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SPECTROSCOPY

1. Hd v Image spectra may be acquired using KestrelSpec imaging spectroscopy software for Windows See pages 14 15 of this brochure of additional detail V CCQ GOM ASGENT versus ALTA SERIES CAMERAS LOWER COSTS Many applications require clean quantitative images but do not require the ultimate in cooling or low readout noise The Ascent is an ideal solution for many applications where several thousand dollars may be more important than a few electrons HIGHER THROUGHPUT Ascent was designed to operate at speeds up to the maximum allowed by USB2 Digitization speed is programmable so you can choose your ideal trade off between speed and noise All speeds digitize at a full 16 bits ASCENT LOW READOUT NOISE Alta s readout electronics were designed to minimize readout noise The higher speed software selectable 12 bit mode is intended for focussing and not optimized for low noise ADVANGED COOLING To maximize heat dissipation Alta s large inner chamber back plate and heatsinks are machined from a single block of aluminum The four fans have four programmable speeds VERY LARGE FORMAT CCDS The Alta platform is available in several housing sizes accomodating CCDs up to 50mm on a side OPTIONAL ETHERNET An optional ethernet 100baseT interface is available for the Alta platform COMPACT HOUSING The Ascent s smaller more lightweight housing fits in many pla
2. eos E V BACK ILLUMINATED amp OPEN ELECTRODE CCDs CCD47 10 1024 1024 1048576 Apogee also offers a variety of spectroscopic vx ceca ww sel oer FRONT ILLUMINATED EMCCDs We U6 70 U16M Ew TETCo47 esa 4o6 320068 10 el soj Sef saj MC U9000 ES a FRONT ILLUMINATED CCDs A 40 Camera Total Pixel Size Atr y size mm Imaging Area Diagonal Mono M Model Kodak CCD Array Size Pixels microns mm2 mm Color C Ed m E13 Absolute QE 2 ure kareson 406 e iernne 9 369 3e9 asso sai M t OO N NO Ne CO KALAD U2000 A2000 KAI 2021 1600 1200 1920000 74 1L8 89 105 1 EM247 3 UE NES ET ES CJ Wavelength nm A complete set of camera data sheets as well as i oes V WWW CC d COM Back illuminated Kodak Blue Plus Microlensed KAI 11002 CAMERA DATA SHEETS mechanical drawings are on our Integration Starter Kit CD or at www ccd com U16M KAF 16803 4096 4096 16777216 36 9 36 9 1359 0 521 M UIMM 4096 4096 9 369 369 DI M mm i U9 0 U9 A9 KAF 6303E 3072 2048 6291456 9 276 184 509 6 m ZOE aa I v rumes o 208 seco mi FRONT ILLUMINATED CCDs U32 A32 KAF 3200 2184 1472 32148
3. increments to a maximum of 336 milliseconds per row shift The minimum TDI shift time is the digitization time for one row TDI cannot be done with cameras using interline CCDs such as the U2000 and U4000 www ccd com KINETICS MODE Kinetics Mode assumes that the user has optically masked off all but the top most section of the CCD This exposed section is illuminated shifted by x rows then exposed again until the user has exposed the entire surface of the CCD with y image slices Exposed Area Region of Interest User Defined Fixed Height The image in the exposed area is shifted to the masked area per software command pre set shift frequency or external trigger The number of rows per section is predetermined and constant Exposure 2 When the number of desired exposures has been reached or the CCD has been filled whichever comes first the entire array is read out and digitized If you want to use the entire CCD including the exposed area then the light source needs to be shuttered after the final exposure externally electronically or electromechanically or using an Exposure 5 IMAGE SEQUENCES Image sequences of up to 65535 images can be acquired and transferred to camera computer memory automatically A delay may be programmed between images from 3277 microseconds to 21 43 seconds This does not mean you can acquire images every 327 microseconds it means you can program
4. 1020 Sundown Way Ste 150 o e e Roseville CA 95661 USA tel 916 218 7450 fax 916 218 7451 INSTRUMENTS INC http www ccd com 2007 Apogee Instruments Inc
5. Venezuela University of Auckland New Zealand University of Bern Switzerland University of Birmingham UK University of Bologna Italy e Universidad de Entre Rios Argentina University of Chicago Universities of Alaska Arizona Arkansas California Colorado Georgia Hawaii Idaho Illinois Indiana Iowa Maryland Massachusetts Michigan Nevada North Carolina Pennsylvania Texas Virginia Washington Wisconsin and Wyoming University of the Free State South Africa University of Hong Kong University of Latvia e University of Leicester UK University of Ljubljana Slovenia University of London Observatory UK University of Manchester Jodrell Bank Observatory UK University of Manitoba Canada University of Melbourne Australia University of Miami University of Munich Germany University of Notre Dame University of Sao Paulo Brazil University of St Andrews Scotland University of Toronto Canada University of the West Indies University of Zurich Switzerland e US Naval Observatory Valencia University Observatory Spain Vanderbilt University Vatican Observatory Virginia Military Institute Visnjan Observatory Croatia e Warsaw University Observatory Poland Waseda University Japan Wayne State University Weizmann Institute Israel Westinghouse Wise Observatory Israel Yale University Yerkes Observatory University of Chicago Yonsei University Korea
6. and minimum exposure time Alta cameras use three shutter types depending on the aperture Apogee shutters use lower voltage coils then those listed as standard by the shutter manufacturers roughly 1 2 of the standard voltage requirement The lower voltages extend the lifetimes of the shutters D1 housing small format sensors Vincent Uniblitz 25mm Shutter D2 housing medium format sensors Melles Griot 43mm Shutter D7 housing large format sensors Melles Griot 63 5mm Shutter Full frame CCDs typically require an electromechanical shutter unless the light source is gated in some other way Otherwise light falling on the sensor during the readout process corrupts the image Interline CCDs shift the charge from the photodiode section of each pixel to the masked storage diode For low light applications the mask is sufficiently opaque to prevent smearing However in high light applications interline CCDs require electromechanical shutters to prevent smearing during readout COMPACT DESIGN The Alta systems are designed to be very compact At 6 x6 and only 2 2 thick with no external electronics the Alta system packs a lot of power into a small package The Alta systems are more than a kilogram lighter than than their predecessor Alta cameras with small format CCDs have a 0 69 17 5 mm C mount back focal distance for direct interface to microscopes and C mount lenses Medium format sensors use the D2 hous
7. 848 68 149 100 148 7 SUE A8300 U2 A2 KAF 1603ME 1536 1024 1572864 9 138 92 127 4 U13 KAF 1301E 1280 1024 1310720 16 20 5 164 335 5 262 M UB 1280 1004 ef 205 22 M ULAI KAF 0402ME 768 512 393216 46 319 83 M E32 E2 E200 El g 76 50 o 9 B M es m0 ADR The U10 uses an E2V formerly Atmel formerly Thomson TH7899 CCD INTERLINES 50 INTERLINE TRANSFER CCDs g 4 A16000 U4000 OD Camera Total Pixel Size Array size mm Imaging Area Diagonal Mono M A11000 E4000 30 Model Kodak CCD Array Size Pixels microns mm2 mm Color C T A16000 KAI 16000 4872 3248 15824256 866 5 m A11000 KAI 11002 4008 2672 10709376 9 36 24 867 5 U4000 A4000 KAI 4021 2048 2048 4194304 229 7 EMCCD 0 400 440 480 520 560 800 840 880 920 960 1000 KESTRELSPEC SPECTROSCOPY SOFTWARE Alta and Ascent cameras are supported by KestrelSpec real time Windows imaging spectroscopy software from Catalina Scientific KestrelSpec content 1996 2007 Catalina Scientific Instruments LLC Download a demo version of KestrelSpec Lite from www catalinasci com along with the user manual and a tutorial LITE amp FULL VERSIONS FEATURES e Completely integrated camera and spectrograph control for supported instruments e Calibrate single order spectrographs using least squares spline or polynomial fit e Calibrate scanning spectrographs using 1 poi
8. CD with a maximum well depth of 28Ke and a typical noise of 20e With higher gains ccd output noise approaches le with a severe reduction in usable well depth The A247 uses an interline frame transfer CCD eliminating the need for a mechanical shutter and reducing smear COMPACT DESIGN The Ascent systems are extremely lightweight 0 6 kg and compact At 5 7 x 3 2 14 5 x 8 1 cm and only 1 2 3 cm thick with no external electronics the Ascent is a marvel of compact electronics The standard back focal distance for all models is about 0 32 0 8 cm OPTIONAL LIQUID CIRCULATION Apogee offers optional Ascent liquid recirculation back as well as temperature regulated liquid recirculators for customers wanting to remove heat dissipation from the area of the camera wanting to house the camera inside an enclosure or wanting supplemental cooling The limitation the temperature of the recirculating liquid must not go below the dew point SINGLE 6V POWEH SUPPLY Ascent camera systems include a 6V international power supply 100V 240V input but can be operated from a clean 6V source Specifications subject to change without notice CDs come in many shapes and sizes as well as several different architectures Some architectures were developed specifically to address the needs of extremely low light applications like spectroscopy and astronomy back illuminated CCDs Other technologies can be adapted to sp
9. CDs shutter the exposure by shifting the charge from the photodiode section of the pixel to the storage diode of the pixel exposure times can be as short as a few microseconds Time between exposures is determined by the time required to read out the entire CCD which varies from camera to camera Interline transfer CCDs cannot do time delayed integration also known as drift scan mode because charge is not transferred from photodiode to photodiode but rather into the masked storage diode ANTI BLOOMING Anti blooming AB bleeds off excess charge from individual pixels so that it does not spill over into its neighbors and cause a white stripe down the column For applications like astrophotography AB preserves the aesthetics of the image For photometric applications AB can be used if exposure times are carefully controlled to avoid excess charge The disadvantages of AB normally it lowers full well capacity and quantum efficiency SPECSMANSHIP CCD manufacturers as well as camera manufacturers both describe their products in terms of typical performance and in some cases specify worst acceptable performance A CCD data sheet may for example say typical 15 electrons noise and maximum 20 electrons noise under very specific and perhaps irrelevant conditions Asa result camera manufacturers using such a CCD must also use typical performance or sort CCDs at a potentially large increase in cost The differ
10. D is cooled Defects on CCDs do not grow over time nor do lower grade CCDs wear out faster Most lower grade Kodak CCDs no longer allow column defects These lower priced CCDs are excellent bargains You may get an unwanted surprise if you do not check the data sheets for each CCD carefully before purchasing a system Some large format CCDs allow several column defects in the standard grade CCD DARK CURRENT Thermally generated signal or dark current is not noise The shot noise component of the dark current is one element of noise which is the square root of the dark current You can correct for the dark current itself if you can measure it which requires the camera s cooling to be programmable and stable The deeper the cooling the less correction you re going to have to do E2V CCDs AIMO amp NIMO E2V s AIMO Advanced I Metal Oxide aka MPP CCDs have hundreds of times less dark current than non IMO NIMO CCDs Some variations of their CCDs such as deep depletion devices with high QE in the near IR are only available as NIMO devices KODAK BLUE PLUS CCDs CCDs create charge due to the photoelectric effect In order to create an image rather than random electricity the charge must be held where it was created Traditional CCDs using from one to four polysilicon gates carry a voltage that traps the charge until transferred Polysilicon has limited transmissivity Indium tin oxide ITO gates hav
11. OUT Alta and Ascent cameras support readout of an arbitrary sub section of the array in order to speed up frame rate Reading half the array for example does not increase the frame rate by two because of overhead required in discarding unwanted pixels TWO YEAR WARRANTY All Apogee cameras have a standard two year warranty and a lifetime guarantee against condensation in the camera EXTERNAL TRIGGERING The Alta and Ascent camera systems accept external hardware trigger signals through their camera I O ports for a number of purposes Software and hardware triggers can be used together For example a software or hardware trigger may be used to initiate a single exposure or a sequence of exposures of a specific duration and specific delay between exposures Alternatively a software trigger may be used to start a sequence and the external trigger can be used to trigger each subsequent image in the sequence In addition the external trigger can be used to trigger row shifts for time delayed integration or can be used to trigger block shifts for kinetic imaging SEALED INNER CHAMBERS The sensors for Alta and Ascent cameras are sealed into an inner chamber filled with argon The chamber has a lifetime guarantee against condensation PROGRESSIVE SCAN CONTINUOUS IMAGING Interline transfer CCDs first shift charge from the photodiode in each pixel to the masked storage diode and then march the charge through the storag
12. Research Organization Japan High Frequency Active Auroral Research Program HAARP Hiroshima University Japan Hitachi Hong Kong University of Science amp Technology e mation Indian Institute of Astrophysics Industrial Technology Research Institute ATRD Taiwan Institute for Astronomy Hawaii Institute of Astronomy Switzerland Institute of Astronomy and Astrophysics Taiwan e Institute of Atomic and Molecular Sciences Taiwan Institute for Quantum Physics Switzerland Instituto de Astrofisica de Andalucia Spain Instituto de Astrofisica de Canarias Spain Inst Estudis Espacials de Catalunya Spain International Science amp Technology Centre Russia s IVIC CBB Venezuela J Paul Getty Museum Jagellonian University Poland Japan Atomic Energy Agency Jet Propulsion Laboratory Johns Hopkins University Kimberly Clark Kim Hae Observatory Korea e Kitt Peak National Observatory Konkoly Observatory Hungary Korea Astronomical Observatory Korea Research Institute of Standards and Science Kwasan Observatory Japan Kyoto University Japan Lancaster University UK Landessternwarte Heidelberg K nigstuhl Germany Las Cumbres Observatory Lawrence Berkeley National Laboratory Lawrence Livermore National Laboratory Lick Observatory e Liverpool John Moores University UK Lockheed Martin e London Health Sciences Centre Canada Los Alamos National Laboratory Lucent Technologi
13. SPECTROSCOPY CATALOG 2007 2007 Apogee Instruments Inc 1020 Sundown Way Ste 150 il ita i fA iP EA O ee Roseville CA 95661 USA 7 7 d tel 916 218 7450 ijae fax 916 218 7451 T INSTRUMENTS INC http www ccd com SYSTEM OVERVIEW pogee Alta and Ascent cameras are designed for a wide range of demanding scientific applications In Ascent we have reduced the size and cost of our electronics and housings while at the same time maintaining the key features of our popular Alta Series cameras We ve added high speed 16 bit electronics and some new sensors with resolutions up to 16 megapixels The larger Alta cameras offer lower noise and deeper cooling than the Ascent cameras They also support very high quantum efficiency back illuminated CCDs For both camera series the direct USB 2 0 link between camera and computer allows easy installation portability and fast data transfer rate Ascent maintains compatibility with our Alta ActiveX drivers as well as Linux and Mac OS X drivers m T A li zw ME Apogee INSTRUMENTS INC DIV Y ADDS STRENGTH Since 1993 pea Instruments has been manufacturing cooled CCD cameras for scientific applications Our cameras are now used in more than 50 countries from government and private research laboratories to the best of world class professional observatories Within spectroscopy Apogee cameras have been used for a variety of techniques including LIBS
14. UAL DIGITIZATION With our fast USB2 systems we offer dual digitization high precision low noise 16 bit performance as well as high speed 12 bit for focussing and other high frame rate needs Digitization depth is selectable image by image in software MGF2 COATED FUSED SILICA OPTICS Professional grade details like magnesium flouride coated fused silica windows Apogee also offers custom windows including wedge windows and customer supplied optics SINGLE 12V POWER SUPPLY Alta camera systems include a 12V international power supply 100V 240V input but can be operated from a clean 12V source CABLE LENGTH Ethernet cabling can go to 100m USB2 cables are limited to 5m between hubs with up to 5 hubs for a total of 30m However there are USB1 and USB2 extenders available for operation up to 10 km The USB1 extenders slow the transfer to a maximum of 500 kpixels per seoond but this rate is still a far higher throughput than the E Series systems USB2 extenders are available using Cat5 cable or fiber optic cable Specifications subject to change without notice OPTIONAL ETHERNET The Alta E Series cameras first read the entire image into the camera head memory and then transfer the image to the host computer at a maximum of 200 kpixels second An Alta U47 camera with 1 megapixel reads the entire 1mage to the computer in about 1 5 seconds An E47 reads the image to the camera memory in 1 5 seconds but then
15. XEL SIZE The smaller the pixel the lower the signal that can be stored in the pixel full well capacity If the noise per pixel is the same for two cameras lower full well means lower signal to noise or compromised image quality DYNAMIC RANGE Interline transfer CCDs have at most a full well capacity of about 50K electrons If the electronics limits the read noise to 8 10 electrons this is a dynamic range of 50K 10 5000 1 or about 12 3 bits Most argue for oversampling by an extra bit or some argue even two However a 16 bit analog to digital AtoD converter does not upgrade a 12 bit imager into a 16 bit imager A Kodak KAF 1001 E Alta U6 camera using the low noise aka high gain output amplifier can be operated at 6 electrons noise with a full well of 200K electrons or a dynamic range of more than 30K 1 about 15 bits CCD GRADES Each manufacturer s specification sheet for an imager defines the cosmetic grades for that specific imager Different manufacturers use different procedures a grade of Imager A may allow column defects but a grade 2 lower grade of Imager B may not Kodak usually grades their CCDs at about 25 C and most of their defects disappear in cooled cameras when the images are flat fielded In most cases you cannot see the difference between the grades Other companies such as E2V grade their CCDs at low temperatures so their defects are less likely to disappear when the CC
16. a delay of 327 microseconds between the end of a readout and the start of the next exposure The Ascent and Alta platforms allow for three types of image sequencing Application Driven Sequencing This is the most common form of image sequencing The application merely takes a specified number of successive images This type of sequencing is suitable when the time between image acquisitions is not short and where slight differences in timing from image to image are not important Precision back to back sequencing Alta and Ascent incorporate a firmware controlled back to back image sequencing mode suitable for image 1mage intervals from 327uS to a maximum of 21 43 seconds in 327uS intervals This provides for precision spacing of images in a sequence where windows applications cannot respond Fast back to back sequencing Ratio Imaging Interlines only This is a special form of precision back to back sequencing designed for a fixed 1 microsecond spacing between a pair of interline CCD exposures The caveat with this mode is that the exposure times for each image must be greater than the readout time for the image For example if using the A2000 the readout time for a full frame is about 0 2 seconds so your exposure would need to be in excess of 0 2 seconds El lm ALTA SERIES CAMERAS OVERVIEW ADVANCED COOLING The Apogee cooling system has long been one of the most advanced in the industry The Alta contro
17. ces that the larger Alta cannot overview of the differences See camera data sheets to get details of a specific model Up to 20 Mpixels sec Note 1 40C below ambient Note 2 32 Mbytes Feature Ascent Digitization 16 bit programmable speed SHORT BACK FOCAL DISTANCE All Ascent cameras have short back focal distances of approximately 0 32 0 8cm Maximum throughput Dual channel interline readout Maximum cooling Programmable gain USB2 interface Ethernet 1OObaseT interface EMCCD SUPPORT The Texas Instruments TC247 EMCCD is supported in the Ascent platform 2 gt Optional external Note 4 Standard internal Note 5 Electromechanical shutter Vane shutter 2 gt Programmable fan speed Standard BK7 optional fused silica Field upgradeable firmware Chamber window 8 pin connector Standard Standard Peripheral communications General purpose I O port Programmable LEDs ON Power input Internal memory 32 Mbytes Wide variety of CCDs External triggering C on Optional external Note 7 Warranty against condensation Maximum speed varies from model to model Maximum cooling varies from model to model Electromechanical shutters are standard for full frame CCDs and optional for interline CCDs Electromechanical shutters are optional for all models Vane shutters are standard for smaller full frame CCDs optional for interline CCDs Standard Standard Up to 4 x height
18. curve and any unknown sample curve are then transformed by a proprietary algorithm to produce a linear function of relative intensity versus frequency Omega The temperature of the unknown source can then be calculated from the slope of this relationship between relative intensity and frequency The software calculates a least squares fit to the function and determines the temperature of the unknown source including a sigma error coefficient The accuracy of the temperature calculation can be optimized by adjusting the spectral range over which the least squares fit is operating A Back Body a 5 Vet Ts 2991 87 K peces 9149 SO of Res 00148 T uir 5 ODIUM o ra E a 4 ere ee 17500 213000 245200 T5000 Laser beam profiler display for X and Y cross section plots THANKS A PARTIAL LIST OF APOGEE INSTRUMENTS CUSTOMERS Apogee Instruments would like to express our gratitude to the thousands of customers from around the world that have brought so much to our lives since 1994 Aerospace Corporation Air Force Research Laboratory Aloe Ridge Observatory South Africa e American Red Cross Anglo Australian Observatory Ankara University Observatory Turkey Apache Point Observatory Appalachian State University Argonne National Laboratory e Astronomical Institute of the Czech Republic Astronomical Observatory Belgrade Yugoslavia Astrophysical Observatory College of Staten Island Auckland Observat
19. e diodes to the serial register Acquisition of a new image in the photodiodes during readout of the previous image is called progressive scan Alta and Ascent cameras both support progressive scan with interline CCDs FACE PLATE ADAPTERS Flange adapters allow you to attach anything from an SLR camera lens to a large instrument pack to your Apogee camera We have sizes to fit all Alta and Ascent cameras These units are machined precisely for accurate concentricity TIME DELAYED INTEGRATION More formally known in astronomy as time delay integration TDD this technique is a powerful tool for applications requring the scan of an area larger than the CCD s field of view The image is clocked down the CCD in syncronization with the object s movement The CCD must be precisely aligned with the movement of the scene The simplest way to illustrate TDI is an astronomical application The telescope is kept stationary and the CCD is precisely aligned with the sky As the Earth rotates and the sky drifts the image on the CCD is precisely clocked to continue building the image When the image reaches the last row it is read to the host computer and added to a continuous strip of sky The TDI capability utilizes a 25 MHz time base Ascents use a 48 MHz time base and local memory to achieve consistent high resolution performance TDI mode allows the user to adjust the row shift rate Timing may be adjusted in 5 12 microsecond
20. e higher transmissivity but lower charge transfer efficiency Kodak s combination of one polysilicon gate and one ITO gate is marketed as Blue Plus because of the increase in blue sensitivity The overall sensitivity of Blue Plus CCDs is much higher than multi phase front illuminated CCDs using only polysilicon gates However when researching point sources of light it is good to keep in mind that there is a marked increase in quantum effiiency on the ITO side of each pixel See MICROLENSES below MICHOLENSED CCDs Many CCDs now use microlenses over each pixel In the case of interline transfer CCDs the microlenses focus the light onto the photodiode In the case of Blue Plus CCDs see above the microlenses focus the light onto the ITO gate side of the pixel Microlenses greatly improve overall quantum efficiency but introduce some angular dependency Fill factor is normally less than 100 See data sheets for individual CCDs for details www ccd com INTERLINE TRANSFER CCDs Interline transfer CCDs up to the scale of 35mm film have inherent anti blooming but less dynamic range and lower quantum efficiency than Kodak s other front illuminated offerings Interlines also have high dark current in the storage diodes as well as some leakage through the storage diode masks Mass markets for interline CCDs mean much lower prices per pixel and a great entry point into professional level imaging Because interline C
21. ectroscopy with excellent results but a bit more patience and diligence may be necessary interline transfer CCDs Here are some ideas to keep in mind QUANTUM EFFICIENCY Higher sensitivity higher quantum efficiency shorter exposures to get the same results The peak value of a quantum effiiciency curve does not tell the full story of a CCD s sensitivity The area under the curve gives the true comparison of a CCD s relative sensitivity Twice the area under the curve half the time making the exposure Or use the same exposure time but get twice the signal Apogee supports back illuminated front illuminated and interline transfer devices Back illuminated CCDs have the highest overall sensitivity However they are subject to etaloning aka fringing in the near infrared Front illuminated CCDs are much less expensive than back illuminated CCDs UV amp NIR WAVELENGTHS Between 200 300 nm Hamamatsu and E2V Back illuminated UV enhanced CCDs E2V open electrode CCDs U30 only TI EMCCD EM247 only Between 300 400 nm most Kodak CCDs have zero QE at 300 nm increasing linearly to 24096 at 400 nm Near Infrared Back illuminated CCDs have the highest QE but they are also subject to fringing also known as etaloning in the near infrared simply put the light is reflected inside the CCD itself Some companies have developed proprietary versions of CCDs that minimize though not eliminate the effect PI
22. ence between typical and guaranteed is sometimes large such as a factor of two in dark current CCD SELECTION Alta Series cameras with a USB2 interface use a U prefix for example U42 Alta Series cameras with an ethernet interface use an E prefix for example E42 Al Alta models are available with either interface except the U16 U16M and U9000 USB2 only Ascent CCD SIZES QUANTU M EFFICI ENCY models use an A prefix except the EM247 In addition to the following CCDs the Ascent supports a variety of spectroscopic format back illuminated CCDs listed on a following page BACK ILLUMINATED The QE curves below give general representations of the relative differences between the 7 various types of CCDs For additional detail please see the data sheets for each camera l l BACK ILLU M NATE D CCDs l U42 U30 E30 model at www ccd com QE of back illuminated CCDs depends on the coating midband For nearly 30 years back illuminated CCDs have represented the ultimate in high performance imaging The highest sensitivity Tabl h db ona l M h E42 broadband UV enhanced There are also variations in front illuminated CCDs all AE EE GE DE DE polysilicon gates Blue Plus polysilicon and indium tin oxide gates microlenses anti eae Total Biss Array size mm Imaging Area Diagonal U47 blooming See individual camera data sheets for details regarding each sensor Model E2V CCD Array Size Pixels microns mm2 mm Bel ne Gesig 20 a0
23. es Lund Observatory Sweden Mauna Loa Observatory Max Planck Institute Germany McGill University Canada MIT MIT Lincoln Laboratory e Mt Cuba Astronomical Observatory Mt Diablo Observatory e Mt Stromlo Observatory Australia Mt Wilson Observatory Multiple Mirror Telescope Nagoya University Japan NASA Goddard SFC NASA Marshall SFC e NASA Langley Research Center National Astronomical Observatory Japan National Central University Taiwan National Cheng Kung University Taiwan National Health Research Taiwan National Institute for Advanced Interdisciplinary Research Japan National Institute of Advanced Industrial Science and Technology Japan National Institute for Materials Science Japan National Institute of Standards amp Technology National Oceanographic and Atmospheric Administration National Solar Observatory National Sun Yat Sen University Taiwan National Tsing Hua University Taiwan e National University of Ireland e Naval Post Graduate School e Naval Research Laboratory Northwestern University e NTT Japan Oak Ridge National Laboratory Observatoire C te d Azur France Observatoire de Geneve Switzerland Observatorio Carl Sagan Mexico Occidental College Okayama Astrophysical Observatory Japan Oxford University UK Osaka University Japan Oulu University Finland Panasonic e Physical Research Laboratory India Police Scientific D
24. evelopment Branch Scotland Yard UK Pomona College Portland State University e Princeton University e Purdue University Purple Mountain Observatory China Queens University Canada Rice University Riken Japan e Rockefeller University Royal Military College of Canada Royal Observatory Edinburgh Scotland Russian Academy of Sciences Sandia National Laboratory Science and Technology Centre of Ukraine e Shamakhy Astrophysical Observatory Azerbaijan Smithsonian Observatory South African Astronomical Observatory Stanford University State Universities of Arizona Georgia Iowa Louisiana Michigan Montana New York SUNY North Carolina Ohio Pennsylvania Tennessee and Texas Stanford University Starkenburg Observatory Germany Sternberg Astronomical Observatory Russia Steward Observatory Stockholm Observatory Sweden Subaru Telescope s Swarthmore College Tel Aviv University Temple End Observatory UK Tenagra Observatories e Texas A amp M University Texas Tech University Tokyo Institute of Technology Tokyo University Toshiba e Tuorla Observatory Finland Turku Centre for Biotechnology Finland Universidad de Buenos Aires Argentina Universidad de Sonora Mexico Universidade Federal da Paraiba Brazil e Universit t Hamburg Germany Universitat Innsbr ck Austria University College Dublin Ireland e University of Amsterdam Netherlands University of the Andes
25. ing with 2 thread Large format sensors use the D7 housing with a 2 5 thread Back focal distance for the D2 and D7 housing is approximately 1 04 26 4 mm All cameras have a bolt circle with metric threads for adaptation to a wide variety of flanges OPTIONAL LOW PROFILE HOUSINGS Lower profile housings are available for all Alta models to achieve lt 0 5 lt 12 7mm back focal distances without internal shutters TWO SERIAL COM PORTS amp GENERAL I O PORT ES Er Single Interface Cable USB2 Network cM Specifications subject to change without notice Our general purpose I O port can tell you when the shutter is open or can be used for a wide variety of external trigger inputs including line by line control of TDI shifts Our two serial COM ports can control periph erals like filter wheels through the camera s control cable USB2 or ethernet Self Test Cap Drive Signals Exposure Trigger TDI Row Trigger Digital Shutter Output 30V Open 4V Hold 1 Amp Apogee Guider Filter Wheel 6 channel Selectable Function I O PC Device Control RS232 Ports for Telescope Mount Control Filter Wheels Focussers Spectrographs www ccd com ASGENT SERIES CAMERAS OVERVIEW CCD SELECTION CCD SELECTION PROGRAMMABLE DIGITIZATION Unlike previous generations of Apogee cameras with fixed digitization rates for each bit depth the Ascent cameras feature programmable readout rates u
26. l system has been expanded to 12 bits allowing a temperature control range of 213K to 313K 60 to 40 C with 0 024 degree resolution Sensors have been added to monitor the heat sink temperature A power indicator has been added to give the user an idea of how much drive is being given to the CCD cooler The automatic back off function is now handled by the firmware and driver If the system cannot reach the desired temperature the system automatically backs off to a point where regulation can be maintained 2 degrees above the maximum temperature reached The new set point is given to the user Cooling deltas of 40 60C depending on sensor area are typical with simple air cooling Apogee now offers liquid recirculation backs for Alta cameras For customers desiring greater temperature performance where the camera housing will not go below the dew point specifying liquid recirculation will assure a lower dark count than is possible with forced air cooling PROGRAMMABLE FANS Some customers require a complete absence of vibration during an exposure The Alta systems have been designed for complete control of the cooling fans The fans may be turned off or run at a much slower speed to maintain adequate cooling with no vibration For applications where vibration is not an issue the fan speed may be maximized for greatest cooling The fans used in the Alta system were selected for minimum vibration www ccd com D
27. laser induced breakdown spectroscopy Raman atomic emission scanning and echelle spectroscopy They have used for water soil and gem analysis detection of anthrax development of methods and technologies for detection of land mines and improvised explosive devices IEDs analysis and detection of contaminants at nuclear reactors In other fields our cameras have been used to image fingerprints without chemicals x ray inspection of car parts fluorescent imaging of cell tissues and microtitre plates munitions testing laser beam profiling poacher surveillance mammography optics testing discovery of thousands of astronomical objects and radiometry of a wide variety of light sources By expanding into broad markets with diverse demands Apogee has had to develop a wide variety of technologies to solve our customers problems Our spectroscopy customers demand low noise high sensitivity and high quantitative accuracy Our life science customers demand speed and ease of use Both groups are constantly pushing for higher performance at lower prices Ascent and Alta cameras address these demands HIGH PERFORMANCE COOLED CCD CAMERAS A DECADE OF IMPROVEMENTS We continue to refine not just our electronics and our mechanical designs but also our procedures documentation and customer recordkeeping It s quite an accomplishment T to manufacture and sell thousands and thousands of cameras but unless they are rob
28. m like GRAMS or MATLAB e mport export image data in binary integer ASCII text Windows bitmap or grayscale TIF formats Swap byte capability for importing 16 bit image data created on a Macintosh Print plots and images in grayscale or color Copy plots or images to the clipboard for pasting into other applications e Save spectral and image data in a proprietary KestrelSpec format so files can be saved on disk and then opened later for analysis Pea 2 1 T TAE AAM FA s 28 12 AREA 2145277 BO ec 75000 600 00 1050 00 1500 00 sa gie m e m Ad I ra JE e IE di j e TAFT oe 1 3 J 3 LE H de A a r dir oe 8 A LM adim 4 lt a ame Y c 7 xJ iJ ar 9 T ER PO KestrelSpec has versatile graphing and data analysis options The Control Palette above yields quick access to numeric keypad peak finder zooming panning XY cursor and other tools E DATARI lA B Spectrum Catalog displays up to 25 thumbnails in one window to give an overview of current spectral curves in memory Cut and paste the thumbnails or mark them for deletion Select a thumbnail plot to be expanded to a full window ADDED FEATURES IN FULL VERSION KESTRELSCRIPT In the full version the scripting system for KestrelSpec software lets you send commands to KestrelSpec from another program including National Instruments LabView KestrelScript commands include standard me
29. mic range or apparent sensitivity by collecting more light into a superpixel See additional detail under CCD University on our website www ccd com PROGRAMMABLE LEDs Two LEDs on the side of the cameras can be programmed to show status of a variety of the camera functions such as the camera has reached the set temperature the shutter is open or the camera is waiting for an external trigger Alternatively the LEDs can be turned off if you are concerned about stray light The E Series cameras also have two green LEDs that indicate status of the network connection SOFTWARE MaxIm DL CCD software is standard with every Alta as well as an ActiveX driver that is universal to all Apogee Alta and Ascent cameras as well as legacy AP and KX cameras If you write custom code for an Apogee camera you won t have to change it later if you change models Our cameras are also supported by other programs like CCDSoft A Linux and Mac OS X drivers are also available UPGRADEABLE FIRMWARE The Alta and Ascent systems load all camera operating code on camera start These configuration files can be updated via the web as we add features and make improvements Each camera head has coded information identifying the type of system its configuration and type of CCD used as well as the firmware revision in use This allows automatic configuration of the camera in the field and better customer support from our offices SUBARRAY READ
30. nt KestrelCal Calibrate multiple order echelle spectrographs using 2 point KestrelCal TRUE SPECTRUM FLAT FIELDING KestrelSpec provides true spectrum flat fielding using one or more reference light sources to correct for absorbing medium between the source and spectrograph spectrograph optics grating efficiency camera quantum efficiency and interference effects etaloning when using back illuminated CCDs e Simple accurate relative intensity correction by using an incandescent reference source with a known temperature e Full automatic intensity correction using a reference spectrum from any continuous spectrum light source with a known spectrum Powerful broadband intensity correction by joining spectra of multiple reference sources e For echelle spectrographs automatic rescaling of the flat field curve to accomodate different spectral resolutions FULL VERSION ADDED FEATURES e KestrelTemp automated temperature measurement from blackbody spectra KestrelScript capabilty enables other Windows programs like LabView from National Instruments to send commands to and receive data from KestrelSpec using Dynamic Data Exchange DDE e Element Identification process to identify the elements contained in a sample spectrum Ideal for LIBS laser induced breakdown spectroscopy DATA ACQUISITION e Select arbitrary areas from the CCD for spectral curves Up to 10 000 curve memories in RAM for spect
31. nu items as well as other instructions which transfer spectral data from KestrelSpec to the controlling program adjust the wavelength calibration of KestrelSpec etc KestrelScript effectively lets you use KestrelSpec as a very high level driver for the CCD ELEMENT IDENTIFICATION In the full version of the KestrelSpec software there is an option to identify common elements in spectral curves which is ideal for LIBS laser induced breakdown spectroscopy The Element Identification option on the main Process menu allows the user to search for elements in any spectral curve that is calibrated in nm units Use either NIST tables or user defined tables of reference wavelengths for each element include All Elemeniz in Search MF Use Peak Cenlraid Non ionized Peaks Only 7 lanieed Peaks Only Ignore weak sample peaks below ol maximum le Aloo nnose weak reference peaks From mo nm Ta 100 0 nm Peak Finder Threshold 100 Wavelength Tolerance 6 01 x Minimum Matches for ID E peaks Curve Mamory gt 4 s l gt Bad 5 ok Raman image and spectrum KESTRELTEMP In the full version of the KestrelSpec software there is an option to acquire and display spectral curves in Temperature Mode KestrelTempTM is a method of calculating the unknown temperature of spectral data once a temperature reference curve with a known temperature has been defined This known temperature reference
32. of CCD Standard IMAGING FORMAT BACK ILLUMINATED CCDs Back illuminated CCDs are much more expensive than front illuminated CCDs so they are chosen when absolutely necessary for maximum signal to noise under low light conditions Their higher dark current per square millimeter requires the higher cooling of larger Alta housing with the exception of the small spectroscopic format back illuminated CCDs Image sequences Hardware binning Subarray readout TDI readout Note 6 Kinetics mode C mount interface Note 7 Software universality Housing size Warranty Lifetime Interline CCDs cannot do TDI readout CCDs gt 1 video format are too large for C mount optics larger than a KAF 3200ME Some housings are larger The primary differences between the Ascent and Alta Series cameras Ascent is very compact with much lower costs much faster digitization and programmable gain Alta is larger with better cooling and lower noise electronics See the chart below for an ASGENT amp ALTA SHARED FEATURES ASCENT amp ALTA SPECIAL MODES OF OPERATION INTERNAL MEMORY 32 Mbytes of SDRAM image memory is included in the Alta U Series and Ascent camera heads 24 Mbytes of image memory is included in the Alta E Series camera head Local memory serves some important functions First with any network connection and even USB2 0 connection consistency in download rates cannot be guaranteed Some manufacturers go
33. ory New Zealand Bacs Kiskun Observatory Hungary Baja Astronomical Observatory Hungary Ball Aerospace Bang amp Olufsen Denmark Baton Rouge Observatory Baylor University Bechtel e Beijing Observatory China Big Bear Solar Observatory Boeing Bohyunsan Optical Astronomy Observatory Korea Boston University Brigham Young University California Institute of Technology Centre National de la Recherche Scientifique France Centro de Investigaciones en Optica M xico Chiang Mai University Thailand Chiba University Japan Chinese University of Hong Kong Clemson University e Colorado School of Mines Columbia University e Complejo Astron mico El Leoncito Argentina Copenhagen University Denmark Cork Institute of Technology Ireland Corning Crimean Astrophysical Observatory Ukraine Czech Technical University Czech Republic Daimler Benz Aerospace Germany Department of National Defence Canada DLR e V Germany Dublin Institute for Advanced Studies Dunsink Observatory Ireland e Dworp Observatory Belgium e Eastman Kodak Ege University Turkey Florida Institute of Technology SARA Ford Motor Fox Chase Cancer Center e Fudan University China Fuji Fujitsu e Gemini Telescope Project G teburg University Sweden Harvard Smithsonian Center for Astrophysics Harvard College Observatory Heron Cove Observatory Hida Observatory Japan High Energy Accelerator
34. ral plots with up to 65 000 points per curve e Select CCD pixel grouping binning modes kinetics mode external triggering Fully adjustable temperature control on all CCD cameras Maximum frames second depends on binning mode subarray size readout rate and number of curves per image 16 bit per pixel images 32 bit per pixel spectral curves Curve data can be either long integer or floating point Programmable sequences with control of number of exposures adjustable delays between exposures number of scans and summation of multiple image exposures Real time dark background and flat field image buffers Automatic background subtraction and flat field correction e Automatic flip image horizontal when image is reversed e Automatic save of images and curves to disk Conversion of data to log or absorbance scales Calibrate spectral data in wavelength nm or Raman shift cm Autoscan and autocalibrate spectra with fully integrated spectrograph control option for supported spectrographs COUNTS 823 p 45 00 i i abi An TOR AO WAVELENGTH TEE i TN CHE 1 a 3 d 5 B T B CURVE NUMBER j X 75 632 28 nm Channel profile graph bottom shows a slice at a constant wavelength along the Z axis time of 3D spectral curves DATA ANALYSIS amp DISPLAY mage display 256 gray levels positive negative 23 level pseudocolor with quantitative color coded legend 2 D and 3 D c
35. requires an additional 5 seconds to transfer the image to the host computer UNIQUE MAC ADDRESS The Alta E Series cameras each have a unique MAC address so they can be plugged directly into the internet for remote operation We provide MaxIm software for remote control of the camera They cannot be controlled through your browser Because the camera has slave serial I2C and auxiliary filter wheel support an entire setup can be controlled from behind a single camera interface For WAN or WWW connections a full TCP IP protocol gives safe data transfers at slower speeds A special bi directional digital interface with 6 I O lines can also be used to interface to other system components High level shutter signals as well as digital strobes and triggers are available LIQUID CIRCULATION Apogee offers Alta and Ascent liquid recirculation backs for customers wanting to remove heat dissipation from the area of the camera wanting to house the camera inside an enclosure or wanting supplemental cooling The limitation the temperature of the recirculating liquid must not go below the dew point SHUTTERS Apogee Instruments uses the finest shutters available for our cameras from Vincent and Melles Griot These shutters have been carefully integrated into our camera heads with minimum impact on back focal distance and camera size These shutters have a huge advantage of simple rotating blade shutters in terms of light blockage
36. sing 16 bit digitization You can choose the best trade off between noise and readout speed image by image Some CCDs like the interline transfers can read two channels at up to 10 MHz each for a total throughput of over 20 megapixels per second Other CCDs like the full frame Kodaks typically have a maximum useful throughput rate of about 7 to 10 MHz See individual data sheets for specifics regarding each camera system PROGRAMMABLE GAIN AND OFFSET All Ascent models feature programmable gain and bias offset programmable in the analog to digital converter ANTI REFLECTIVE COATED BK7 OPTICS The standard chamber window for the Ascent system is low cost BK7 An optional fused silica window is also available for applica tions requiring higher throughput in the ultraviolet VANE SHUTTERS Ascent cameras with full frame CCDs have internal shutters intended to prevent smearing during readout for low light applications The same professional grade electromechanical shutters available as standard and internal in the Alta cameras are also available as housed external options with the Ascent cameras www ccd com EMCCD SUPPORT The EMCCD is unique among CCDs It has a special charge multiplication circuit that intensifies charge on ccd before readout Gains of 1 to 2000 are possible on ccd using this technology resulting in detection of extremely low light levels With a gain of 1 the ccd behaves much like a normal C
37. to great lengths to attempt to lock Windows up during downloads to ensure that no pattern noise results from breaks in the digitization process but such a lockup is not possible with network interfaces The Alta and Ascent systems buffer the image transfer to protect from noise producing interruptions Second on heavily loaded USB2 ports slower USB1 1 applications loaded networks or slower TCP IP transfers the maximum digitization rate could be limited without a local buffer Local image memory allows very fast digitization of image sequences up to the limit of the internal camera The maximum digitization to memory rates for 100baseT systems is 1 4 megapixels per second while the maximum digitization to memory rates for Alta USB systems is 11 megapixels per second and Ascent is 20 megapixels second There is a fundamental difference in the way the Alta USB2 and network image buffers function The USB2 image buffer is capable of transferring data to the host while digitization of the CCD is active As long as the USB2 transfer speed is greater than the digitization rate the memory buffer will never fill The network memory buffer requires the image digitization to complete prior to transfer across the network HARDWARE BINNING Every Alta and Ascent camera supports hardware binning up to 8 in the horizontal direction and up to the height of the CCD in the vertical direction Binning can be used to increase frame rate dyna
38. urve overlays or vertically stacked curves Channel profile Y t plot Z axis slice Line bar cityscape and scatter plot styles Graphic spectrum catalog with thumbnail plots Baseline Correction click on spectrum to select points for nth order polynomial regression curve used in baseline flattening Real time spectral peak finder determines the centroid and width Join Curves joins multiple spectra with overlapping wavelength coverage into a single linearized spectrum for scanning spectrographs Curve Math add subtract multiply or divide curves with other spectral curves or apply a constant value to curves e Smooth curves according to an adjustable threshold Renormalize X axis accurately linearizes spectra for all types of spectrographs Laser beam profiler display with XY profile graphs Above Echelle spectrograph image from deuterium tungsten source UV at top Below linearized spectrum created from the image generated by linking the multiple orders together Echelle spectrographs offer much higher sampling resolution by taking advantage of the area of imaging CCDs z BOO 24000 1 Deuterium Tungsten Source 20000 16000 COUNTS 12000 Sipi 4000 200000 400 000 gon n0 gon OON 1000 000 WAVELENGTH nm OTHER FEATURES e Import export spectral data in ASCII text format Exported curve data can then be imported into a spreadsheet program or an analysis progra
39. ust the result is a customer service nightmare di b l m In our effort to improve our process we ve achieved the following benchmarks FCC compliance CE compliance ROHS compliance ISO 9000 compliance in process ATION CD LA 3 II Apogee has collected all the specification sheets and machanical drawings for all camera models onto an Integration Starter Kit CD together with software drivers and documentation Apogee Instruments Inc 1020 Sundown Way Ste 150 Roseville CA 95661 USA tel 916 218 7450 fax 916 218 7451 Instruments Inc Alta 1s a registered ademark of Apogee Instruments Inc EE EN EE VA cd com a 9 wi E uu au RS RN N I d Our most exciting new product for specitroscopy is a series of low cost Ascent cameras using very high quantum efficiency Hamamatsu back illuminated CCDs VATED SPECTROSCOPIC FORMAT CCDs These back illuminated CCD systems will be mies a new standard for low cost specitroscopic systems Monochrome only RA FRITZ I ES Twp T JI 1 Y E i i kS v Camera Hamamatsu Total Pixel Size Array size mm Imaging Area Diagonal Model CCD Array Size Pixels microns mm2 mm Ano siono 205 TEE EE A1108 S10141 1108 1024 512000 Len sesnem we el E E esp sk mel es LS pe LX ow NE SW NE WI Hi cw Absolute Quantum Efficiency 96 HAMAMATSU BACK ILLUMINATED SPECTROSCOPIC FORMAT CCDs mal EE EE DE EE ED A HN EH EE HL am Al

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