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black box a330 manualHigh-quantum efficiency and ultra-low-noise electronics make PIXIS cameras ideal for demanding low-light applications. The high sensitivity amplifier reduces read noise for weak signals, and the high capacity amplifier offering increased effective dynamic range. This software also fully supports IntelliCal automated wavelength and intensity calibration. By proceeding navigation on this page, you agree to the use of cookies according to the terms of our Privacy Policy. This detector provides excellent response from the vacuum UV to the NIR. The high system reliability is ideal for OEM and laboratory applications.Thank you, for helping us keep this platform clean. The editors will have a look at it as soon as possible. It fully supports the company’s PIXIS, PI-MAX 3, ProEM, PyLoN and Quad-RO cameras as well as Acton series spectrographs, including the LS785. The proprietary and patent-pending IntelliCal spectrograph calibration method ensures pixel-by-pixel wavelength and intensity accuracy by using NIST-traceable references. The company’s PI-MAX 3 intensified CCD cameras can be controlled through LightField via a virtual dashboard akin to a laboratory oscilloscope. The automated IntelliCal feature enables calibration of entire spectra in both the wavelength and intensity scales against the NIST database. The spectral response of all elements in the detection path, including that of the grating and the camera, has been taken into account. The accuracy of IntelliCal calibration can be as much as 10 times better than standard calibration, the company says, allowing researchers to compare their data on absolute scales. Researchers performing time-resolved imaging and spectroscopy will benefit from the new release. Whenever a PI-MAX 3 intensified CCD camera is connected, LightField automatically displays SuperSynchro timing and intensifier control. Users can interactively drag and adjust the gate delay, width, SyncMaster and auxiliary delays on the fly.https://1-pigeon.com/userfiles/1601528454.xml
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Synchronizing the camera with external lasers is simple.Additional features include automatic hardware detection with intelligent default setup, automatic saving of every acquisition (complete with raw data and experiment settings), direct streaming of multigigabyte pixel data to hard drive, “live vs. The software runs on Microsoft Windows 7 Professional and Ultimate operating systems. Visit company website About this supplier There are 134 companies listed in the Photonics Buyers' Guide.Single-Rail Positioning Stage H2W Technologies Inc. Compact LED Drivers Cuvee Systems Fluorescence Live-Cell Imaging System CytoSMART Technologies Scratch Inspection System Xiris Automation Inc. Subscribe FREE to our newsletters. By using this website, you agree to the use of cookies unless you have disabled them. High QE and ultra low-noise electronics make the PIXIS: 1024 series of cameras ideal for demanding, low light applications such as astronomy, Bose-Einstein Condensate (BEC), solar cell inspection, chemiluminescence and fluorescence imaging. Dual speed operation at 100kHz or 2MHz enables these cameras to be used both for steady state as well as fast kinetics studies.Find out more. The unique mechanical design, where the fibreoptic faceplate extends outside the vacuum, offers flexibility for optimizing performance at specific x—ray energies. The PIXIS-XF offers increased effective dynamic range with a high capacity amplifier. This software also fully supports IntelliCal automated wavelength and intensity calibration. By proceeding navigation on this page, you agree to the use of cookies according to the terms of our Privacy Policy. This version has been partly inspired by Joe Lowney’s GitHub project ( ). The module looks for Picam.dll either at a path provided by the user or at the path provided in the environment variable PicamRoot, which is created by the PICam installer.http://gopherscopes.com/userfiles/em1000-electricity-meter-manual.xml It supports most of the standard featuresI have decided not to implement a non-blocking version of the imageHowever, this function does not check for overlapping ROIs! If camID is None, this functions connects to the first available camera (default). It reads all available data at once into a numpy buffer and reformats data to a usable format. If there is no parameter of this name, the function returns None and prints a warning. This number is essentially limited by the available memory. This parameter is important when using external triggering. In order to apply all changes, sendConfiguration() has to be called. If the parameter value cannot be changed, a warning is printed to stdout. If an error occurred, it prints the error message to stdout. This technical note will first provide a review of critical problems inherent to traditional calibration techniques and then present basic IntelliCal theory, comparative data, and key implications of the new method. The development of IntelliCal was fueled by the desire to surmount several shortcomings associated with traditional wavelength calibration methods, especially overreliance on user input for accuracy. By and large, the post-calibration wavelength accuracy is not known by the software programs utilized in these traditional routines, so its determination is left up to the user. Figure 1. IntelliCal source installed on an Acton Series SP2300 spectrograph from Princeton Instruments. Using a source with multiple known emission lines to illuminate the entrance slit of the spectrograph, it is possible to determine a direct wavelength-to-detector pixel coordinate correlation. There are two common types of wavelength space calibration: (1) a polynomial fit where only two or three emission lines are used and (2) a fit to the Czerny-Turner model. Some routines utilize a polynomial fit to define the spectral dispersion across the focal plane and thus obtain calibration results at the pixel level. This technique, in which a polynomial is fit to a plurality of known emission lines, is both the more accurate and more tedious of the aforementioned methods. The user must not only determine which emission lines are seen by the detector, but must redo the calibration each time the grating is moved. All rights reserved. The most commonly utilized wavelength space calibration is a fit to the Czerny-Turner model. Here, the user is prompted to select a known emission line and the grating is moved so as to position the selected line at two or more locations across the CCD. The grating is then moved to a different line. This process is repeated at least once. Next, the wavelength space residual is defined and minimized with respect to the. IntelliCal simulates the entire observed spectrum; the number of observables is always equal to the number of horizontal pixels in the CCD array. No significant user input is required. The ultimate aim of IntelliCal is to minimize the residual difference between observed and calculated emission line spectral intensities. This goal is realized. The comparisons are made in terms of wavelength error as a function of calibration line wavelength. Figure 5. Wavelength error as a function of calibration line wavelength shows comparative calibration accuracy of IntelliCal versus Czerny-Turner model (500 mm focal length). Figure 6. Wavelength error as a function of calibration line wavelength shows comparative calibration accuracy of IntelliCal versus Czerny-Turner model (300 mm focal length). Unlike traditional methods, the software is now aware of the instrument it is calibrating. Furthermore, the fully autonomous IntelliCal routine eliminates user error. Of course, the name of the game is accuracy. By treating every pixel in the detector as an. It’s that easy! For additional information about IntelliCal technology, please contact Princeton Instruments.Prices are indicative only and may vary by country, with changes to the cost of raw materials and exchange rates. Read the press release. See soft x-rays and more. Princeton Instruments SOPHIA-XO cameras are engineered to deliver the highest direct-detection performance for applications that involve x-ray spectroscopy, x-ray imaging, x-ray microscopy, x-ray plasma diagnostics, and EUV lithography. Looking for ultra-low-noise CCD cameras. Visit the SOPHIA camera page. Products Detectors Fiber Optics Instruments Interferometry Lasers Light measurement Lightsources Optical Components OEM Components and Parts Enquiry If you continue to use this site we will assume that you are happy with it. Ok Privacy policy. We are a non-profit group that run this service to share documents. We need your help to maintenance and improve this website. The Moment is a true global shutter CMOS camera with an ultra-compact form factor, powered through USB 3.2 Gen 2. The PVCAM driver SDK can also be used integrate into other software packages. Advanced fluorescence microscopy techniques take advantage of this. Stories and images from scientists using our high-performance sCMOS, EMCCD and CCD cameras to advance their research. USB 3rd gen. device driver (32.2.4) improvements. Updated PVCamTest application (3.10.318) with Improved streaming to disk with Kinetix.Existing PVCAM Drivers for Mac OSX will continue to be available for legacy products. Users are welcome to test this configuration for suitability on their systems. Please contact your sales representative or a Teledyne Photometrics service professional with questions or to provide feedback. Teledyne Photometrics is not able to provide support for this version of PVCAM. Ubuntu 18.04, kernel 4.18 recommended. Implemented user memory pinning for DMA in PCIe driver, enabled for kernel 5.3 and newer. Added support for virtual frame rotation and flipping. Added support for SW trigger feature. Improved polling acquisition behavior on Linux. Minor bug fixes and performance improvements.If you experience any issues with the connection or performance on AsMedia-based USB controllers, please try this alternative USB controller driver. However, these updates cause performance drops in the functionality of Texas Instruments (TI) FireWire Controllers which ship with some older Teledyne Photometrics cameras. These performance drops manifest with the following symptoms: This remedies any problems caused by the updates. Includes PCIe device driver version 3.26.404 that improves the reliability of Prime-95B data transfers over sequences longer than 10,000 frames. Requires Prime-95B firmware 19.27 or newer. PVCamTest application now supports latest cameras and latest camera features. Fixed an acquisition timeout for cameras that support Variable Timed Mode on USB interface. (Retiga R-series). Improved RsConfig tool, no longer requires administrator rights. No new PVCAM SDK is required for use with the new PVCAM runtime. See Manual for details If unsure, we recommend two specific configurations from Dell and HP below. These configurations are used in-house when testing currently supported cameras. We recommend verifying the number of available PCI-Express lanes on the CPU prior to the purchase and making sure at least 8 lanes can be dedicated to the camera interface. For this reason, the 4 x 16 GB option is recommended. If this scenario is required when operating the camera, we recommend the Dell configuration above. By proceeding navigation on this page, you agree to the use of cookies according to the terms of our Privacy Policy. 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To make your purchase as simple and easy as possible, please refer to the detailed policies listed below.Some specific purchases aren't covered by eBay Money Back Guarantee Learn more eBay Money Back Guarantee disclaimer - opens in a new window or tab. All Rights Reserved. User Agreement, Privacy, Cookies and AdChoice Norton Secured - powered by DigiCert. By continuing to browseFind out about Lean Library here Find out more and recommend Lean Library. This product could help you Lean Library can solve it Simply select your manager software from the list below and click on download.Simply select your manager software from the list below and click on download.For more information view the SAGE Journals Sharing page. Search Google ScholarSearch Google ScholarFind out about Lean Library here Search Google ScholarBy continuing to browse. Page Count: 62 No part of this publication may be reproduced b y any means without the written permission of Princeton Instruments, a division of Roper Scientific, I nc. (“Princeton Instruments”). Printed in the United States of America. IntelliCal and SpectraSense are trademark s, and IsoPlane and LightField are registered trademarks of Roper Scientific, Inc. T he in f or ma t io n i n t h is p ub l ic a t io n is be l ie v e d to be a c cu ra t e a s o f t he p u b li ca t io n r e le a se d a te. H ow ev e r, Pr in c e to n I n st r um e nt s do e s n ot as s um e a ny re s po ns i b il i ty for a ny con s e qu e nc es in c lu d ing a ny da mag e s re su lt in g f r om th e u se th ere of. Th e i nfo r ma ti on c on t ai n ed he re in is sub jec t t o c han ge w it hou t n oti ce. Re vis ion of th is pu bl ica ti on may be i s su e d to inc or po ra te su c h c ha nge. Its advanced optical design reduces astigmatism to zero, increasing spatial and spectra l resolution dramaticall y over traditional spectrographs. Large-diameter optics and interchangeable triple-grating turrets permit operation from the UV to NI R with extremel y low light leve ls at high, low or intermediate spectral resolution. IsoPlane includes 32-bit microprocessor controlled scanning, built-in USB and RS-232 interfaces, and a micrometer-controlled entrance slit. In addition, it has a direct digital grating scan mechanism with full wavelength and grating control capabilities. Figure 1- 1. Light Path within the I soPlane SCT 320 Connect the USB port of the IsoPlane to the USB port on the control computer using the USB cable provided. RS-2332 may also be used if a USB port is not available. 5. Install the grating turret that is shipped in the same shipping box with the IsoPlane but is packaged outside the IsoPlane housing to protect the gratings during shipment. See Section 2.7 Turret Installation (starting on page 12 ) for detailed installation instructions. 6. Turn on the power switch on the IsoPlane power suppl y and the IsoPlane should initialize to zero wavelength. Light Field combines complete c ontrol over Princeton Instruments’ spectrographs and detectors with easy- to -use tools for experiment setup, data acquisition, and post-processing. 2.2.1.2 WinSpec WinSpec is a 32-bit data acquisition platform that has been optimized specifically for digital spectroscopy. WinSpec provides complete control over the IsoPlane and all other Acton Series spectrometers. This software control extends to all instrument options, such as multiple gra tings, multiple entrance and exit ports, and motorized slits. SpectraSense software will control and acquire data from both single channel detection systems, which require scanning of a monochromator, and CCD-based detection systems that may or ma y not re quire rep ositioning of a spectrograph. 2.2.2 Controllin g the IsoPlane at th e Command Leve l Although it requires more programming on the user’s part, the IsoPlane can also be controlled with direct commands through its USB port or RS-232 port. This operation is described in Appendix A Using the Monochromator Control Software (starting on page 39.) 2.3 Computer Interface Connectors: USB and RS- 232 Figure 2- 1. Details of the RS-23 2, USB, and Po wer Connections on th e IsoPlane 2.3.1 Cables and Connection s for IsoPlane The following computer cables are supplied with the IsoPlane: ? 3650-USB-06 USB Cable Type A to Type B. ? CC -4 99 - 2 I B M A T or c o mp at i bl e 9 -p in f e ma le ( DB 9S ) c o nn ec t or t o 9- pi n ma le c o nn ec t or ( DB 9 P). If neither of these cables is compatible with your sy stem, consult Princeton Instruments for a custom cable.I f the shutter is installed, it is located in the Turret Compartment and is mounted to the spectrograph wall. Its shutter cable plugs into a keyed 2-pin shutter connector in the floor of the IsoPlane. The e xternal connector is below the detector mounting plate and can be connected via a shutter cable to a d et ector with a SHUTTER connector. If a detector does not have a SHUTTER connector (PI-MAX detecto rs, for example), the Princeton Instruments SHC-EXT Shutter Control Box can be used to control the opening and closing of the internal shutter. If the control box is not available, the internal shutter can be removed. Instructions for installing and removing the internal shutter assembly are provided in Sections 2.13.1 and 2.13.2, respectively. 2.6 Mounting Accessories to an IsoPlane Slit Assembly All Princeton Instruments spectroscopy accessories come with their own set of instructions for proper mounting and operation. The instructions below a re only general information. Please refer to the individual instructions for detailed infor mation. Accessories: The full range of spectrog raph accessories mount directl y to the IsoPlane entrance slit assemb ly (m anual or motorized). To assist you in mounting accessories, a drawing I n t his case, Princeton I nst ruments provides spe cial slotted ho les in the lig ht source housing to facilit ate mounting the sou rce to the slit. 2.7 Turret Installation If you have just received an IsoPlane spectrograph, y ou will need to install the grating turret. T he grating turret has been shipped in the same shipping box with the IsoPlane but is packaged in a plastic container outside the IsoPlane housing to protect the grating s during shipment. CAUTION 1. The optical sur faces in the spec trograph are extr emely delicate and can be perm anently dam aged by contact with so lid objects as wel l as with most liquid s and aeroso ls. 2. DO NOT T OUCH optical surfaces w ith anything. Wear thin protectiv e powderless glov es to minim ize damage from body oils if you accidental ly touch any optical surface, esp ecially the grating. 3. Avoid talking or s neezing n ear optical surfaces. Do not brea the directly on them. The following procedure is for the initial installation of a grating turret.Th is se ts th e t orq ue o n the sp in d le co rre ctly. Note: You cann ot overtigh ten this screw. It is designe d to slip once the co rrect torque is attained. 11. Pl ac e t he T u rr et Co ver o n t he spe ct rog ra ph. R ep la ce a nd ti gh ten a ll of t he cov er s cr ew s. 12. Re pla c e the pl ast ic co ver on t he s tor ag e c on ta ine r a nd s tore i t in a sa fe l oca tio n. 13. Pl ug th e p owe r s upp ly i n to a n ou tl e t a nd c onn ec t th e s upp ly to t he Is o Pl ane. Tu rn on the I soP la ne to a ll ow f or au to -id ent ifi ca ti on of th e g rat ing tu r re t. Not e t hat if t he p ow er s up ply is on w hi le a t ur ret is be ing in st al le d, t he Is oP la ne sh oul d a lw ay s be re - st ar ted af ter war d s. Figure 2- 4. Center Torque Screw Figure 2- 5. Location of Ho le on Turret Grating Assembly Hole Center Torque Screw Figure 2- 9. Mounting Plat e Note: Refer to the detector’s system manual for specif ic instructions on how t o mount the array detector to the m ount ing plate. These in structions vary with the detector no se desig n. The basic actions are listed below. Refer to Chapter 3 of this manual for detailed LightField and WinSpec instructions for performing this function. For other application software, refer to t hat software’s manual or help file. 1. Make sure the computer interface cables (for the spectrograph and de tector) are connected. 2. Verify that the power supplies are plugged into an AC source a nd are connected to the spectrograph and detector. 3. Turn on the power to the spectrogra ph and the detector. 4. Start the application software. 5. Loosen the rotation adjustment screws (see Figure 2-9) enough that you can rotate the detector.This general procedure assumes that you have already mounted the array detector to the exit port of the spectrograph and that there is a light source at the entrance port. Note that as foc us is improved, the intensity of the spectral line will increase. It is important to adjust the acquisition time to keep the entire spectral line on scale. 6. Tighten down the locking set screw. 7. Place the Micrometer Compartment cover on the spectrograph. Replace and tighten a ll of the cover screws. Figure 2- 11. Micrometer Lockin g Set Screw Locking Set Sc rew Micrometer Com partment H ow ev er, in so me i ns ta nce s w he n a CC D ca me ra is a tt a ch ed, th e cen ter p ix e l o f th e C CD c am er a may be lo ca te d sl ig ht ly a bo ve or be low th e op ti c al ax is of t he sp e ct ro g rap h. I n m os t a pp lic at io ns thi s i s no t cr it ic al: h owe ver, i f i t is im por ta nt to ha ve t he e xit fo c al pl a ne im age pre ci se ly c en ter e d o n th e CCD, th e h e ig ht of th e e xit be a m c an be a dj us te d us ing t he p roc edu re i n thi s sec ti on. If you have an optical fiber and fiber adapter that can precisely center the beam at the center of the I soPlane focal plane, then that can be used as a g uide in positioning the exit focal plane. If the IsoPlane is equipped with a standard 3 mm manual entrance slit or optional 3 mm motorized entrance slit, you can also install the supplied 4 mm high slit baffle a nd use the 4mm high image as a guide in positioning the exit focal plane.Refer to the drawing be low. Note: Dam age May Be Done I f Slit Jaws Are Opened Wider Than 3.0 m m. Slit Width Microm eter Settings Slit Width Adjustable from 10 Micrometers to 3000 Micrometers (3 mm) Figure 2- 13. Slit Width Setting: 200 Micrometers (0.20 0 mm) Figure 2- 14. Slit Width Setting: 1380 Micrometers (1.38 mm) When the power to a spectrograph is turned off, the slit remains in the position to which it was last set. Lift the cover and screws off of the IsoPlane and set them aside. 2. Remove the grating turret. If you are not sure how to do this, refer to Section 2.14 Turret Removal on page 24. 3. Use extreme care so as not to touch the grating surfaces. 4. Mount the shutter assembly on the two soc ket head screws above the entrance slit. Make sure the connector on the cable aligns with the connector in the floor. 7. Re -install the grating turr et. If you are not sure how to do this, refer to Section 2.7 Turret Installation on page 12. 8. Place the Turre t Compartment cover on the spectrograph. Replace and tighten all of the cover screws. Screws Shutter Shutter Cable Connector This is because there is no way for these detectors to keep the shutter open or to open the shutter during an acquisition. If you a re not sure how to do this, refer to Sect ion 2.7 Turret Installation on page 12. 9. Place the Turret Compartment cover on the spectrograph. Shutter Shutter Cable Connector Screws Do not brea the directly on them. The following procedure is recommended for re moving the grating turret from the IsoPlane’s Turret Compartment. I f th e tu rr et ca n no t b e l ift e d up, y ou may ne ed to lo ose n t he Ce nt er To rqu e S c re w m or e. 5. P ut th e r em ove d g rat ing t ur re t a sse mb ly in to th e p rot e ct i ve c ont ain er i t w as sh ipp ed in. Figure 2- 15. Center Torqu e Screw Center Torque Screw Ot he rwi se, y ou n eve r h ave to in ter c ha nge t u rr ets. The IsoPlane is supplied with one on-axis mounted triple grating turret assembly, but you may order up to three (3) grating turrets for the spectrograph. If you have multiple turrets (2 or 3), the built-in sensing mechanism will auto-identify for the software which grating turret is installed. You may, however, want to label the turrets (for example, with the spectral range used). CAUTION 1. The optical sur faces in the spec trograph are extr emely delicate and ca n be permanent ly damaged by contact with so lid objects as wel l as with most liquid s and aerosols. 2. DO NOT T OUCH optical surfaces w ith anything. Wear thin protectiv e powderless glov es to minim ize damage from body oils if you accidental ly touch any optical s urface, especial ly the grating. 3. Avoid talking or s neezing n ear optical surfaces. The following procedure is recommended for interchanging gra ting turrets. B ec ome fa mil iar wi th the gr a ti ng tur r et a nd it s co mpo nen ts. 5. L oos e n th e Ce n ter T or que S cr ew (s ee Fi g ur e 2 - 17 ). I f th e tu rr et ca n no t b e l ift e d up, y ou may ne ed to lo ose n t he Ce nt er To rqu e S c re w mor e. 7. P ut th e r em ove d g rat ing t ur re t a sse mb ly in to th e p rot e ct i ve c ont ain er i t w as sh ipp ed in (a lig n th e po st a nd h ole ). Th is se ts th e tor que o n the sp in dl e co rre ctly. I t designed to slip once the co rrect torque is attained. 15. Pl ac e t he T u rr et Co ver o n t he spe c tr ogr aph. R epl a ce an d t igh ten a ll of t he c ove r scr ew s. 16. Pu t the re mo ve d g ra tin g t ur re t i n to t he sto r ag e c ont a in er: a li gn th e ho le in th e g ra ti ng tu rre t a ss e mb ly wi th the ve rt ica l po st on the bo tto m p lat e of t he sh ipp ing co nta ine r, an d ti gh te n th e Ce nte r To rqu e S cr ew unt il it c li c ks. Re pla ce t he pl as ti c c ov er an d sto re the co nta ine r in a saf e lo ca ti on. 17. I f t he I soP lan e’ s p owe r s upp ly i s o n, r e-s tar t t he I s oP la ne t o a ll ow a ut o- ide nt ifi ca ti on of the ne w g ra ti ng tur r et. I f the po we r s upp ly i s o ff, t he a ut o- ide nt if ica tio n w il l o ccu r t he ne xt ti me y ou tur n the su pp ly o n. Figure 2- 17. Center Torqu e Screw Center Torque Screw Lift Turret up out of the Turret Compa rtment Figure 2- 19. Loca tion of Hole on Tu rret Grating Assembly Figure 2- 20. Loca tion of Post on Grating Spindle Assemb ly Hole Post This chapter also points out how to perform alignment using the software. Further information about operating the system can be found in the appropriate software manual or help file. Warnings: 1. A PyLoN with an internal shutter or a SPEC- 10 with an internal shutter CAN NOT be used with an IsoPlane spectrog raph. 2. If the detector ha s a flange m ount and has an interna l shutter, DO NOT USE the Sh utter connector to drive a shut ter internal to an I soPl ane. If both the d etector and spect rograph have shu tters, the IsoPlane shutter w ill have to be rem oved or a Pri nceto n Instrum ents SHC-EXT Shutter Contr ol Box can be used to cont rol the opening and closing of the IsoPlane’s in ternal shutter. The detector is mounted to the IsoPlane. ? The detector and IsoPlane are connected to the computer via the a ppropriate communications cables. ? The detector and IsoPlane are powered on. ? If the detector is LN-cooled, the Dewar has been filled. 3.3 Initialization When power is turned ON to the IsoPlane, it initializes to a wavelength of 0.0 nm for grating number 1. If the power is switched OFF and then ON again to the IsoPlane, it will re-initialize. Initialization gives the system a refere nce, or starting position to keep track of wavelength position, grating location, and other parameters. Alternative start-up parameters can be programmed if the factory defaults are not suitable (s ee Appendix A ). Before you can design a new experiment or run an existing one, the appropriate device icons must be dragged into the Experiment Devices panel. Once there is at least one device, the Experiment Settings panel will be populated with expanders for groups of experiment settings. Note: I f the IsoPlane (SCT- 320) icon is the only dev ice in the Experiment Dev ices panel, the Spectrograph expan der will be th e only expander in the list. When y ou drag a detector in to the panel, the Calibration expande r and all of the detector- related e xpanders will be d isplayed. 3.4.1 Define the Dete ctor and Spec trograph Figure 3- 1. LightField Ava ilable Devices panel 1. After LightField opens, you should see an icon representing your detector in the Available Devices area.Because this is a new experiment, the default settings for the detector will be active. The Status bar (a t the bottom of the window) displays an icon for temperature status.