Frequently Asked Questions
Can I purchase directly from FLI?
Yes, you can purchase directly from FLI or through one of our distributors. Please contact FLI for pricing.
How are Kodak's financial troubles going to affect deliveries of CCDs?
Kodak sold the CCD division to Truesense Imaging in 2011. Truesense is not affected by what is going on at Kodak.
Should I buy a color or monochrome CCD?
For most scientific applications, a monochrome CCD is the best choice for several reasons. First of all, you have control over the filter sets used. You may want to change from RGB to CMY to photometry filters or narrow band filters. A color CCD has a fixed set of filters, typically in a Bayer pattern (red-green-green-blue). If you use a blue filter in front of a color CCD, only one of 4 pixels will see any significant amount of light. Color CCDs can deliver a color image in a single shot, but they compromise spatial sampling. A 10 megapixel color sensor is not delivering 10 megapixels of red, and 10 megapixels of green, and 10 megapixels of blue. A monochrome sensor acquiring a red, green, and blue image using a filter wheel acquires 10 megapixels of each. Typically you cannot bin color CCDs (you can, but the results will have limited utility).
What's the difference between an interline and a full frame CCD?
Interline CCDs use part of each pixel to collect light, and part of each pixel to store and move charge. The storage area has a metal mask to prevent corruption of the image during readout. New CCDs have a microlens over each pixel to focus incoming light onto the photodiode portion of the pixel so that light is not lost landing on the metal masks. Because only part of the pixel is used to collect light, the full well capacity of interline CCDs is typically lower than comparably sized full frame pixels. Interline transfer CCDs shutter the image by moving the charge from the photodiode to the storage diode side of the pixel. As a result, interline exposures can potentially be very short. For FLI cameras, interline exposure times can be as low as 30 microseconds (as opposed to about 30 milliseconds for an electromechanical shutter). Usually interline CCDs are used without electromechanical shutters. However, it is complicated to take a dark image without a shutter unless you have some way of keeping the camera in a 100% dark environment. Full frame sensors use 100% of each pixel to collect, store, and transfer charge. They require an electromechanical shutter unless the camera is going to be used in a 100% dark environment. Full frame devices typically have higher full well capacities and higher quantum efficiencies than interline sensors.
What's a back-illuminated CCD?
CCDs are slabs of silicon like photovoltaic cells. Gate structures are added to the top (usually polysilicon or indium tin oxide) so a charge can be applied to corral electrons where they were created (in order to get an image). These gate structures block incoming light and reduce the quantum efficiency (QE). One way to improve QE is to flip the CCD over so that the gates are on the bottom, then grind down CCD until it is about 15 microns thick. The gates are still close enough to the front surface that charge is captured where it is created. Back-illuminated or thinned CCDs have very high quantum efficiencies, but typically cost much more than front-illuminated CCDs.
What is etaloning?
Near infrared light can penetrate 200 or more microns into CCDs. As a result, when CCDs are thinned to 15 microns thick, NIR (especially beyond 800 nm) can penetrate to the back of the CCD and reflect off the back (and again off the front, and again off the back, etc), creating a ring of halos around a bright point source. Deep depletion CCDs have high QE in the NIR, but they also have etaloning. Front-illuminated CCDs such as the Truesense KAF-1001E have less QE in this region but do not suffer from etaloning.
Residual bulk imaging. CCDs are normally 500 microns thick. The gate structures are at the top, and create wells that extend 10 or 15 microns into the CCD. But near IR light can penetrate into the CCD far beyond the reach of the wells created by the gates. This charge gradually leaves the CCD (over hours or days), creating a ghost image in subsequent images. If the CCD is warmed up, the charge will leave the CCD. However, it is not practical to warm up the CCD between images. Alternatively, some cameras provide a pre-flash that uniformly illuminates the CCD, leaving no place for such charge to accumulate below the epitaxial layer. This preflash does slightly lower the full well capacity of the sensor.
What's the purpose of cooling the sensor?
CCDs create charge from incoming light (the photoelectric effect, for which Einstein got a Nobel prize) but also from thermal energy. For very short exposures with plenty of light (the kids at a soccer game), you don't notice the thermal part of the image. But for low light applications like astronomy and fluorescence, you want to minimize thermally generated charge so you get a better image of light-generated charge. Cooled sensors must be housed in a sealed, dry environment in order to prevent condensation of moisture from the air.
How does FLI cool the sensor?
FLI uses Peltier devices, which are thermoelectric coolers that get cold on one side and hot on the other when electricity is applied. Designing a CCD chamber than can keep a seal for many years is part of the engineering; efficiently dissipating the heat generated by the cooling is another part. Typically the temperature sensor for a camera is installed in a copper block that links the CCD to the Peltier cooler. If there is a problem with contact between the copper block and the sensor, the block may be cold but the sensor may not be fully cooled. In this case, you can see dark current values that are inconsistent with reported temperature of the camera.
What do AIMO and NIMO mean?
Why do some e2v CCDs have much higher dark
current than others?
AIMO = Advanced Inverted Mode Operation. NIMO = non-IMO. Some e2v CCDs, such as deep depletion devices, cannot be operated in inverted mode. As a result, dark current is 100-200X higher than AIMO CCDs. Instead of 0.1 electron per pixel per second (eps) of dark current, for example, expect 10 eps. AIMO vs NIMO is not a choice made by a camera manufacturer like FLI. The CCD is manufactured by e2v either as AIMO, IMO, or NIMO.
How much does binning increase speed?
How many pixels can I bin? Binning is the process of adding pixels together on the CCD itself in order to increase the signal to noise ratio. Binning 2x2 (adding together 4 pixels) does not increase readout speed by a factor of 4, but rather by a factor of about 2. The amount of time to do vertical transfers is not reduced; however, the amount of time required for digitization is almost cut in half. FLI cameras allow arbitrary X and Y binning (2x2, 2x8, 1x20, etc.). The limitation is the full well capacity of an individual pixel versus the full well of the serial register versus the full well of the output. Usually the serial register and output have about twice the capacity of a pixel. If the amount of charge in the pixels is low, then binning many pixels will not exceed the capacity of the serial register. However, if the exposure time is nearly filling the wells of individual pixels, then binning needs to be carefully limited.
What's the difference between a ProLine and MicroLine camera?
The MicroLine cameras are much smaller and lighter than ProLine cameras. For most sensors, the ProLines are 3 or 4 degrees colder than the MicroLines. The ProLines provide power and USB for accessories such as filter wheels and focusers, so you only have to run one set of cables to the camera, and a short set of cables from the camera to accessories. Both the inner (CCD) and outer (electronics) chambers of the ProLine are sealed.
Which CCDs does FLI support?
FLI supports over 40 CCDs, not including variations such as midband versus broadband, or color versus monochrome. Please see the chart here
I´m looking for narrowband filters. Should I go for 12nm, 6nm or even 3nm FWHM?
Usually most people are happy with the 12nm filters. They give you a huge contrast improvement, theyīre not too expensive, there is a broad range of wavelengths available. If you live under very light polluted skies or if youīre after the faintest traces of gas out there, you will think about the 6nm or even the 3nm filters. The rule is quite easy: The narrower the filter, the stronger is the contrast and you will get rid of most stars. But before getting 3nm filters you should have a look at some physical laws: A astronomical interference filter is usually designed for light hitting the surface of the filter at 90°. If the angle of incidence is reduced there is something happening: The transmission curve shifts and changes itīs shape. If you do have a fast instrument like f/3 this causes a shift of several nanometers. (The exact value depends on the design of the filter, but the shift itself ALLWAYS happens) With a 12nm filter this is usually no problem: We (Astronomik) have designed the transmission curve in such a way, that these filters can be used with f/10 or f/4. Very universal, no problem! But if you now look at an 3nm H-alpha filter showing you a transmission curve precisley centered on 656,3nm and you will use it at f/5 or even f/3 the transmission might drop to something like 35% or even less. This is caused by the shift of the transmission curve explained above. So if you go for a 3nm filter make sure that itīs transmission curve is matched to the focal ratio of your imaging instrument. And do not forget to get a new filter when you switch to an faster or slower instrument. (Of course the filter will still work, but it wonīt give you the result of a matched filter!)
Because of this very limited range we (Astronomik) decided to go for 6nm filters. The contrast improvement is enormous, but for example you may use the same filter at f/3.5 and f/5.8 without a major loss in performance. No letīs look even closer on your optical system: You have one of those really nice astrographs: Huge corrected field, matched by the chip in your camera, nice small spots of stars. And itīs a really fast system to keep exposure times short.
You get a matched 3nm narrowband filter to -letīs say f/3- and use it. The rays of light from the outer part of the optics are perfectly transmitted -you got a matched filter- but what about the light traveling closer to the optical axis? Itīs blocked the stronger the closer it is to the optical axis! So you waste the nice and crisp central rays and get the one from the outer part, which have a stronger effect on all residual abberations. OK, you want the central part? Go for a filter with another transmission curve, but this time you will block all the light from the outer part of your optics and youīll have to expose longer. These are the reasons why Astronomik does 6nm filters only: They simply make more sense and they will give you amazing images!
Iīm living under a light polluted sky, but I want to do LRGB imaging. What shall I do?
Propably moving house would be the best option... But if you have to stay in your current backyard or balcony you should get the Astronomik CLS-CCD filter. The CLS-CCD filter is designed for astrophotography: It gives you an excellent surpression of any kind of light pollution and still gives you neutral colors (when imaging with a OSC camera). If youīre using a monochrome camera use the CLS-CCD instead of your normal L-filter: Light pollution has the strongest impact on the S/N of the L-channel, and by using the CLS-CCD filter you get rid of it. In this way you get the complete color information from the object from the RGB images and a good, contrasty L-channel from the images taken with the CLS-CCD. If you have very strong light pollution, it might be a good idea to place the CLS-CCD in front of the filterwheel, so it will also work for the color channels.
By the way: The "-CCD" does mean that the filter has a built-in IR-blocker. So you donīt need to worry about any unwanted IR in your image: Itīs blocked by the filter.