Frequently Asked Questions

What type of diffraction gratings (a.k.a. gratings) does Wasatch Photonics manufacture?

We make volume phase holographic gratings (VPHGs) recorded interferometrically in DiChromated Gelatin (DCG) sealed in glass. While there are many other optical recording media, DCG possesses the required combination of characteristics to produce very low polarization dependent loss (PDL), very high efficiencies, and wide bandwidths. These translate into benefits that enable telecom and other companies to leverage and capitalize on their own technologies.

How does your Volume Phase Holographic Grating (VPHG) technology differ from surface relief grating technology?

VPHGs, have a constant thickness (T) with a periodic, typically sinusoidal, change in refractive index (n). Surface relief gratings have a periodic change in thickness with a constant refractive index. Most VPHGs are made in transmission geometry while most surface relief gratings are made in reflection geometry. Surface relief gratings are copied mechanically, and thus both the surface relief grating original and copies will degrade over time as the number of copies increases.

How do VPH gratings achieve such high 1st order diffraction efficiency?

High 1st order diffraction efficiency is a key characteristic of volume phase holographic gratings (VPHGs) made using dichromated gelatin (DCG) as the holographic medium. The use of holographic techniques in their manufacture creates a sinusoidal index modulation profile, which favors diffracting light into a single order. We manufacture our own holographic recording media, which allows us to have precise control over parameters which are critical for maximizing diffraction efficiency. Building upon years of knowledge and experience, we are able to use the outstanding characteristics of DCG, such as high dynamic range and superb optical clarity across a wide spectral range, to make high performance gratings.

What are some of the other properties of VPHGs?

VPHGs possess low stray light and low absorption in the visible and NIR. They are sealed in glass making them long-lived, easy to handle, scratch resistant, and easy to clean. VPHGs usually have anti-reflection (AR) coatings applied to one or both surfaces to minimize Fresnel reflections and increase overall output.

How do you clean VPHGs?

VPHGs, whether they are AR coated or not, can be easily be cleaned just as you would any other glass optic to remove fingerprints, dust, and contaminants. Use the standard optics cleaning method of “drop and drag”. Gently wipe the grating with a clean, lint-free cloth/wipe using acetone or alcohol without much pressure; reagent-grade methanol or Windex may also be used. Do not use MEK, polishing compounds, etc. Hard rubbing with such chemical or polishing compounds may damage the AR coating. AR coated surfaces will pass the “Scotch Tape” test.

What information is available on your gelatin recording medium and is it stable over time?

Our gelatin recording medium is very similar to the gelatin that has been used in the photography industry for more than 100 years. As you may know, properly processed photographs are very stable and will retain their properties for decades. One of the major reasons for this excellent stability of photographs is the stability of the gelatin base. The discoloration of very old black and white photographs is a result of insufficient removal of fixer from the paper base, which results in a yellowing of the paper. It has nothing to do with the gelatin.

Wasatch Photonics uses a dichromated gelatin (DCG) mixture as its recording medium of choice. Once this mixture is processed and the chromium removed, it is essentially pure gelatin and is very stable. During the past thirty years, there has been no measurable degradation in gelatin gratings that are properly sealed. The DCG holographic scanning disks used in some of the early optical bar code scanners still function exactly as they did over 20 years ago.

What is a Dickson Grating® and why is it different from other gratings?

A Dickson Grating® is a highly specialized volume phase transmission grating. It can diffract both orthogonal linear polarizations with equal and high efficiency at included angles greater than 90 degrees over 40 nm bandwidths. Other gratings designed to be used at these high diffraction angles will have much greater PDL, lower diffraction efficiency, and a greater variation in diffraction efficiency across a 40 nm bandwidth. The 40 nm bandwidth and favorable high dispersion angles combined with efficiencies near 95% make the Dickson Grating® highly desirable for Telecom applications such as Mux/Demux/Remux, OSA, monitors, filters and Raman Spectroscopy. The grating is named after the grating designer, and Wasatch Photonics Co-Founder, Lee Dickson.

What kind of performance characteristics can be expected from a Dickson Grating®?

Dickson Gratings® can easily be designed for almost any spectral range. For instance, a 940 lpmm Dickson Grating® designed for 1525-1565nm will have these high performance characteristics:

  • High Dispersion
  • Extremely High Efficiency (>90%)
  • Extremely Low PDL (<0.25dB)
  • Flat Response Across C, S, or L Bands
Can gratings with different dispersion angles be made?

VPHGs can be made at almost any angle. Dickson Gratings® perform in narrow angular ranges, it is this limitation that allows them to work as well as they do. There are however two classes of realizable Dickson Gratings® with the first working near a half angle of 46.5 degrees in air and the other working at internal angles too high to escape from a flat substrate which must therefore be used with prisms. This latter design is termed the Dickson Grism® and has nearly TWICE the dispersion per pass of a Dickson Grating®. In January of 2005, we delivered samples of our latest high dispersion product, the Dickson 1350® for 1525-1565nm which produces >2 times the dispersion of a 940 lpmm Dickson Grating®.

Over what wavelengths can your gratings operate?

We cover 350 – 2400 nm (the entire visible range and NIR) with a selection of glass substrates and prisms.

What Physical sizes can be made?

Typical ruggedized sizes with perfect hermetic seals begin at approximately 20 mm x 30 mm. Smaller sizes have to be externally sealed. Gratings as large as 300 x 300 mm have been made by the Wasatch Photonics team.

What wavefront uniformity/distortion can be expected?

1/4 wave is typical. We can offer very low wavefront error with a Dickson Grating®.

What environmental tests have been performed on your gratings?

Our telecom-grade, epoxy sealed gratings have survived boiling water for several days with no degradation and 95° C at saturated humidities for more than 2 weeks. A collapse of the grating structure has been observed after several days at 120° C. Some of our similar, but non-Dickson design, gratings are currently in commercial multiplexers and are surviving real world tests as well as having passed standard compliance testing. The DCG is hermetically sealed between various substrates such as BK-7, Borofloat, low iron sheet glass and fused silica, making it impervious to everything but extreme heat.

What are the thermal and aiming characteristics?

Aiming stability over time and temperature is completely dependent upon the substrate used. Near zero drift is obtained by using a substrate with a low thermal coefficient of expansion (TCE) such as fused silica.

How is DCG affected by DWDM and input signal conditions?

There is hardly any absorption in a phase grating. The more common reflection gratings absorb as much as 20% and get really hot. It is not uncommon for communication signals to be between 5 and 50 mw, so adding up a hundred or more channels is a lot of heat. The gratings can take the heat but the losses at the fiber ends will be measured in watts, so heat dissipation probably has to be considered in a device’s package. Total absorption and scatter in the grating is about 2 or 3% so it is not a problem. Depending upon the glue, it can begin to soften or degrade between 10 to 100 watts per square cm continuous wave. Properly hardened gelatin can withstand >100 watts per square cm continuous wave. Peak power from pulsed laser energy applications can have energy densities in the megawatts.

Is grating performance affected at temperature extremes or as a result of temperature cycling?

Test results over a temperature range of 0-100°C indicate no significant change in efficiency, <0.5%, for a typical Dickson Grating®. Gratings can also withstand repeated temperature cycling with no measurable degradation in performance.

Are your gratings affected by radiation?

The effect of high energy radiation on gelatin is also important to anyone intending to put DCG HOE’s into space or into solar collectors outdoors or into creative lighting designs in buildings where the windows are DCG gratings. Gelatin, like all organic and many inorganic substances will be damaged by photons of more than 4 or 5 electron volts. Eventually all the bonds will be broken if the flux and energy are high enough for long enough. The gel will then be decomposed into loose atoms and molecules incapable of maintaining the original physical form. Fortunately the process takes a very long time to complete, if the gel is protected between two pieces of glass.

We have tested holographic scanners sandwiched between two pieces of 1.5 mm thick glass by placing them near a 250 watt low pressure mercury arc lamp for over 24 hours or until the glass itself solarized and became dark near the exposed surface. The gelatin was unchanged in diffractive properties but the glue line and the gel were slightly yellowed which would reduce transmission in the blue region. Less severe tests on display holograms were carried out from 1977 to 1979 where the test pieces were placed out in the open to take on whatever the weather in Salt Lake city and also in New Jersey could dish out. In all cases, for a year or for a month, the glue that we were using then became noticeably yellow but the gelatin and glass remained unchanged within the limits of our ability to measure it optically.

Another test was carried out on DCG and three other recording materials that were all prepared in our Paradise lab in 1989 for Northrop electronics division. Several Sample gratings were recorded on thick fused silica substrates and then baked and capped with another silica plate. This time the wave-fronts were measured and photographed before and after the radiation treatments. Neither the efficiency or any other property of the hologram changed from high energy radiation equivalent to several years of direct exposure in space. A few of our customers have put our large gratings into green houses as panes of glass and they appear to have survived at least since 1986 or so. Several 16 inch diameter hoes have gone to NASA Goddard where they are used in outdoor LIDAR since about 1991. One early reflection hoe which was not baked out has drifted a little to the blue, nothing that was baked thoroughly before sealing has changed. — By Richard Rallison

Holographically recorded gratings normally have a special efficiency dependence across the grating caused by a laser’s Gaussian beam profile. Do your holographic gratings have this spatial dependence?

We have developed novel techniques that significantly reduce variations in diffraction efficiency across our gratings.

What is the minimum & maximum integration time for the Cobra-S OCT spectrometer?

The minimum integration time for the Cobra-S spectrometer is 1.3 μs. The maximum integration time is 655.35 μs.

How do I set up my Cobra OCT spectrometer?

Detailed instructions, a summary of data flow, and camera link commands can be found on our guide, Cobra Spectrometers: Getting started.

What optical fibers should I use with my Cobra OCT spectrometer?

Cobra spectrometers in the 800nm passband would include a FC/APC to FC/PC patch cable with a Nufern 780HP fiber type. (0.13NA, ~5um mode field diameter e.g. Thorlabs P5-780A-PCAPC-1).

Spectrometers using 300nm excitation would typically use a 630HP or SM600 fiber type (0.13NA, ~4um mode field diameter e.g. P5-630A-PCAPC-1).

VIS units would include a 405 or 460 fiber depending on the spectral range:

SM300, 0.13NA, ~2um MFD e.g. P5-405B-PCAPC-1
CS550-555/80, CS550-573/115, CS550-600/200
SM400, 0.13NA, ~3um MFD e.g. P5-460B-PCAPC-1

NIR units use SM980-5.8-125, 0.13NA, ~5.8MFD e.g. P5-980A-PCAPC-1. Other acceptable fiber types in this passband include 980HP and SMF28.

The goal with the fiber size is to keep the core small enough to ensure single-mode operation across the wavelength range of the spectrometer. Some of our spectrometer spectral ranges exceed the operating wavelength specifications of commonly available fibers, and in those cases it is generally preferred to use a fiber that ensures single mode operation on the low end of the spectrometer’s spectral range.

OCT systems built by Wasatch typically use patch fibers from Thorlabs or Neptec.

How can I work with my Cobra OCT spectrometer in LabView?
How do I communicate with e2v Octoplus camera?
How do I operate a Cobra-S camera in 80-bit mode for 250kHz operation with MX4 frame grabber?
How do I install Cobra-S CameraLink and WPOCT SDK?
How do I update MX4 firmware?
How do I configure Xtium-CL MX4 frame grabber triggering?
How do I maximize data rate for my Octoplus camera?

The Octoplus CL BA3 (3 is the highest speed class) can support anything from 2Tap 12-bit 80khz up to 8tap 10-bit 250khz. The cameralink geometry is changeable through E2V commcam software, then the frame grabber and software need to be configured to match how the camera is configured. The Octoplus BB series has higher dynamic range (around 200ke-1 vs 140ke-1 well depth).

What should be contained in a fringe calibration file and how the API process the file?

The fringe file the WPOCT processor toolkit reads in can be generated by a Octave/Matlab script and is unique to each spectrometer based on the wavelength calibration coefficients. It is used to characterize the pixel space into a k-linearized wavenumber space as part of the OCT processing which will help to get more consistent axial resolution at different depths after numerical dispersion compensation. The wavelength is converted to wavenumber and then spline interpolated into a range of 1-2048 pixel values.


save calibration_C-0XXXX_MM-DD-YY.txt cal -ascii;
How can I connect two Wasatch spectrometers to a single Xtium-CL_MX4 frame grabber?
To interface with two cameras on one MX4, the firmware configuration of the MX4 needs to be changed to 2x Base Camera Link in the Device Update Tab of the Teledyne DALSA Device Manager. This utility can be found by searching the windows start menu for Device Manager or Firmware Update.

  1. Once the configuration is picked, press Start Update to reflash and reset the frame grabber. Now there will be two resource indexes within the same servername.
    Note that dual base mode means that each camera will need to have one CameraLink cable hooked to PoCL1 port and be in a 2Tap base cameralink geometry with a max line rate capability of ~80 kHz.
  2. Within CommCam, if you answer yes to automatically scan ports, it should look at both direct serial ports of the frame grabber. These can be seen in the Setup → Port Selection option.
  3. Select the 2Tap 12-bit 1×2 example configuration
How can I change the excitation wavelength or other EEPROM fields in ENLIGHTEN?

Read how in our guide to ENLIGHTEN’s EEPROM Editor.

Can I use any FC/PC fiber with my Raman laser purchase from Wasatch Photonics?

Most of the Raman lasers we sell can be mated to our Raman probes using a standard, off-the-shelf 105 μm core FC/PC fiber. However, the Hubner Photonics Cobolt 08-DPL 532 nm laser with HS-03 Heatsink we sell requires a special FC/PC connector with a narrow key. But don’t worry – we will quote and provide this with the purchase of this laser!