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Can someone explain how an IR filter is able to "absorb" IR light? I tried looking for specific explanations, but no luck. Just that they have special "technology" that absorbs it. Is this just a fancy word for a different way of reflecting away IR? Where it's not simply cutting it like a Schneider TruCut, but perhaps using micro particles in the filter that simply scatter the IR light?

The solution is to employ the fact that gratings are most efficient when the rays emerge from the grating as if by direct reflection. By creating tilted facets, or a blaze, in the grating, as shown in figure 97, it is possible to direct the majority of the light (~70%) into the order of interest.

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is there a difference between a hot mirror and a IR filter? if so when would i use a IR and a hot mirror ? is it not both to protect the chip from infrared light ?

Having IR/ND combos has had its problems on a couple shoots I've been on. If you want to stack IR/ND's, there can be reflection issues between the filters, so it's best to just have an IR out in front, then a couple stages behind it for regular ND filters. Besides, with the newer MX and Alexa chips, IR contamination really isn't a huge issue until you go over 1.2 ND or so, as I've been told by DIT folks. So having the lighter grades of ND equipped with an IR overlay is overkill at this point.

The fact that diffraction gratings produce multiple spectra, or orders, each with a different dispersion, makes them very versatile but also very inefficient. Most of the light is directed to the zeroth order, which is undispersed and hence useless for spectroscopy. Only ~10% of the light is directed to the first order, which is the most commonly used order in astronomical spectrographs. Some means of directing all of the light into the order of interest would therefore be highly desirable, as illustrated in figure 96.

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So it just uses the same principle as with any other element in the world that absorbs light and reflects, which makes it the color see. Hence the reason for white balancing when an IR filter is down (because of the green cast), whereas with a Hot Mirror it's not AS necessary it seems.

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Having covered gratings, dispersion, resolution and blaze, you should now be able to understand a typical table from a spectrograph user manual, such as that shown in table 3. The first column gives the grating name, where "R" refers to a diamond ruled grating, "H" to a holographic-etched grating, "1200" (for example) to the number of grooves per mm and "B" to the fact that the grating is optimised for blue light. The second column gives the blaze wavelength of the grating in Å, i.e. the wavelength of peak grating efficiency. The third and fourth columns give the dispersion of the grating in units of Å/mm and Å/pixel, where each detector pixel is 13.5 μm in size. The fifth column gives the wavelength range of the resulting spectrum, obtained by multiplying the dispersion in Å/pixel by the number of CCD pixels in the dispersion direction (4096). Only 3500 of these 4096 pixels are usable, so the sixth column lists the usable wavelength range. The final two columns list the slit widths in arcseconds that must be used to obtain a projected slit width at the detector of 54 μm (i.e. 4 pixels) and 27 μm (i.e. 2 pixels). The latter case corresponds to sampling at the Nyquist critical frequency, and the spectral resolution is then given by twice the dispersion. Using a slit which projects to less than 2 pixels will not improve the spectral resolution, as the slit will then be undersampled by the CCD pixels. The 54 μm projected slit width is well matched to the typical seeing on La Palma, resulting in good throughput but oversampling by the CCD pixels; the spectral resolution in this case will then be defined by the slit, not by the pixels.

as far as i know there are combined IR ND filters but only straight hot mirrors - any reason for why there is no ND hot mirror ?

The difference would be that an IR filter absorbs the IR, while the hot mirror reflects it away, and passes the visible light. For camera filters, it doesn't make a difference. It matters where you have so much light that the heat of the unwanted IR is significant, like in digital projectors. You need to not burn up the chips.

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Basically the same thing, and they serve the same purpose, I think it just depends on whether a specific brand chooses to call theirs an IR or Hot Mirror. Different brands have different characteristics in regards to how much IR they remove, so it's worth testing between say Tiffen or Schneider, to name a couple.

blazes The fact that diffraction gratings produce multiple spectra, or orders, each with a different dispersion, makes them very versatile but also very inefficient. Most of the light is directed to the zeroth order, which is undispersed and hence useless for spectroscopy. Only ~10% of the light is directed to the first order, which is the most commonly used order in astronomical spectrographs. Some means of directing all of the light into the order of interest would therefore be highly desirable, as illustrated in figure 96. figure 96: Top: the diffraction pattern produced by a white light source incident on an unblazed (top) and blazed (bottom) diffraction grating, where only the orders n = 0, +1, +2, +3 are shown. Note how the spectra get fainter as the order increases in the unblazed case, and how most of the light is directed into the order of interest (n = +1) in the blazed case. The solution is to employ the fact that gratings are most efficient when the rays emerge from the grating as if by direct reflection. By creating tilted facets, or a blaze, in the grating, as shown in figure 97, it is possible to direct the majority of the light (~70%) into the order of interest. figure 97: Left: a microscopic view of the tilted facets in a typical blazed diffraction grating. Right: an illustration of the saw-tooth profile of a blazed reflection grating. The tilt of the facet ensures that most of the light is diffracted to the first order rather than the zeroth order.    Having covered gratings, dispersion, resolution and blaze, you should now be able to understand a typical table from a spectrograph user manual, such as that shown in table 3. The first column gives the grating name, where "R" refers to a diamond ruled grating, "H" to a holographic-etched grating, "1200" (for example) to the number of grooves per mm and "B" to the fact that the grating is optimised for blue light. The second column gives the blaze wavelength of the grating in Å, i.e. the wavelength of peak grating efficiency. The third and fourth columns give the dispersion of the grating in units of Å/mm and Å/pixel, where each detector pixel is 13.5 μm in size. The fifth column gives the wavelength range of the resulting spectrum, obtained by multiplying the dispersion in Å/pixel by the number of CCD pixels in the dispersion direction (4096). Only 3500 of these 4096 pixels are usable, so the sixth column lists the usable wavelength range. The final two columns list the slit widths in arcseconds that must be used to obtain a projected slit width at the detector of 54 μm (i.e. 4 pixels) and 27 μm (i.e. 2 pixels). The latter case corresponds to sampling at the Nyquist critical frequency, and the spectral resolution is then given by twice the dispersion. Using a slit which projects to less than 2 pixels will not improve the spectral resolution, as the slit will then be undersampled by the CCD pixels. The 54 μm projected slit width is well matched to the typical seeing on La Palma, resulting in good throughput but oversampling by the CCD pixels; the spectral resolution in this case will then be defined by the slit, not by the pixels. table 3: Details of the gratings available in the blue arm of the ISIS spectrograph on the 4.2 m William Herschel Telescope on La Palma. ISIS wavelength coverage and resolution with EEV12 Grating Blaze Dispersion (Å/mm) Dispersion (Å/pix) Total Spectral range (Å) Unvignetted range (3500 pixels) Slit-width for 54 mu at detector (in arcsecs) Slit-width for 27 mu at detector (in arcsecs) R158B 3600 120 1.62 6635 5670 0.8 0.4 R300B 4000 64 0.86 3539 3024 0.8 0.4 R600B 3900 33 0.45 1825 1560 0.9 0.45 R1200B 4000 17 0.23 940 803 1.1 0.55 H2400B Holo 8 0.11 442 378 1.2 0.6 grisms removed from course ©Vik Dhillon, 18th September 2012

Absorbtion works in IR just like in visible light. A green filter absorbs the red and blue wavelengths, and passes the green. Dyes are big complicated molecules, and some of the bonds in those molecules capture certain wavelengths, and turn the energy into motion on the molecular level, which is heat. Of course it's only a significant amount of heat if you have a huge amount of light, like in digital projectors. For camera filters, it's too little to matter. But the gels that we use on lights do fade and/or burn after a while.

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The one sorta goofy thing is that what we call an IR filter absorbs IR and passes the visible light, while what we call a green filter passes the green and absorbs the rest. So, the names are the other way around....

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