a spectrum by pressing the button in the in the Spectrometer tab. RAYSPHERE

40 5: Operation Procedure To record a spectrum from a manually triggered pulse, 1. Press the Setting button ( ). The Photocurrent/Trigger Settings dialog box appears. 2. Set the Trigger Source to Manual. 3. Press the button in the Spectrometer tab. Each time you press the button, a spectrum is recorded. Notes The Photocurrent data is also logged and displayed if the play( Settings tab has been pressed. ) button on the Trigger The message Invalid Data appears on the Classification tab and in the certificate if the play( ) button button has not been activated. This has no effect on spectral data. 30 RAYSPHERE

41 Signal Path of Trigger 5: Operation The following schematic illustrates the signal path. Knowledge of the signal path of the trigger signal provides a deeper knowledge of RaySphere s functionality. The External trigger signal is applied at the power supply. The signal travels from there to the trigger electronics where the signal is being delayed and sent out to the trigger inputs of the spectrometer. RAYSPHERE

42 5: Operation Timing and Delays The timing is a key issue for getting reasonable results. A timing diagram for Flash mode and External mode is given below to illustrate how they function in RaySphere. 32 RAYSPHERE

43 5: Operation The terms used in this diagram are defined below: Delay: The delay can be set in the software. Valid values are between 0 ms and 160 ms. The delay values are stored in the trigger electronics to minimize jitter. Fixed delay: The spectrometers have an internal fixed delay of 768 µs for the QE65000 and 1034 µs for the NIRQuest512. These are the minimum delays and are always present. The QE65000 has an additional fixed delay of 266 µs. As a result, both spectrometers start integration at the same time for identical user set delays. All types of delay are taken into account for visualizing of the integration time interval of the spectrometer in the photocurrent graph. The delays are active for the External, Flash and Manual modes. Integration time: Time interval for spectrum recording. The output represents the average value of intensity of the light during this time interval. Data transfer: It takes several ms to send the data to the computer. During this time the RaySphere will not react to further trigger signals from the trigger electronics. The spectrometers do not react for trigger signals until the data transfer is completed. To ensure correct timing, the maximum speed for data recording is 1 Hz. If SpectraSuite is being used for data recording, use a maximum speed of 5 Hz. RAYSPHERE

44 5: Operation 34 RAYSPHERE

45 Chapter 6 Using Preconfigured Configuration Files Overview RaySphere is designed as a tool which should be usable for beginners in optical measurement. To do this, preconfigured files, named config-files, have been created which contain all information needed for setting the RaySphere. Loading these preconfigured files into the RaySphere software enables you to perform measurements under previously defined conditions. How to Use Configuration Files Procedure 1. Load the configuration file by pressing the button in the RaySphere software. All relevant parameters are now set. 2. Measure a dark spectrum. 3. To start a measurement, press the button (to get the system into ready status. A spectrum will be recorded automatically when the next flash or trigger signal is detected. A complete procedure for validating a solar simulator using a preconfigured configuration file is provided in Validating a Solar Simulator and in the RaySphere Quick Start Instructions (see Product-Related Documentation). Note You are allowed to change settings in the RaySphere software after loading a configuration file. RAYSPHERE

46 6: Using Preconfigured Configuration Files Contents of a Configuration File The configuration files have a naming pattern such as Configuration_Date_Time_name.cfg and are ASCII files. The numbers in the name represent the date and time when the file was saved. The name is chosen by the user. An example of a configuration file is shown below: :03 Amplifier grade: 2 Amplifier fine : 5 Trigger level : 551 Trigger mode : Manual Operation mode : Auto Infos of the QE : SN: QEB1351 Cal.file: E:QEB1351_ _OOIIrrad.cal Delay[ms]: It: 10 TEC[ C]: -12 Scan2Avr: 1 Boxcar: 5 Infos of the NR : SN: Cal.file: Delay[ms]: It: TEC[ C]: -10 Scan2Avr: 1 Boxcar: 5 Straylight correction File: E:QEB1351_EasyCorrM_.txt The entries have the following meaning: Field Meaning :03 Date and time clock Amplifier grade: 2 Decade of amplification of photocurrent: 1 = gain1; 2 =gain2; 3 = gain3 Amplifier: 5 Trigger level: 551 Trigger mode/operation mode: Manual mode => External triggering => Amplification value Trigger level for optical trigger Choose Flash the following parameters: Manual/Manual External/Manual 36 RAYSPHERE

47 6: Using Preconfigured Configuration Files Field Flash/continuous mode => Flash/Autotest => Operation mode: Auto Infos of the QE: SN: QEB1351 Cal.file:E:QEB1351_ _OOIIrrad.cal Delay[ms]: It: 10 TEC[ C]: -12 Scan2Avr: 1 Boxcar: 5 Meaning Internal/Manual Internal/Auto Choose Continuous/Valuefind or Autotest/Singlespec Serial Number of the spectrometer. This number must be correct. Name of the calibration file and its location (information must be correct). Delay of the QE65000 spectrometer Integration time of the QE65000 spectrometer in ms (delimiter is. ) Detector temperature in C Scans to average to get one spectrum Boxcar setting NOTE: Similar information is also displayed for the NIRQuest512 spectrometer for RaySphere Model Straylight correction File: E:QEB1351_EasyCorrM_.txt The name of the stray light correction file and where it is stored (both must be correct). How to Create a Configuration File Procedure 1. Create a configuration file by pressing or in the System tab of the RaySphere software. 2. Follow the wizard to save data. All settings of the actual status are taken over into the configuration file. A configuration file is in ASCII and can be edited manually. RAYSPHERE

48 6: Using Preconfigured Configuration Files 38 RAYSPHERE

49 Chapter 7 Classifying the Solar Simulator Overview and Displaying the Results RaySphere is designed for the spectral match test as described in detail in the international standard IEC For six wavelength intervals of interest, the percentage of total irradiance is specified in the table shown below: Interval Wavelength Range in nm Percentage of Total Irradiance in Wavelength Range 400 nm 1100 nm % % % % % % The solar simulator requirements for classification for the spectral match test are as follows: Classification Spectral match to all intervals specified in the table above A B C The RaySphere software displays the results from spectral match test, the spectrum in absolute irradiance mode, and the timing diagram with photocurrent in the software section Classification tab as shown in the example below. See Classification Tab for more information. RAYSPHERE

50 7: Classifying the Solar Simulator and Displaying the Results Saving Results All measured results can be saved using the -save all function ( ) in the System tab of the software. A Save wizard appears. It is recommended to enter the serial number of the tested solar simulator or anything else to identify the solar simulator by another specific notable feature. A test report is generated automatically from the data. Validating a Solar Simulator The following procedures enable you to validate a flashing or continuous light-emitting solar simulator. For best results, follow the applicable procedure and check the resulting test report (see Validating a Solar Simulator). Using RaySphere with a Flash Solar Simulator Procedure 1. Place the assembled RaySphere main body close to the test plane so that its aperture is centered in the middle of the test plane. 40 RAYSPHERE

51 7: Classifying the Solar Simulator and Displaying the Results 2. If you are using an electrical trigger signal, select the correct input level for trigger signal at the power supply and apply the signal cable to the BNC-connector on the power supply. 3. Make sure that the RaySphere software has been installed on the computer you intend to use. 4. Switch on the RaySphere power supply. Caution Always be sure to switch on the power supply before connecting the RaySphere to your computer. 5. Connect RaySphere via USB cable with your computer. 6. Start the RaySphere software. 7. Press Load Config ( ) on the System tab to load your solar simulator configuration file. 8. Wait 20 minutes for RaySphere to reach the thermal equilibrium and measure a dark spectrum again. 9. Press QE65000 ( ) and NIR ( ) in the Spectrometer tab. Use the opening dialog box for recording a dark spectrum measurement. 10. Press Start ( ) in the software interface. 11. Generate 5 single flashes with a maximum speed of 1 Hz within 3 minutes. RaySphere records the data. 12. Select Save All ( ). in the RaySphere software. Include the serial number of the flasher in the name of the file. The test report is generated automatically. Using RaySphere with a Continuous Solar Simulator Procedure 1. Switch on the solar simulator. 3. Make sure that the RaySphere software has been installed on the computer you intend to use. 4. Switch on the RaySphere power supply. RAYSPHERE

52 7: Classifying the Solar Simulator and Displaying the Results Caution Always be sure to switch on the power supply before connecting RaySphere to your computer. 5. Connect RaySphere via USB cable with your computer. 6. Start the RaySphere software. 7. Wait 20 minutes for RaySphere to reach thermal equilibrium. 8. Press Load Config ( ) on the System tab to load your solar simulator configuration file. 9. Cover the RaySphere aperture (you can use the dust protector). Take a dark spectrum measurement by pressing QE65000 ( ) and NIR ( ) in the Spectrometer tab. 10. Uncover the RaySphere aperture. 11. Place the assembled RaySphere main body close to the test plane so that its aperture is centered in the middle of the test plane. 12. Press Sample ( ) in the RaySphere software interface 5 times each second. The RaySphere records the data. 13. Select Save All ( ) in the RaySphere software. Include the serial number of the flasher in the name of the file. The test report is generated automatically. Validating the Test Results Check the following to be sure that you are collecting valid data: The RaySphere was allowed to warm up for at least 20 minutes before starting the test. No error or warning messages were received when the calibration file was loaded. The spectra recording was during the stable flash time phase. Check that all marks for Start and End of Recording in the Photocurrent graph are at a stable flash time. 42 RAYSPHERE

53 Overview Chapter 8 Test Report When all data are saved then the certificate for the solar simulator is created automatically. An example certificate is shown below. RAYSPHERE

54 8: Test Report 44 RAYSPHERE

55 Overview Chapter 9 Nonlinearity Correction and Calibration The signal from the spectrometer has to be processed for several corrections to get the highest possible precision. The most important processes are described in the following paragraphs. Nonlinearity Correction The spectrometer s signal is automatically corrected for nonlinearity by an internal algorithm. The function cannot be disabled in the RaySphere software. Wavelength Calibration The wavelength (measured in nanometers) of the spectrometer(s) in your RaySphere unit has been calibrated before leaving Ocean Optics. See the appropriate spectrometer manual (NIRQuest and/or QE65000) for more information on spectrometer wavelength calibration in Product-Related Documentation. Absolute Irradiance Calibration Absolute irradiance calibration of the RaySphere system is done in the calibration laboratory of Ocean Optics GmbH Germany. For recalibration, it is recommended that any recalibration, if necessary, be done there as well. The equipment used for calibration is listed on the Ocean Optics calibration certificate. Ocean Optics calibration light sources are traceable to NIST standards and all other equipment used is ID-traceable to NIST or German PTB standards. The spectral data use physical units of µw/cm^2/nm and the wavelength is in nanometers. Uncertainties Calculation The calculation of uncertainty is done in accordance with the IEC Guide 115 Application of uncertainty of measurement to conformity assessment activities in the electrotechnical sector. RAYSPHERE

56 9: Nonlinearity Correction, Stray Light Correction and Calibration Sources of Uncertainty The following parameters have influence on the uncertainty of calibration. Each parameter is taken into account when calculating for uncertainty. Quantity Source of Uncertainty 1. I_DC Uncertainty of DC current 2.1 T and F Influence of temperature [T] and humidity in air [F] for wavelength range 300 nm to 1100 nm 2.2 T and F Influence of temperature [T] and humidity in air [F] for wavelength range 1100 nm to 1700 nm 3.1 d Misalignment: Horizontal distance [d] from calibrated light source to entrance plane of aperture 3.2 alpha Misalignment: Tilting of the RaySphere to the light source 4. Dark Noise of dark-level [dark] 5. T_TEC Influence of sensor temperature [T_TEC] 6. Irr_Kal Uncertainty of calibration lamp 7. D_Lambda Uncertainty of wavelength calibration 8. StrayL Influence of spectrometer s internal stray light Uncertainty of DC Current The lamp manufacturer has defined the current for operating the calibration lamp. The current is monitored during calibration of RaySphere with calibrated equipment. The measurement has an uncertainty which is given the in the device s calibration documents of the power supply. Influence of Temperature and Humidity The ambient temperature during the calibration procedure may influence the uncertainty of the calibration. It is recommended by NIST to monitor temperature and humidity. The influence of humidity can be neglected for a wavelength range of 300 to 1100 nm since the atmosphere components do not a significant influence on the result. For a higher wavelength, there is a significant influence on the accuracy since water in the air has several absorption bands. The correlation of humidity and absorbance is not taken into account for calculations of uncertainty. 46 RAYSPHERE

57 Misalignments 9: Nonlinearity Correction, Stray Light Correction and Calibration The resulting uncertainties resulting from hardware misalignments are taken into account. Noise of Dark Level The dark level is the signal which is recorded if the spectrometer measures the intensity of light in an absolutely dark room. The dark signal results from the sensor s temperature and the noise of the signal follows Poisson s distribution. Influence of Sensor Temperature The sensitivity of each silicon-based sensor depends on its temperature and changes result in a significant change in sensitivity in the IR range from 700 nm to 1150 nm. The figure below illustrates the effect. Ocean Optics spectrometers have always thermalized and temperature-controlled sensors to minimize the effect of thermal instability. The confidence interval for temperature to control the detector temperature [TEC] is K. Uncertainty of Calibration Lamp The uncertainty of the calibration lamp is given by the manufacturer s calibration report for an interval of confidential of k = 2. The traceability to NIST is reported as well. Uncertainty of Wavelength Calibration Each wavelength calibration has an uncertainty which is reported in the wavelength calibration documents for spectrometers from Ocean Optics. The resulting uncertainty is estimated from statistical analysis and from typical intensity distribution of the light source. RAYSPHERE

58 9: Nonlinearity Correction, Stray Light Correction and Calibration Influence of Spectrometer s Internal Stray Light The spectrometer s internal stray light is defined as irregularly reflected light inside the spectrometer, resulting in a sensor signal. Most of the incoming light is reflected and diffracted to be measured at the detector s active surface. A small amount of light (typical 5 x 10^-5 per photon) is reflected irregularly by scattering or reflections from order sorting filters and optical elements. This light is not wavelength resolved and causes in an increased signal at the detector. Standard Uncertainties and Expanded Uncertainty for k = 2 The Expanded uncertainty for k = 2 is calculated from the above described factors and listed in the table below. Standard Uncertainties and Uncertainty Budgets Wavelength[nm] I_DC ,1 T and F Nk 3.,1 d 3.,2 alpha 4. Dark T_TEC Irr_Kal d_lambda StrayL ntia 9. LinCorr Standard Uncertainty Expanded uncertainty for k = The uncertainty resulting from stray light effects inside the RaySphere spectrometers cannot be neglected for the wavelength range of 300 nm to 350 nm. Not listed values are below 0.1 % of standard uncertainty, not known [kn] or not taken into account [ntia]. Values are round to two positions after decimal point. 48 RAYSPHERE

59 9: Nonlinearity Correction, Stray Light Correction and Calibration Calculation of Uncertainty Each wavelength calibration has an uncertainty which is reported in the wavelength calibration documents for spectrometers from Ocean Optics. The resulting uncertainty is estimated from statistical analysis and from typical intensity distribution of the light source. Uncertainty for Spectral Match Test It is difficult to extract the uncertainty for a spectral match test since no documents from national metrology institutes or an international norm have defined how to perform this calculation for the special case of a solar simulator. Nevertheless, Ocean Optics provides a procedure to estimate the uncertainty of spectral match test. Sources of Uncertainties The following sources of uncertainty for the Spectral Match test were identified. They are explained in the following sections. Quantity Source of uncertainty 1. Spec_Distr Uncertainty of Spectral Distribution. Data from RaySphere Test. 2. Dark Noise of dark-level [dark] 3. T_TEC Influence of sensor temperature [T_TEC] 4. Rep Repeatability when measuring a solar simulator. 5. StrayL Influence of spectrometer s internal stray light Uncertainty of Spectral Distribution The values for the uncertainty of spectral distribution are extracted from the data from the test of calibration at the independent optical test lab at Heraeus Noblelight. Each RaySphere system is tested with a 1000 W FEL light source calibrated by German PTB. The optical output is well defined. The uncertainties for absolute irradiance for k = 2given by the PTB (Kalibrierzeichen: PTB) are between 1.1 % at 400 nm and 1.3 % at 1100 nm. The spectrum of the calibration lamp is shown in the following graphs. The blue curve represents the output power of the used calibration lamp at Heraeus Noblelight in absolute irradiance. In an ideal case no difference between output power from the calibration lamp and measured spectrum from Raysphere is present. Nevertheless, deviations are present and can be verified. Typical data for data from 400 nm to 1050 nm and 900 nm to 1700 nm are shown in the graphs. The red curve represents deviation and belongs to the right axis. Note: The zero value for deviation is not at the wavelength axis. RAYSPHERE

60 9: Nonlinearity Correction, Stray Light Correction and Calibration The Deviation in [%] is defined as: Deviation[%]= (1 - SP_Cal/SP_Raysphere) x 100 Variables are defined as follows: SP_CAL = Spectrum from calibrated light source from Heraeus (calibrated by German PTB) SP_RaySphere = measured spectrum from RaySphere The peaks in the infrared at ~1400 nm and ~1700 nm results from water adsorption of humidity in the air. The humidity in the air at the Ocean Optics calibration lab is different than the humidity at Heraeus Noblelight during the calibration test. Uncertainty in Absolute Irradiance and Uncertainty in Spectral Distribution The spectral match test measures the spectral distribution of the solar simulator. The exact value of absolute irradiance is not of importance in principle. Since standards are available only for absolute irradiance and not for spectral distribution one has to quantify the uncertainty of spectral distribution from the spectrum in absolute irradiance. The deviation between RaySphere s data and emission spectrum from the calibration lamp at Heraeus test lab is the basis for extracting the uncertainty for spectral match test. The deviation can be described as an offset and a change in spectral distribution. The offset can be subtracted without changing the spectral distribution. An example with generated data is shown in the graph below. 50 RAYSPHERE

61 9: Nonlinearity Correction, Stray Light Correction and Calibration The change in deviation (or slope of the curve) is taken into account for estimating the uncertainty in spectral distribution. Arithmetic meanings of deviation are calculated in intervals which are defined for the spectral match test. The following are the results: Wavelength band Arithmetic average of deviation in wavelength band [%] Arithmetic average minus offset in wavelength band [%] ΔI_B_rel 400 nm nm ΔI_B_rel 500 nm nm ΔI_B_rel 600 nm nm ΔI_B_rel 700 nm nm ΔI_B_rel 800 nm nm ΔI_B_rel 900 nm nm ΔI_G_rel 400 nm nm The offset is chosen to minimize the interval of deviation. The percentage of total irradiance in a wavelength Band R_B for one wavelength band is defined as: R_B=I_B/I_G There are two measured values I_B and I_G with measurement uncertainties ΔI_B and ΔI_G. Using the equations: ΔI_B = I_B x ΔI_B_Rel and ΔI_G=I_G x ΔI_G_Rel and the formula for the Gaussian error propagation RAYSPHERE

62 9: Nonlinearity Correction, Stray Light Correction and Calibration Resulting in: The root is defined as the uncertainty of spectral distribution Spec_Dist. The values are listed below. Caption for nomenclature of variables: Variables: I: Absolute Irradiance [W/cm^2/nm] R: Percentage of total irradiance in a wavelength Band B Suffixes: _B: Wavelength band as defined for spectral match test _G: Wavelength band of 400 nm to 1100 nm _Rel: Relative value of variable Prefix: Δ: Uncertainty NOTE: Values for uncertainties of stray light are not given. For Dark and TEC, see Nonlinearity Correction and Calibration. Uncertainty of Repeated Measurements Ocean Optics has tested the uncertainty of repeated measurements together with several manufacturers of Solar simulators. The uncertainty for spectral match test can be rated to be lower than 0.02 % for each spectral band. Quantitative Uncertainties The following quantitative values for uncertainties can be found when the above described sources of uncertainty are taken into account. 52 RAYSPHERE

63 9: Nonlinearity Correction, Stray Light Correction and Calibration Wavelength range 400 nm 500 nm 500 nm 600 nm 600 nm 700 nm 700 nm 800 nm 800 nm 900 nm 900 nm 1100 nm 1. Spec_Distr [%] ,1 Dark [%] ,1 T_TEC [%] ,2 StrayL [%] ntia Standard Uncertainty [%] Expanded Uncertainty [%] for k = A missing value indicates that the value is less than 0.1 % or not known. How to Estimate the Uncertainties for the Spectral Match Test An example illustrates the procedure for a measurement with a solar simulator. The following spectrum is recorded. RaySphere calculated the percentage of total irradiance in the wavelength range of 400 nm to1100 nm. RAYSPHERE

64 9: Nonlinearity Correction, Stray Light Correction and Calibration Wavelength range [nm] Percentage of total irradiance in the wavelength range of nm With uncertainty 400 nm nm nm nm nm nm nm nm nm nm nm nm The standard uncertainties for this test can be calculated using the formula: ΔR_B = R_B x Standard uncertainty for k = RAYSPHERE

65 Overview Appendix A Components Technical Notes This appendix contains technical notes for the RaySphere components. QE65000 Spectrometer A QE65000 spectrometer is mounted inside the RaySphere main body. See the QE65000 documentation for more information (see Product-Related Documentation). NIRQuest Spectrometer The RaySphere1700 has a NirQuest512 spectrometer mounted inside the main body. See the NIRQuest documentation for more information (see Product-Related Documentation). Trigger Electronics The trigger electronics is a newly developed unit to fulfill the requirements for validating solar simulators. The unit has a USB connection for communication. Other parts are the following: Photodiode Analog comparator for detecting flash events Cpld-Microprocessor for logical operations like delays and triggering Atmel-chip for PC communication The trigger electronics is a standalone unit. All values for triggering are stored in the onboard FPGA. This offers an extended range of use in combination with the SpectraSuite spectrometer operating software. Trigger parameters can be set in the Photocurrent/Trigger Settings dialog box. See Changing Photocurrent and Trigger Settings for more information. The parameters that need to be defined are: Delay for QE65000 Delay for NirQ512 RAYSPHERE

66 A: Algorithms Used Amplification. Settings for GainX and value of 1 to 10. Trigger source When these parameters are set, the values are saved inside the electronics until the electronics loses electrical power. To preserve the parameters do not disconnect the USB connection or switch off the electrical power. Close the RaySphere software and start the SpectraSuite software. The spectrometers can be operated now with SpectraSuite and all functions which are provided by SpectraSuite can be used. Set the spectrometer into Hardware Trigger mode in SpectraSuite to use external triggering or triggering by flash. See the SpectraSuite Spectrometer Operating Software Installation and Operation Manual for more information on SpectraSuite (see Product-Related Documentation). USB-Hub An internal USB hub inside the RaySphere main body controls the communication with trigger electronics, QE65000 spectrometer and NirQuest512, and bundles the communication into one USB output that is connected with your computer. 56 RAYSPHERE

67 Appendix B Specifications and Mechanical Diagram Specification Value Physical: Dimensions (l x w x h) Weight RaySphere RaySphere 1700 Slit size QE65000 NIRQuest Maximum Integration Time with RaySphere Software Measurement Speed Second Order Filters 30.7 cm x 23.5 cm x 6.6 cm 4.2 kg (main body) 5.7 kg (main body) 25µm 200µm 170 ms 1 set of spectra per second installed Electrical: Input voltages Input frequency Power Overvoltage protection Fuse Trigger connection VAC Hz 75 W % of main output M1.6 A BNC connector Connector: SMA 905 RAYSPHERE

68 B: Specifications and Mechanical Diagram Specification Value Optical: Optical input power 150 W to 2000 W Wavelength range*: RaySphere RaySphere nm 300 nm 1700 nm Optical Trigger: Trigger delay ms Time resolution 0.87 µs Jitter 150 ns Internal time resolution 2.54 µs Maximum sample time 160 ms Electrical Trigger: Electrical trigger type High level Edge trigger 5 V to 24 V Minimum high time 100 ns Mounting Options for RaySphere Main Body The technical drawing shows the back side of the RaySphere main body. The system can be mounted at the indicated M6 rods only. Do not bend the system for tight mounting! WARNINGS Mounting on uneven surfaces may bend the RaySphere system. This may cause increased measurement uncertainties. 58 RAYSPHERE

69 B: Specifications and Mechanical Diagram RAYSPHERE