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1. The OCR is calculated in Kepler by dividing the total number of good events by the real time for the run 4 6 5 Dead Time Percentage The dead time is a measure of the fraction of time when the module was not sensitive to input data displayed in percent and has three sources At significant count rates dead time is dominated by the time required to measure the energies of the pulses a minimum of twice the peaking time plus the gap time per pulse see sections 4 1 1 and 4 1 2 The other sources are the recovery time required per preamplifier reset see 3 3 3 and times the module s processor must spend on minor housekeeping functions Because of the latter two terms there will always be a small amount of dead time even when the input count rate is very small and the peaking times is small as well Kepler calculates the dead time percentage as 1 ICR OCR 100 Page 19 Manual Kepler Software Package mdo Kepler MAN 001 1 preliminary 4 7 Unavailable functions while a run is active While a data acquisition run is active there are numerous functions that are locked out since they would interfere with the proper operation of the module The functions listed below either will not respond while the run is active or their button menu items will be grayed out indicating that they are unavailable All items under Saturn Acquisition Settings All items under Saturn Detector Settings All items under Saturn Baseline Settings
2. mdo Kepler MAN 001 1 preliminary 0 6 Calibrating er 30 6 7 Saving and Loading Specia esor ieri E 30 6 8 PrintinG Speci d essione aa E EA 31 7 Diagnostic Tools Available for the Saturn ss usssssunseunnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnn 32 7 1 Oscilloscope and Fast Fourier Transform FEIT 32 7 2 Baseline History and Histogram esssesssseeeessrreerinnesnennasernneeennnesninnessennnaaennn 34 8 CAAVanGed KT 36 8 1 DSP Paramete Edtor a a E a e aa 36 g2 Handel Emor AO Ae eege ege e ae ee ea ede ee ata 37 Ap EU UE 39 Appendix 1 GIOSSALY EEN 39 Appendix 2 Command Short Cuts cecccsecceceeeeeeeceeeeeeeeeeeeeeeeeeeneeeeeeeeeeeeeeeees 39 Appendix 3 EPP Port Requirements ssnnnsnseneeseenrnnnseeseennrrnrennstnnntnnnnnnereene nnn 40 Appendix 4 Common Problems cece eeeeeeceeeeeeeeeeeseeseceaaeeeeeeeteeeeas 40 Appendix 5 Index icnis aided daia ahaa ee oases Gees 40 Page ii Manual Kepler Software Package mdo Kepler MAN 001 1 preliminary End Users License Agreement NOTICE TO USER THIS IS A CONTRACT PLEASE READ IT CAREFULLY BY INSTALLING THIS SOFTWARE OR DOWNLOADING THE ASSOCIATED INSTALLATION FILE YOU ACCEPT ALL OF THE TERMS AND CONDITIONS OF THIS AGREEMENT IF YOU DO NOT AGREE WITH THE TERMS AND CONDITIONS OF THIS AGREEMENT YOU WILL NOT BE ABLE TO USE THE SOFTWARE REGARDLESS OF HOW YOU ACQUIRE THE SOFTWARE ELECTRONICALLY PRELOADED ON MEDIA OR OTHERWISE BY USING IT YOU AGREE TO THE TERMS OF THI
3. Saturn Run Control Peaking Time Saturn Run ControbRun Time Saturn Run Control Run to Saturn Run Control Clear Spectrum at Run Start or its alternate value of Saturn Run ControbRetain Spectrum at Run Start e Diagnostics Oscilloscope Acquire Trace or the button Acquire Trace on the Oscilloscope window e Writing any DSP parameters in the DSP Parameters window e Calibrate button in the ROI region of the Kepler window Some functions are not available when the run is active Kepler will not let you change things that will affect data taking that is in progress 5 6 2003 Page 20 Manual Kepler Software Package mdo Kepler MAN 001 1 preliminary 5 Graph usage in Kepler Cursor 2 61111 Events 5790 0 ERD d 53051 0 Cursor Statistics Mini Zoom Window ROI Cursor Events Counts Zoom Center Crass Hair Cursor I D 1 1 I D 1 1 I D I I I D I 1 I 500 1000 1500 2000 2500 3000 3500 4000 4500 5000 5500 6000 6500 7000 7500 8000 8500 Energy eV Figure 5 A typical spectrum with important controls labeled The controls are discussed in detail in the text All graphs within Kepler have the same zooming panning scaling and data presentation tools A typical spectrum graph view is shown in Figure 5 please refer to it as you read the section in Chapter 5 All graphs in Kepler also mhe conmo limenu thar have the ability to save and overlay references from memory allowing eas
4. no data taking run is active Note this is a red indicator that is not indicating a problem with the system Page 7 Manual Kepler Software Package mdo Kepler MAN 001 1 preliminary e Save File if green displays the last either saved or loaded hardware configuration file INI if red indicates that the current configuration has never been saved or loaded e GUI Save File if green indicates that the Kepler GUI configuration window placement etc has been saved and the name of the file is displayed if red then the GUI configuration has never been saved 2 9 Menus 5 6 2003 There are drop down menus at the top of the Kepler window for most operations When in doubt on how to perform a particular action check the menus at the top of the Kepler window Manual Kepler Software Package mdo Kepler MAN 001 1 preliminary 3 Configurations Saving Loading and Restarting 3 1 INI files The standard file used to maintain hardware configurations for Kepler INI files save the is called the INI file This file contains all settings relevant to data taking setup hardware configuration and all firmware pointers for the XIA module The INI file is read and written of the module using the Handel library and the format is beyond the scope of this document All settings contained in this file are accessible via Handel and you should never need to modify the file directly For more information about INI fil
5. or Manual Kepler Software Package mdo Kepler MAN 001 1 preliminary Kepler Application Notes Kepler Quickstart Guide Handel Guide 1 3 Hardware Requirements 1 3 1 Supported Spectroscopy Modules 1 3 1 1 Saturn X ray Spectrometer Kepler supports the XIA Saturn digital x ray processor in both its reset and RC feedback preamplifier designs The host computer running Kepler should have only a single Saturn connected at any time 1 3 1 2 Polaris Gamma ray Spectrometer Kepler will support the XIA Polaris digital y ray processor soon Please check XIA s website for release information 1 3 2 System Requirements The host computer that runs Kepler must have the following minimum capabilities e 300 MHz or greater processor speed running most Microsoft Windows Operating systems 95 98 Me 2000 NT XP e Enhanced Parallel Port EPP capabilities This must be confirmed and set in the BIOS settings of the computer Anything but full EPP support will not be sufficient to control the Saturn module Note most computers support EPP but may not have their BIOS settings configured for the operation booting to the BIOS and double checking this setting is important e XIA recommends an EPP certified cable Most EPP cables have been found to work but we only guarantee operation with an EPP certified cable obtainable from XIA or most computer stores 1 4 Support By Mail Attn Support X ray Instrumentation Associates
6. read write parameters In order to edit a parameter simply click on the number to the right of the parameter name change the value and press the lt Return gt key It is imperative that the lt Return gt key is pressed or the value will revert to its previous value change is canceled The keyboard arrow keys can be used to navigate around the DSP parameter list 8 1 3 Saving Save Params To save the DSP parameters and values to a file press the Save Params button and choose a filename and location The file is stored in a simple name value text format To assist in debugging of some problems XIA personnel use these files as system snapshots 8 2 Handel Error File The main location of the Handel error file is stored in the windows registry and is accessible from the panel accessed with the Tools Options menu item 5 6 2003 Tools Hardware Errors lt Ctr1 F8 gt Saturn Advanced Hardware Errors All communication with the XIA modules is facilitated through a C software library called Handel For debugging purposes Kepler provides an interface to Handel s error reporting routines shown in Figure 10 Hopefully this will never be used but there may be cases where the error file produced by Handel should be sent to XIA to aid in diagnosing problems The on screen display of the error file can be updated at any time using the Read button located on the Error Reporting window 8 2 1 Enabling Output The Han
7. time Please review the hardware manual if this is a concern ICR is the rate of events detected by the trigger algorithm OCR is the rate of events added to the spectrum Dead time percentage is the fraction of time the module is not sensitive to incoming events 5 6 2003 4 6 1 Real Time The real time is the total time elapsed during a data acquisition run 4 6 2 Live Time The live time is the total time that the module was sensitive to incoming pulses The live time will always be less than the real time and depends on many factors the interplay between input count rate and peaking time being the dominant effect Please read the hardware manual for more details about how your module measures live time 4 6 3 Input Count Rate ICR The input count rate is the rate of events being detected by the module s trigger algorithm Each time the trigger algorithm in the module detects an event the total number of input counts for the run is incremented The ICR is calculated in Kepler by dividing the total number of input counts by the live time 4 6 4 Output Count Rate OCR The output count rate is the rate of good non piled up events being detected by the module These events may either be written into the spectrum memory or counted as overflows and underflows if their reconstructed energies lie outside of the spectrum limits as determined by the number of histogram bins 4 1 4 and the spectrum bin width 4 1 3
8. 8450 Central Ave Newark CA 94560 USA By e mail software _support xia com By phone 510 494 9020 5 6 2003 Page 3 Manual Kepler Software Package mdo Kepler MAN 001 1 preliminary 2 General Kepler 2 1 Installation Valid for Windows 95 98 ME NT XP and 2000 1 Insert the CD into the CD ROM drive If the installation does not start automatically follow steps 2 amp 3 2 Click the Start button and select the Run command 3 Type X Setup exe and click OK Remember to replace the X with the proper drive letter for the CD player on your computer 4 Enter the information as requested to indicate where to install KEPLER or click OK to accept the defaults The Default stores the Handel DLLs in the C Windows System C Winnt System32 for NT based operating systems folder and the Kepler software in C Program Files XIA Kepler When returned to the Desktop the installation is complete 2 2 Getting Around Kepler Cursor statistics are only shown when a cursor is active on a graph The action performed by a left click of the mouse is determined by the default mode shown on the far left of the graph display bar 5 6 2003 Getting around Kepler requires basic knowledge of the Windows operating environment If you are unfamiliar with any of the following terminology i e clicking and drop down list box refer to your Windows manual for more details 2 2 1 Selecting Items and Moving Around
9. MAN 001 1 preliminary 4 Taking Data with Kepler 4 1 Acquisition Values Egy Acquisition Settings V Peaking Time 16 0 us V Gap Time 0 15 us Actual 2 4 us Y Spectrum Bins 2048 Y Spectrum Bin Width 10 0 eV V Trigger Threshold 1008 3 eV V Energy Threshold is Disabled The general acquisition settings section of the DAQExplorer H d Baseline Settings V Baseline Cutis Enabled V Baseline Cut 5 0 V Baseline Filter Length 0 The baseline settings section of the DAQExplorer Peaking and gap time are Digital filter parameters used by all XIA modules the peaking time is approximately equal to twice the shaping time of an analog amplifier while the gap time is analogous to a rise time setting 5 6 2003 The values discussed in this section directly affect the data acquired with the XIA module The hardware manual for the specific XIA module you are using should be referenced for detailed descriptions of these values The information provided here is only intended as a refresher or brief introduction Within Kepler the values can be modified from the two DAQExplorer sections shown in the sidebar to the left 4 1 1 Saturn Acquisition Settings Peaking Time Saturn Run Controlb Peaking Time Peaking Time In order to determine the energy of pulses from the preamplifier the spectroscopy module time averages the pulses using a trapezoidal shaping filter that is characterized by a peaking
10. ROIs are not visible at the bottom of the Kepler window locate the separator bar near the bottom of the window and drag it higher Click the left column in the ROI data table to make a different ROI active Please refer to 6 2 for general information regarding regions of interest ROIs 5 6 2003 6 2 1 ROI Data Table Region of interest data are displayed in a table just below the spectrum graph in the Kepler window see Figure 6 Each ROI occupies a single row in the table and each column in the table shows different information about the ROI Note if the ROI table is not visible the separator that divides the window between the spectrum display and the ROI table is set too low find the separator near the bottom of the screen below the spectrum and drag it higher All bold characters in the first row and the letters ACT in the first column identify the currently active ROI 6 2 2 Adding and Deleting ROIs Manually Add ROT Delete ROT A new ROI can be added to the table by clicking the Add ROT button which adds a row to the bottom of the ROI data table and makes the new ROI the active one Likewise the active ROI can be removed by clicking the Delete ROT button If there is no active ROI the delete operation cannot be performed To select a new active ROI click on the far left column of the desired ROI row in the ROI data table and that row will become the active ROI 6 2 3 Adding ROIs with the A
11. Time 34 Save FFT 34 Save Oscilloscope 34 Preamplifier Decay Time 10 Gain 9 Parameters 9 Polarity 9 RC Feedback Type 10 Reset Interval 10 Reset Type 10 Type 10 Printing Baseline Histogram 37 Baseline History 37 FFT 35 Oscilloscope 35 Spectrum 32 Reference Data Sets Copy from Graph 25 Copying To 25 Displaying 25 Modify Display 26 Removing 26 5 6 2003 mdo Kepler MAN 001 1 preliminary Saving Loading Files 26 Scaling before Displaying 26 Related Manuals 2 ROIs Active ROI 29 Adding 28 Adding Automatically 28 AutoROI Function 28 Bounds 30 Color 29 Data Table 28 Deleting 28 Desired Peak Position 30 Display Parameters 29 FWHM 30 Locking 30 Mean 30 Moving ROI Boundaries 29 Name 31 OCR 30 Visibility 30 Runs Dead Time 20 ICR 19 Input Count Rate 19 Live Time 19 OCR 19 Output Count Rate 19 Preset Run Types 18 Preset Stop Value 18 Real Time 19 Resuming 17 Run Events 18 Run Time 18 Run Times 17 Run Types 17 Starting 16 Stopping 16 Stopping Accuracy 18 Unavailable Functions 20 Update Interval 17 User Intervention 18 Save Files FFT 34 Histogram 36 History 36 INI Files 9 Kepler 6 Oscilloscope 34 Reference Data Sets 26 Saving DSP Parameters 39 Spectrum 31 Selecting Items Fields 4 Settings 13 ADC Percent Rule 15 Baseline Cut 14 Manual Kepler Software Package Baseline Filter Length 14 Bin Width 13 Calibration Energy 15 Dec
12. Windows DAQExplorer This area is located to the left of the main Kepler window and provides the main way to navigate through the Kepler application To access more items click the small sign to expand a feature heading and display more options Click the small sign to reverse the process Display Controls This area is located on either the lower or upper edge of all graphs within Kepler and determines the default behavior of the graph window Settings in this region determine the functionality of the mouse in the display region and how to represent the graph The right hand side of the display bar provides cursor statistics when they are active Menu Bar The menu bar provides a secondary access point to most major functions and windows within Kepler The various windows and functions of Kepler can be selected in three different ways Hot Keys Each menu menu selection function and most fields contain a hot letter a letter in the word that is underlined To access menus functions and fields press and hold the Alt key and then press the item s Hot Key To access menu items simply press the Hot Key Manual Kepler Software Package mdo Kepler MAN 001 1 preliminary Mouse Single clicking on any menu menu selection or function will give you access to that item In addition single clicking in any window field will select that field for editing Keyboard To select a menu press ALT and use the left an
13. Zoom then click amp drag 2 Resize the white box in the mini zoom window 5 6 2003 There are two main methods to zooming in on a feature of the graph The first method of zooming uses the main graph display and the mouse to directly expand the view The second zooming method utilizes a small inset window that is called the mini zoom window located in the upper right corner of all graph displays This window shows the full graph area with an inset white box that shows the current view area being displayed by the main graph Changing the size and location of the white box within the mini zoom window produces zooming and panning in the main graph window Both methods are described in the following sections At any time the view of the full graph can be returned by either lt Ctrl A gt or using the right click menu option within the graph Full Scale Restoration of the full graph display is a very useful way to return to reality if you have zoomed into a small region and forget where you are in the full graph display However unlikely should a bug in the Kepler program make it impossible to continue zooming or panning using Full Scale will restore the graph display to normality 5 2 1 Main Window Zooming The following description applies when the graph is set to Zoom as the default mode or when the zoom hotkey is pressed set in the Options window at the same time as the left mouse button The most co
14. can be printed separately to the default printer A window will open asking for information regarding the conditions under which these data were taken which will also be printed Page 35 mdo Kepler MAN 001 1 preliminary Manual Kepler Software Package 8 Advanced Tools 8 1 DSP Parameter Editor Tools DSP Parameters lt Ctrl F6 gt Saturn Advanced DSP All XIA modules contain a DSP at the heart of their operation and Kepler provides an interface for directly editing exposed DSP s parameters shown in Figure 9 It can not be stressed strongly enough that the results of such changes can produce unforeseen results and should only be undertaken by experts or under direction from XIA personnel To refresh the values displayed doing in the DSP Parameters window to match the values on the module simply press the Read Params button Warning Changing these parameters is really risky if you don t know what you are 4 DSP Parameters Miel ES Decimal DI Name ASCTIMEOUT BASEBINNING BASECNTDWN BASEEVTSO BASEEVTS1 BASELEN BASEMEAND BASEMEAN1 BASESTART BASETHRESH BINFACT1 BLCUT BLFILTER BLFILTERF CODEREV CONTINUE DECIMATION DELTAFINT DIAGMODE DISABLEEVT ERRINFO EVTBLEN EVTBSTART EVTSINRUNO EVTSINRUN1 FASTGAP FASTLEN FASTPEAKSO FASTPEAKS1 FIPCONTROL FIPPIREV FIPPIVAR GAINDAC HDWRVAR HIGHGAIN HSTLEN HSTSTART INPUTENABLE LIVETIMEO LIVETIME1 LIVETIME2 MAXWIDTH MCALIMHI MC
15. energy see the hardware manual for more details on this process It is important to watch for a noise peak appearing at very low energies if the noise peak is too big comparable to any peak of interest then the threshold should be raised till the noise peak is either small or entirely gone 4 1 6 Energy Threshold Saturn Acquisition Settings Energy Threshold The energy threshold is used for detecting very low energy X rays Similar to the trigger threshold this threshold enables the measurement of the energy of the pulse from the detector but operates with much lower noise X rays with energies below 200 eV can be analyzed with the proper detector setup and configuration of the Saturn module 4 1 7 Baseline Cut Saturn Baseline Settings Baseline Cut In order to properly measure the energy of a pulse from the detector the module continuously tracks the baseline value of the preamplifier output The module allows a cut to be applied that determines if a baseline is good enough to contribute to the average baseline or an outlier to be excluded see the hardware manual for more details This cut is determined by moving out along the tails of the baseline histogram see 7 2 until the histogram is down a percentage from its peak The percentage used in this method is set by the baseline cut value in Kepler This cut can also be enabled and disabled using Saturn Baseline Settings Baseline Cut is 4 1 8 Baseline Filt
16. hardware manual 3 3 5 Decay Time Saturn Run Control Decay Time When using a preamplifier of the RC feedback type the signal generated by the preamplifier rises by some amount dependent on the incident energy then slowly decays exponentially with a RC time constant set by the value of the resistor in parallel with the preamplifier s charge integrating capacitor The RC decay time of this resistor capacitor combination determines how quickly the signal from the preamplifier will return to its baseline value In order to perform ballistic deficit corrections the module must know this parameter The accuracy of setting this parameter can drastically affect the energy resolution of some detector setups Please review this concept in the hardware manual if it is new to you 3 4 Troubleshooting problems setting the initial gain 3 5 Configuration methods K There are two ways to configure a system using Kepler either load an INI file or enter the information regarding configuration individually Once you have an INI file you can load it and the settings will be applied to the hardware module The other option is to enter all the necessary information into a configuration panel and have Kepler apply the information to the module The easiest method is to use the INI files that are distributed by XIA and bootstrap your way to the correct settings using the functions described in 3 3 and 4 1 As changes are made to the set
17. is set in the DAQExplorer through the entry Saturn Run Control Run Time while the event based stop condition is set in the DAQExplorer entry Saturn Run ControlRun Events 4 5 2 2 The Four Preset Modes The four preset modes are e Preset Real Time run until a preset real time expires Please see 4 6 1 for an explanation of real time in this context e Preset Live Time run until a preset live time expires Please see 4 6 2 for an explanation of live time in this context e Preset Input Counts run until a preset number of input counts are acquired Please see 4 6 3 for an explanation of input counts e Preset Output Counts run until a preset number of output counts are acquired Please see 4 6 4 for an explanation of output counts 4 5 2 3 Stop Accuracy Because of the design of XIA s spectroscopy modules Kepler cannot stop runs with perfect precision Time stopped runs may exceed the desired run time by up to 1 6 ms while event stopped runs may exceed the requested number of events by up to 1 6 ms times the event rate where the event rate is ICR or OCR depending on the run type In all cases Kepler will detect that the run is over as soon as the next auto update time expires and will change its status accordingly just as if you had hit the stop run button If more accurate sub microsecond stop times are required this can be achieved using the module s external Gate input Please contact XIA
18. the column will toggle its display between the two means 6 4 3 ROI FWHM The full width at half maximum FWHM of the data within the ROI is displayed in the column labeled either Gau FWHM or Gau FWHM In both cases the FWHM is found from a simple Gaussian fit to the data within the ROI Gau FWHM displays the absolute FWHM while Gau FWHM displays the FWHM as a percentage of the Gaussian mean Left clicking anywhere in the column will toggle the display between the two values 6 4 4 ROI OCR The OCR for each ROI is displayed in the column labeled OCR see 4 6 4 for general information about OCR The displayed OCR is the number of events in the ROI divided by the real time 6 5 Other ROI Data Meaningful names for the ROIs can make it easy to reference them later in other parts of Kepler 5 6 2003 6 5 1 Desired Peak Position Typically a ROI covers a single peak in a spectrum whose energy has a known value The column labeled Desired stores this energy value which can be used to calibrate the energy of the spectrum as discussed in 6 6 6 5 2 ROI Name Each ROI can be given a name as a reminder of what it subtends in the spectrum For example the Ka peak of Fe might be given the name Fe55 Ka This name is also used when scaling reference sets for display in the spectrum see 5 7 3 Page 29 Manual Kepler Software Package mdo Kepler MAN 001 1 preliminary 6 6 Calibrating peaks Filling in desired
19. time and a gap time The filter s peaking time determines the amount of averaging performed when determining the energy of a signal from the detector Setting the peaking time to larger values typically will improve your energy resolution up to a point However longer peaking times also increase dead times directly reducing the maximum count rates at which you can effectively acquire data This trade off is important but beyond the scope of this document Peaking time is probably the single most important quantity for most applications so please review the description provided in your XIA hardware manual if you need to learn more 4 1 2 Gap Time Saturn Acquisition Settings Gap Time The trapezoidal filter s gap time allows the filter to be insensitive to the risetime characteristics of the preamplifier output pulses The gap time should therefore always be set larger than the longest rise time of the pulses from the detector preamplifier In principle the gap time should be barely larger 50 ns than the maximum rise time to maximize the throughput of data into a spectrum Because of limitations of the firmware on XIA modules it is not always possible to set the gap time exactly to the desired value depending on the peaking time setting Kepler will always remember your desired value and attempt to set that value each time the peaking time is changed Kepler will also report the value that is actually set on the module labeled as Act
20. upper right and lower left corner mdo Kepler MAN 001 1 preliminary the main window shows the full scale view the white box will be nearly invisible on the edge of the mini zoom window When the box is selected two cursors will appear on the lower left and upper right edges of the box which can be dragged to resize it Since the area within the box corresponds to the display in the main graph this has the effect of zooming in the main graph To make it easier to adjust the zoom double clicking on the mini zoom window greatly expands the window size double clicking again will return the mini zoom window to its original size 5 3 Panning The four panning methods 1 Double click and hold 2 Single click in Pan mode 3 Drag an axis and 4 Drag the white area in the mini zoom window There are four methods to pan around the graph 1 Double click the left mouse button and hold on the 2 click Then drag the mouse and the graph will follow the mouse location 2 Set the default mode to Pan and then proceed to single click on whichever point you want centered within the graph window This form of panning will not allow you to move beyond the boundaries of the data currently contained in the graph 3 Each of the axes can be dragged with the mouse When the mouse moves over an axis the pointer will turn to a hand While the left mouse is pressed the axis will follow the mouse 4 The wh
21. with creating ROIs as defined in Tools Options then click and drag the mouse over the desired region on the spectrum Once the limits have been initially set the methods listed here can still be used to change the settings at a later time 3 Ifthe active ROI has limits a pair of cursors will bracket it in the spectrum window The mouse can be used to drag each cursor independently to a new position the mouse pointer changes to a left right arrow when this action can be performed Alternatively you can single click a cursor to select it it will change its color to white and then use the left and right keyboard arrow keys to move the ROI boundary in single bin steps Direct editing of the lower and upper bounds in the ROI table is not currently possible but will provide a fourth method in the next release of Kepler 6 3 Region of Interest Display Parameters For visible and locked status the background color of the column can be a quick indicator Green is unlocked or visible Red is locked or invisible 5 6 2003 Several columns in the ROI data table affect the display of the ROI in the spectrum graph 6 3 1 Active ROI The column on the far left labeled with ROD of the ROI table displays the characters ACT in the row of the ROI that is currently active This row is also displayed with the bold typeface 6 3 2 Color Both the Active ROT and Color columns 2 from left always match the color used t
22. ALIMLO MINWIDTH NEGTDACSTEP NUMASCINTO NUMASCINT1 NUMDRDOSO NUMDRDOS1 NUMDRUPSO NUMDRUPS1 NUMRESETSO NUMRESETS1 NUMUPSETSO NUMUPSETS1 POSTDACSTEP PRESET PRESETLENO PRESETLEN PROGNUM RCALLEN RCALSTART REALTIMEO REALTIME REALTIME2 REDTHR RESETBASE RESETINT RESETWAIT RUNERROR RUNIDENT RUNTASKS SGRANULAR SLOPEDAC SLOPEFACT SLOPEFACTE SLOPEMLT SLOPEMLTE LG el Ellen e e ellene B Walaisa elei BR SLOWTHRESH SLPGAINFACT SLPGAINFACTE SPECTLEN SPECTSTART SYSMICROSEC TCALLEN TCALSTART TDACOFFSET TDACPERADC TDACPERADCE TOACSTEP TDACWIDTH TDQPERADC TOQPERSDCE TESTUPON THRESHFACT THRESHFACTE THRESHOLD TPBANK TRACE WAIT TRKDACVAL UNDRFLOWSO UNDRFLOWS1 USERI USER2 WHICHTEST YELLOWTHR Figure 9 The DSP parameter editor Only experts should access this window since arbitrarily changing DSP parameters can lead to unforeseen behavior of the module 5 6 2003 Manual Kepler Software Package Red Read Only Green Read Write Use arrow keys to quickly navigate the DSP parameter list mdo Kepler MAN 001 1 preliminary 8 1 1 Numeric Base Display The numeric base for displaying the DSP parameters can be changed from decimal to hexadecimal using a drop down list box located at the top of the DSP Parameters window 8 1 2 Editing Parameters DSP parameters come in two flavors read only displayed in red and read write displayed in green As the names imply Kepler can only modify
23. BUG x10p_pstl c line 2907 psIDoADCTrace Actual tracewait 500 000000 DEBUG x10p_psl c line 2914 psIDoADCTrace Preparing to wait waitTime 0 004000 DEBUG x10p_psl c line 2918 psIDoADCT race Finished waiting DEBUG x10p_psl c line 2919 psIDoADCT race Preparing to poll board DEBUG s10p c line 3103 dxp_control_task_data type CT_DXPX10P_BASELINE_HIST DEBUG Up e line 2969 dxp_end_control_task runtasks Ox47b DEBUG x10p_psl c line 2856 psIDoADCTrace dinfo 1 500 000000 DEBUG x10p_psl c line 2874 psIDoADCTrace tracewait 500 000000 clockTick 50 000000 minTracewait 100 000000 DEBUG x10p_psl c line 2889 psIDoADCTrace Setting TRACE WAIT to 8 DEBUG xerxes c line 4867 dxp_start_control_task Entering dxp_start_control_task ISEMI AO x Figure 10 The error reporting window in Kepler This window echoes Handel errors within Kepler Experts interpret the output displayed in this window to debug the performance of Kepler 5 6 2003 Page 38 Manual Kepler Software Package mdo Kepler MAN 001 1 preliminary Appendices Appendix 1 Glossary DAQExplorer refers to the tree of information and options along the left side of the Kepler main window module refers to an XIA spectroscopy module host computer refers to the computer on which Kepler is running Saturn The XIA digital x ray processor module Polaris The XIA digital y ray processor mod
24. F R 2 101 consisting of Commercial Computer Software and Commercial Computer Software Documentation as such terms are used in 48 C F R 12 212 or 48 C F R 227 7202 as applicable Consistent with 48 C F R 12 212 or 48 C F R 227 7202 1 through 227 7202 4 as applicable the Commercial Computer Software and Commercial Computer Software Documentation are being licensed to U S Government end users A only as Commercial Items and B with only those rights as are granted to all other end users pursuant to the terms and conditions herein Unpublished rights reserved under the copyright laws of the United States XIA 8450 Central Ave Newark CA 94560 8 Verification of Compliance with Licenses If you are a business or organization you agree that upon request of XIA or XIA s authorized representative you will within thirty 30 days fully document and certify that your use of any and all XIA software at the time of the request is in conformity with your valid licenses from XIA 9 Sample Programs The Software may contain sample programs that are furnished by XIA as examples These examples have not been thoroughly tested under all conditions XIA therefore cannot guarantee or imply reliability serviceability or function of these sample programs You may copy modify and distribute these sample programs in any form without payment to XIA for the purposes of developing using marketing and distributing application programs conformi
25. INI files e Save your interface setup e Transparent operation from one session to another 2 acquire data using the module and 3 party detector and e User settable run times 4 different stop conditions controlled by the module e Dynamic control of runs you can start and stop runs at will e Display data as it is acquired by the module at settable rates e Resume previous runs without losing spectrum data 3 analyze spectrum data Scale energy measurement to match known spectral lines Dynamic regions of interest ROT controls Gaussian fits to ROIs Panning and zooming to examine spectrum features Linear and logarithmic displays Save and load spectra 4 diagnose problems with any detector setup e Digital oscilloscope and fast fourier transform FFT mode e Track baseline measurements e Directly edit DSP variables running on the module e Monitor and control the error reporting between the host computer and the module Kepler allows you to configure a module using either built in panels or configuration INI files There are multiple built in tools that aid you in debugging both detector and the module problems You can acquire data from the module in one of several modes both fixed length and indeterminate runs are supported Once a spectrum has been acquired with the XIA module Kepler allows you to perform some simple analysis on the spectrum e g peak fitting ROIs 5 6 2003 Page 1 Manual Kepler Software Package mdo Kepler MA
26. Manual Kepler Software Package mdo Kepler MAN 001 1 preliminary End Users License Agreement ceeceeceeeceeeeeseeeceeeeeeeesensceaeeeseeeseseeesnaeeeseeesneeeeeees iii 1 Jottrodueton deefe SEENEN acc te ts a nde cei ented eh Ee Ee NEE 1 1 1 Manual Conventions ccccccceeeeeeeeeeecaeceeeeeeeeecacaeeeeeeeeeseccueaeeeeeeeseeessiaaeees 2 1 2 Related documentation 2 1 3 Hardware Heouirements testrenn nn 3 E STEEN 3 2 General Kepler aeaeaie aaaea eaaa ain ane iaaa aana daaa Veecdetesdadestesedduertes 4 El E UE Le nseni ia ae gel een i leis ae eres 4 2 2 Getting Around Kepler u 0s 2cceci sete ete ete eve cies eb eee et enn 4 2 3 Hardware Setup EE 5 2 4 Starting and Stopping Rene 5 2 5 Kepler Save ies 6 2 6 ToolS Options SettingS sea ae aee REEERE EEEE EA AER T EAEAN 7 SC Help DIET E NAEP E EA E ETE T EE A ETE dees 7 PEE ADT EE A A A A E E E E E et E 7 E WEE 8 3 Configurations Saving Loading and Restarting ccccesseeeeseseeeeeeeseeneeeeseenes 9 3T UN TEE 9 3 2 Firmware Definition Database FDD les 9 3 3 Preamplifier Parameters ccceccccecceceeeeeeeceeceeeeeeeeeesecseeaeceeeeeeesensncaneeeeeneees 9 3 4 Troubleshooting problems setting the initial gain cceeeeeteeeeeeeeees 10 3 5 Configuration methods nentrn tnn nenene ent 10 A Taking Data with Kepler ccccseseeecesseneeeeeeeeeeeeseeeeeenseeneeeeeessneesessseeeeesesenenseeeees 13 4 1 Acquisition Valles isiro pok
27. N 001 1 preliminary 1 1 Manual Conventions Convention Description Example The symbol leads you through nested menu items The sequence DAQExplorer items and dialog box options File Page Setup Options directs you to pull down the File menu select the Page Setup item and choose Options from the sub menu item Bold Bold text denotes items that you must select or click Saturn Run Controlb Auto Update on in the software such as menu items and dialog this doesn t seem to be clickable per se box options Bold text also denotes parameter names indicates the entry starting with Auto Update in the Run Control section of the Saturn section of the DAQExplorer Bold Bold text within denotes a command button Start Run indicates the command button labeled Start Run monospace Items in this font denote text or characters that you Setup exe refers to a file called enter from the keyboard sections of code file setup exe on the host computer contents and syntax examples This font is also used Examples of the other items for the proper names of disk drives paths directories programs subprograms subroutines device names functions operations variables and filenames and extensions window Text in quotation refers to window titles Options indicates the window accessed via Tools Options Italics Italic text denotes variables emphasis a cross Monday
28. S AGREEMENT This William K Warburton dba X ray Instrumentation Associates XIA End User License Agreement Agreement sets forth the terms and conditions under which you are licensed to use the Software Software means A all of the contents of the disk s CD ROMS s or other media with which this agreement is provided including but not limited to i XIA or third party software ii related explanatory written materials Documentation and B modified versions upgrades updates additions and copies of the Software if any licensed to you by XIA collectively Updates XIA grants to you a nonexclusive license to use the Software provided that you agree to the following 1 Use of the Software i The term Permitted Number of Computers means the number of computers for which you have purchased or been granted licenses by XIA ii You may install one copy of the Software onto a hard disk or other storage device of up to the Permitted Number of Computers iii You may install one copy of the Software on a single file server for the purpose of downloading and installing the Software onto a hard disk or other storage device of up to the Permitted Number of Computers that are on the same network as the file server No other network use is permitted iv You may make one backup copy of the Software provided your backup copy is not installed or used on any computer You must reproduce the copyright notice s
29. Software Trademarks shall be used in accordance with accepted trademark practice including identification of trademark owners names Trademarks can only be used to identify printed output produced by the Software and such use does not grant you any rights of ownership in that trademark Except as stated above this Agreement does not grant you and intellectual property rights in the Software This Agreement provides the terms and conditions under which you are licensed to use the Software It is not an agreement for the sale of the Software to you 4 DISCLAIMER OF WARRANTIES XIA MAKES NO WARRANTIES EXPRESS IMPLIED OR STATUTORY AS TO ANY OTHER MATTERS INCLUDING BUT NOT LIMITED TO NON INFRINGEMENT OF THIRD PARTY RIGHTS MERCHANTABILITY OR FITNESS FOR ANY PARTICULAR PURPOSE XIA DOES NOT AND CANNOT WARRANT THE PERFORMANCE OR RESULTS YOU MAY OBTAIN BY USING THE SOFTWARE Some states or jurisdictions do not allow the exclusion of implied warranties or limitations on how long an implied warranty may last so the above limitations may not apply to you To the extent permissible any implied warranties are limited to ninety 90 days 5 6 2003 Page iii Manual Kepler Software Package mdo Kepler MAN 001 1 preliminary 5 Limitation of Liability IN NO EVENT WILL XIA BE LIABLE TO YOU FOR ANY CONSEQUENTIAL INDIRECT INCIDENTAL PUNITIVE OR SPECIAL DAMAGES INCLUDING ANY LOST PROFITS OR LOST SAVINGS EVEN IF A REPRESENTATIVE OF XIA HAS BEEN AD
30. T Resume Run Two methods to set the next run to be resumed 5 6 2003 Saturn Run ControlbClear Spectrum at Run Start Saturn Run Control Retain Spectrum at Run Start Kepler Run Controb gt Resume Run CR Page 16 Manual Kepler Software Package Resuming a run after any change in module settings will not produce reliable results mdo Kepler MAN 001 1 preliminary At every run start the spectrum memory and statistics from the last run can either be cleared or retained If cleared the statistics are reset to zero and the spectrum memory is emptied If retained then the new run picks up where the last run stopped Resuming a run after changing any acquisition settings is generally not recommended Stop the run then start anew Two of the methods to set the resume run status are shown in the sidebar 4 4 Update Interval E ne Run Control E Stop Run Y Run to Preset None Y Preset Value None Y Auto Update every 1 0 second The run control section of the DAQExplorer Auto update varies the interval used to continuously readout module data spectrum and statistics If auto update is disabled Kepler still checks if the run is finished every second Saturn Run Control Auto Update After a run is started Kepler can periodically update the spectrum display with the most recent data stored on the module This is very useful for monitoring the success or failure of the current run allowing th
31. VISED OF THE POSSIBILITY OF SUCH DAMAGES OR FOR ANY CLAIM BY ANY THIRD PARTY Some states or jurisdictions do not allow the exclusion or limitation of incidental or consequential damages so the above limitations may not apply to you 6 Governing Law and General Provisions This Agreement will be governed by the laws in force in the State of California excluding the application of its conflicts of law rules This Agreement will not be governed by the United Nations Convention on Contracts for the International Sale of Goods the application of which is expressly excluded If any part of this Agreement is found void and unenforceable it will not affect the validity of the balance of the Agreement which shall remain valid and enforceable according to its terms You agree that the Software will not be shipped transferred or exported into any country or used in any manner prohibited by the United States Export Administration Act or any other export laws restrictions or regulations This Agreement shall automatically terminate upon failure by you to comply with its terms in which event you must destroy all copies of the Software This Agreement may only be modified by a writing signed by an authorized officer of XIA although XIA may vary the terms of this Agreement in connection with the licensing of any Updates to you 7 Notice to U S Government End Users The Software and Documentation are Commercial Items as that term is defined at 48 C
32. a is also the module not the exact provided to help track down sources of coherent noise Since the oscilloscope input signal display is literally a view of the ADC output on the module we refer to the oscilloscope display as an ADC trace 2 Oscilloscope Of x File Print Acquite Trace Sample Time ns 500 E Zoom yj AutoX x AutoY yJ Linear pea 1050 1000 ECH 900 850 800 750 700 ADC Counts 1 0 0 2 0 4 0 6 0 8 1 1 2 1 4 1 6 d 2 22 24 26 28 3 32 34 3 6 3 8 4 Time milliseconds Not Active Iterations 1 E Zoom zi AutoX Auer yf Linear z Power ADC Counts 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 D 150 200 250 300 400 450 500 550 600 650 700 750 800 850 300 1000 Frequency kHz Figure 7 The oscilloscope display in Kepler An ADC trace is displayed in the upper pane and the FFT of the same ADC trace is shown in the lower pane 7 1 1 Acquiring ADC Trace Acquire Trace Stop Acquire 5 6 2003 Page 32 Manual Kepler Software Package The sample time acts like the time scale on a digital oscilloscope changing the time delay between samples that are displayed in the trace The FFT of the trace helps you find coherent noise problems in your detector and electronics setup It can be an invaluable diagnostic tool in some situations 5 6 2003 mdo Kepler MAN 001 1 preliminary Any time a data taking run is not active anew ADC trace can be acquired by pressing the Acquire Trace button o
33. age 15 Manual Kepler Software Package The trigger algorithm is based on a digital filter similar to the energy measurement filter The peaking and gap times for the trigger filter determine its efficacy mdo Kepler MAN 001 1 preliminary response time is determined by setting its peaking time the shorter the trigger peaking time the faster the response and the more accurate the measurement of the pulse start time which in turn directly improves the energy measurement for that pulse However there is a tradeoff between the speed of the digital filter and its ability to reject noise when detecting pulses the longer the trigger peaking time the greater the ability to avoid noise triggers Typically the Saturn performs well with a trigger peaking time of 100 ns there should be no need to change this setting 4 1 9 4 Trigger Gap Time This parameter helps the trigger filter with noise immunity please read 4 1 9 3 for more details Typically the Saturn performs well with a trigger gap time of 0 ns there should be no need to change this setting 4 2 Starting and Stopping Runs E ne Run Control Start Run al gt Start Run E IC Run Control SES E Stop Run The buttons left and DAQExplorer right entries for starting and stopping runs 3 Ways to Start Stop a Run 1 DAQExplorer entry under Run Control 2 Menu item under Run Control 3 Button above the spectrum Only the y axis scale mode is a
34. an ini file which saves the module configuration analysis being performed but do not include the settings required to configure You can save either or any XIA module The hardware configuration related to setting acquisition both 5 6 2003 Page 6 Manual Kepler Software Package mdo Kepler MAN 001 1 preliminary values see 4 1 and related quantities on the Saturn itself are contained in an initialization IND file see 3 1 2 6 Tools Options Settings The Options panel contains global settings that affect the entire program The configuration panel contains settings that dictate how Kepler initially starts The graphics panel contains settings that affect the operation of the various graphs within Kepler The configuration panel contains the following settings e Default Kepler Save File location of the GUI configuration file used at Kepler startup e Default Hardware Save File location of the INI file used to configure a module at Kepler startup e Default Error File location of the Error file generated during Kepler operation this should be send to XIA along with any error reports e Automatically Initialize Hardware this checkbox controls whether a module connected to the host computer is automatically configured using the Default Hardware Save File at program startup The graphics panel contains the following settings e Zoom Enable Key controls the hotkey used to per
35. ay Time 10 Default 7 Detector Rise Time 13 Energy Threshold 14 Expert 15 Gap Time 13 Global Options 7 Graphs 7 MCA Bins 14 Number of Bins 14 Peaking Time 13 Polarity 9 Preamplifier Gain 9 Preamplifier Type 10 RC Feedback Preamplifier 10 Reset Interval 10 Reset Preamplifier 10 Spectrum Bin Width 13 Spectrum Bins 14 Trigger Gap Time 16 Trigger Peaking Time 16 Trigger Rise Time 16 Trigger Threshold 14 Spectrum Printing 32 5 6 2003 mdo Kepler MAN 001 1 preliminary Reading from Module 28 ROIs 28 Saving Loading Files 31 Spectrum Analysis 28 Starting Kepler Program 5 Runs 16 Starting and Stopping Runs 16 Statistics Dead Time 20 ICR 19 Input Count Rate 19 Live Time 19 OCR 19 Output Count Rate 19 Real Time 19 Status Configured 7 Current GUI Save File 8 Current Save File 8 Program State 7 Run Active 7 Stopping Kepler Program 5 Runs 16 Support 3 Window Tabs 5 Windows Navigating Moving Around 4
36. column values as ROIs are added to Kepler makes calibration much easier All these values are saved in the Kepler GUI save files so it only has to be done once Several calibration passes may be required depending on the precision desired for the peak position and how far the calibration has to move the peak Calibrate Initially the peaks of spectral lines are unlikely to fall exactly at their known energies in the spectrum This problem is resolved by calibrating the module s gain using a peak at a known energy for x ray detectors this is typically the 5 9 keV peak of a Fe source To calibrate the module 1 As discussed in 6 5 1 store this known energy value in the Desired column of the ROI table for the peak of interest 2 Be sure that the ROI that contains the calibration peak is the active ROI 3 Move the mouse over the Calibrate button the background color of the desired column and active row should turn to green indicating that the calibrate operation is ready to proceed 4 Press the Calibrate button which will cause the gain of the module to be scaled by the ratio of the desired position to the Gaussian mean 5 Collect a new spectrum The peak should now appear closer to the desired peak position However due to non linearities in the module s gain setting electronics the peak will probably not be exactly at the requested position In addition the ROIs will probably not be exactly optimal anymo
37. d right arrow keys to highlight menus and press Enter or the down arrow key to open menus Use the up and down arrow keys to highlight menu selections and press Enter to select Once inside a function window the Tab key can be used to move forward between fields and Shift Tab to move backwards through the fields Press and hold the Shift key and then press the Tab key while still holding the Shift key down NOTE Pressing Enter inside a function window will save any changes and exit the function 2 2 2 Window Tabs Several windows in Kepler have tab sections e g expert configuration expert acquisition values and options These tabs look similar to manila file folder tabs found in most filing cabinets These tabs provide access to different sections for entering information and can be selected by the same methods mentioned above Hot Keys mouse and keyboard Tab Shift Tab 2 3 Hardware Setup The quick start guide in the hardware manual is the best place to successfully start using Kepler 2 3 1 Saturn Setup Please refer to the Saturn hardware manual provided by XIA for details on setting up your Saturn module 2 3 2 Polaris Setup When Kepler support for Polaris becomes available you should refer to the Polaris hardware manual provided by XIA for details on setting up your Polaris module Kepler maintains a persistent state across sessions The state is saved when Kepler is closed and restored when it is
38. del error reporting can be turned on or off using the checkbox in the upper left corner of the Error Reporting window The error information is piped to a file on the disk of the host computer which is determined by default using the setting of an entry in Tools Options see 2 6 This file can be overridden by either clicking on the file selection button near the top of the Error Reporting window or by directly entering a new file in the text box also located at the top of the window 8 2 2 Reporting Levels Page 37 Manual Kepler Software Package mdo Kepler MAN 001 1 preliminary The Handel library can report errors of different severity debug Only messages reported informational warning and error Each error level is more serious to the at the error level are continued running of Handel but only errors are critical to the continued critical to the continued operations of the XIA module The desired error reporting level can be set with operation of Kepler the drop down list box located at the top of the Error Reporting window H Error Reporting Ai x j d Error Filename a c Program Files ia Kepler config xiaEr Find Read Close DEBUG x10p c line 2803 dxp_begin_control_task runtasks Ox5fb DEBUG x10p c line 2620 dxp_begin_run Entering dxp_begin_run DEBUG vip ce line 2635 dxp_begin_run resume 0 gate 0 DEBUG Up e line 2658 dxp_begin_run Exiting dxp_being_run DE
39. directly for details 4 5 3 Run Time Run Events Saturn Run ControbRun Time Saturn Run Control Run Events As discussed above this entry in the DAQExplorer determines either the amount of time or the number of acquired events that will cause the module to automatically end the run The DAQExplorer display will change automatically to accommodate the run type chosen in Saturn Run Control Run to and you can select either one of the pre defined choices or enter your own custom value by clicking on the Saturn Run ControlyRun Time or Saturn Run ControlbRun Events 5 6 2003 4 6 Run Related Statistical Information The statistics of the run event rates times etc are updated every time Kepler reads out spectrum data from the module shown in Figure 4 This can occur automatically during an auto update cycle or be forced by pressing Page 18 Manual Kepler Software Package 16 0us RealTime 12 68 s ive Time 12 39 s Z 79 Events JCR 2 20 keps OCR 1 91 kcps E mdo Kepler MAN 001 1 preliminary the Refresh button The following statistics are displayed in a bar at the top of the spectrum display Figure 4 The run statistics bar in Kepler This bar shows a summary of run statistics updated automatically at the end of all runs and at the user defined update interval The statistics can also be updated by pressing the Refresh button Many factors can affect the ratio of live to real
40. display 5 7 5 Modifying a Reference s Graphical Display References Reference 1 2 3 4 Selecting either the menu item or the DAQExplorer entries References Reference 1 2 3 4 opens the Reference Configuration window which allows you to modify each reference s line color width and style When the Line Color button is pressed a color selection box will appear the line color can be set to any of the predefined colors or to a custom color Up to 16 custom colors are allowed located at the bottom of the color selection box for use within Kepler The line style and width are selected with the drop down list box next to the appropriate label The larger the line width selected the thicker the lines used for displaying reference sets Currently any change to the graphical representation of a reference set will affect all sets of the same numeral in all graphs 5 7 6 Saving and Loading a Reference Set from Disk References Reference 1 2 3 4 Clicking on either the menu item or the DAQExplorer entries References Reference 1 2 3 4 opens the Reference Configuration window which allows you to load reference sets from disk and save them to disk On the right side of the Reference Configuration window is a drop down list box that lists all the reference sets currently stored in memory with the following names e Spectrum graph from the spectrum display in the Kepler window e Oscilloscope graph from the osc
41. e please refer to the Handel documentation 3 2 Firmware Definition Database FDD files All XIA modules have a digital signal processor DSP and field peas E SE programmable gate arrays FPGAs that must be configured any time the DSP and FPGAs module loses power XIA distributes the configurations in files called firmware programs and are definition database FDD files which contain all the configuration data for both distributed by XIA DSP and FPGAs on the modules The files are ASCII but should not be edited except by XIA personnel The details of the format are beyond the scope of this document 3 3 Preamplifier Parameters The parameters discussed here are important during the initial E Detector Preamplifier Settings configuration of the module A more detailed description is provided in the V Preamplifier has Positive Polarity r gh quick start guide located in your hardware manual See the sidebar for a picture eset Interval 10 0 us j Y Preamplifier Gein 4911 mvjkeV of the section of the DAQExplorer that is used to change the preamplifier The preamplifier parameters section of the 3 3 1 Preamplifier Gain DAQExplorer Saturn Run ControbPreamplifier Gain The preamplifier gain is a measure of the voltage gain of the preamplifier for signals generated by the detector For Kepler this value must be measured in millivolts of preamplifier signal per keV of x ray energy mV keV 3 3 2 Preampl
42. e Fixed Scale mode except that zooming and panning are both allowed Thus without user intervention the scale Page 23 Manual Kepler Software Package mdo Kepler MAN 001 1 preliminary remains at a fixed value even if the data exceed that value Invoking Pan or Zoom allows the scale to be changed arbitrarily Zooming and panning can be very sensitve while using logarithmic display 5 5 Linear and Logarithmic Display The y axis of any graph can be set to either logarithmic or linear display At present the x axis can only be displayed as linear Note zooming and panning can become very sensitive when the y axis is in logarithmic mode It is often easier to use the linear display for selecting a viewing region and then switching the display to logarithmic 5 6 Cursors Cursors cannot be added to a graph if there is no data in the display After selecting add cursor right or left clicking anywhere but in the graph will cancel the add cursor action Drag a cursor with the mouse or select it and use the keyboard arrow keys The crosshair cursor can be handy for comparing vertical levels of data in a graph Save time by using the autoROI function to define reasonable regions of interest 5 6 2003 Cursors allow you to measure a particular point in a graph or the differences between 2 points of a graph Each graph in Kepler can have at most 2 cursors added to the display Information about the cursor
43. e operator to make adjustments as needed The interval between spectrum updates can be set with the DAQExplorer entry see the sidebar Saturn Run Control Auto Update Simply click on the entry and choose an update interval The module itself limits the minimum auto update rate readout time is typically less than 10 ms If auto update is disabled then Kepler will only read out the spectrum when the run is stopped either by you or by the module Once each update Kepler performs two important functions to keep itself synchronized with the module First if auto update is enabled for any time interval then Kepler also reads the statistical information see 4 6 about the run in addition to the spectrum Second Kepler will also check if the run has been stopped for any reason by the module If so Kepler will update its own display appropriately including reading out the spectrum and statistical information one final time If auto update is disabled Kepler will still monitor the run status once every second an action that does not require reading the spectrum or statistical information and requires less than ms of the host computers time does not affect data taking at all 4 5 Run Types and Times Five data collection modes are supported one is infinite the other four are preset 5 6 2003 Saturn Run Control Run to Saturn Run Controb Run Time Saturn Run Control Run Events Kepler supports five diff
44. er Length Saturn Baseline Settings Baseline Filter Length The baselines for the module are averaged as an infinite impulse response IIR digital filter The value used in calculating the energy of a pulse from the detector uses the output of this IIR filter The effective length of the IIR is set with the baseline filter length setting Up to a point increasing the number in the average reduces the noise in the baseline average the point being determined by the amount of low frequency noise in the preamplifier output Experimentation is usually required to determine the best value for a particular detector preamplifier setup 4 1 9 Expert Settings Right click on Page 14 Manual Kepler Software Package gt System Settings x System Settings Energy Data Trigger Data Peaking Time us 16 0 a Peaking Time us 0 2 J Gap Time us p 15 S Actua 2 4 Gap Time us 0 0 S Calibration Energy ke 5 3 S Trigger Threshold eV 1968 6 S ADC Percent Rule E Energy Threshold eV 0 0 Histogram Data Spectrum Bins 4096 D MCA Bin Width e bin 20 mdo Kepler MAN 001 1 preliminary Saturn Acquisition Settings Saturn Baseline Settings For more advanced settings Kepler provides the system settings window shown in Figure 3 All the values described in 4 1 are available for editing in this window along with some more advanced settings calibration energy ADC percent rule trigger peaking time tr
45. erent modes for data collection Select the desired mode by clicking on the DAQExplorer entry see the sidebar of 4 4 Saturn Run ControlRun to The length of the run will be determined by the setting of Saturn Run ControlRun Time or Saturn Run Control Run Events depending upon the run type selected At any time you can interrupt the run by stopping the run in one of the ways described in 4 2 The five modes of operation are described below 4 5 1 User Intervention This mode programs the module to run indefinitely The only way to stop this run is by user intervention i e using Kepler to stop the current run For this mode the setting of Saturm Run Control Run Time does not influence the length of the run Page 17 Manual Kepler Software Package Some runs end after a set time others after a set number of events are collected The module automatically stops preset runs Kepler will detect that the run has stopped and update the display appropriately The gate input can be used for precise run control operations If this is a concern for your experiment please contact XIA for more information mdo Kepler MAN 001 1 preliminary 4 5 2 Preset Runs 4 5 2 1 Stop Control Value Each of the four preset modes will automatically stop when the run type stop condition is satisfied The stop conditions are either time based or event based depending on the run type selected The time stop condition
46. es de AER Ea e eaa 13 4 2 Starting and Stopping Hung 16 43 RESUMING a PUM EE 16 44 Update Interval aitsitetetecteri Adie deed 17 4 5 Run Types and Times nenna aah whee ane ad aera 17 4 6 Run Related Statistical Information 0 cccccceeceececeeeeeeeeeeeneeeeeeeeeeeeeneees 18 4 7 Unavailable functions while a run iS active nssesssssrennseeeeeenrrnnernssrrerenne 20 5 Graph usage in Kep leta a sect corcatecccctacthee seanevnncvastncenecnsduncunelotcnesnedeecevnctbectees 21 5 1 Default Modes 0 eccccccccceceeeeeeeeeaeeeceeceeeeeceeaneeceeeeesaecaneeeeseeeesaesnsaneeeneeees 21 D 2 gt LOOMING iss oes sas See E E AE E awa de ch E ade needs Rashnsy Papakea es 22 9 3 PINN BEEN 23 9 4 Axis Scaling MOES aiarra TTEA AE Ee ES 23 5 5 Linear and Logarithmic Display cccceeeeceeeeeeeeeeeeeetneeeeeeenaeeeeeenaeeeeeeaes 24 RE EEN 24 5 7 Reference Data Geis a ehir e a ar e eE a AE 25 6 Spectrum AnalySiS siiiu tasinia anaenda rentas Anifah Para oeiia unaa r inpia a Paraan 27 6 1 Reading data from the module 0 0 ee eeceeeee settee ee eete eect etaeeeeetaeeeeeetiaeeeeeeaaes 27 6 2 Regions of Interest Oe 27 6 3 Region of Interest Display Parameters ccccceeeeeeeeeeneeeeeeeeneeeeeeneeeeeenas 28 6 4 Region of Interest Statistics 0 cece ee eeneeeeeeeneeeeeeaaeeeeesaeeeesenaeeeeeeaes 29 6 5 Other ROM Data e a aaa ee eege Re ege 29 5 6 2003 Page i Manual Kepler Software Package 5 6 2003
47. form zooming in graph windows lt hotkey left mouse button gt e ROI Setting Key controls the hotkey used to create ROIs within the spectrum window lt hotkey left mouse button gt 2 7 Help Displays If confused about the action of a control in Kepler check the help bar on the lower edge of the Kepler window it might answer your question The panel at the lower edge of the Kepler window contains some detailed context sensitive help for many controls This Help Display changes depending on where the mouse is located When the mouse is not over a control within Kepler the Help Display shows information about Kepler s current running state run active unconfigured hardware etc 2 8 Status Display The status display can give you a quick overview of the state of Kepler e g if a run is active if the system is configured what save files are in use 5 6 2003 In addition to the help display the lower panel shows some general status messages for Kepler In general if the Status Display shows a red square then something is wrong if it s green then Kepler is running properly A list and brief description of the panel items follows e Type if green shows the current configured board type if red there is no valid hardware configuration e Configured if green then the hardware is configured if red the hardware is unconfigured e Run Active if green then a data taking run is active if red
48. hod for detecting and eliminating sources of coherent noise such as radio stations or computer monitors in the vicinity of the detector To provide more detail in the FFT Kepler allows multiple ADC traces to be acquired and averaged into a single FFT The value in the text box labeled Iterations in the Oscilloscope window changes the number of traces that are acquired If the chosen sample time and number of iterations takes too long the acquisition can be interrupted at any time however the current acquisition run must complete before control is returned to you After an aborted acquisition any data shown in the Oscilloscope should not be trusted 7 1 4 Saving and Loading Oscilloscope Graphs Save Oscilloscope Oscilloscope Graphs Load Oscilloscope Oscilloscope Graphs Save FFT Oscilloscope Graphs Load FFT Both oscilloscope and FFT data can be saved to a file on disk at any time using the menu items in the Oscilloscope window 7 1 5 Printing Oscilloscope Graphs Print Oscilloscope Oscilloscope Graphs Print FFT Page 33 Manual Kepler Software Package mdo Kepler MAN 001 1 preliminary The oscilloscope and FFT graphs can be printed separately to the default printer A window will open asking for information regarding the conditions under which these data were taken which will also be printed E Baseline Information File Print Get History Baseline Histor
49. ifier Polarity Saturn Run Control Preamplifier has X Polarity The output of the preamplifier will produce either an upward or a downward voltage pulse in response to an event in the detector Kepler refers to pulses that move upward as positive while downward pulses are negative 5 6 2003 Page 9 Manual Kepler Software Package Valid for detectors with reset preamplifiers only Valid for detectors with RC feedback preamplifiers only mdo Kepler MAN 001 1 preliminary 3 3 3 Preamplifier Type All XIA modules support both reset and RC feedback preamplifier type This setting can be changed at any time but does require new firmware to be downloaded and a jumper to be changed on the module If needed please review your hardware manual for details 3 3 4 Reset Interval Saturn Run Control Reset Interval When using a preamplifier with a reset circuit the output signal can briefly contain non linear components following each reset If the module processes these signals the resulting energy measurements will be wrong All XIA modules allow a settling time after a reset is detected which is defined by the Reset Interval During this settling time the module does not process any signals from the detector and this time is not counted as live time see 4 6 2 Improper setting of the reset interval can drastically affect the energy resolution of some detector setups For further information please review this concept in the
50. igger gap time and enable veto gate Undo Changes Figure 3 The expert settings window accessed within Kepler This is a central location for all acquisition settings as well as a few settings not recommended for the timid user Calibration energy and ADC percent rule set the gain of the module 5 6 2003 4 1 9 1 Calibration Energy In conjunction with the ADC percent rule Calibration Energy determines the module s gain setting Typically a calibration peak is used from a radioactive source which has a spectral line near the energy range of interest to your measurement e g Ee has a spectral line at 5 9 keV For purposes of setting the module s initial gain set the Calibration Energy to the energy of the line you intend to use for energy calibration e g 5 9 keV 4 1 9 2 ADC Percent Rule The ADC percent rule is used in conjunction with the calibration energy to determine the modules initial gain Depending upon the gain a typical pulse from the detector will use a certain percentage of the ADC s measurement range in the module this is the ADC percent rule For reset detectors this is typically set to 5 for RC feedback detectors it is set to 40 The Setup Wizard initially uses these standard values 4 1 9 3 Trigger Peaking Time In order to detect a pulse from the detector the module utilizes a trigger based on a fast digital filter referred to as the trigger filter The trigger filter s P
51. illoscope graph in Oscilloscope window e PowerFFT graph from the power spectrum of the FFT in the Oscilloscope window e BLHistory graph from the baseline history graph in the Baseline Information window e BLHistogram graph from the baseline histogram graph in the Baseline Information window To load a data file from disk click on the Load Ref button and select the file to load If successful the reference set will appear in the drop down list box and be accessible from the correct graph To save a reference set to file first use the drop down list box to select the reference set and then click on the Save Ref button Page 26 Manual Kepler Software Package mdo Kepler MAN 001 1 preliminary 6 Spectrum Analysis 6 1 Reading data from the module Refresh There are three times when spectrum and statistics for the current or last run are read from the module at the end of an auto update period see 4 3 at the end of a run either ended by you or the module and when you press the Refresh button ROI C V _ L_ Lower Upper Events OCRicps Gau Mean Gau FWHM Desired Name 5950 0 3268630 1436 35 5790 30 428193 5620 0 6220 0 6500 0 6 2 Regions of Interest ROIs 164 45 172 88 5900 ROI 1 0 ROI Z Add Delete SEH 188 16 6367 56 Figure 6 Region of Interest ROI data from Kepler The buttons at the right are used to add delete and calibrate ROIs If
52. ite box located in the mini zoom window of every graph can be dragged to any point in the window This will reposition the view area such that the main window subtends the same region as the white box in the mini zoom window 5 4 Axis Scaling Modes Fixed auto scale mode is set for the y axis when starting a new run The mode prior to starting the run is restored after the run is stopped Float scale mode allows arbitrary zooming and panning 5 6 2003 Both the x and y axes behave independently as data is being acquired or the view is manipulated via panning or zooming operations The following axis scaling modes are set using two drop down list boxes one for each axis located either in the upper or lower left of all graphs 5 4 1 Fixed Scale This mode will keep the axis limits fixed at their presently set values Zooming and panning are forbidden while in fixed mode 5 4 2 Fixed Auto Scale This mode automatically keeps the axis limits properly set such that the entire range of data for that axis is displayed Thus as data is acquired during a run the axis limits will grow to accommodate the data and zooming and panning are forbidden 5 4 3 Auto Scale This mode behaves similarly to the Fixed Auto Scale mode However zooming and panning are allowed If a zoom or pan is performed while in auto scale mode the mode will automatically change to Float Scale 5 4 4 Float Scale This mode acts similar to th
53. lease contact XIA for details on the format The spectrum file can be reloaded into the spectrum window at a later time for offline analysis and printing All run parameters that affect analysis and Page 30 Manual Kepler Software Package mdo Kepler MAN 001 1 preliminary statistics are saved and restored with the spectrum data e g peaking time real time etc 6 8 Printing Spectra Saturn Spectrum Print Spectrum Kepler Spectrum Print Spectrum lt F9 gt The current view zoom level and logarithmic linear scaling in the spectrum display can be printed to the default printer It is not possible to change the printer destination using the current version of Kepler This ability is planned for future versions 5 6 2003 Page 31 Manual Kepler Software Package mdo Kepler MAN 001 1 preliminary 7 Diagnostic Tools Available for the Saturn 7 1 Oscilloscope and Fast Fourier Transform FFT Tools Oscilloscope lt CtrHF5 gt The oscilloscope tool lets Saturn Diagnostics Oscilloscope you take a peak at what the module sees It acts The XIA modules can provide data that emulate the actions of a digital like a very simple digital oscilloscope shown in Figure 7 This data is very useful for exploring problems oscilloscope looking at with detector setups since it provides a direct view of the signal that the module the detector signal inside sees coming from the preamplifier An FFT of the oscilloscope dat
54. lues which means more historical information than just the last few baselines reported by the history In particular since the histogram does not apply the baseline cut to its entries one can see both where the cut is applied and what kinds of events are falling outside the cut Bimodal baseline distributions for example are characteristic of periodic background noise 7 2 2 Gaussian Fitting of the Baseline Histogram To aid in diagnosing the health of the baseline measurement a Gaussian fit is performed on the baseline histogram and the results are reported directly below the histogram The fit searches for the largest peak in the histogram and fits the region between half the height on either side of the peak which can cause bad fit values if the distribution is not dominated by a single Gaussian peak but if that is the case the baseline has already done its job by showing a serious noise problem somewhere 7 2 3 Saving and Loading Baseline Information Graphs Save History Baseline Information Graphs Load History Baseline Information Graphs Save Histogram Baseline Information Graphs Load Histogram Both baseline history and histogram data can be saved to a file on disk at any time using the menu items in the Baseline Information window 7 2 4 Printing Baseline Information Graphs Print History Baseline Information Graphs Print Histogram The baseline history and histogram graphs
55. mmon method of zooming is clicking and dragging in the main graph window The point where the mouse is clicked will follow the mouse position while simultaneously holding the point in the lower left corner fixed A cross hair indicating the start of the zoom appears where the mouse was first clicked and remains in the same location providing a reference to the current zero zoom point Moving the mouse back to the center of the cross hair will effectively undo the current zoom The simplest way to zoom in on a feature of interest is to follow these steps 1 Move the region of interest into the lower left comer of the graph using one of the panning methods 5 3 Double clicking and dragging is probably the simplest method 2 Make sure the default mode for the graph is set to Zoom 3 Left click around the feature and drag the mouse toward the upper right corner of the graph until the desired view of the feature is achieved 5 2 2 mini zoom Window To facilitate zooming in the main window there is a mini zoom window inset within each graph which always shows the full scale view of the graph window i e all graph data is displayed as if lt Ctrl A gt had been pressed in the main window Within the mini zoom window is a white box that shows the current portion of the graph being displayed in the main graph Note when Page 22 Manual Kepler Software Package To drag the box click near the diagonal line joining the
56. n the Oscilloscope window Since under some conditions the acquisition of the ADC trace can take a noticeable time it is possible to interrupt the current ADC trace acquisition A minimum of one ADC trace must be taken so Kepler may not respond immediately see 7 1 2 for more details To stop the ADC acquisition run press the same button that was used to start the acquisition 7 1 2 Time between Samples The time interval between the samples in the ADC trace display can be changed to provide a longer history The minimum setting is the time required for the module s DSP to capture a value from its ADC 100 75 ns for a Saturn Polaris module The value in the text box labeled Sample Time in the Oscilloscope windows sets the time between samples The length of the ADC trace from the module is limited to 8K samples so the total time covered by the ADC trace is 8k times the selected sample time It is important to note that each captured value is only a single sample from the module s ADC as opposed for example to an average of the samples in the interval This has implications for how high frequency noise is aliased into the FFT If you wish to use the FFT for critical work and these implications are not clear to you we recommend referring to a text on Fourier Transform theory 7 1 3 FFTs and Averaging For each ADC trace acquired Kepler calculates a simple FFT and displays the power spectrum This is a very powerful met
57. nd the selected file will be shown in the right box Double clicking on an INI filename will download the settings in the INI file to the hardware module If an INI file is not desired then the Detector Preamplifier Configuration tab is the place where all relevant information for configuration is entered Note an INI file contains all the information represented in this Page 11 Manual Kepler Software Package 5 6 2003 mdo Kepler MAN 001 1 preliminary panel so this panel is an alternative method for configuration Unless modified by you this panel reflects the data used in the last successful configuration of a module not necessarily the information contained in the currently selected INI file or on the module Most of these parameters are discussed in 3 3 please refer to the hardware manual quick start guide for a detailed description of all these parameters When all the information is input in the panel pressing the OK or Apply button at the bottom of the configuration window will configure the system the OK button will also close the expert configuration panel If at any time while changing the configuration settings you wish to undo the changes press the Cancel button After the settings are final and you you have successfully configured the module using the Apply button the configuration can be saved to an INI file by pressing the Save to INI button Page 12 Manual Kepler Software Package mdo Kepler
58. ng to the application programming interface for the operating platform for which the sample programs are written provided that You agree to defend hold harmless and indemnify XIA from and against any and all claims liabilities damages expenses and costs arising out of or in connection with your use or distribution of the sample programs modifications thereof or your application program s and You do not state that XTA certifies or guarantees the operation of the sample programs or modifications thereof with any hardware and or software Each copy or partial copy of the sample programs or any modifications thereof must include a copyright notice as follows Copyright c year your company name Portions of this code are derived from XIA Sample Programs Copyright c XIA All rights reserved These sample programs may require additional software to operate The right to redistribute a sample program does not include the right to redistribute software that is a prerequisite for its operation In particular your right to redistribute a sample program does not include the right to redistribute the Software 5 6 2003 Page iv Manual Kepler Software Package mdo Kepler MAN 001 1 preliminary 1 Introduction The Kepler program provides four basic abilities 1 configure an X Ray Instrumentation Associate s XIA spectroscopy module e Dynamically configure XIA spectroscopy modules e Configure XIA modules via save files
59. o display that row s ROI Left clicking on the Color column labeled with a C not necessarily the active ROI row brings up a dialog box used to change the ROI s color 6 3 3 Visible ROI s in Kepler can be either visible or invisible To toggle this property left click on the column labeled with V An invisible ROI will still report statistical information for the data that it covers Page 28 Manual Kepler Software Package mdo Kepler MAN 001 1 preliminary 6 3 4 Locked The upper and lower bounds for an ROI may be locked to fix their settings and prevent accidental changes Left clicking on the column labeled by L will toggle the ROI s locked status The ROI mean can be displayed as a simple weighted average or as the result of a Gaussian fit The FWHM is always the result of a Gaussian fit but can be displayed as an absolute value or as a percentage of the Gaussian mean 6 4 Region of Interest Statistics 6 4 1 ROI Lower and Upper Bounds The columns labeled Lower and Upper display the ROI s lower and upper boundaries 6 4 2 ROI Mean The mean of the ROI region can be displayed in two forms arithmetic mean labeled Ari Mean and Gaussian mean labeled Gau Mean The arithmetic mean is a weighted average of all the points in the ROI while the Gaussian mean is the result of fitting a simple Gaussian no background or multi Gaussian peaks to the data within the ROI Left clicking anywhere in
60. on such copy of the Software 2 Restrictions i You may not copy transfer rent modify use or merge the Software or the associated documentation in whole or in part except as expressly permitted in the Agreement ii You may not reverse assemble decompile or otherwise reverse engineer the Software iii You may not remove any proprietary copyright trade secret or warning legend from the Software or any Documentation iv You may not modify sell rent transfer except temporarily in the event of a computer malfunction resell for profit or distribute this license or the Software or create derivative works based on the Software or any part thereof or any interest therein 3 Copyright The software and any copies that are owned by XIA and its structure organization and code are the valuable trade secrets of XIA The Software is also protected by United States Copyright Law and International Treaty Provisions You must treat the Software just as would any other copyrighted material such as a book You may not copy the Software except as set forth in the Use of the Software section Any copies that you are permitted to make pursuant to this Agreement must contain the same copyright and other proprietary notices that appear on or in the Software You agree not to modify adapt or translate the Software You also agree not to reverse engineer decompile disassemble or otherwise attempt to discover the source code of the
61. open 5 6 2003 2 4 Starting and Stopping Kepler There are two ways to quickly get Kepler running e Double click the Kepler Icon on your desktop e Choose Kepler from Start programs Kepler Kepler After installation Kepler by default is located in C Program Files XIA Kepler or whatever location was chosen during installation Within the installation directory are located two directories that contain files to help you get started for the first time The firmware directory will contain a file called saturn fdd which contains the firmware programs downloaded to the Saturn module The config directory will contain saturn std ini which is a simple initialization file that works with most detector setups Fine tuning of the setup parameters can occur after Kepler is running Page 5 Manual Kepler Software Package mdo Kepler MAN 001 1 preliminary Display Controls DAQ Explorer Spectrum Window y y KI a7 KU i y y J a4 KR 22 a H a5 rege eV Bor e jV i jisver E rents OCR eps Cou Mean Cou Te pate ene Regions of Interest ROIs Heb Eed Double Ohh o chch on s la more actora Right Okk ter configuation Options Wie Ce Oo AC C Status Indicators Figure 1 Overview of Kepler This figure shows all the main elements of the Kepler program with labels for the important areas of the control interface A shortcut for Kepler should have been created on the De
62. play for all reference sets can be changed color line style line width to suit your preferences Each graph in Kepler has 4 associated reference sets into which you can copy the current data in the graph and store it in memory 5 7 1 Copy Graph Data to a Reference Set To copy a graph s data to a reference set right click on the graph to bring up the popup menu and select the Copy to ref menu Within this menu is a list of all 4 reference sets pick one The data is now saved in the reference set that was selected and the entry of this menu will show a checkmark by the reference number 5 7 2 Display a Reference on the Graph To display a reference set on a graph right click on the graph and select the Display ref menu The references that are available will be displayed in black while the ones with no stored reference set are grayed out Pick a black reference set and it will appear overlaid on the graph 5 7 3 Scale Reference Data then Display A reference set can be scaled before being displayed by right clicking on the graph and selecting the Scale ref menu A dialog box see Figure XX will appear that allows you to determine how to scale the reference set If the Scale To Area checkbox is checked then the reference data are scaled as follows each bin is multiplied by a constant that is the ratio of the total number of graph events in a selected number of bins to the total number of reference events in the same selected numbe
63. position and difference between 2 cursors if they are both visible are displayed either in the upper or lower right corner of the graph 5 6 1 Adding a Cursor 1 First right click on the graph and select either Place Cursor 1 or Place Cursor 2 from the popup menu 2 Then click on the graph where you want the cursor Note that if any other action is performed after the first step i e left or right clicking anywhere but in the graph display then the add cursor action will be canceled and must be restarted 5 6 2 Moving a Cursor The mouse pointer will change to a left right arrow when moving over a cursor indicating that the cursor is ready to be moved While the mouse pointer is changed left click and drag the cursor to the desired location Alternatively for fine adjustments to the cursor location while the mouse pointer is changed just left click on the cursor which changes the cursor color to to white indicating that it has been selected Now the arrow keys on the keyboard will move the cursor either left or right in single bin increments 5 6 3 Crosshair display The default cursor view is a simple vertical line In some cases it is useful to have a crosshair that shows the vertical level as well as the horizontal position To change the cursor to a crosshair right click on the cursor when the pointer changes to left right arrow and select the Crosshair entry from the popup menu To return the cursor to its default displa
64. r of bins The selected number of bins can either be the whole graph or one of its ROI s as determined by the drop down list box next to the Scale To Area checkbox If the Scale To Area checkbox is not checked then a simple linear combination of the graph and reference data is displayed Each bin of the graph data is multiplied by the constant from the text box on the left of the dialog and added to the same bin number of the reference data times the constant from the text box located on the right of the dialog The values in the two constants can be negative allowing subtraction operations between the reference and the graph For removal purposes this new graph counts as the same reference set number that was just scaled likewise if the same reference set number is displayed again the old scaled data will be lost Page 25 Manual Kepler Software Package Individual control of the graphical display of each graph s references is planned for a future release of Kepler A reference saved to disk can be loaded directly into the graphs and likewise any graph data previously saved to disk can be loaded into a reference 5 6 2003 mdo Kepler MAN 001 1 preliminary 5 7 4 Remove a Reference Set A reference set can be removed from the graph by right clicking on the graph and selecting the Remove ref menu Selecting the desired reference set from the list removes it from the graph display but leaves it in memory for future
65. re either 6 Readjust the boundaries for the active ROI if necessary 7 Repeat until satisfied Be sure to collect adequate statistics so that the location of the peak is determined by the module s gain and not by random fluctuations in the data If the module has been previously calibrated with the current detector and preamplifier convergence should occur in only two or three repetitions of the calibration process Note 1 If the module has never been calibrated before for a particular detector preamplifier combination the change in gain on the first calibration pass may be so large that the calibration peak jumps completely out of its ROI Just reset the ROI on the peak and proceed When the calibration is complete don t forget to save an INI file to record the values for this detector Note 2 if a run is currently active the calibrate operation will display a prompt about stopping the run the current run data will be lost by proceeding By saving your spectrum from runs you can always return at a later time and perform any analysis available in Kepler 5 6 2003 6 7 Saving and Loading Spectra Saturn Spectrum Save Spectrum Saturn Spectrum Load Spectrum Saturn File I O Save Spectrum Saturn File I O Load Spectrum Kepler Spectrum Save Spectrum Kepler Spectrum Load Spectrum lt F7 gt lt F8 gt The spectrum data can be loaded from disk and saved to disk in an XIA specified text format p
66. s are always the worst day of the reference or introduction to a key concept This font week also denotes text that is a placeholder for a word or value that you must supply lt Shift gt Angle brackets denote a key on the keybord not case lt W gt indicates the W key sensitive lt Shift Alt A hyphen or plus between two or more key names lt Ctrl W gt represents holding the control Delete gt or denotes that the keys should be pressed key while pressing the W key on the lt Ctrl D gt simultaneously not case sensitive keyboard Bold italic Bold italics denotes a warning or caution statement Beware of small green men means to watch out for aliens Beware of salesmen bearing gifts means what it says The following terms will be mentioned throughout the manual e DAQExplorer refers to the tree of information and options along the left side of the Kepler main window e module refers to an XIA spectroscopy module e host computer refers to the computer on which Kepler is running Additional terms may be found in the Glossary 1 2 Related documentation 5 6 2003 The following documents are sources of additional information while operating your XIA hardware All documents can be downloaded in the Portable Document Format PDF from XIA s Internet site www xia com In order to request printed copies please send an e mail to su call the company directly Kepler Hardware Manual ort xia com
67. sktop of your windows operating system In addition there should be a Start menu item for running and uninstalling Kepler Each time Kepler is run it will attempt to resume operation in the same configuration as the last time it ran This includes both the window positions for the Kepler program as well as the hardware configuration of any XIA module Some aspects of these configurations can be controlled in the Tools Options menu item within Kepler see 2 6 After starting Kepler you should see a window that looks like Figure 1 which also labels some of the more important parts of the program Most command operations are controlled through the DAQExplorer or with menu items Kepler always shows the spectrum window with its associated regions of interest and display controls The statistics from the most recent run or most recently loaded spectrum are shown at the top of the screen The current program status is shown at the bottom of the screen with the status indicators 2 5 Kepler save files A Kepler configuration file can be saved to disk at any time The Kepler kep configuration files maintain all Kepler settings related to the graphical user interface GUI which include window positions and state minimized maximized or normal run parameters display parameters graph states etc These save files allow customized windows for each type of Note the difference between a kep file which saves Kepler configuration and
68. t F9 gt Print Spectrum lt F12 gt Open About Kepler Panel lt Ctrl F1 gt Edit Reference 1 Properties lt Ctrl F2 gt Edit Reference 2 Properties lt Ctr F3 gt Edit Reference 3 Properties lt Ctr F4 gt Edit Reference 4 Properties lt Ctrl F5 gt Open Oscilloscope Panel lt Ctrl F6 gt Open DSP Parameter Editor Panel lt Ctrl F7 gt Open Baseline Panel lt Ctrl F8 gt Open Handel Hardware Errors Panel lt Ctrl O gt Open the Options Panel lt Ctrl X gt Close Kepler Without Saving lt Ctrl I gt Open the INI File Organizer Panel lt Ctrl C gt Open the Detector Preamplifier Configuration Panel lt Ctrl R gt Toggle the resume run status When a graph is selected lt Ctrl A gt Set the graph to full scale 5 6 2003 Page 39 Manual Kepler Software Package mdo Kepler MAN 001 1 preliminary Appendix 3 EPP Port Requirements Kepler requires that the Saturn module be connected to a parallel port usually LPT1 with an input output range of either 0x278 or 0x378 Appendix 4 Common Problems Symptom Possible Cause Solution Handel error message Epp port not found Firmware bad Error 1111 Error 2222 Gain related errors Appendix 5 Index Axis Auto Scale 24 Fixed Auto Scale 23 Fixed Scale 23 Float Scale 24 Linear 24 Logarithmic 24 Scale Modes 23 Baseline 35 Acq
69. the baseline samples captured by the module to be erroneous in unexpected ways resulting in degraded energy resolution The diagnostic acquisition of baseline information may assist in clearing up problems of this sort Please refer to Figure 8 for a picture of the baseline diagnostics window 7 2 1 Acquiring Baseline Data Get History Page 34 Manual Kepler Software Package Histogram entries do not have the baseline cut applied 5 6 2003 mdo Kepler MAN 001 1 preliminary Get Histogram The module provides two kinds of baseline information a time sequence history of baseline averages and a histogram of baseline measurements The baseline history is simply a list of past baseline averages calculated by the module plotted in time The history plot is useful for investigating periodic or non periodic events that disrupt the baseline correction process For example if low energy pulses are not correctly detected e g the trigger threshold is improperly set then these pulses will distort the baseline showing up as a jump followed by an exponential decay occurring after each undetected pulse Since the baseline cut discussed in 4 1 7 is applied before a baseline is added to the history the baseline history does not contain all captured baseline values and may therefore artificially hide some classes of problems To address these problems the module maintains a baseline histogram that contains many captured baseline va
70. tings an INI file should be saved and updated until you have the desired settings in place 3 5 1 Loading an INI file File I O Load INI File Page 10 Manual Kepler Software Package mdo Kepler MAN 001 1 The INI preview box is read only Editing of the INI file directly will be available in a future versions of Kepler preliminary Configuration Load INI File lt F4 gt Using any of the options above opens a dialog box that allows the selection of an INI file to load from disk All settings will be automatically applied to the module 3 5 2 General Configuration Right Click on Saturn Configure and select INI File Organizer or select Detector Preamplifier Configuration Configure INI File Organizer or Detector Preamplifier Configuration lt Ctri C gt or lt CtrH I gt The general configuration panel consists of a tabbed panel window with two tabs as shown in Figure 2 One tab contains the INI File Organizer which presents a simple file view of INI files for the currently selected directory The other panel shows the Detector Preamplifier Configuration panel that allows direct input of all parameters required to get the module up and running The INI File Organizer tab contains two large boxes the one on the left is a list of INI files in the current working directory while the right shows the contents of the INI file that was last selected with the mouse from the left box this box is read only Using the file selec
71. tor box just above the INI file box you can change the current working directory for the INI file box which is E Configuration x Ei Configuration x INI File Organizer Detector Preamplifier Configuration INI File Organizer ia H Double click on a file to configure the system saturn_rc_std ini Path is C Program Files xia Kepler Configs Close detector definitions a Kevex Detector Aa Preamplifier Configuration alias detectorl number_of_channels 1 ifi Les type reset Preamplifier Type Eesel type_value 10 0 ResetDelay us joo channel oam 6 6 channal0_polarty Preamplifier Gain m V keV laan Preamplifier Polarity Potwe zl firmware definitions START 1 Firmware Configuration alias firmware filename c program files xia Kepler FDD Location Je program files xia Kepler firmware saturn_re el firmware saturn_reset fdd module definitions Save to INI START 1 E slina m sesch de Cancel Figure 2 The panel on the left shows the INI file organizer and on the right is the detector preamplifier configuration panel Right clicking on configure module type and selecting either the INI file organizer or detector preamplifier configuration will access these panels Double click on an INI file to download settings to the hardware module 5 6 2003 displayed on the lower left of the panel all INI files in the selected directory will be added to the left box a
72. ual 4 1 3 Spectrum Bin Width Saturn Acquisition Settings Spectrum Bin Width The spectrum bin width represents the size in energy eV of each bin in the spectrum display The full energy range dynamic range of the displayed spectrum is therefore the spectrum bin width times the number of spectrum bins The module will also keep track of the number of valid events that were Page 13 Manual Kepler Software Package Saturn modules allow any number of spectrum bins from I to 8192 A noise peak at low energies in the spectrum is undesirable The most common way to remove the peak is to increase the trigger threshold Saturn specific capability The baseline cut removes outliers that would adversely affect the baseline average The trigger algorithm does not detect these events Depending on the type of noise in the system a bigger filter length might improve energy resolutions 5 6 2003 mdo Kepler MAN 001 1 preliminary acquired but fell outside this energy range counting them as either underflows or overflows 4 1 4 Spectrum Bins Saturn Acquisition Settings Spectrum Bins The spectrum bins selects the number of bins in the spectrum display 4 1 5 Trigger Threshold Saturn Acquisition Settings Trigger Threshold The trigger threshold shows the amplitude in energy units required for a pulse from the detector to generate a trigger and initiate the process of measuring the pulse s
73. uire Histogram 36 Acquire History 36 Guassian Fitting 36 Histogram 35 History 35 Load Histogram 36 Load History 36 Printing 37 Save Histogram 36 Save History 36 Configuration 10 Loading an INI File 10 Conventions 2 Cursors Adding 24 AutoROI function 25 Crosshair 25 Moving 24 Removing 25 DSP Editor 38 5 6 2003 Editing Parameters 39 Navigating Parameters 39 Numeric Base 39 Parameter Colors 39 Saving Parameters 39 Error File 39 Enabling Output 39 Error Report Levels 40 File Location 39 FFT See Oscilloscope Fields Selecting 4 Files FDD Files 9 INI Files 9 Gain Setting Calibrating Peaks 31 Desired Peak Position 30 Gain Setting Problems 10 Global Options 7 Graphs Axis Auto Scale 24 Fixed Auto Scale 23 Fixed Scale 23 Float Scale 24 Axis Scale Modes 23 Cursors see also Cursors 24 Default Modes 21 Page 40 Manual Kepler Software Package Linear 24 Logarithmic 24 Mini Zoom window 22 Panning 23 Reference Data Sets See also Reference Data Sets 25 Zooming 22 Zooming Main Window 22 Zooming Mini Zoom Window 22 Hardware Requirements 3 Polaris 3 Saturn 3 Hardware Setup 5 Polaris 5 Saturn 5 Help 7 Items Selecting 4 Kepler Getting Around 4 Load Files Histogram 36 History 36 INI Files 10 Reference Data Sets 26 Spectrum 31 Oscilloscope 33 Acquire Trace 33 FFT 34 FFT Averaging 34 Load FFT 34 Load Oscilloscope 34 Printing 35 Sample
74. ule handel A C library that is used by Kepler to perform I O operations to all XIA modules Further details on Handel is available on the XIA website DSP digital signal processor A small processor used to perform calculations and other slow control tasks in the XIA modules FPGA field programmable gate array A FPGA is generally a re programmable logic device FIPPI filter and pulse pile up inspector In the XIA modules the FIPPI is implemented in an FPGA and performs all real time operations in the XIA modules EPP enahanced parallel port EPP is the required communication protocol for the Saturn module GUI graphical user interface A term that generally refers to the graphical look and feel of the program When Kepler saves a GUI file it is saving the graphical state of the program INI initialization This is a term that generally refers to an initialization file For Kepler we refer to files that contain the hardware configuration as INI files Spectrum The data acquired during a run by the module This is also referred to as Multi Channel Analyzer MCA data FFT Fast Fourier Transform A FFT is a Frequency space representation of data Appendix 2 Command Short Cuts lt F1 gt Save GUI File lt F2 gt Load GUI File lt F3 gt Save INI File lt F4 gt Load INI File lt F5 gt Start Stop Run Toggle Run Status lt F7 gt Save Spectrum lt F8 gt Load Spectrum l
75. utoROI function A region of interest ROI can be defined based on an internal algorithm and the location of the cursor The algorithm first finds the nearest local maximum to the cursor position which is used as the starting point for the algorithm The data are then searched both left and right till a bottom is found the data start rising again Taking 0 25 of the difference between the peak height and the bottom sets the level used to define the ROI limits The first point to the left and right that fall below this level define the ROI limits Page 27 Manual Kepler Software Package There are 3 ways to set ROI limits e AutoROI ona cursor e Default mode Create ROI e Move ROI Cursors Move the ROI s cursors to change its boundaries mdo Kepler MAN 001 1 preliminary The AutoROI function will act on the currently active ROI please see 6 2 for details about the ROI section of Kepler If no ROI is active then one is created and the results of the AutoROI are applied to this new ROI 6 2 4 Changing ROI boundaries You may want to change the boundaries of an ROI In particular when a new ROI is added it will initially have no settings for its lower and upper bounds Kepler has three methods of setting boundaries all of which work only on the active ROI 1 Use the autoROI function associated with cursors see 6 2 3 below 2 Set the graph to the create ROI default mode or hold the hotkey associated
76. utomatically changed during data collection Saturn Run Control Start Run Saturn Run Control Stop Run Run ControlStart Run Run ControlStop Run Start Run Stop Run lt F4 gt A data acquisition run can be started using several methods within Kepler two of which are shown in the sidebar Once the run is started it can be stopped using the same control or any of the other methods The text on the control should change to indicate the status of the control The methods to control run starts and stops are 1 Single clicking the entry in the DAQExplorer Saturn Run ControbStart Run with the left mouse button 2 Using the menu item Run Control Start Run which can be accessed by either left clicking on the menu item or using the hotkey lt F4 gt 3 Using the button located on the upper left corner of the spectrum display to start or stop a run When a run is started the y axis scale mode for the spectrum display see 5 4 is set to fixed auto scale which will keep the spectrum in full view while data is being acquired This mode does not apply to the x axis allowing X axis zooming to view a particular portion of the spectrum After the run is completed stopped either by you or by Kepler Kepler restores the y axis scale mode that existed prior to the run Sections 4 3 4 5 4 6 and 4 7 discuss more controls in Kepler related to data acquisition management 4 3 Resuming a run Y Clear Spectrum at Run Start I
77. y 92 30 88 86 84 82 80 78 76 74 Baseline ADC Counts 72 70 68 66 64 62 Pi i D 1 j o 5 10 agent v woy vi Linear Time ms E Zoom Glatz Baseline Histogram 34000 32000 30000 28000 26000 24000 22000 20000 18000 Counts 16000 14000 12000 10000 H 20 1 1 1 1000 D 1000 Baseline Energy eV Mean 63 39 eV 1 1 1 1 H H 4000 3000 2000 2000 3000 4000 Zanen v soy vI inex 25 30 Zoom Close FWHM 144 97 eV Figure 8 The baseline history and histogram display in Kepler The left pane shows the baseline history and the right shows the histogram 7 2 Baseline History and Histogram Baselines are integral to the energy measurement and their history can be very useful in tracking certain classes of hardware problems 5 6 2003 Tools Baseline lt CtriH F7 gt Saturn Diagnostics Baseline As noted in 4 1 1 the spectroscopy module determines the energy of pulses from the preamplifier by time averaging them using a trapezoidal shaping filter For each pulse the peak value of the filter output is captured and corresponds to the energy of the event that produced the pulse In order for this process to be accurate the module must track the amplitude of the filter output when no pulses are being processed which is called the filter s baseline At times noise or other events can cause
78. y appear when you right comparisons between past and present data However only the spectrum click on the graph axes display in the Kepler window allows detailed analysis of ROIs are different from those There are two methods to access all the settings described below that ap Jp ear when y On 1 through the series of drop down list boxes in the upper or lower left right click on the main E bak depending on the graph corner of the graph display or plotting area 2 by right clicking on the graph itself and using the drop down menus that appear Different drop down menus are available on the axes and the main graph area but all should be self explanatory 5 1 Default Modes In the graph display bar the first drop down box on the left lets you set the default mode The chosen default mode defines how the graph will act when the left mouse button is pressed on the graph window in combination with no 5 6 2003 Page 21 Manual Kepler Software Package mdo Kepler MAN 001 1 preliminary other keys The choices are Zoom Pan and None for most graphs while the spectrum window has the additional option for Create ROI Each of these options is described in more detail below If None is selected then no action is performed when the left mouse button is pressed 5 2 Zooming When problems are encountered while zooming or panning lt Ctrl A gt can be very useful for recovering The two Zoom methods 1 Select
79. y select the same entry from the menu again 5 6 4 AutoROIl function This cursor function will automatically create a region of interest ROT based on the current cursor position Please refer to 6 2 for general information regarding ROIs and 6 2 3 for more details about the autoROI function Page 24 Manual Kepler Software Package mdo Kepler MAN 001 1 preliminary 5 6 5 Removing a cursor To remove a cursor from the plot right click on the cursor and select Delete Reference sets can be created from data in Kepler or from files on disk At any time a reference set can be saved to disk A reference set that has data in memory will have a checkmark by the appropriate number The menu item of a reference set available for display or scaling is shown in bold face Scaling a reference to the area in the graph data is a good way to compare two sets of data taken with different run times and or input count rates 5 6 2003 5 7 Reference Data Sets Reference data sets or reference sets can be very useful for comparing data taken under one condition with data taken under slightly or not so slightly different conditions Reference sets in Kepler behave in a similar manner to digital oscilloscope references storing data in memory and allowing you to recall the data at a later time Kepler also allows you to both save reference data sets to disk and load data from disk as a reference set The graphical dis

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