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Section 1 - Introduction o o o o o o o o o o o o o Support for USB cameras Support for Ethernet (Ethernet to Parallel) for our older parallel cameras Read FITS files Save in several formats (including ASCII format that imports to Excel). Multiple images open at once New universal drivers Works with all 32-bit Windows OS (95/98/Me/NT/2000/XP). Version 5 (Gold Icon) can co-exist with Version 4 (Black Icon). Focus Mode Dialog has big numbers for peak brightness to aid focusing. Added 1xN, 2xN and 3N readout modes to ST-7/8/9/10/1001 Magnified preview in crosshairs window Sharpen preview in contrast dialog. Dockable Icon bar.

Getting Started

NOTE: The USB driver installation process described in the CCDOPS Manual must be completed by anyone installing an SBIG USB camera for the first time on a particular computer. The USB drivers must be installed on the computer before connecting the camera for the first time. If you wish to run your SBIG USB camera from more than one computer, you must go through the USB driver installation process for each computer you intend to use.
This manual describes the STL-1001E, STL-1301E, STL-4020M, STL-6303E and STL-11000M CCD Camera Systems from Santa Barbara Instrument Group. This Section contains a one page Quick Start Guide followed by detailed instructions on handling, connecting and maintaining the camera. For users new to the field of CCD Astronomy, Sections 2, 3 and 4 offer introductory material about CCD Cameras and their applications in Astronomy. Users who are familiar with CCD cameras may wish to skip sections and go directly to the software manual. The CCDOPS version 5 manual gives detailed and specific information about the SBIG software. Sections 5 and 6 of this manual offer some basic hints and information about advanced imaging techniques and accessories for CCD imaging that you may wish to read after your initial telescope use of the CCD camera. Finally, section 7 may be helpful if you experience problems with your camera, and the Appendices provide a wealth of technical information about these systems.

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1.1.1. Quick Start Guide Summary
Before First Light: 1. Attach the 2 nosepiece or other adapter to secure the camera to your telescope, or the camera lens adapter if you intend to use a lens rather than a telescope. 2. Attach the handles if desired. 3. Install filters if needed. 4. Install software on the computer(s) that you will use to control the camera. Before each imaging session, with your computer on and software ready: 5. Attach the remote guiding head to the camera if you intend to use remote guiding. Do not connect or disconnect the remote head with the power on. If you are unsure it is a good idea to attach it anyway because if you decide to use it in the middle of an observing session you will have to shut down the main camera before connecting the remote head. This could be inconvenient. You can always select the internal guider when the remote head is connected. 6. Attach the STL-RC adapter and relay cable to the camera. 7. Attach the water supply and return tubes and have the water supply and/or pump ready if you intend to use water-cooling. 8. Attach the power to the camera. 9. Attach the USB cable to the camera last. With the camera powered up and the USB cable attached you should see the STAT LED flicker as the camera downloads the drivers from your computer (this is automatic). After a couple of seconds the fan should come on and the STAT LED should glow steady. 10. Referring to your software instructions, use your camera control software to Establish a Communications link between your computer and the camera. Your camera is now ready to be controlled by your computer. You should refer to your software manual or instructions for details on focusing, capturing images, taking dark frames, selfguiding, etc.

1.1.12. Extending the USB cable
The camera is supplied a standard 15 (~4.6 meter) USB cable. If you wish to operate the camera remotely, there are several ways to extend this distance between your computer and the camera: Active USB Extension Cable. These accessories are commonly available at computer stores and Radio Shack. They are 15 foot extension cables that get their power from the USB output port of your computer. These are good if your computer is located no more then about 30 feet (~9 meters) from the camera. Powered USB extenders. Powered extenders such as the Icron Ranger (www.icron.com) are also commonly available in computer stores and by mail order over the Internet. These extenders require power at one end of the cable (either end) and will let you operate the camera (or any USB device) up to 100 meters from the computer. Ethernet (LAN). SBIG provides server software that allows our USB cameras to be connected to a computer near the camera and operated remotely over a local network (wired or wireless) by another computer on the local network. Page 15
1.1.13. Opening the Front Cover - Changing Filters
The filter wheel is contained inside the front cover plate. To access the filter wheel remove the eight socket head screws located in recessed slots around the perimeter of the front cover. With the camera lying on its back plate (or on the camera handles if attached), remove the front cover by lifting straight up away from the main body. You will notice resistance as the front cover is still connected to the main body through a self-aligning electrical plug. This plug will separate and the front cover will come free with a firm but gentle pull. It may be easiest to hold the main body with your hands and push up on the corners of the front cover nearest the connectors with your thumbs. Filters may be inserted and removed with the filter carousel in place. The filter carousel accepts both 48mm threaded filter cells (below right) and 50mm round unmounted filters (below left). Thick unmounted filters may be held in place by turning the shouldered retaining washers (arrows) upside down to capture the filter. We recommend the 50mm filters for minimum vignetting, particularly with the KAI-11000M CCD. If you have more than one set of filters you may find it easier to purchase one or more additional carousels and populate them with your filter sets. In this case, you can change sets by swapping carousels. The filter carousel is held in place by a single screw in its center. Remove this screw and carefully remove the carousel by sliding it up and away from the motor. Be careful not to lose the small flat washers that go between the carousel and the front cover. These must be replaced when reassembling the filter wheel to the cover or the carousel will not work properly. After installing or changing filters, replace the carousel taking care to replace the small washer between the carousel and the inside of the front cover. The small steel washer fits into a recessed cutout in the cover, then the larger white Teflon washer goes on top of the steel washer. The carousel is put in place next and the assembly is secured with a screw and Teflon bearing through the center of the filter carousel. DO NOT OVERTIGHTEN THE CENTRAL SCREW. It is only necessary to tighten the central screw until it is snug. Over-tightening the screw may impair the operation of the filter wheel. When reassembled, replace the front cover assembly containing the filter carousel on the camera. Orient the front cover so that the self-aligning connector plugs are together and gently push straight towards the main body to seat the front cover. Replace the 8 retaining socket head screws to hold the front cover in place.

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Installing the USB Drivers for the First Time
If you are installing an SBIG USB camera for the first time you must install the USB drivers BEFORE attempting to connect the camera to the computer. This is true for each computer you intend to use to control the camera. Please refer to the CCDOPS manual for instructions on installing the USB drivers and camera control software.
1.2.1. Establish Communications with CCDOPS
Once you have installed the USB drivers and CCDOPS control software on your computer, you can connect the camera to the USB port and establish a communications link. If you are using software other than CCDOPS please refer to the instructions for your particular software package. With CCDOPS software, you must first select USB as the communications mode in the Misc menu. Select Misc, then Graphics/Comm Setup After you click on the menu item you will see a Graphics/Comm Setup dialog box as shown below. Pick USB as the Interface from the drop down list of interface items. Then click OK. CCDOPS will remember the interface setup the next time you use the program so this step only needs to be done the first time you use the program unless you change the interface type for a different camera. If you re-install CCDOPS for any reason, be sure to re-set this item. After you have selected USB as the interface, establish communication with the camera. Select the Camera menu and click on Establish Com Link. After a few seconds should see Link:[STxxx]USB in lower-right corner of CCDOPS main window where STxxx is the camera model. You are now talking to the camera. From this point you should follow the software instructions in the CCDOPS manual to Set Up the cameras cooling, Focus, Grab images, etc. You must establish a comm link with the camera each time you connect it to the computer.

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1.2.2. Capturing Images with the CCD Camera
Unfortunately there really aren't many shortcuts you can take when using the CCD camera to capture images. Refer to your software manual for detailed instructions. However, to begin we suggest: Find some relatively bright object like M51, the Ring Nebula (M57) or the Dumbbell Nebula Take a 1 minute exposure using the Grab command with the Dark frame option set to Also Display the image. Process the image.
If you happen to have purchased a camera lens adapter for your CCD Camera you can use that to take images in the daytime. Be aware that these cameras are extremely sensitive and will saturate in the shortest exposure times when imaging in daylight conditions if steps are not taken to attenuate the amount of light reaching the CCD. If you are testing the camera with a lens during the daytime, the tests should be performed in a darkened room with the lens aperture set to about f/16.

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Section 2 - Introduction to CCD Cameras
Introduction to CCD Cameras

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Section 2 - Introduction to CCD Cameras possible readout noise. At 10e- to 15e- rms per read these cameras are unsurpassed in performance.

2.4.3. Dark Frames

No matter how much care is taken to reduce all sources of unwanted noise, some will remain. Fortunately, however, due to the nature of electronic imaging and the use of computers for storing and manipulating data, this remaining noise can be drastically reduced by the subtraction of a dark frame from the raw light image. A dark frame is simply an image taken at the same temperature and for the same duration as the light frame with the source of light to the CCD blocked so that you get a "picture" of the dark. This dark frame will contain an image of the noise caused by dark current (thermal noise) and other fixed pattern noise such as read out noise. When the dark frame is subtracted from the light frame, this pattern noise is removed from the resulting image. The improvement is dramatic for exposures of more than a minute, eliminating the many "hot" pixels one often sees across the image, which are simply pixels with higher dark current than average.

2.4.4. Flat Field Images

Another way to compensate for certain unwanted optical effects is to take a "flat field image" and use it to correct for variations in pixel response uniformity across the area of your darksubtracted image. You take a flat field image of a spatially uniform source and use the measured variations in the flat field image to correct for the same unwanted variations in your images. The Flat Field command allows you to correct for the effects of vignetting and nonuniform pixel responsivity across the CCD array. The Flat Field command is very useful for removing the effects of vignetting that may occur when using a field compression lens and the fixed pattern responsivity variations present in all CCDs. It is often difficult to visually tell the difference between a corrected and uncorrected image if there is little vignetting, so you must decide whether to take the time to correct any or all of your dark-subtracted images. It is always recommended for images that are intended for accurate photometric measurements. Appendix D describes how to take a good flat field. It's not that easy, but we have found a technique that works well for us.

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Section 3 - At the Telescope with a CCD Camera star diameter. This can be tedious. It helps considerably if a pointer or marker is affixed to the focus knob so you can rapidly return to the best focus once you've gone through it. For critical focus, an exposure of about 1 second is recommended to smooth out some of the atmospheric effects. While you can use the Full frame mode to focus, the frame rate or screen update rate can be increased significantly by using Planet mode. In Planet mode the Focus command takes a full image and then lets you position a variable sized rectangle around the star. On subsequent images the Planet mode only digitizes, downloads, and displays the small area you selected. The increase in frame rate is roughly proportional to the decrease in frame size, assuming you are using a short exposure. The telescope focus is best achieved by maximizing the peak value of the star image. You should be careful to move to a dimmer star if the peak brightness causes saturation. In order to avoid saturation, move to a dimmer star if the peak brightness counts are 40,000 or more. Another point you should also be aware of is that as you approach a good focus, the peak reading can vary by 30% or so. This is due to the fact that as the star image gets small, where an appreciable percentage of the light is confined to a single pixel, shifting the image a half a pixel reduces the peak brightness as the star's image is split between the two pixels. The Kodak CCD pixels are so small that this is not likely to be a problem. Once the best focus is found, the focusing operation can be greatly shortened the second time by removing the CCD head, being careful not to touch the focus knob. Insert a high power eyepiece and slide it back and forth to find the best visual focus, and then scribe the outside of the eyepiece barrel. The next time the CCD is used the eyepiece should be first inserted into the tube to the scribe mark, and the telescope visually focused and centered on the object. At f/6 the depth of focus is only 0.005 inch, so focus is critical. An adapter may be necessary to allow the eyepiece to be held at the proper focus position. SBIG sells extenders for this purpose.
Finding and Centering the Object
Once best focus is achieved, we suggest using "Dim" mode to help center objects. This mode gives a full field of view, but reduces resolution in order to increase the sensitivity, and digitization and download rate. If you have difficulty finding an object after obtaining good focus, check to be sure that the head is seated at best focus, then remove the head and insert a medium or low power eyepiece. Being careful not to adjust the focus knob on the telescope, slide the eyepiece in or out until the image appears in good focus. Then visually find and center the object, if it is visible to the eye. If not, use your setting circles carefully. Then, re-insert the CCD head and use FOCUS mode with an exposure time of about ten seconds, if it is dim. Center the object using the telescope hand controls. Note: With a 10 second exposure, objects like M51 or the ring nebula are easily detected with modest amateur telescopes. The cores of most galactic NGC objects can also be seen.

Taking an Image

Take a CCD image of the object by selecting the Grab command and setting the exposure time. Start out with the Image size set to full and Auto Display and Auto contrast enabled. The camera will expose the CCD for the correct time, and digitize and download the image. One can also take a dark frame immediately before the light image using the Grab command.

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Section 3 - At the Telescope with a CCD Camera Because the Research Series cameras have regulated temperature control, you may prefer to take and save separate dark images, building up a library at different temperatures and exposure times, and reusing them on successive nights. At the start it's probably easiest to just take the dark frames when you are taking the image. Later, as you get a feel for the types of exposures and setpoint temperatures you use, you may wish to build this library of dark frames.

Displaying the Image

The image can be displayed on the computer screen using the graphics capability of your PC. Auto contrast can be selected and the software will pick background and range values which are usually good for a broad range of images or the background and range values can be optimized manually to bring out the features of interest. The image can also be displayed as a negative image, or can be displayed with smoothing to reduce the graininess. Once displayed, the image can be analyzed using crosshairs, or can be cropped or zoomed to suit your tastes.

Processing the Image

If not done already, images can be improved by subtracting off a dark frame of equal exposure. You will typically do this as part of the Grab command although it can also be done manually using the Dark Subtract command. By subtracting the dark frame, pixels which have higher dark current than the average, i.e., "hot" pixels, are greatly suppressed and the displayed image appears much smoother. Visibility of faint detail is greatly improved. The CCDOPS program also supports the use of flat field frames to correct for vignetting and pixel to pixel variations, as well as a host of other image processing commands in the Utility menu. You can smooth or sharpen the image, flip it to match the orientation of published images for comparison, or remove hot or cold pixels.

Advanced Capabilities

The following sections describe some of the advanced features of SBIG cameras. While you may not use these features the first night, they are available and a brief description of them is in order for your future reference.
3.9.1. Crosshairs Mode (Photometry and Astrometry)
Using the crosshair mode enables examination of images on a pixel by pixel basis for such measurements as Stellar and Diffuse Magnitude, and measurement of stellar positions. The 16 bit accuracy of SBIG systems produces beautiful low-noise images and allows very accurate brightness measurements to be made. With appropriate filters stellar temperature can be measured. In the crosshair mode, you move a small cross shaped crosshair around in the image using the keyboard or the mouse. As you position the crosshair, the software displays the pixel value beneath the crosshair and the X and Y coordinates of the crosshair. Also shown is the average pixel value for a box of pixels centered on the crosshair. You can change the size of the averaging box from 3x3 to 31x31 pixels to collect all the energy from a star.

Connecting the Power

The desktop power supply is designed to run off voltages found in most countries (90 to 240 VAC). In the field however, battery operation may be the most logical choice. In that case you need to use the optional 12V power supply or a 12VDC to 110 VAC power inverter.
Connecting to the Computer
The Research Series CCD cameras are supplied with a 15 foot cable to connect the system to the host computer. The connection is between the camera and the Host Computer's USB port. If it is necessary or desirable to extend the distance between the camera and the computer, third party USB extenders such as the Ranger made by Icron (http://www.icron.com) may be used for remote operation up to 100 meters.
Connecting the Relay Port to the Telescope
The Research Series camera systems can be used as autoguiders where the telescope's position is periodically corrected for minor variations in the RA and DEC drives. The host software functions as an autoguider in three modes: the Track mode, the SBIG patented Track and Accumulate mode, and the SBIG patented Self-Guided mode (except for the ST-1001E). In the Track mode and Self Guided mode the host software corrects the telescope as often as once every second to compensate for drift in the mount and drive system. The host software and the CCD camera operate in tandem to repeatedly take exposures of the designated guide star, calculate its position to a tenth of a pixel accuracy, and then automatically activate the telescope's controller to move the star right back to its intended position. It does this tirelessly to guide long duration astrophotographs. In the Track and Accumulate mode the software takes a series of images and automatically co-registers and co-adds the images to remove the effects of telescope drift. Typically you would take ten 1 minute "snapshots" to produce an image that is comparable to a

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single 10 minute exposure except that no guiding is required. The reason no guiding is required is that with most modern telescope mounts the drift over the relatively short 1 minute interval is small enough to preserve round star images, a feat that even the best telescope mounts will not maintain over the longer ten minute interval. The Track and Accumulate software does allow correction of the telescope position in the interval between snapshots to keep the guide star grossly positioned within the field of view, but it is the precise coregistration of images that accounts for the streakless images. The host software and the CCD camera control the telescope through the 9-pin Telescope port on the camera. This port provides active low open collector signals to the outside world. By interfacing the camera to the telescope's controller the CPU is able to move the telescope as you would: by effectively closing one of the four switches that slews the telescope. Note: You only need to interface the camera's Telescope port to your telescope if you are planning on using the camera system as an autoguider or selfguider, or feel you need to have the Track and Accumulate command make telescope corrections between images because your drive has a large amount of long term drift. Some recent model telescopes have connectors on the drive controller that interface directly to the camera's TTL level Telescope port. All that's required is a simple cable to attach the 9 pin Telescope port to the telescope's telephone jack type CCD connector. SBIG includes its STL-RC adapter and cable for this express purpose although it is easy to modify a standard 6-pin telephone cable for interface to the Telescope port (see Appendix A for specific pin outs, etc.). The STL-RC plugs into the 9-pin port on the camera, and a standard phone cable, which we supply, connects the adapter to the telescope drive. Note: phone cables come in a few variations. We use the six-pin cable, and the pin order is reversed left to right relative to the connector from one end to the other. This is identical to what is typically sold at Radio Shack stores as an extension cable.

Terrestrial Imaging

An optional accessory for the Research Series cameras is the camera lens adapter (see Section 6.3). This accessory is made to accommodate popular 35mm Nikon lenses. You may attach a camera lens in place of your telescope and use the CCD camera for terrestrial views in daylight. Begin with a tenth second exposure at f/16 for scenes at normal room light and adjust as necessary for your conditions.

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Taking a Good Flat Field
If you find that flat field corrections are necessary due to vignetting effects, CCD sensitivity variations, or for more accurate measurements of star magnitudes, try either taking an image of the twilight sky near the horizon or take an image of a blank wall or neutral grey card. The Kodak CCDs may have a low contrast grid pattern visible in the sky background. A flat field will eliminate this. Finding areas of the sky devoid of stars is very difficult after twilight. Therefore, you should take flat field images of the night sky after sunset, but long before you can see any stars. If this is not possible, take an image of a featureless wall or card held in front of the telescope. However, if using this second method, be sure that the wall or card is evenly illuminated. Appendix C describes how to do this. You will know if the flat field is good if the sky background in your images has little variation across the frame after flat fielding, displayed using high contrast (a range of 256 counts is good for showing this). If you plan on flat fielding Track and Accumulate images you should also refer to section 6.8. Since the same flat field is added to itself a number of times, be sure that you do not saturate the flat field image by starting with pixel values too high. Typically try to keep the pixel values between 10% to 20% of saturation for this purpose. For single flat field images, try to keep the values to approximately 50% of saturation.
Building a Library of Dark Frames
The Research Series cameras have regulated temperature control, and therefore it is possible to duplicate temperature and exposure conditions on successive nights. You can set the camera TE cooler temperature to a value comfortably within reach on your average night, and then take and save on disk a library of dark frames for later use. This is a good project for a rainy night. We recommend you build a file of 5, 10, 20 ,40, and 60 minute dark frames at zero degrees Centigrade for a start. Otherwise you will find yourself wasting a clear night taking hour-long dark frames! Note: Dark frames taken the same night always seem to work better. The adaptive dark subtract will help if the ambient temperature changes slightly.

Changing the Camera Resolution
The Camera Setup command allows you to select the resolution mode you wish to use for taking and displaying images. The Research Series have High, Medium, Low and Auto modes. The High Resolution mode is the best for displaying the greatest detail since it utilizes the maximum number of pixels for your particular camera. The Medium Resolution Mode operates by combining 2x2 pixels giving the same field of view as High Resolution Mode, but with 1/4 the resolution. This results in significantly faster digitization and download times. Also, in Medium Resolution Mode, with larger pixels and comparable readout noise there is a better signal to noise ratio for very dim diffuse objects. This improved signal to noise ratio combined with faster digitization and download times makes Medium Resolution Mode ideal for finding and centering dim objects, and for imaging most objects. Additionally, a Low resolution mode is provided which bins the CCD 3x3 before readout. Low resolution mode is

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sensational for displaying faint nebulosity with short exposure times. In Auto Resolution Mode, the camera and software will always use High Resolution for all imaging and display functions except when you are in Full Frame Focus Mode. It will then automatically switch to Low Resolution Mode. If you further select Planet Mode for focusing, the camera will switch back to High Resolution on the selected box area. The small pixel size, is best for critical focusing. Planet mode will result in fast digitization and download times since only a small portion of the frame is read out. In general, you should pick a binning mode that yields stars with two to three pixels full width at half maximum. This is easily measured by using the crosshairs to determine the peak brightness of a relatively bright star, and determining the number of pixels between the 50% values on either side of the peak. More than 3 pixels per stellar halfwidth merely wastes sensitivity without improved resolution.

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Section 8 Glossary

Common Problems

This section discusses some of the more common problems others have encountered while using our CCD cameras. You should check here if you experience difficulties, and if your problem still persists please contact us to see if we can work it out together. Achieving Good Focus - Achieving a good focus is one of the most difficult areas in working with CCD cameras due to the lack of real time feedback when focusing. Focus can take a good deal of time, and as with all forms of imaging, focus is critical to getting the most out of your camera. Once you have achieved a good focus with your system, it can be very useful for future observing sessions to scribe an eyepiece or mark down or log positions of each component so the next time you will at least be close to focus at the start. If you know where the focal plane lies for your telescope, you can use Table 3.1 to calculate exactly where the CCD is with respect to your system. By placing the CCD close to the focal plane initially, you can save a lot of time. The best kind of object to focus on is a star. As you converge towards focus, more light from the star will be concentrated onto one pixel. Thus, watching your peak reading while focusing and focusing for a maximum reading is a good way to get best focus. This is how we do it. It helps to have a dial or indicator on the focus knob so you can rapidly return to the best point after going through focus. Elongated Guided Images - When using Track and Accumulate or Self Guiding, if you notice guiding errors resulting in elongated star images, you are probably using too long a snapshot time. If the snapshot time is longer than the amount of time your drive can track unguided with acceptable guiding errors, you will see elongated stars in your final images. If your snapshot times are getting down to 30 seconds or less you should improve your drive. If you are using your camera as an autoguider for film photography and are noticing unacceptable guiding errors, please check the following before calling SBIG: 1. Can you move the telescope using the Move command? This is an indicator as to whether or not you are properly connected to your drive system via the relay cable from the CPU. 2. Be sure that your calibration time gives at least 10 to 50 pixels of movement for each step of the Calibrate Track command. 3. Check for flexure between the CCD camera head and your system. Check for flexure between the guide scope or off-axis guider and your telescope system. This is a very common source of guiding errors. A very small movement of the CCD head with respect to the guide scope during an exposure can cause unacceptable streaking. 4. If your mount is stable, try longer exposure times while tracking to average out the atmospheric effects. Finding Objects - The easiest method of finding objects is to use a reticule eyepiece, if the object is bright enough to see. Pull the CCD optical head from the eyepiece holder and Page 61

Telescope Flat White Surface

Flat White Surface

Flashlight
The key aspects of this geometry are that the reflection off two diffuse surfaces is used, and the large flat surface is square to the illumination from the small flat surface. When we do this, the first flat surface is typically a white T-shirt worn by the operator! Take care that no apparent shadows are cast onto the larger flat white surface. Use an exposure at the camera that yields an average light level equal to about half of full scale.

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Appendix E Third Party Vendors Supporting SBIG Products
Appendix D Camera Specifications
Model STL-4020M Typical Specificaitons
CCD SPECIFICATIONS Imaging CCD Pixel Array Total Pixels Pixel Size Kodak Enhanced KAI-4020M (Class 2) 2048 x 2048 pixels, 15.2 x 15.2 mm 4.2 million 7.4 x 7.4 microns 40,000 e1e-/pixel/second @ 0 degrees C ABG only READOUT SPECIFICATIONS Shutter Exposure Electromechanical 0.01 to 3600 seconds, 10ms resolution Yes 16 bits 0.72e/ADU <15e RMS 1 x 1, 2 x 2, 3 x 3 9.8 seconds SYSTEM SPECIFICATIONS Cooling - standard Two-Stage Thermoelectric, Water Assist, -50 C from Ambient Typical 0.1C 10 18VDC, 12VDC nominal, Universal AC to 12VDC desktop supply USB 1.1 Windows 95/98/NT/2000/Me/XP Dual CCD Self-Guiding Standard, Remote Guiding Head Optional PHYSICAL SPECIFICATIONS Dimensions Weight Internal Filter Carousel Mounting Backfocus 6.5 x 6 x 3.5 (16.5 x 15.2x8.9cm) 4 pounds (1.8 Kg) without filters 5 positions for 48mm threaded cells or 2 unmounted filters (optional) 2 nosepiece included Approximately 1.7 inches (~4.3 cm) with 2" nosepiece attached
Full Well Capacity (NABG) Dark Current Antiblooming
Correlated Double Sampling A/D Converter A/D Gain Read Noise Binning Modes Full Frame Download
Temperature Regulation Power Computer Interface Computer Compatibility Guiding
KAI-4020M CCD Quantum Efficiency (Spectral Response)

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Model STL-11000M Typical Specificaitons
CCD SPECIFICATIONS Imaging CCD Pixel Array Total Pixels Pixel Size Full Well Capacity (NABG) Dark Current Antiblooming Shutter Exposure Correlated Double Sampling A/D Converter A/D Gain Read Noise Binning Modes Full Frame Download Cooling - standard Temperature Regulation Power Computer Interface Computer Compatibility Guiding Dimensions Weight Internal Filter Carousel Mounting Backfocus Kodak Enhanced KAI-11000M 4008 x 2745 pixels, 36 x 24.7 mm 11 million 9 x 9 microns 50,000 e1.5 e-/pixel/sec @ o degrees C ABG only READOUT SPECIFICATIONS Electromechanical 0.01 to 3600 seconds, 10ms resolution Yes 16 bits 0.8e/ADU 11e RMS 1 x 1, 2 x 2, 3 x seconds SYSTEM SPEIFICATIONS Two-Stage Thermoelectric, Water Assist, -50 C from Ambient Typical 0.1C 10 - 18VDC, 12VDC nominal, Universal AC to 12VDC desktop supply USB 1.1 Windows 95/98/NT/2000/Me/XP Dual CCD Self-Guiding Standard, Remote Guiding Head Optional PHYSICAL SPECIFICATIONS 6.5 x 6 x 3.5 (16.5 x 15.2x8.9cm) 4 pounds (1.8 Kg) without filters 5 positions for 48mm threaded cells or 2 unmounted filters (optional) 2 nosepiece included Approximately 1.7 inches (~4.3 cm) with 2" nosepiece attached

KAI-11000M Quantum Efficiency (Spectral Response)

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Model STL-6303E Typical Specificaitons
CCD SPECIFICATIONS Imaging CCD Pixel Array Total Pixels Pixel Size Full Well Capacity (NABG) Dark Current Antiblooming Shutter Exposure Correlated Double Sampling A/D Converter A/D Gain Read Noise Binning Modes Full Frame Download Cooling - standard Temperature Regulation Power Computer Interface Computer Compatibility Guiding Dimensions Weight Internal Filter Carousel Mounting Backfocus Kodak Enhanced KAF-6303E 3060 x 2040 pixels, 27.5 x 18.4 mm 6 million 9 x 9 microns 100,000 e1e-/pixel/second @ 0 degrees C NABG standard, ABG optional READOUT SPECIFICATIONS Electromechanical 0.11 to 3600 seconds, 10ms resolution Yes 16 bits 2.3e/ADU 15e RMS 1 x 1, 2 x 2, 3 x seconds SYSTEM SPECIFICATIONS Two-Stage Thermoelectric, Water Assist, -50 C from Ambient Typical 0.1C 10 - 18VDC, 12VDC nominal, Universal AC to 12VDC desktop supply USB 1.1 Windows 95/98/NT/2000/Me/XP Dual CCD Self-Guiding Standard, Remote Guiding Head Optional PHYSICAL SPECIFICATIONS 6.5 x 6 x 3.5 (16.5 x 15.2x8.9cm) 4 pounds (1.8 Kg) without filters 5 positions for 48mm threaded cells or 2 unmounted filters (optional) 2 nosepiece included Approximately 1.7 inches (~4.3 cm) with 2" nosepiece attached
KAF-6303E Quantum Efficiency (Spectral Response)

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Model STL-1301E Typical Specificaitons
CCD SPECIFICATIONS Imaging CCD Pixel Array Total Pixels Pixel Size Full Well Capacity (NABG) Dark Current Antiblooming Shutter Exposure Correlated Double Sampling A/D Converter A/D Gain Read Noise Binning Modes Full Frame Download Cooling - standard Temperature Regulation Power Computer Interface Computer Compatibility Guiding Dimensions Weight Internal Filter Carousel Mounting Backfocus Kodak Enhanced KAF-1301E 1280 x 1024 pixels, 20.5 x 16.4 mm 1.3 million 16 x 16 microns 150,000 e5.6 e-/pixel/second @ 0 degrees C. NABG standard, ABG optional READOUT SPECIFICATIONS Electromechanical 0.11 to 3600 seconds, 10ms resolution Yes 16 bits 2.3e/ADU 15e RMS 1 x 1, 2 x 2, 3 x seconds SYSTEM SPECIFICATIONS Two-Stage Thermoelectric, Water Assist, -50 C from Ambient Typical 0.1C 10 - 18VDC, 12VDC nominal, Universal AC to 12VDC desktop supply USB 1.1 Windows 95/98/NT/2000/Me/XP Dual CCD Self-Guiding Standard, Remote Guiding Head Optional PHYSICAL SPECIFICATIONS 6.5 x 6 x 3.5 (16.5 x 15.2x8.9cm) 4 pounds (1.8 Kg) without filters 5 positions for 48mm threaded cells or 2 unmounted filters (optional) 2 nosepiece included Approximately 1.7 inches (~4.3 cm) with 2" nosepiece attached