In this thread, I introduce a user-extension DetectorToTIFF to save Detector Viewers as TIFF images. Presently, the user-extension supports Detector Rectangle, which are saved as monochrome 8-, or 16-bits TIFF images. This user-extension is meant to complement the Output Image File field of the Detector Viewer's settings. Version Current version: 0.7   This extension has been developed and tested on OpticStudio 19.4 SP2. The latest release, v0.8, can be found in my latest reply to this thread. Installation To install the user-extension, download the archive DetectorToTIFF.ZIP and extract it on your computer. This archive contains a local version of this thread and the user-extension DetectorToTIFF.EXE, which you must copy to your \Documents\Zemax\ZOS-API\Extensions folder of OpticStudio. Use To use the user-extension, open a non-sequential file, such as User aperture sample.zmx from the \Documents\Zemax\Samples\Non-sequential\Miscellaneous folder of OpticStudio. Then, run a ray t

In case you missed it, our sag maps now have an automatic setting that will automatically report sag in off-axis coordinates.  This is helpful for users who regularly work with off-axis mirror and freeforms. (We’ve added this option to our slope and curvature maps, as well.) The sag is reported in a new coordinate system centered on the off-axis vertex and with tilt across the aperture removed.  Tilt values are reported out in the graphic.  Exact sag data can be retrieved using the SSAG operand, where the “off-axis” option is also available.  Tilts and other information about the data can be retrieved using the DSAG operand. 

Update 2021-09-24This forum thread is answer some frequently asked questions about the volume hologram model in OpticStudio.In OpticStudio 21.1, we have implemented volume hologram model for these sequential surfaces: Hologram 1, Hologram 2, Toroidal Hologram, Optically Fabricated Hologram. This allows users to analyze the diffraction efficiency with give material information. More infomraiton can be found in Help file in OpticStudio 21.1 and this knowledge base article: Simulating diffraction efficiency of a volume holographic grating using Kogelnik’s method  1. Can I make the hologram with any kind of user defined shape?When we say surface shape, it could be the substrate or the aperture. Here we will talk about both.The shape of substrate only supports Standard (conic sphere), Toroidal (cylinder), Extended Polynomial (freeform) for now, but we can investigate if users request more.If more shape of substrate are needed, except sending a feature request to Zemax product team, the fast

The f-number (F/#) is defined as the focal length divided by the entrance pupil diameter. In ZEMAX, the Effective Focal Length (EFL) is calculated by tracing an on-axis parabasal ray, and the Entrance Pupil Diameter (EPD) is the diameter of the paraxial image of the stop in object space. However, measuring EFL with a single ray in the real world is challenging, and the paraxial EPD image doesn't match the actual EPD image. This often results in a discrepancy between the Image Space F/# in ZEMAX and the measured f/#.The measurable EFL is determined by measuring the image height with a known incident angle. The Trioptics ImageMaster® HR, a common testing device, projects a double slit from infinity with a half-width angle of about 0.573 degrees. EFL is calculated as ImageHeight / TAN(0.573 degrees). To calculate measurable EFL in ZEMAX, insert a field with a 0.573-degree object angle and use CNEY to obtain the image height. The EFL can then be calculated in the merit function editor. Usi

The f-number (F/#) is defined as the focal length divided by the entrance pupil diameter. In ZEMAX, the Effective Focal Length (EFL) is calculated by tracing an on-axis parabasal ray, and the Entrance Pupil Diameter (EPD) is the diameter of the paraxial image of the stop in object space. However, measuring EFL with a single ray in the real world is challenging, and the paraxial EPD image doesn't match the actual EPD image. This often results in a discrepancy between the Image Space F/# in ZEMAX and the measured f/#.The measurable EFL is determined by measuring the image height with a known incident angle. The Trioptics ImageMaster® HR, a common testing device, projects a double slit from infinity with a half-width angle of about 0.573 degrees. EFL is calculated as ImageHeight / TAN(0.573 degrees). To calculate measurable EFL in ZEMAX, insert a field with a 0.573-degree object angle and use CNEY to obtain the image height. The EFL can then be calculated in the merit function editor. Usi

The attached are two files that shows how to simulate CMOS diffraction using the static link in OpticStudio.More information about using static link can be found in the following article:How to load grating data from Lumerical into OpticStudio – Ansys Optics When the files are opened, it might look as below. It’s not difficult to find object 21 is set up with the static link, which is supposed to simulate how CMOS can diffract lights and cause straylight when it comes back.The Stochastic mode is turn on because rays will revisit the CMOS many times and generate so many calculations.The Test Mode is set to 9 for a special handling to the grating data. Normally, when light hits CMOS, most of the power is absorbed and converted to electric power in the pixels. And only a certain ratio of power is diffracted in the reflection direction. If the grating data is generated from Lumerical, there will be only reflection diffraction and no any transmission order. The trick of Test Mode = 9 is it

This discussion presents methods for evaluating equivalent system performance in sequential and non-sequential modes. The key areas covered include Surface/Object Face Sag Maps, GEO MTF, and spot sizes, with corresponding pathway settings detailed below: Compare Surface/Object face Sag Map Configuration steps:   SEQ:  The Analyze Tab (sequential ui mode) » Polarization and Surface Physics Group (the analyze tab, sequential ui mode) » Surface » Surface  NSC: The Analyze Tab (non-sequential ui mode) » Polarization and Surface Physics Group (the analyze tab, non-sequential ui mode) » NSC Surface Sag    Compare GEO MTF (Geometrical Modulation Transfer Function) for non-diffraction-limited aberrated systems Configuration steps:   SEQ: The Analyze Tab (sequential ui mode) » Image Quality Group » MTF » Geometric MTF  NSC: The Analyze Tab (non-sequential ui mode) » Image Quality Group (non-sequential) » NSC Geometric MTF.    Compare spot sizes  Configuration steps:   SEQ: To match the NSC

The definition of a solid angle can be found in the Wiki.https://en.wikipedia.org/wiki/Solid_angleFrom the Wiki, you may know a solid angle can be calculated from the following formula.（Eq.１）And the relationship between (θx,θy) and (θ,φ) is as shown in the following equation.The variables in (Eq 1) are (θ,φ). We will convert them to (θx,θy) by the way of variable transformation.https://math.libretexts.org/Courses/Monroe_Community_College/MTH_212_Calculus_III/Chapter_14%3A_Multiple_Integration/14.7%3A_Change_of_Variables_in_Multiple_Integrals_(Jacobians) Finally we can get the result as below.（Eq. 2）(Eq. 2) can be used to calculate the solid angle from a specific pixel coordinate.However, there is no analytical solution for this equation. We know that a numerical solution can be calculated.In fact, our algorithm is not this method. When OpticStudio calculate the radiant intensity, a iteration method is used.Theoretically, the result is the same. One of our users has verified this.

Hi, all!I have a question: how is RAY TRACE in NSC realized?In my impression, RAY TRACE assumes a bundle of rays, which consists of a certain number of analysis rays, e.g. 100 0000, then trace each ray, and record them on the detector. The operation is purely geometry optics (reflection, refraction,...) However, why can it be used to simulate interference, which in fact belongs to the scope of wave optics?I would highly appreciate any inspiration!best,YJ

It would be nice if a field for rounded corners existed in the aperture properties of the Rectangular Aperture/Obscuration. This seems basic enough to not require a UDA. A value of 0 would result in square corners, and a value larger than the minimum of the X and Y half-widths would default to that minimum.  

 Nonsequential mode is designed to quickly trace millions of rays through complex geometries.  But for the setup or initial optimizations of systems, it is sometimes useful to trace and optimize just a few important rays.  One can use the NSTR operand and the Source Ray objects to do this.  The process requires some manual setup, but can easily be automated using the ZOS-API.As an example, I have a system that contains a plate and an off-axis parabola (OAP).  I’ve manually moved the detector, but I would like it to be centered on the gut ray and tilted to find the image.An off-axis system in need of detector positioning.In the Nonsequential Component Editor (NCE), I’ve added 9 Source Ray objects.  I’m separating them in the Y direction, at field points of 0, 0.2° in +Y, and 0.2° in +X.  Each set of three rays that have the same field angle should come to a focus in the image plane, as shown in the layout plot below. Adding individual rays in the Nonsequential Component Editor (NCE).A l

Hey Peeps,SPIE has a new book out: https://spie.org/Publications/Book/100014 called Optics Using Python.I have bought but not received a copy yet, so no review, but it looks interesting and generally applicable to anyone who uses Python to connect to ZOS-API.Mark 

Dear ExpertsI have calculated two end coordinate points of an off-axis parabolic mirror lets say (184, 13.5) and (217, 18.8), may i ask if i can design this mirror in zemax by using these coordinate points and focal length of 200 micron.  Please advise All units are in micrometer. sincerelysaif

In OpticStudio, an option is available for assigning Coherence Length to a source as shown below. This works based on randomizing the wavelength of each ray. In this post, an another method is demonstrated for simulating coherence length. In this method, it’s assume light with different wavelength cannot interfere. In other words, the interference pattern of a multi-wavelength source is the incoherent sum of the interference pattern of each wavelength themselves.In fact, light with different wavelength could interfere. However, the interference pattern cannot be detected because the pattern changes with very high frequency and vanishes when sensor averages it over time. The following picture explains it. To calculate the interference pattern of each wavelength and incoherently sum them, we need to do it manually. Here we provide a simple case and an ZOS-API code to demonstrate how to do it.To see how it works, users just need to open the attached ZAR file, turn on Interactive Extension

Like the exit pupil, the entrance pupil can be found using real rays; rays at different field angles must cross at any internal pupil of the system.  Adding a dummy surface at the location of the entrance pupil allows us to place optimization operands on that surface, to control location, diameter, tilt, etc. of the entrance pupil.  Finding the entrance pupils is especially useful in the case of wide-angle systems, where the entrance pupil may be decentered and tilted, leading to images that are significantly darker at the edges.In the wide-angle system shown below, the full field of view is 100 degrees and the stop is in the center of the system, as shown below.  Using the Draw Real Entrance Pupil option in the 3D Viewer shows that the entrance pupil moves down and to the left with increasing field angle.A system with a full FOV of 100 degrees, with the entrance pupil shown for each field angle.Isometric view showing the outline of the entrance pupil at each field angle.Below, I’ve se

Over a year ago, I posted an initial version of a user-defined surface that models an idealized perfect lens satisfying the sine condition, see:This is distinctly different than a paraxial lens surface that does not, in general, satisfy the sine condition.  As a result, a paraxial lens is a poor substitute for a well-corrected high-NA lens (e.g., a microscope objective, in which a paraxial version yields the wrong NA for a given EPD, and vice versa).Since my initial posting, I have revised the model and published the details in Applied Optics.  The new model simulates both a perfect imaging lens and a perfect Fourier transform lens.  The paper, as well as the DLL and several example model files, are all freely available at:Ray-tracing model of a perfect lens compliant with Fermat’s principle: the Cardinal Lens .I’ve removed the older version of the DLL now that this new one is available.Please feel free to try it out and provide feedback.Regards,Jeff

Hi, everyone.  Often, we need to control the size and location of the exit pupil in an optical design so that filters or other elements can be placed there.  It’s fairly easy to place a dummy surface at the exit pupil and then use operands on thickness, diameter, or global position to control the exit pupil location and size.For the Double Gauss system below, I’ve added two surfaces at rows 13 and 14: one going to the exit pupil, and one returning to the original position using a pickup.  Surface 14 will be located at the exit pupil, then.  I’ve also moved the original thickness traveled to the image plane down to surface 15, preceding the image plane. Additional surfaces inserted so that surface 14 can be optimized to fall at the exit pupil.To move the dummy surface to the exit pupil, I rely on the fact that rays that intersect at the stop should also intersect (or nearly so) at the exit pupil.  To find the Z location of the exit pupil at wavelength 2 for the on-axis field position, I

OpticStudio supports Q-type aspheres.  Type 0 indicates Qbfs polynomials, and Type 1 indicates Qcon polynomials.  The functional forms of the Q-type polynomials are fairly complex due to the requirement that the polynomials be orthonormal for a circular aperture.  Occasionally, it is convenient to know the functional form of the polynomials for testing and comparison purposes. Below, we list the first 10 Qbfs polynomials, and also share how to calculate them in the Mathematica file GenerateQbfsPolynomials.nb.  The .nb files for Mathematica can be used by downloading the free Wolfram Player: https://www.wolfram.com/player/.Important equations for the Q-bfs polynomialsThe equations used below come from Shape specification for axially symmetric optical surfaces, G.W. Forbes, Optics Express 5218, Vol. 15, No. 8, 16 Apr 2007.  Forbes watned to find a function whose slopes are orthogonal.  So the slope equations must obey:where u is the radial coordinate in the aperture of an optical surface

Asphericity is a useful value when manufacturing an asphere or a freeform surface.  It is typically defined as the distance between the smallest best-fit sphere (BFS) that touches the surface without intersecting and the ideal surface shape, as sketched below.  (The BFS usually contacts the surface at one radial location; in the part sketched below, the BFS contacts the part at the outer edge.) OpticStudio can return both the BFS and the asphericity using the Surface Sag map and/or the DSAG operand in the Merit Function.  Choose Analyze/Surface/Sag to open the Sag map of the surface and then set “Remove” to “Best Fit Sphere” with the “Minimum Volume” option, as shown below.  The peak-to-valley of the resulting plot is the asphericity.  The radius of curvature of the minimum volume BFS is also listed.Use the Surface Sag map to find the asphericity of a surface.Both values can also be retrieved using the DSAG operand with Remove = 2 and BFS = 0.  Data = 2 retrieves the P-V of the sag map

Although there is no a “Cylindrical Detector” object in Non-Sequential, there are several workarounds to make it, since most objects may act like a detector (To make any objects a detector, choose "Object Is A Detector" from the Type tab of the Object Properties dialog box). Once the object is set to be a detector, the intensity detected will be displayed on the Shaded Model display, and on the text listing tab of the Detector Viewer window. There is a Cylinder Pipe object in OpticStudio but it cannot be used as a detector because the curves of the object are modelled exactly within OS—the curves are not approximated by facets. Only objects which are faceted can be used as detectors. But there are some alternative object types that all have a faceted representation and so would work as a detector: You could create a cylinder pipe object and then export it as a STL file and use this new object as your detector. (See Export CAD files: The File Tab > Export Group > CAD

Every time I use Convert to NSC Group I’m amazed at how useful it is. I well remember life without it. Thank you for the gift that keeps on giving. And Merry Christmas to all!

Hello,I'm currently working on simulating a splitting rhomb with one input and three outputs, each responsible for 33% of the total power. After completing the design in the 3D CAD model, I imported it into Zemax non-sequential and exploded the CAD model. However, I've encountered an issue: despite applying a 33% coating to the faces of the rhombs in Zemax, the software seems to ignore it, allowing the beam to pass through unaffected. Any insights on how to resolve this would be greatly appreciated.  

Speckle is created by the interference of multiple, mutually coherent optical fields that have random phases at any point on a detection surface.  This could be associated with laser light scattering from a rough surface or from the interference of multiple modes emanating from a multimode fiber.  For multimode fibers, it may be best to use POP in a sequential model in which the beam leaving the fiber is modeled as a coherent superposition of LP (or LG) modes.  Alternatively, we show here how a simple non-sequential ray-based model can be used to simulate speckle arising from rough-surface scattering. To model light leaving a rough surface, we can employ Huygens’ Principle and use a set of point sources that are randomly phased over (0,2pi).  This assumes the height variations on the surface are large enough to create such a random process.  Ideally, we would use a single non-sequential source that emits rays uniformly over some spatial region and within a defined cone angle.  However,

Hi all.  It is frequently useful to have the Zernike Standard Polynomials available in Cartesian form, rather than just in the standard polar form.  The Cartesian forms can be used for a few different things, such as:Generating or fitting data that is sampled on a uniform XY grid Converting Zernikes into other surface shapes, such as Extended Polynomials.Below, I’ve listed the first 37 Standard Zernike coefficients.  See the attached files for all 231 terms in text form and a Mathematica notebook that generates them. (See https://www.wolfram.com/player/ to read the .nb file.) 

Long ago, people reverse engineered the .zmx file format.  However, this was never a supported file format.What interest exists for an open source file format for lens systems?Such a file format (analogous to STEP) would enable inter-operability between commercial and open source software.Not all of us can afford to purchase all the software that Ansys offers.  I can’t work entirely in the Ansys eco-system.  Can you?  An open source format would allow me to work better with other software vendors and state-of-the-art software developed in universities or in open source.