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OPTIS Labs

2013

Table of Contents

Optical Property Editors ...................................................................................... 6 Surface Optical Property Editors ....................................................................... 6

Overview ............................................................................................... 6 Optical Polished Surface ........................................................................ 13 Perfect Mirror Surface ........................................................................... 13 Unpolished Surface ............................................................................... 13 Simple Scattering Surface Editor ............................................................ 15 Advanced Scattering Surface Editor ........................................................ 16 BSDF - BRDF - Anisotropic Surface Viewer ............................................... 17 Coated Surface .................................................................................... 27 Polarizer Surface Editor ......................................................................... 27 Retro Reflecting Surface Editor ............................................................... 30 DOE and Thin Lens Surface Editor .......................................................... 31 Grating Surface Editor ........................................................................... 35 Fluorescent Surface Editor ..................................................................... 36 Rendering Surface Editor ....................................................................... 37 LCD Surface ......................................................................................... 39 Rough Mirror Surface Editor ................................................................... 40 View ................................................................................................... 41 Tools .................................................................................................. 43 Others Options ..................................................................................... 48

Spectrum Editor ........................................................................................... 49 Using the Spectrum Editor ..................................................................... 49 Parameters of a Spectrum ..................................................................... 50 Color Rendering Index .......................................................................... 50 Spectrum Generation ............................................................................ 51

User Material Editor ...................................................................................... 52 Using the User Material Editor ................................................................ 52 Parameters of a User Material ................................................................ 53 Material Color ...................................................................................... 61 Editing the Preferences ......................................................................... 63

Labs .................................................................................................................. 64 Photometric Calc .......................................................................................... 64

Using Photometric Calc .......................................................................... 64 Parameters of Photometric Calc .............................................................. 64

Virtual 3D Photometric Lab ............................................................................ 65 Using Virtual 3D Photometric Lab ........................................................... 65 Managing the Display ............................................................................ 66 3D Map Post-Processing ........................................................................ 66 Surface and Section Analysis ................................................................. 67 Editing the Preferences ......................................................................... 69

Virtual Human Vision Lab .............................................................................. 69 Using Virtual Human Vision Lab .............................................................. 69 Importing an Image .............................................................................. 70 Exporting ............................................................................................ 70 Managing the Display ............................................................................ 74 Reading Precision ................................................................................. 76 Analyzing Colorimetric Data ................................................................... 76 Doing Color Management ...................................................................... 77 Look At ............................................................................................... 79 Vision Parameters ................................................................................. 81 Glare Effect ......................................................................................... 86 Doing Time Adaptation .......................................................................... 87 Doing Analysis ..................................................................................... 87 Legibility and Visibility Analysis .............................................................. 89 Using Sun Glasses / Colored Filter .......................................................... 92 Night Vision Goggles ............................................................................. 94 Surface and Section Analysis ................................................................. 95

Virtual Lighting Controller ...................................................................... 98 Editing the Preferences ....................................................................... 100

Virtual Photometric Lab ............................................................................... 100 Using the Virtual Photometric Lab ......................................................... 100 Importing and Exporting...................................................................... 101 Managing the Display .......................................................................... 110 Reading Precision ............................................................................... 111 Analyzing Colorimetric Data ................................................................. 112 Surface and Section Analysis ............................................................... 112 Virtual Lighting Controller .................................................................... 115 Using Sun Glasses or Colored Filter ....................................................... 117 Night Vision Goggles ........................................................................... 117 Editing the Preferences ....................................................................... 119 Managing the Filtering ......................................................................... 119

Virtual Reality Lab ...................................................................................... 121 Virtual Reality Lab Icons ...................................................................... 121 Using Virtual Reality Lab...................................................................... 122 Virtual Lighting Controller .................................................................... 123 Creating an Immersive View ................................................................ 124 Human Vision..................................................................................... 124 Stereo OptisVR ................................................................................... 126 Creating an Observer View .................................................................. 129 Virtual Reality Lab Management ........................................................... 129 MultiScreen ....................................................................................... 130 Using the SIM2 HDR Monitor ................................................................ 140 Virtual Reality Peripheral Network ......................................................... 140

3D Energy Density Lab ................................................................................ 141 Using 3D Energy Density Lab ............................................................... 141 Managing the Display .......................................................................... 142 Volume and Section Analysis ................................................................ 143 Virtual Lighting Controller .................................................................... 144 Editing the Preferences ....................................................................... 145

Viewers ........................................................................................................... 146 Intensity Viewers ....................................................................................... 146

Eulumdat Viewer ................................................................................ 146 IESNA LM-63 Viewer ........................................................................... 147 OPTIS Intensity Viewer ....................................................................... 149 Curves .............................................................................................. 150

Optical Design Viewers ................................................................................ 153 Coupling Efficiency Viewer ................................................................... 153 Gaussian Propagation Viewer ............................................................... 158 Glass Map Viewer ............................................................................... 158 Paraxial Data Viewer ........................................................................... 160 Real Aberrations Coefficients Viewer ..................................................... 167 Real Aberrations Viewer ...................................................................... 170 Spot Diagram Viewer .......................................................................... 172

Ray File Tools .................................................................................................. 176 Source Generator ....................................................................................... 176

Using the Source Generator ................................................................. 176 Parameters ........................................................................................ 176 Parameters of Position and Orientation .................................................. 183

Post-Processing .......................................................................................... 184 Intensity Distribution Post-processing ................................................... 184 XMP Map Post- processing ................................................................... 185

Ray File Editor ........................................................................................... 188 Using the Ray File Editor ..................................................................... 189 Importing and Exporting...................................................................... 189 Using Data Downloaded from OSRAM Opto Semiconductors ..................... 190 Parameters of Ray File Editor ............................................................... 192

Preferences ..................................................................................................... 194 Monitor ..................................................................................................... 194 Colorimetry ............................................................................................... 195 Printing ..................................................................................................... 195 Spectrometer ............................................................................................. 195 Virtual Photometric Lab ............................................................................... 196 Directories ................................................................................................. 196 3D View .................................................................................................... 196 Virtual 3D Photometric Lab .......................................................................... 198 Devices Preferences .................................................................................... 199 Real Time .................................................................................................. 199 TFCalc....................................................................................................... 199

Index .............................................................................................................. 200

of 207 OPTIS Labs User Guide

OPTICAL PROPERTY EDITORS

Surface Optical Property Editors

Overview

Surfaces Overview

You must create a geometry before applying optical properties.

Surfaces describe light's behavior when hitting the surface.

When the light hits the surface, three occurrences may happen: Light is absorbed, reflected or

transmitted.

With the surface editor you can parameterize these behaviors with regards to the wavelength and the

polarization.

You can then create your own coated surface filling in a table with your absorption and transmission

coefficients for each wavelength, and polarization.

Light Behavior Models

For transmission and reflection, light behavior is described with a combination of three models.

With these models you can create very precise surface taking into account that you can use them to

define light's behavior with regards to wavelength and polarization.

SPECULAR MODEL

Specular reflection on a surface

Rays propagate following the Snell -

Descartes law. The proportion of

transmitted and reflected rays is given by

the Fresnel laws (Optical polished and

Scattering models).

LAMBERTIAN MODEL

Lambertian reflection and

transmission on a surface.

The probability to be reflected in a given

direction is the same for all the direction

of the space.

Optical Property Editors of 207

GAUSSIAN MODEL

Reflection: Gaussian (10%) and

Lambertian (90%).

The light has a Gaussian probability to be

reflected with a particular angle around

the main direction defined by Snell -

Descartes laws.

BRDF, BTDF, BSDF, Anisotropic Measurement Models

MODEL PARAMETERS REMARKS USE

ADVANCED SCATTERING SURFACE

Theta incident Reflection and/or transmission

For surfaces that fits well

the Gaussian /

Lambertian model

Wavelength Not anisotropic (no dependency

with Phi incident)

Specular, Gaussian and

Lambertian for

reflection &

transmission

Fitted data

ANISOTROPIC SCATTERING SURFACE

Theta, Phi incident Reflection and/or transmission

For surfaces that fits well

the Gaussian /

Lambertian model

Specular, Gaussian and

Lambertian for

reflection &

transmission

Anisotropic (dependency with

Phi incident)

Reflection/Transmissio

n spectrum Fitted data

Vector for orientation Same colors for reflection and

transmission

COMPLETE SCATTERING SURFACE

Theta incident Reflection only

General reflective

surfaces Iridescent

surfaces

Theta, Phi reflection

Wavelength

Not anisotropic (no dependency

with Phi incident) Polarization | and //

both for incidence and

reflection

SIMPLE BSDF

Theta incident - Theta,

Phi reflection/

transmission - 1

Reflection/Transmissio

n spectrum

Reflection and/or transmission

- Not anisotropic (no

dependency with Phi incident) -

Same colors for reflection and

transmission

General isotropic

reflective/transmissive

surfaces (same colors for

reflection and

transmission) Not for

iridescent surfaces

ANISOTROPIC BSDF

Theta, Phi incident Reflection and/or transmission

General isotropic /

anisotropic reflective /

transmissive surfaces. Not

for iridescent surfaces.

Theta, Phi

reflection/transmission

Anisotropic (dependency with

Phi incident)

1 Reflection spectrum Different colors for reflection

and transmission

1 Transmission

spectrum

Does work for isotropic

surfaces as well


MODEL PARAMETERS REMARKS USE

Vector for orientation

To get a very precise description, you can use the Complete Scattering Surface (BRDF), BSDF Surface

or Anisotropic BSDF Surface which enables the description of almost every isotropic surface.

Complete Scattering Surface

Polarization

Polarization is linked with the physical nature of a photon. It is an electromagnetic wave like radio,

radar, X rays or gamma rays. The difference is just a question of wavelength. A wave is something

vibrating, in the case of a piano or a guitar, it is a cord. When talking about a photon, it is an

electromagnetic field (an electric and a magnetic field which are vibrating together).

In our software, we only take into account the electric field as the magnetic field can be deduced from

it in materials we are using for light propagation.

This electric field is vibrating in a plane which is orthogonal to the photon's direction and it describes

an ellipse centered on this direction.

Polarization is this ellipse defined by its orientation, ellipticity and rotation sense.

Birefringent materials, polarizer surface or optical polished surfaces (Fresnel) are using the

polarization.

Lambertian reflection is depolarizing. It converts polarized photons into unpolarized ones by changing

randomly its polarization while processing the reflection.

Application

The polarization is the main physical property LCDs are working with. LCDs are used together with

polarizer.

According to the applied voltage, they rotate or not the polarization axis of the light by 90°. So when

this light tries to cross the polarizer, it is stopped (black state) in case of a 90° angle of the

polarization axis with the easy axis of the polarizer or transmitted (white state) if this angle is 0°.

We saw that even the simplest surface quality (optical polished) has an effect on polarization. This is

the surface quality used each time one deal with a light guide in automotive (dashboards) or in

telephony (to enlight the keypad for example).

Since such devices are using multiple reflections inside they light guides, it is important to have an

accurate model to describe the light behavior on this surface.


It is possible to build a light guide with a birefringent material in order to build a special function for

the polarization. For example, a backlight for a LCD without any polarizer between the backlight and

the LCD reducing the losses due to the polarizer.

Example of Polarizers

Polarizer is an optical component which has a linearizing effect on incoming photons' polarization.

A perfect polarizer acts as a filter. It only allows one polarization component to cross the polarizer.

It is characterized by an easy axis indicating the polarization direction which is allowed crossing, the

other polarization component is absorbed.

Polarizer and Lens

In SPEOS Standalone software, light sources are always unpolarized. To obtain a linearly polarized

beam you can consider a collimated light source followed by a polarizer.

This polarizer is absorbing half the energy emitted by the source.

To check the light is linearly polarized after the polarizer, you can add a second polarizer which is

crossed compared the first one.

As its easy direction is orthogonal to the photon's polarization, it stops all remaining light.


Now a lens can be inserted between both polarizers. Its influence on polarization can be seen by

setting an irradiance sensor.

A known figure on the simulation's result can be seen.

The minimum of the energy is on the axis of each polarizer.

The maximum of the energy is at 45° between each axis.

Multiple Polarizer

Crossed polarizer (angle between easy axes is 90°) are stopping the light. This next example is a

successive polarizer with easy axes angles different from 90°.


Following picture gives the transmission in function of the angle between the easy axis.

In the Polarizer and Lens example, without the lens the light is completely stopped. In this example,

you can replace the lens by a polarizer whose easy axis is at 45° from the two others.

The light crossing the first polarizer in linearly polarized at 45° from the second one.

So the second polarizer only stops a part of the light and transmits photons whose polarization is 45°

from the last polarizer's easy axis. This makes that the last polarizer doesn't stop all the remaining

light. Moreover, the polarization of the light which goes out of the system is orthogonal to the easy

axis of the first polarizer. This system acts as a polarization rotation tool. We could achieve a better

transmission coefficient by making more rotation steps (here we made two 45° steps).

This is basically the way LCDs are rotating the polarization: The molecules in the liquid crystal may be

considered as small polarizer and their orientation is evolving along the light path making the

polarization rotate progressively reducing losses.

Brewster Angle

Even a simple glass has an influence on polarization. Its optical polished surface behavior on light is

described by Fresnel's law. This law is different for S and P polarization.


S polarization

P polarization

Parallel and perpendicular (orthogonal) refers to the electric field vector of the polarization and the

light incidence plane.

Parallel = P polarization = TM (transverse magnetic).

Orthogonal = Perpendicular = S polarization = TE (transverse electric).

S and P are named belong to the German words Senkrecht and Parallel.

We can see on the P polarization curve that there is an angle which only reflects S polarization. As a

consequence, for this angle, a reflected beam has same properties as a beam which crossed a

polarizer. Its polarization is linear. This angle is called Brewster angle.

We can check this by making the reflected beam go through a polarizer and measure the energy that

crosses the polarizer which only selects P polarization.


Here is a curve giving this energy with respect to the incidence angle of the beam.

We can see the minimum is for the angle value given on the right of the Fresnel curves giving the

Brewster angle. It indicates that the reflected polarization is one hundred percent S for this angle.

Optical Polished Surface

Every reflection and transmission is calculated following the Fresnel Laws.

This surface is often used for polished plastics.

Perfect Mirror Surface

With Perfect Mirror Surface, you can take into account specular reflection and absorption only.

There is no dependency on incidence or wavelength.

Absorption parameter is in percent.

Reflection parameter is in percent. It is a calculated parameter.

Unpolished Surface

The unpolished model is used to simulate any configuration of light arriving on an unpolished surface

(transmission or reflection). This modeling is made independently from the materials on each side of

the surface.


On the following drawing, you can see a configuration that cannot be modeled by a BSDF. Indeed, with

a BSDF model you model a whole film, with its two diopters, whereas, with the unpolished surface

model, you can characterize only the diffusion of a single diopter. This type of model is close to the

BSDF model, but only the normal distribution is kept, and the model adapts to the underlying material

refraction indices using Fresnel formula. Material properties are computed during the simulation

according to the VOP of the OPTIS software used.

This technology can apply to any unpolished surface, for instance surfaces treated by electro-erosion,

wet etching or sandblasting for instance.

Example of an unpolished surface (diffuse surface).

.unpolished files are measured with OMS4. You can get files either:

from measurements made on materials from libraries like VDI or Charmilles.

from specific measurements made on request.

For specific measurements, please contact your OPTIS sales representative (http://www.optis-

world.com/contact.htm).

Typical application for this type of surface state is the modeling of a diffuse surface in a light guide.

Propagation of light in a light guide.

http://www.optis-world.com/contact.htm

http://www.optis-world.com/contact.htm


For additional information concerning this surface model, you can view Simulation.

Simple Scattering Surface Editor

With Simple Scattering Surface Editor, you can simulate the surface's behavior with the classical model

(specular, Lambertian, Gaussian) for both transmitted and reflected rays.

You can modulate the Gaussian angle in respect of the parallel or perpendicular plan.

Using the Simple Scattering Surface Editor

1. From Start menu, click All Programs, OPTIS, OPTIS Labs, Optical Property Editors, Surface

Optical Property Editors, Simple Scattering Surface Editor.

-Or-

1. Click Simple Scattering surface .

A window appears.

You can create, open or save a surface. In this case you can save your surface as a

.simplescattering file.

2. Set the parameters see page 15.

You can view Scattering surface curve see page 41.

You can edit surface properties see page 43.

You can edit preferences see page 47.

Parameters of a Simple Scattering Surface

The surface quality does not depend on incidence angle, polarization... It works according reflection

only, transmission only, or reflection and transmission.

A global absorption is when there is no dependency with the wavelength.

A Lambertian reflection is when there is dependency with the wavelength.

In all cases, when a photon hits a surface with this surface state, the surface absorption and the

percentages of reflection and transmission are first computed according to the photon incidence

and wavelength.

In the case of propagation with photon weight, the absorption is subtracted to the photon energy.

The photon is propagated after the interaction with the surface with the new energy.

In the case of propagation without photon weight, the absorption is the probability for the photon

to be absorbed.

A random number is then computed in order to choose the interaction type (reflection or transmission,

specular, Gaussian or Lambertian, and absorption in the case of propagation without photon weight)

and their respective probabilities.

Calculations take into account incidence following the Snell law.

Absorption

In Absorption box, you must type the value of the absorbed energy in percent.

When you open a Lambertian reflection you can describe a colored surface. In this case Absorption

parameter is not available.

Non Absorption

This Non absorption box gives the non absorbed energy.

Non absorption = P = (100 - Absorption).


P is computed and used as following:

Reflection or transmission only: The percentages of Lambertian, Gaussian or specular reflection (or

transmission) are percentages of P. All other percentages of transmission (or reflection) are set to

0.

Reflection and transmission:

If Use Fresnel is selected, the Fresnel law gives the percentages of reflection (Rf) and

transmission (Tf) according to the photon incidence and wavelength.

If User is selected, you must type the percentage of reflection (Rf) and the transmission (Tf) is

computed as 100-Rf. The global percentages are respectively:

Rt = P * Rf / 100

Tt = P * Tf / 100

Then Lambertian, Gaussian or specular percentages are percentages of Rt and Tt.

Reflection

You can select the Reflection check box.

In Reflection gaussian angle box, you must type the angle value of the gaussian diffusion in

reflected light in degree.

In Lambertian box, you must type the percentage of Lambertian diffusion in reflected light.

In Gaussian box, you must type the percentage of Gaussian diffusion in reflected light.

In Specular box, you must type the percentage of specular reflection in reflected light.

Transmission

You can select the Transmission check box.

In Lambertian box, you must type the percentage of Lambertian diffusion in transmitted light.

In Gaussian box, you must type the percentage of Gaussian diffusion in transmitted light.

In Specular box, you must type the percentage of specular reflection in transmitted light.

In Transmission gaussian angle box, you must type the angle value of Gaussian diffusion in

transmitted light in degree.

Use Fresnel / User

If both Reflection and Transmission check boxes are selected, you can view Use Fresnel and User.

If you select Use Fresnel, the ratio between reflected energy and transmitted energy follows the

optical Fresnel laws. Otherwise reflection and transmission percentages are used.

If you select User, you must type the reflection percentage.

Advanced Scattering Surface Editor

With Advanced Scattering Surface Editor, you can define more complex surface quality which can

depend on incidence angle, polarization...

Two additional effects compared to the Simple Scattering Surface Editor are the dependence of the

diffusion on incidence angle and of the diffusion on spectrum (colored surface).

Transmitted and reflected rays are described with a specular behavior, a Lambertian diffusion and a

Gaussian diffusion. Calculations take into account wavelength and incidence, and you can define up to

eleven parameters to give a precise description of the ray behavior.

This editor is commonly used with measurements.

Using the Advanced Scattering Surface Editor


Optical Property Editors, Advanced Scattering Surface Editor.


-Or-

1. Click Advanced Scattering surface .

A window appears.

You can create, open or save a surface. In this case you can save your surface as a .scattering

file.





You can get some help to generate the surface see page 47.

Parameters of an Advanced Scattering Surface

For each wavelength and each incidence, you have to define ten parameters.

Absorption is a self-calculating value.

You must type a specular reflection value in percent.

You must type a Lambertian diffusion value around reflected ray in percent.

You must type a Gaussian diffusion value around reflected ray in percent.

You must type a Gaussian angle value in the incidence plane in degree.

You must type a Gaussian angle value in the perpendicular plane in degree.

You must type a specular transmitted ray value in percent.

You must type a Lambertian diffusion value around transmitted ray in percent.

You must type a Gaussian diffusion value around transmitted ray in percent.

You must type a Gaussian angle value in the incidence plane in degree.

You must type a Gaussian angle value in the perpendicular plane in degree.

If needed, you can Add incidence or Delete incidence .

If needed, you can Add wavelength or Delete wavelength .

BSDF - BRDF - Anisotropic Surface Viewer

With BSDF - BRDF - Anisotropic Surface viewer, you can display the 3D view of any BSDF, BRDF,

Anisotropic scattering or Anisotropic BSDF surface files.

Using the BSDF - BRDF - Anisotropic Surface Viewer


Optical Property Editors, BSDF - BRDF - Anisotropic Surface Viewer.

-Or-

1. Click BSDF - BRDF - Anisotropic surface .

A window appears.

2. Click File, Open... and select a supported file.

Supported files are Simple BSDF see page 19, Anisotropic BSDF see page 19, Complete scattering

see page 23, BSDF180 see page 25 , unpolished see page 13 and coated see page 27 files.



You can save a surface.

You can save the surface as measure file saving it in a binary compressed format. Be aware that

this can not be undone.

You can build BSDF180 surface see page 25.

You can export to conoscopic map see page 26.



Parameters of Scattering Surface

Display

By selecting the View shading check box, you can display a shading view of the intensity

envelope.

By selecting the View Mesh check box, you can display the intensity envelope with wireframe.

By selecting the Pure Lambertian curve check box, you can display the pure Lambertian curve.

By selecting the Incident direction check box, you can display the incident direction.

By selecting the Tangent plane check box, you can display the tangent plane.

By selecting the Axis System check box, you can display the axis System.

By selecting the Decorations check box, you can display the 3D view tool.

For more details, you can view Using 3D view tool.

By selecting the BRDF check box, you can display the BRDF.

By selecting the Probability density check box, you can display the probability density.

By selecting the Logarithmic View check box, you can display the logarithmic view.

By clicking , you can edit 3D view preferences see page 196.

Incidence

With Incidence group box, you can view the incidence dependency (theta and phi).

Wavelength

With Wavelength group box, you can view the wavelength dependency.


Optical Properties

With Optical properties group box, you can modify optical properties.

Anisotropy Vector

With Anisotropy vector group box, you can modify the anisotropic vector for anisotropic surfaces.

Simple BSDF Surface

From OPTIS Labs 2012 release, it is strongly recommended to use the Anisotropic BSDF Surface see

page 19 model instead of Simple BSDF Surface model.

Anisotropic BSDF Surface

Anisotropic BSDF Surface Overview

You can measure surface properties with OMS² or OMS4 software.

For more information on the use of this model, you can view Parameters of Interpolation Enhancement.

With Anisotropic BSDF Surface, you can simulate both isotropic and anisotropic surfaces from

goniometric measurement data.

The model handles BSDF as well as BRDF only or BTDF only surfaces.

Anisotropic BSDF uses an approximation to deal with the spectrum.

With following diagram you can view angle definitions for incoming and outgoing directions according

to the surface normal (Z) and the fixed anisotropic vector.

The incoming photon is displayed in blue.

Z vector Surface normal

X vector Constructed for a given incoming photon as the projection of its

direction on the surface plane

Y Computed from X and Z

Anisotropic vector Directs the surface when the vector given in the file is not in the tangent

plane at the impact point, an orthogonal projection of it is used instead

Anisotropic angle Phi_i Angle between X and the anisotropic vector using trigonometrical

convention (Phi_i is positive on the diagram)

Theta_i Incidence angle

Output direction

(Theta_o, Phi_o)

Displayed in red and is given using standard spherical coordinates in the

X,Y,Z axis system


Theoretical specular direction is always (Theta_o, Phi_o) = (Theta_i, 0) regardless what the Phi_i angle

is.

Intensity values corresponding to (Theta_o, Phi_o) is BRDF*cos(Theta_o).

Angles ranges:

Theta_i must be in the [0° 90°] interval.

Theta_o must be in the [0° 90°] interval for reflection and in the [90° 180°] interval for

transmission.

Phi_i and Phi_o must be in the [0° 360°] interval.

Structure of Anisotropic BSDF Files

Line 1

It is a header line and it must be:

OPTIS - Anisotropic BSDF surface file v1.0

Line 2

It is a comment line.

Line 3

It contains the anisotropy vector in the global coordinates system.

Line 4

It contains two Boolean values (0=false or 1=true).

The first bReflection tells whether the surface has reflection data or not.

The second bTransmission tells whether the surface has transmission data or not.

Line 5

It contains a Boolean value bIsBSDF describing the type of value stored in the file:

Set to 1, it means the data is proportional to the BSDF.

Set to 0, it means the data is proportional to the measured intensity or to the probability density

function.

Line 6

There is one integer giving the number nIncidence of incidence samples in the file (at least one

sample).

Line 7

It contains the list of nIncidence incidence sample values (not necessarily an equidistant sampling).

Line 8

There is one integer giving the number nAnisotropy of anisotropy angle samples in the file. If only one

sample is present, the surface is isotropic.

Line 9

It contains the list of nAnisotropy anisotropy angle sample values (not necessarily an equidistant

sampling)

Others Lines

From this point to the end, the contents of the file depend on the bReflection and bTransmission

boolean values.

If(bReflection is true)

{


Here comes the reflection spectrum data.

On the first line come two angles Theta and Phi corresponding to the light incident

direction for this measurement. If unsure, use "10 0"

Second line is a comment line

The third line contains the number nWavelengthR of wavelength samples (at leat 2)

Follows nWavelengthR lines each contains 2 values, a wavelength and the reflection

coefficient for this wavelength.

The wavelength samples are not necessarily equidistantly sampled.

} If(bTransmission is true)

{

Here comes the transmission spectrum data.

On the first line come two angles Theta and Phi corresponding to the light incident

direction for this measurement. If unsure, use "0 0"

Second line is a comment line

The third line contains the number nWavelengthT of wavelength samples (at leat 2)

Follows nWavelengthT lines each contains 2 values, a wavelength and the transmission

coefficient for this wavelength.

The wavelength samples are not necessarily equidistantly sampled.

}

The next part of the file contains all the goniometric measurement data. The format will be described

as pseudo code:

If(bReflection is true)

{

for a=1 to nAnisotropy

for i=1 to nIncidence

Put the BRDF(a,i) block in the file

} If(bTransmission is true)

{

for a=1 to nAnisotropy

for i=1 to nIncidence

Put the BTDF(a,i) block in the file

}

BRDF and BTDF blocks share the same structure, only the Theta-o angle range changes (from 0° to

90° for reflection and from 90° to 180° for transmission).

The first line of these blocks contains two integers nTheta and nPhi giving the number of sample for

the Theta-o and Phi-o angles.

The second line contains the list of the nPhi Phi-o angle samples that are not necessarily equidistantly

sampled.

Next following lines are nTheta lines.

The first value on the line is the Theta-o angle sample value (first column) and then the nPhi sampled

goniometric data (BSDF or intensity/probability density function according to the bIsBSDF Boolean

value)

Example

OPTIS - Anisotropic BSDF surface file v1.0

TestFile

0 1 0

1 0

0

1

0

3

0 45 90

10 0

Reflection Spectrum

2

100 50

1000 50

5 4

0 10 350 360


0 0 0 0 0

30 1 0 0 1

45 1 0 0 1

60 1 0 0 1

90 0 0 0 0

5 6

0 15 45 315 345 360

0 0 0 0 0 0 0

30 0 0 0 0 1 0

45 1 0 0 0 0 1

60 0 1 0 0 0 0

90 0 0 0 0 0 0

5 6

0 15 45 315 345 360

0 0 0 0 0 0 0

30 0 0 0 0 0 0

45 1 1 0 0 1 1

60 0 0 0 0 0 0

90 0 0 0 0 0 0

If your anisotropic surface shows a symmetry in its behavior, it is possible to put the data for the [0°

90°] or the [0° 180°] intervals for the Phi_i angle instead of [0° 360°].

For more details, you can view anisotropic BSDF surface examples from

LAB_Anisotropic_BSDF_Surface.zip (../Common/LAB_Anisotropic_BSDF_Surface.zip).

Specular Constant for Anisotropic BSDF

For more information on the use of this model, you can view Parameters of Interpolation Enhancement.

Generally speaking, the directional part of a BRDF is measured with OMS4 and the reflection spectrum

is measured with the integrating sphere. When modeling anisotropic BSDF models, the measure does

not allow to make the difference between the diffuse /lambertian parts and the specular/gaussian

parts. The model applies the color measured with the integrating sphere to the whole BRDF. The result

is that the specular reflection is the same color as the diffuse part, which is often not the case in real

situations. The specular constant model allows to make the difference between the diffuse/lambertian

parts and the specular/gaussian parts for anisotropic BSDF.

As this new model is based on the separation between diffuse and specular data brought by incidence

interpolation, you can only use it on surfaces for which you activate incidence interpolation.

The validity of the model relies on the accuracy of the specular/diffuse separation. Any flaw will result

in calculation errors.

On the following example you can view a sphere with a colored reflection spectrum illumined by a

white source.

Before, the specular highlight had the same spectrum as the diffuse part, both had the same color.

../Common/LAB_Anisotropic_BSDF_Surface.zip


With the new model, the specular highlight is white and the diffuse part remains unchanged.

Complete Scattering Surface (BRDF)


With Complete Scattering Surface (BRDF), you can simulate a BRDF.

This surface is scattering light only in reflection.

Complete Scattering Surface model is new from the OPTIS Labs 2008 release.

Due to file compatibility issues, the file extension is a .bdrf however the file itself reflects a full BSDF

function.

The new model replaces the former one while keeping compatibility by importing the former model

files.

The polarization dependency has been removed.

The Complete Scattering Surface is now able to handle transmission as well as reflection.

Complete scattering is not able to deal with anisotropy.

File Format

The model uses a text format file.

Line 1

It is a header used to discriminate from older file format.

OPTIS - brdf surface file v3.0

Line 2

It is a file description.

Surface description

Line 3

There are two boolean values for reflection and transmission.

1 value is set when there is reflection/transmission.

0 value is set when there is not reflection/transmission.

1 1

Both reflection and transmission example

Line 4

It contains a boolean value.

0 value is set when the data is proportional to intensity.

1 value is set when the data is proportional to BSDF.

Line 5

It contains the number of samples in incidence and in wavelength.

There is a minimum of two incidence samples and two wavelength samples.

2 2


Line 6

It contains the list of the incidence samples in degree.

0 90

Line 7

It contains the list of the wavelength samples in nanometer.

400 700

Others Lines

The next contain is organized as blocks of data.

The blocks organization is described first, then the blocks contents.

Blocks Organization

if the surface has reflection

{

for I=1 to Incidence Sample Number

{

for W=1 to Wavelength Sample Number

{

Write Reflection Block(I,W)

}

}

}

if the surface has transmission

{

for I=1 to Incidence Sample Number

{

for W=1 to Wavelength Sample Number

{

Write Transmission Block(I,W)

}

}

}

It means the reflection comes first if present and the transmission comes after if present according to

the boolean values from line 3.

Block Content

The first line contains the reflection or transmission coefficient in percent.

50

If 50% of the light is reflected/transmitted

The second line contains the number of samples in theta and the number of samples in phi.

Theta is the polar angle (the poles are on the surface normal direction) its origin is on the reflection

pole.

Phi is the azimuth angle, its origin is defined by the specular reflection.

2 3

On the third line, there is the list of the phi samples.

0 180 3 60

Next, there are as many lines as there are theta samples.

The first value on each line is the theta angle sample value.

Then there is one value per phi sample corresponding to the intensity (or the BSDF depending on

boolean from line 4 of the file.)

0 1 1 1

90 1 1 1

For reflection, theta goes from 0° (normal) to 90° (grazing).

For transmission, theta goes from 90°(grazing) to 180°.


The Intensity or BSDF values do not need to be absolute values as the reflection/transmission

coefficient is present at the beginning of each block and is used to normalize the values appropriately.

Anisotropic Scattering Surface

From OPTIS Labs 2012 SP3 release, it is strongly recommended to use the Anisotropic BSDF Surface

see page 19 model instead of Anisotropic Scattering Surface model.

BSDF180 Surface

BSDF180 Overview


Some optical films have asymmetrical optical properties according to which surface the light interacts

with first.

Two distinct measurements are required to characterize such films.

With BSDF180 surface, you can combine both measurements and orient them to simulate the complete

film behavior.

With BSDF - BRDF - Anisotropic Surface viewer, you can display 3D view of BSDF180 file.

When using BSDF180, you can select .anisotropicBSDF or .brdf file format.

Building BSDF180 Surface

1. Click File, Build BSDF180....

A window appears.

2. In Normal BSDF box, you must browse one BSDF file for the normal direction.

3. In Opposite BSDF box, you must browse one BSDF file for the opposite direction.

Normal BSDF Opposite BSDF


4. Click OK.

The new BSDF180 file combines both data.

The normal BSDF is observed for Theta varying between 0° and 90° and the opposite BSDF for

Theta varying between 90° and 180°.

Exporting to Conoscopic Map

In conoscopic map, there is one layer per incidence. The map gives selected incidences' reflection

and/or transmission.

1. Click File, Export to conoscopic map....

A window appears.

In Map sampling box, you must enter a map sampling value in pixels.

In Wavelength of conversion box, you must enter a wavelength of conversion value in

nanometers.

In Anisotropic angle of conversion box, you must enter a Anisotropic angle of conversion value

in degrees.

You must select a reflection or transmission type.

2. Browse a Map file.

This is a .xmp format.

3. Click OK.

Change Reflection or Transmission Spectrum

Changing Reflection or Transmission Spectrum

Change reflection or transmission spectrum is only available for anisotropic BSDF files.

1. Click File, Change reflection or transmission spectrum.

A window appears.


3. Click OK.

4. Save the file.

Parameters to Change Reflection or Transmission Spectrum

Reflection

In Reflection group box, you can select the check box to set the reflection spectrum.


In Theta and Phi boxes, you must then set Theta and Phi values to set the lighting direction used for

the spectrum measurement.

You must then open the corresponding reflection spectrum.

Transmission

In Transmission group box, you can select the check box to set the transmission spectrum.

In Theta and Phi boxes, you must then set Theta and Phi values to set the lighting direction used for

the spectrum measurement.

You must then open the corresponding transmission spectrum.

Coated Surface

Using the Coated Surface Editor


Optical Property Editors, Coated Surface Editor.

-Or-

1. Click Coated surface .

A window appears.

You can create, open or save a surface. In this case you can save your surface as a .coated file.


You can make a TFCalc import see page 48.

You can view Coated surface curve see page 41.



You can auto-calculate value see page 49.

You can set values for polarization see page 49.

Parameters of a Coated Surface

You must fill the table with absorption and transmission coefficients for each wavelength and

polarization.

You can Add incidence or Delete incidence .

You can Add wavelength or Delete wavelength .

Polarizer Surface Editor

With Polarizer Surface, you can model a perfect polarizer.

As OPTIS software is propagating the polarization with their rays, it may be very useful to know about

the polarization of a beam or to create a beam with a linear polarization.

The coordinates of the easy axis of the polarizer in the global axis system are stored in a .polarizer

file. This means that if you rotate the surface on which you apply the polarizer, you have to rotate this

vector the same way. It is required that you keep this vector in the plane of the surface.


Using the Polarizer Surface Editor


Optical Property Editors, Polarizer Surface Editor.

-Or-

2. Click Polarizer Surface .

A window appears.

You can create, open, edit and save a new polarizer surface.

In this case you can save your surface as a .polarizer file. New files are always saved in V2.0

version.

You can open, edit or save an existing .polarizer surface.

V1 versions are saved as V1.0 polarizer files, V 2.0 versions are saved as V2.0 polarizer files.


You can click to convert directly a V1.0 polarizer file into a V2.0 polarizer file.

You can also view Polarizer Surface V1.0 see page 29 and Polarizer Surface V2.0 see page 30 to create

V 1.0 or V 2.0 polarizer files directly in a text file.

Parameters of a Polarizer Surface

Polarizer Surface V1.0

Open a polarizer surface V1.0 to access this parameters.

Description

Define a name for you polarizer surface.

Easy Axis

It is the easy axis vector.

Set the X, Y, Z values.


Open an existing polarizer surface V2.0 or create a new polarizer surface to access this parameters.

Description

Define a name for you polarizer surface.

X Axis

It is the X axis vector defined in the global axis system.


Y Axis

It is the Y axis vector. It has to be perpendicular to the X axis.


The angle between two axes should be at least equal to 45°.

X axis vector and Y axis vector do not need to be normalized. Vector length can be different than 1.

Values are automatically normalized when saving the surface. You can click to preview the

normalized values.

Jones Matrix

It is the Jones Matrix defined in the X and Y base.


In case the Jones Matrix contains complex values, the convention is (a,b) with a the real part and b

the imaginary part.

Polarizer surfaces v2.0 are perfect. There is no loss of energy. Jones matrices are normalized for

calculation.

Jones Matrix Examples

EXAMPLE JONES MATRIX JONES MATRIX IN THE POLARIZER SURFACE V2.0 FILE

Linear polarizer along Ox

1

0

0

0

Linear polarizer along Oy

0

0

0

1

Left circular polarizer

1

(0,1)

(0,-1)

1

Right circular polarizer

1

(0,-1)

(0,1)

1

1/2 is a normalization coefficient avoiding to create energy when the light goes through the

polarizer. As code of the polarizer surface V2.0 file takes into account the normalization, this

coefficient is not required in the Jones Matrix.

Quarter-wave plate with fast axis along

X

1

0

0

(0,1)

Half-wave plate with fast axis along X

1

0

0

-1

No global phase angle difference equal on X and Y is taken into account in theses matrix because

photons' phase is not kept in calculations.


With Polarizer Surface, you can model a perfect polarizer.



The coordinates of the easy axis of the polarizer in the global axis system are stored in a .polarizer

file. This means that if you rotate the surface on which you apply the polarizer, you have to rotate this

vector the same way. It is required that you keep this vector in the plane of the surface.

File Format

Line 1

It is a header line.

OPTIS - Polarizer surface file v1.0

Line 2


My polarizer

Line 3

It is the easy axis vector.

1 0 0



With Polarizer Surface, you can model a perfect polarizer as well as any plate that can be described by

a Jones matrix.



The coordinates of the X and Y axis of the polarizer in the global axis system, and the Jones Matrix

defined in the X and Y base are stored in a .polarizer file. This means that if you rotate the surface on

which you apply the polarizer, you have to rotate these vectors the same way. It is required that you

keep these vectors in the plane of the surface.

File Format

Line 1

It is a header line.

OPTIS - Polarizer surface file v2.0

Line 2


My polarizer

Line 3

It is the X axis vector defined in the global axis system.

-0.7071067 0.4673925 0.5306073

Line 4

It is the Y axis vector. It has to be perpendicular to the X axis.

0.6831709 0.2579829 0.6831709

X axis vector and Y axis vector do not need to be normalized. Vector length can be different than 1.

Line 5 and 6

It is the Jones Matrix defined in the X and Y base.

1 (0,1)

(0,-1) 0

In case the Jones Matrix contains complex values, the convention is (a,b) with a the real part and b

the imaginary part.

Polarizer surface v2.0 are perfect. There is no loss of energy. Jones matrix are normalized for

calculation.

The angle between two axes should be at least equal to 45°.

Retro Reflecting Surface Editor

With Retro Reflecting Surface Editor, you can assume that the ray may be reflected towards the

direction it comes from.

This surface is very useful to simulate reflector such as those installed on back of cars, bicycles...

Indeed some surfaces as cars reflectors reflect a part of the incident light in the direction of the source.

A part of the light is reflected following Descartes' laws and another part is reflected in the direction of

the light. Both reflections are defined by a specular ray for one part and a Gaussian diffusion for the

other part.


Using the Retro Reflecting Surface Editor


Optical Property Editors, Retro Reflecting Surface Editor.

-Or-

1. Click Retroreflecting surface .

A window appears.

You can create, open or save a surface. In this case you can save your surface as a

.retroreflecting file.



Parameters of a Retro Reflecting Surface

Absorption is an auto-calculate value.

Total Reflection plus Absorption is equal to one hundred percent.

Lambertian

In Lambertian box, you must type a Lambertian diffusion value in percent.

Back Scattering

In Specular box, you must type a specular reflection value in the incident direction in percent.

In Gaussian box, you must type a Gaussian diffusion value in the incident direction in percent.

In Gaussian angle (FWHM) box, you must type a Gaussian angle value in the incident direction

in degree.

FWHM angle (Full Width at Half Maximum) is used as following.

Front Scattering

In Specular box, you must type a specular reflection value in the classical reflection direction in

percent.

In Gaussian box, you must type a Gaussian diffusion value in the classical reflection direction in

percent.

In Gaussian angle (FWHM) box, you must type a Gaussian angle value in the classical reflection

direction in degree.

DOE and Thin Lens Surface Editor

With DOE and Thin Lens Surface Editor, you can simulate a diffractive surface.

DOE and Thin Lens Surface Overview

Diffractive Surface

With diffractive surface, you can model thin lens that corresponds to a theoretical lens.

Two possibilities are available: Thin lens or Diffractive optical element (DOE).

Note that diffractive lenses are modeled by choosing the Diffractive optical element mode.

For the diffractive optical element, this surface type models the DOE effect on light.


This model can only figure simple DOEs (not complex holograms for example) like a holographic lens.

The example of a lens with a DOE on one of its face is used industrially in CD reader devices.

With this you can have a simple optical system to make very little focus point.

The advantages are a simple mechanical structure, a low weight and a low price.

The DOEs can be used to focalize on something else than a point: an ellipse for example.

It is possible to replace a parabolic mirror by a plane DOE.

It is possible to replace a complex optical element by a plane DOE with the right function.

Transmission

Basic Fresnel interactions for transmission trough a surface gives the following changes on photons

direction (in the local surface’s base).

Ni Material index

(li,mi,ni

)

Direction vector of the ray

This direction change is modified as follows by a DOE surface:

Where f is the user defined phase function:

lo The base wavelength at which the DOE has been

designed

f The diffractive focal of the DOE (at lo)

r² x² + y²

bi The radial coefficients of the polynomial

P(x,y) The whole polygon (not with only radial

coefficients)


For a reflection

Equations are:

The surface is 100% transmitting or 100% reflecting.

There is no diffused light.

If all coefficients are null, the surface acts as 100% specular simple scattering surface with reflection or

transmission only.

Thins lens

With Thin lens you can focus a collimated beam without modeling a real lens.

DOE applied on a lens.

We can use the DOE surface model on one plane face of a lens as follows:

1. Define a lens (with default parameters for example).

2. Define a box with x=50 y=50 z=10 dimensions and DOE surface defined in the previous EDIT box.

3. Make a Boolean operation: lens-box.


You can also create a source and watch the effect of the surface on light:

Without DOE

With DOE

This test shows that DOE surface model can be applied on lenses with a diffractive optical element on

one of its faces only.

It is possible to test some coefficients because of their simple effect:

We can use l = 532 nm as the base wavelength and f = 10 mm for the diffractive focal.

We can see that a DOE with all its bi and aij coefficients null has no effect on light.

We can now let b1 = -0.5 and see that a collimated beam converges on one point located 10 mm

from the DOE. If b1 = 0.5 the beam diverges.

The aij coefficients are used to break the revolution symmetry:

If b1 = -0.5, we can use a10 and a01 to move the focal point in the I and/or J vectors direction.

If a10=d / f the focal point moves d millimeters away.

The a20 and a02 coefficients let us using different focal lengths on x and y-axes: -0.05 for a 10 mm

length.

Simple Lens

The setup for a simple lens is:

1. Select DOE surface.

2. Set the base wavelength.


3. Set the focal length of the lens.

4. Set all coefficients to zero, except B1 = -0.5.

Using the DOE and Thin Lens Surface Editor


Optical Property Editors, Thin Lens Surface Editor.

-Or-

1. Click DOE and Thin Lens surface .

A window appears.

You can create, open or save a surface. In this case you can save your surface as a .doe file.


Parameters of a DOE and Thin Lens Surface

In Position box, you must type the absolute coordinates of the origin taken into account to

compute the x and y values used in the phase function or the focal length.

In Vector I box, you must type the absolute coordinates of the x axis vector.

In Vector J box, you must type the absolute coordinates of the y axis vector.

You must select Transmission or Reflection check box.

You can select the Thin lens check box.

In Focal length box, you must type the focal length value of the thin lens.

You can select the DOE surface check box.

In Base Wavelength box, you must type the wavelength value for which the DOE has been

optimized (focal distance, aberrations).

In Diffractive focal box, you must type the focal distance value of the DOE (lens definition) at

the base wavelength.

In Radial parameters Bi table, you must type the parameters values which describe the DOE

function. These parameters are dimensionless and give a rotation invariance (see phase

function).

In Polynomial coefficients table, you must type polynomial parameters aij. These parameters

describe the DOE function and are dimensionless.

Note that aij refers to the xiyj term.

Grating Surface Editor

With Grating Surface Editor, you can model the effect of a grating on light.

It is preferably used with an incidence plane orthogonal to the grating lines.

The transmission of the first order of diffraction as well as specular reflection and transmission are

taken into account by the model.

It is possible to vary the direction of the grating lines, to sample in terms of incidence and wavelength

specular reflection and transmission coefficients, absorption as well as light quantity and first order

direction.

Using the Grating Surface Editor


Optical Property Editors, Grating Surface Editor.


-Or-

1. Click Grating surface .

A window appears.

You can create, open or save a surface. In this case you can save your surface as a .grating file.


Parameters of a Grating Surface

Vector

You must set orthogonal direction to grating lines.

The vector defines the orthogonal direction to grating lines. It is absolutely necessary the vector is

located in the surface plane, the latter defined as being the grating.

In simulation it is better that the light incidence plane is orthogonal to grating lines (co-linear to the file

vector). This relates to the standard usage of a grating.

Absorption represents an one hundred percent complement of the total amount of the first order

transmission, specular transmission and specular reflection percentages.

%A = 100% - %Rs -%Ts - %T1

Rs(%)

You must set reflection in specular direction in percent.

Ts(%)

You must set transmission in specular direction in percent.

T01(%)

You must set transmission for order 1 in percent.

A01(°)

You must set angle for order 1 in degree.

Fluorescent Surface Editor

With Fluorescent Surface, you take into account a spectrum for absorption and use another spectrum

for emission.

Using the Fluorescent Surface Editor


Optical Property Editors, Fluorescent Surface Editor.

-Or-

1. Click Fluorescent surface .

A window appears.

You can create, open or save a surface. In this case you can save your surface as a .fluorescent

file.


You can save as measure file.

You can export as RDH file.



Parameters of a Fluorescent Surface

Absorption

In Spectrum box, you can type a description.

You can use the spectrum editor to select .spectrum files. The description is then added in

Spectrum box.

When saving, spectrum data of these files is directly included in the fluorescent surface file so that

.spectrum files are no more used.

For more details, you can view Spectrum Editor see page 49.

In Efficiency box, you must type the efficiency of fluorescence.

Lambertian Fluorescence

In Spectrum box, you can type a description.

You can use the spectrum editor to select .spectrum files. The description is then added in

Spectrum box.

When saving, spectrum data of these files is directly included in the fluorescent surface file so that

.spectrum files are no more used.


In Reflection box, you must type the reflection of fluorescence.

Table

For details, you can view Parameters of an Advanced Scattering Surface see page 17.

Rendering Surface Editor

With Rendering Surface Editor, you can easily define surface quality without knowing about optics as it

is the case for non optical designers.

Using the Rendering Surface Editor


Optical Property Editors, Rendering Surface Editor.

-Or-

1. Click Rendering surface .

A window appears.

You can create, open or save a surface. In this case you can save your surface as a .rdr file.



You can edit Lab/Gloss surface properties see page 46.


Parameters of a Rendering Surface

In the first box, you must type the name of the material.

Then you must set optical parameters for reflection and refraction.

First scheme shows the global behavior of the surface property according to the point of view on a

spherical object.

Second scheme is a simplified viewer of the surface property's BRDF. The incident light is 45°. To be

independent of wavelength, the curve is drawn using global coefficients without considering the color.


Diffuse

In Diffuse box, you must edit the diffuse coefficient value by editing the box, using the arrows or the

blue slider.

This coefficient is the Lambertian diffusion in reflected light.

You must then select a file for the color . For more details, you can view Color Selection see page

38.

Specular

In Specular box, you must edit the specular coefficient value by editing the box, using the arrows or

the blue slider.


38.

Roughness

In Roughness box, you must edit the roughness coefficient value by editing the box, using the arrows

or the blue slider.

This coefficient is the Gaussian diffusion in reflected light.

If it is equal to zero the face is assumed to be specular.

Transparency

In Transparency box, you must edit the transparency coefficient value by editing the box, using the

arrows or the blue slider.

This coefficient is the specular transmission in transmitted light.


38.

Color Selection

In the list of value box, you must select the way to define the color using a color picker (RGB / LCH

definition), the RAL classic system or the RAL design system.

RAL colors are often used in industry as a standard for color references.

RGB / LCH Color

You must select a basic color, a custom color previously defined, a color using the mouse, a color using

the RGB values or a color using the LCH values.

The corresponding spectrum is selected in the OPTIS library in order to get the real color with the

wavelength dependency of the surface absorption.

RAL Classic System

You must select the global index and then the classic color.

RAL Design System

You must select the RAL design color.

The colored circle helps to select the correct hue.

With arrows, you can increase or decrease the hue value.

The center of the colored circle displays the selected color.


The references of the color are displayed in the status bar.

The colors are displayed in an array according to the lightness and the chromaticity.

LCD Surface

With LCD Surface, you can model a shift in wavelength, which is fixed whatever the wavelength of the

incident photon. This means that the incident spectrum has been moved.

LCD Surface is only available from SPEOS Standalone software.

LuCiD is required and has to be installed.

This surface state should be better used on plane surfaces because of the anisotropic vector. It may be

possible to get results on an aspheric surface but this is not very natural for a LCD.

Using the LCD Surface Editor

1. Click LCD surface .

A window appears.

You can create, open or save a surface. In this case you can save your surface as a .lcd file.



Parameters of a LCD Surface

Anisotropic Vector

In Anisotropic vector box, you must type x, y, z values to define a preferred direction on surface.

Intensity distribution is oriented around the normal because of this direction.

When used on a non-plane surface, the anisotropic vector that is actually used for calculation will be

the projection of this vector on a plane tangent to the surface at the photon's point of impact. If the

projection is a point then a vector tangent to the surface will be taken at random.

The anisotropic vector is used for X-axis, the normal in the direction of the photon is used for Z-axis

and Y-axis is then Y=ZX.

Wavelength Shift: Delta

In Wavelength shift: Delta box, you must type a Delta value.

When a photon arrives on a surface with a Lambda wavelength the photon is transferred with a

Lambda plus Delta wavelength.

Absorption

In Absorption box, you must type a value to define LCD surface absorption in percent.

Theta / Phy

In Theta / Phy table, you must type Theta and Phy values.

A polar distribution in /: It is intensity distribution (Watt/sr) and not BRDF distribution (1/sr).

as angle according to the normal.

as angle according to the anisotropic vector.

The values between two sampling points are interpolated in a linear way.

If the value for = 90° is not specified it will be equal to zero.

Symmetry:


If maximal angle is = 90°, distribution will be completed by making a symmetry according to

the plane defined by both the normal and the anisotropic vector, then making a second symmetry

according to a plane orthogonal to this plane, which also contains the normal (consequently the

normal is the symmetry axis of distribution).

If maximal angle is = 180°, distribution will be completed by making a symmetry according to

the plane defined by both the normal and the anisotropic vector.

If maximal angle is < 90° or 180° or 360°, data about this angle will be re-written in an extra

column as = 90° or 180° or 360°. Then symmetry occurs.

You can Add Phi or Remove Phi .

You can Add Theta or Remove Theta .

Rough Mirror Surface Editor

Using the Rough Mirror Surface Editor

1. From the Start menu, click All Programs, OPTIS, OPTIS Labs, Optical Property Editors,

Surface Optical Property Editors, Rough Mirror Surface Editor.

-Or-

1. Click Rough Mirror surface .

A window appears.

You can create, open or save a surface. In this case you can save your surface as a .mirror file.





Parameters of a Rough Mirror Surface

General

Absorption

In Absolute absorption box, you must type an absorption value in percent.

Reflection

In Relative lambertian reflection box, you must type a Lambertian reflection value in percent.

In Relative gaussian reflection box, you must type a gaussian reflection value in percent.

In Gaussian angle (FWHM) box, you must type a gaussian reflection angle value in degree.

FWHM angle (Full Width at Half Maximum) is used as following.

Following relations between the various parameters are taken for granted:

Absolute total reflection + Absolute absorption = 100

Absolute specular reflection + Absolute Lambertian reflection + Absolute Gaussian reflection =

Absolute total reflection

Relative specular reflection + Relative Gaussian reflection + Relative Lambertian reflection = 100


Incidence Dependency

Incidence (deg)

In Incidence (deg) row, you must type incidence values.

Note that the zero value is for normal incidence.

Relative Absorption (%)

In Relative absorption (%g) row, you must type relative absorption values for each incidence.

This value is relative to the Absolute absorption defined in General tab.

You can Add or Delete column.

Wavelength Dependency

Wavelength (nm)

In Wavelength (nm) row, you must type wavelength value in nanometer.

Relative Absorption (%)

In Relative absorption (%) row, you must type relative absorption value for the above illustrated

wavelength.

This value is relative to the Absolute absorption defined in General tab.

You can Add or Delete column.

View

Coated Surface Curve

Coated surface curve is available from Coated Surface Editor see page 27.

Editing Coated Surface Curve

Coated Surface Curve gives the percentage of reflection or transmission in accordance of the

wavelength, incidence and polarization see page 8.

1. Click View, Coated surface curve... .

A window appears.


3. Click OK.

Parameters of Coated Surface Curve

Display

In Display group box, you must select Reflection or Transmission display.

Polarization

In Polarization group box, you must select Parallel, Undefined or Orthogonal polarization.

Scattering Surface Curve

With Scattering surface curve you can preview the surface quality's behavior.


Scattering surface curve is available from Simple Scattering Surface Editor see page 15, Advanced

Scattering Surface Editor see page 16, Retro Reflecting Surface Editor see page 30, Fluorescent

Surface Editor see page 36, LCD Surface Editor see page 39, and Rough Mirror Surface Editor see page

40.

Editing Scattering Surface Curve

1. Click View, Scattering surface curve... .

A window appears.



3. Click Close.

Parameters of Scattering Surface

Display


envelope.


By selecting the Pure Lambertian curve check box, you can display the pure Lambertian curve.

By selecting the Incident direction check box, you can display the incident direction.

By selecting the Tangent plane check box, you can display the tangent plane.

By selecting the Axis System check box, you can display the axis System.



By selecting the BRDF check box, you can display the BRDF.

By selecting the Probability density check box, you can display the probability density.


Incidence

With Incidence group box, you can view the incidence dependency (theta and phi).


Wavelength

With Wavelength group box, you can view the wavelength dependency.

Optical Properties

With Optical properties group box, you can modify optical properties.

Anisotropy Vector

With Anisotropy vector group box, you can modify the anisotropic vector for anisotropic surfaces.

Preferences of Scattering Surface Curve

With Preferences of Scattering Surface Curve, you can parametrize the sampling.

1. Click Preferences .

A window appears.


Tools

Colorimetric Data

Editing Surface Properties

1. Click Tools, Colorimetric Data... .

A window appears.


Parameters of Surface Properties

Gloss (ASTM 2457-03)

With Gloss (ASTM 2457-03), you can get the Lab/Gloss surface from already defined Surfaces

Optical Properties.

For more details, you can view the following references:

Standard Test Method for Specular Gloss of Plastic Films and Solid Plastics

(http://www.techstreet.com/info/astm.html)

Standards and Technical Documents (http://www.techstreet.com/cgi-

bin/detail?product_id=1132551)

Surface Color

With Surface color, you can see colorimetric data at the pixel on which the cursor is located.

CIE Standard refers to the Colorimetry, Second Edition, CIE Publication 15.2-1986.

You can click Spectrum . For more details, you can view Spectrum Editor see page 49.

For details about Chromaticity coordinates tool, you can view Parameters of Chromaticity Coordinates

Tool see page 44.

http://www.techstreet.com/info/astm.html

http://www.techstreet.com/cgi-bin/detail?product_id=1132551



Parameters of Chromaticity Coordinates Tool

With Chromaticity coordinates tool, you can view colorimetric data at the point on which the cursor is

located.

The white curve indicates the color of a black body source in respect of the temperature.

The triangle indicates the domain where your screen displays real color.

With the first list of values, you can choose the units you want in the chromaticity diagram.

The link between xyY and u'v'Y coordinates systems is given by:

u' = 4.x / (-2.x+12.y+3)

v' = 9.y / (-2.x+12.y + 3)

Current Color

On the chromaticity diagram, you can zoom by drawing a rectangle.

You can view the temperature of the color in the status bar.

The temperature is automatically updated when moving the mouse over the map. This temperature

depends of the spectrum.

Ra value is also displayed in the status bar. You must resize the window to see the value. For more

details, you can view Parameters of the Color Rendering Index see page 51.

Reference Color

You can select the Reference color check box to set a reference color and to calculate the DeltaE

between reference color and selected color.

CLS File

By right-clicking on the diagram, you can display contextual menu and choose to display some

information.

By clicking Standard, Select standard..., you can display Colorimetric Standard File (*.cls) box.

By double-clicking on directories, you can select a .cls file.

The definition of a standard is stored in a .cls file. The installation creates some .cls files in

...\OPTIS\Standards\Colorimetry directory.

You can define or add your own standard by adding .cls files into this directory.

You can define the default standard used by Standard, Draw standard. For more details, you can

view Colorimetry see page 195.

CLS File format is the following for a definition with line equations.

Line 1

This is a header line.

OPTIS standard color v1.0

Line 2

This is a comment line as the standard description.

SAE J578 June 27th

Line 3

This line is the definition with line equations.

0

Line 4

This line is the number of areas.

7


Line 5

This line is the name of first area.

Selective Yellow

Line 6

The colorimetric diagram is a limit of the area.

1

Line 7

The line is the number of lines without limits given by the colorimetric diagram.

3

Line 8, 9, 10

The lines are operators a and b.

Operators a and b correspond to the line equation y= ax+b.

Operators < and > give the position of the area regarding the line.

Use = for x = constant, for example = 0.5 0 for x=0.5.

> 0.58 0.14

> -1 0.97

>1.29 -0.1

N Lines

Next lines are for the next area as described from lines 5 to 10.

CLS File format is the following for a definition with list of vertexes.

Line 1



Line 2


MIL-S-22885/101C

Line 3

This line is the definition with with list of vertexes.

1

Line 4


7

Line 5


Red

Line 6


1

Line 7

The line is the number of vertexes.

4

Line 8

The line is the (x,y) of first vertex.

0.665 0.334


Line 9

The line is the (x,y) of second vertex.

0.659 0.335

N Lines

Next lines are for the (x,y) of the next vertex and then lines for the next area as described from lines 5

to 9.

Lab/Gloss Surface Definition

With Lab/Gloss Surface Definition you can configure the Lab/Gloss surface which defines the Surfaces

Optical Properties.

Editing Lab/Gloss Surface Properties

1. Click Tools, Lab/Gloss surface definition....

A window appears.


Parameters of Lab/Gloss Surface Properties

Gloss

Measurement Angle

In Measurement angle box, you must select 20°, 45° or 60° value.

Gloss Value

In Gloss value box, you must type a Gloss value from 0 to 2030 for measurement angle equal to 20°

and a Gloss value from 1 to 1000 for measurement angle equal to 45° or 60°.

If Gloss value is equal to one thousand, it is a perfect mirror.

Lambertian corresponds to a weak Gloss value.

Two very different surfaces may share the same Gloss value. Gloss value sees them as equivalents

even if they are not.

For more details, you can view the following references:

Standard Test Method for Specular Gloss of Plastic Films and Solid Plastics

(http://www.techstreet.com/info/astm.html)

Standards and Technical Documents (http://www.techstreet.com/cgi-

bin/detail?product_id=1132551)

Gloss value is just one characteristic of the surface, it cannot be used alone to define a surface.

Gaussian Angle (FWHM)

In Gaussian angle (FWHM) box, you must type edit the Gaussian angle value by editing the box,

using the arrows or the blue slider.

FWHM means Full Width at Half Maximum.

FWHM angle is used as following.

For a fixed Gloss value, increasing the Gaussian angle increases the quantity of Gaussian reflected

energy. This may lead to a reflection coefficient higher than one hundred percent.

http://www.techstreet.com/info/astm.html




Current Color

In Current color group box, you must type L value.

Maximum value is one hundred.

If L is equal to fifty, it does not mean there will be a 50% Lambertian contribution in the surface.

Details about CIE can be found here (http://www.cie.co.at). Details about Lab color space can be found

here (http://en.wikipedia.org/wiki/Lab_color_space).

When L is equal to one hundred, it is not possible to add further Gloss to surface. The reflection

coefficient would be higher than one hundred percent.

For the same reason, when the Gloss value is one thousand for 45° or 60°, it is not possible to add a

Lambertian contribution using L>0.

It is not possible to generate the surface in case:

The color is outside the screen gamut (the surface state defines its colors in RGB).

The Gloss parameters, the Gaussian angle and the L value generate a reflection coefficient which is

higher than one hundred percent.


Tool see page 44.

Editing the Preferences

1. Click Tools, Preferences... .

A window appears.

2. Set the preferences see page 194.

Autofill

With Autofill, you get some help to generate an Advanced Scattering Surface.

Using Autofill

1. Click Tools, Autofill....

A window appears.


3. Click Apply.

Parameters of Autofill

Spectrum import

Filename

You must click Open to select a spectrum.

You can edit the spectrum see page 49 .

Select


Wavelength Sampling

You can select Use spectrum sampling check box to use the spectrum sampling.

You can select Use current sampling check box to use the sampling from table included in the main

window.

http://www.cie.co.at/

http://en.wikipedia.org/wiki/Lab_color_space


Other Properties

You can select Put other value to 0.0 check box to set all other values to zero.

You can select Define value for other properties check box to define values manually.

You can select Keep other value unchanged check box to do not change values from table included in

the main window.

Fresnel Contribution

The Fresnel contribution box calculates the Fresnel reflection coefficient between the air and the

material.

Material Filename

You must click Open to select a material.

Select

You must select a reflection type.

Polarization

You must select Parallel, Undefined or Orthogonal check box to define the polarization type.

Thick Transparent

You can select Thick transparent check box to take into account secondary and more reflections.

Fill Transmission

You can select Fill transmission check box to fill transmission column.

Multiply Lambertian Reflection by Fresnel Transmission

You can select Multiply lambertian reflection by fresnel transmission check box to not to have

negative absorption values when adding a Fresnel contribution.

The lambertian reflection is multiplied by the Fresnel transmission coefficient.

Standard applications are painting and varnish.

Apply a Value to a Selection of Cells

You can select one column, all columns, one row or all rows.


You can then apply a value to the specific cell(s).

Others Options

TFCalc Import

TFCalc is only working on 32 bits operating system.

With TFCalc import, you can analyze and design multilayer thin film coatings.

A demo version is given with our software.

A TFCalc coating can be applied on a surface.


2. Click File, Import....


Auto-calculate Value Option

Using Auto-calculate Value Option

1. Click Options, Auto-calculate value.


Parameters of Auto-calculate Value Option

You must select Reflection coefficient, Transmission coefficient or Absorption coefficient to

choose the self-calculating coefficient.

Command formula is A + R + T = 100

Polarization

This polarization option is related to the Coated Surface Editor see page 27.

Using Polarization Option

1. Click Options, Polarization.


Parameters of Polarization Option

You must select Force same values for S and P or Allow different values for S and P to force

same value for both polarization or non-polarization.

Spectrum Editor

With Spectrum Editor, you can easily draw the spectrum curve defining particular points.

The editor calculates every point by linear interpolation.

Using the Spectrum Editor

1. From Start menu, click All Programs, OPTIS, OPTIS Labs, Optical Property Editors,

Spectrum Editor.

-Or-

1. Click Spectrum editor .

A window appears.

You can create, open or save a spectrum. In this case you can save your spectrum as a .spectrum

file.


You can right click on the spectrum plot to export spectrum data.

You can import measure file.

You can print or copy the spectrum.

You can view colorimetric data see page 44.

You can view Color Rendering Index see page 50.

You can view Lumen-Watt ratio.

You can generate a spectrum see page 52.



Parameters of a Spectrum

Value (%)

For each wavelength, you must type a value corresponding to the part of this wavelength power in the

total spectrum power.

If needed, you can Add or Delete a wavelength.

You can add a point by double clicking on the graph.

You can add up to 32767 wavelengths.

If you add too many wavelengths, the displayed spectrum will not be complete.

You must keep in mind that the power of the source is not defined here.

Beware when using spectral maps (illuminance, intensity and luminance) with narrow spectrum

sources (laser, LEDs…).

The default detector wavelength sampling is 13 on a broadband spectrum (from 380 nm to 780 nm).

When using narrow spectrum sources, the detector sampling might not be sufficient and might cause

erroneous results.

This under sampling is also possible when using broadband spectrum with particular peaks as an

example the white LED with blue peak.

Be sure to modify the detector sampling (and/or range) in order to attain a sampling equivalent to the

source spectrum sampling.

The determination of the detector sampling and range must be taken carefully in Indirect simulation or

simulation using fluorescence.

This point is also very important when a very precise colorimetric analysis has to be done.

Absorption Coefficient

Absorption coefficient is used in User Material Editor.

If needed, you can Add or Delete a wavelength.

You can add a point by double clicking on the graph.

Spectrum Format

Line 1


OPTIS - Spectrum file v1.0

Line 2

This is a comment line as the dye description.

Line 3

This line is the number N of wavelength.

3

N lines

Each line contains a wavelength and the corresponding spectral value.

330 0

380 0.3

600 1.7

Color Rendering Index

The Color Rendering Index is the effect of a light source on the color appearance of objects in

comparison with their color appearance under a reference illuminant for specified conditions.

Color Rendering Index is a colorimetric difference calculated between a luminous source and the

closest black body when you light different colored samplings.


Color Rendering Index is available from Virtual Photometric Lab see page 196, Virtual Human Vision

Lab see page 69 and Spectrum Editor see page 49.

Editing the Color Rendering Index Value

You must upload spectral data of xmp first.

The General Color Rendering Index is the average of the first eight Special Color Rendering Index.

From OPTIS Labs 2011 SP1, it is possible to display the Special Color Rendering Index for the fifteen

test samples defined by the CIE.

1. If you have Virtual Photometric Lab or Virtual Human Vision Lab, click Tools, Color

Rendering Index (CRI)....

2. If you have Spectrum Editor, click View, Color Rendering Index (CRI)....

3. If you have Surface / Section window, click .

4. View the parameters see page 51.

5. Close the window.

Parameters of the Color Rendering Index

The first column corresponds to the test sample number.

The third column corresponds to the appearance of the test sample illuminated by the D65 illuminant.

The fourth column shows the color of the sample illuminated by the reference illuminant. This color is

used to calculate the General Color Rendering Index and it changes according to the spectral data.

The fifth column shows the color of the sample illuminated by the present spectrum.

The final column gives the color rendering index of the sample.

The colors are displayed as an indicative way.

Color Rendering Index is also called Ra (Roughness Standard).

Some surfaces from manufacturers like Charmille are described using Ra.

The relation between Ra and Charmille number is the following formula:

N° Ch = 20 log (10 * Ra)

With Ra in micrometers.

Examples

Ra = 1 => N° Ch = 20

Ra = 2 => N° Ch = 26

You can view Ra and Chromaticity Difference (DC) values defined by the CIE.

Details about CIE can be found here

(http://www.cie.co.at/index.php/Publications/index.php?i_ca_id=303).

Ra value is followed by the illuminant reference name used to calculate Ra.

Ra value is also displayed in the status bar of the Colorimetric data diagram. For more details, you can

view Parameters of Chromaticity Coordinates Tool see page 44.

Spectrum Generation

Spectrum Generation is available from Spectrum Editor see page 49.

With Spectrum Generation, you can generate a spectrum corresponding to a black body or a Gaussian

spectrum.

http://www.cie.co.at/index.php/Publications/index.php?i_ca_id=303


Generating a Spectrum

1. Click Tools, Spectrum generation... .

2. When the window asks if you want to save the changes, click Yes or No.

A window appears.



Parameters of Spectrum Generation

You must select Blackbody Spectrum or Gaussian Spectrum.

Blackbody Spectrum

In Temperature box, you must type the temperature in Kelvins.

Gaussian Spectrum

In Center Wavelength box, you must type the center wavelength value in nanometers.

In Diameter at 1/e2 box, you must type the diameter value at 1/e2 in nanometers.

In Lambda Min. box, you must type the minimal lambda value in nanometers.

In Lambda Max. box, you must type the maximal lambda value in nanometers.

In Samples box, you must type the number of samples.

User Material Editor

With User Material Editor, you can build complex materials and store them in a library.

These materials take into account the diffusion, index and absorption variation, gradient index and

birefringent properties.

Using the User Material Editor

1. From Start menu, click All Programs, OPTIS, OPTIS Labs, Optical Property Editors, User

Material Editor.

-Or-

1. Click User Material .

A window appears.

You can create, open or save a material. In this case you can save your material as a .material

file.


You can edit material color see page 61.



Parameters of a User Material

General

In Description box, you can type a comment line.

In Material Type box, you must select the material type.

Isotropic

The refractive index is constant in direction but it can vary with the wavelength.

Birefringent

Birefringent material could only be used with optical polished surfaces. Two birefringent materials

cannot be in contact.

For SPEOS Standalone, birefringent materials are only available for BOX, CYLINDER LENS,

POLYHEDRON CSG and BREP (OSB) geometries.

This material has different refractive index associated with different crystallographic direction.

Birefringents materials are defined starting from a 3*3 matrix called dielectric tensor.

There is a reference in which this matrix is diagonal and whose diagonal elements correspond to the

refractive index for different directions of the reference. This reference could be defined in the .geo

file.

In Additional properties box, you must select Uniaxial negative, Uniaxial positive or Biaxial.

In Vector I and Vector J boxes, you must set coordinate values for Vector I and Vector J.

The reference in which the matrix is diagonal is the same one that the global reference.

Dielectric tensor sample

Gradient Index

The refractive index varies as a function of the location in the material.


Refractive index varies as a function of radius as defined by the displayed formula.

n0 is defined by the index variation.

The r distance is measured compared to a reference axis as shown on the diagram. This axis passes by

the origin of the object.

Sample with A=0.499, n0 = 1.564 at 632 nm

Gradient index materials are only available for BOX and CYLINDER CSG geometries.

Gradient Index and Birefringent Examples

These examples are only with SPEOS Standalone and OptisWorks software.

There are 2 additional parameters in the geo script for gradient index and birefringent materials.

MATERIAL_VECTOR_I

MATERIAL_VECTOR_I is only used when the object is made of birefringent or gradient index material.

With MATERIAL_VECTOR_I, you can define the reference axis for a gradient index material.

Vector's coordinates are given in the local referential.

For Birefringent material, you can define the first axis of the referential in which the dielectric tensor is

diagonal. In this case coordinates of the axis are given in the global referential.

MATERIAL_VECTOR_J

MATERIAL_VECTOR_J is only for birefringent material.

With MATERIAL_VECTOR_J, you can define the second axis of the referential in which the dielectric

tensor is diagonal. It has to be orthogonal to MATERIAL_VECTOR_I.

The same material can be applied to several objects and it must have for each object a different

referential.

For birefringent materials, MATERIAL_VECTOR_I and MATERIAL_VECTOR_J are optional in the geo

script.

If they are not defined in the geo script, the default axes defined with the editor and saved within the

material file will be used.

In OptisWorks software, birefringent material is oriented by the part preferences.

Fluorescent

The material includes fluorescent dyes.


The fluorescent material usage is the same as any other material. The only difference is that you can

enter fluorescence specific data as absorption spectrum, re-emission spectrum, quantum efficiency,

measure concentration and user concentration.

In Fluorescent tab, you can Add or Delete pigment.

You can click to edit measured or user concentration.

Measured concentration is the dye concentration when the fluorescent dye has been measured.

User concentration is the concentration defined by the user for simulations.

Concentration unit has to be the same for both concentrations. As a reminder you can type the used

unit in the comment line of the dye.

You can double click on dye to edit pigment properties. For more details, you can view Dye Editor see

page 59.

Metallic

The metallic material correctly interacts with polarized light. Since the polarization is taken into

account, the material's reflectance changes when the incidence angle varies.

When you apply this material to a part, the reflection automatically takes the effects due to

polarization into account.

It is not the energy penetrating the material which is calculated here, but only the reflected energy.

The metallic material type cannot be used to model thin metallic coats.

Index Variation

For Isotropic, Gradient Index or Fluorescent material, you must select the model used to

describe the index variation. This can be by giving index in function of wavelength, using the

SellMeier formula, using the Kettler-Helmholtz formula or index and constringence.

For Birefringent material, you must select the model used to describe the index variation. This

can be constant index, using the SellMeier formula or using the Kettler-Helmotz formula.

Uniaxial positive material is when na=nb < nc, na and nb are ordinary index.

Uniaxial negative material is when na<nb=nc, nb et nc are ordinary index.

Biaxial material is when na # nb # nc.

na, nb,nc are the refractive index for the referential in which the dielectric tensor is diagonal.

You must have na < nb < nc.

For Metallic material, you cannot use a model to describe the index variation in function of

wavelength. You must set the index values directly in the table.

The Index variation is here composed of two parts : the real part and the imaginary part. This is

because, for a metallic material, the index of refraction is a complex number composed of a real

part and of an imaginary part.

The index of refraction corresponds to n-i*k, n being the real part and k the imaginary part.

You can select the Real and Imaginary check boxes in Spectrum to respectively display real and

imaginary parts' spectra.

If needed, you can Add or Delete a column.

Absorption Variation

The concentration parameters are used when the absorption is due to a pigment diluted in a main

material, typically a colored plastic.

Measured Concentration

When you measure the optical absorption of a plastic that has a known pigment concentration also

called Measured concentration, you put this absorption in the material absorption table.


User Concentration

The User concentration is the pigment concentration used for the simulation.

If the user concentration is the same as the measured concentration, then you are simulating using

exactly the plastic you measured.

You have the possibility to do a simulation with a plastic that has a different pigment concentration

without having to create and measure a new piece of plastic. You have to put the new concentration in

the User concentration box. You are now ready to simulate. The software computes the new

absorption from the absorption spectrum, the measure concentration and the user concentration.

If needed, you can Add or Delete a column.

Scattering Properties

You can define the volume scattering (material like fog).

In General group box, you must select scattering variation model.

Unscattering Material

If you select Unscattering material, the material does not include scattering variation.

Give Particles Specifications: Optical Properties of the Medium will be Evaluated using MIE Theory

If you select Give particles specifications: Optical properties of the medium will be evaluated

using MIE theory, the scattering variation is described by a table of diffusion coefficients (mm-1) for

each wavelength (nm) corresponding to the list of particles.

With the scattering variation tab, you can describe the scattering efficiency according to the scattering

angle.

Transmission = exp (- diffusion coefficient * thickness)

This model is used to describe volume scattering material with small particles. With the material editor,

you can define the size, the index and the density of the particles.

Particles tab is available. For more details, you can view Particles see page 59.

Scattering variation and Scattering phase function tabs are automatically computed and updated.

Scattering phase function tab cannot be modified. For more details, you can view Scattering Phase

Function see page 58.

Give Scattering Coefficient and Phase Function of the Medium

If you select Give scattering coefficient and phase function of the medium, the scattering

variation is described by a table of diffusion coefficients (mm-1) for each wavelength (nm) and by a

phase function.

With Scattering variation tab, you can describe the scattering efficiency according to the scattering

angle.

Transmission = exp (- diffusion coefficient * thickness)

You must then select if phase function is defined by giving scattering efficiency according to the

scattering angle, by using Henyey-Greenstein formula or by using a double Henyey-Greenstein

formula.

Henyey-Greenstein

Henyey-Greenstein model simplifies the phase function's definition for the intensity distribution. With

this model, you have to give the anisotropic factor to describe the intensity distribution. This data can

be found in data sheet.

All the difficulty in diffusing material coding is in the appropriate choice of phase function to be as

closer as possible to physical laws.


Jacques and Prahl [S. L. Jacques, C. A. Alter, and S. A. Prahl. Angular dependence of HeNe laser light

scattering by human dermis. Lasers Life Sci., 1:309{333, 1987.] have shown that the following phase

function is very appropriate to simulate human skin.

Theta is the angle between and .

G = 0 G = 0.8

Double Henyey-Greenstein

Double Henyey-Greenstein model is for diffuse material in volume.

The Double Henyey-Greenstein model formula is the following:

F(Theta)= Ratio*f(Theta, Anisotropy factor1)+ (1-Ratio)*f(theta, Anisotropy factor 2)

For details about Scattering phase function tab, you can view Scattering Phase Function see page

58.

Phase Function Changes According to the Wavelength

In case of MIE theory, if you select the Phase function changes according to the wavelength

check box, you first need to add one particle. For more details, you can view Particles see page 59.

In case of Give scattering coefficient and phase function of the medium, if you select the Phase

function changes according to the wavelength check box, you can Add or Delete a

wavelength and/or an angle.

The wavelength list is the same than the one displayed in the Scattering variation tab. If you want to

add a wavelength to the phase table, you can do it from Scattering variation tab.

With Wavelength to display, you can select the wavelength of the table for which the phase

function's display has been made.


Scattering Phase Function

Phase Function Definition

Volumic diffusion is a physical process which occurs when a particle of material absorbs some energy

of an incident electromagnetic wave, in the direction of propagation.

This energy is then redistributed around this particle according to a specific angular function which is

called phase function.

This function has many parameters as the particle's size, wavelength, and the material and particle

indexes.

According of Monte-Carlo propagation, this phase function can be assimilated to a probability for a

photon which is propagated in direction to be diffused in direction.

This function is named .

You can normalize this function with:

The following phase function corresponds to an isotropic diffusion:

Anisotropy Factor

Anisotropy factor is available when Give scattering coefficient and phase function of the

medium: Define phase function using Henyey-Greenstein formula, or Define phase function

using a double Henyey-Greenstein formula is selected.

When the phase function is not isotropic, you must characterize isotropy with g parameter called

Anisotropy factor with following definition:

When g is converging to 1, the diffused electromagnetic energy is very near initial propagation

direction.

On the other side, when g is equal to 0 you get back an isotropic diffusion and when g is negative you

get retro diffusion properties.

Display


envelope.




By selecting the Axis System check box, you can display the axis system.

You can edit 3D view preferences. For more details, you can view 3D View see page 196.



Particles

Particles tab is available when Give particles specifications: Optical properties of the medium

will be evaluated using MIE theory is activated in Scattering properties.

Particles

You can add , delete or edit a particle.

After selecting the material file, the description from General tab is added to the list of existing

particles. Absorption and index of the new particle are read in this file.

The absorption and the index can depend on the wavelength. You can click Edit... to view or edit these

values.

After selecting a material file to define a new particle, the link with the material file of the particle is

lost.

Particle Size Distribution

For each selected particle, you can define the particle size distribution using User defined

distribution or Log normal distribution.

User defined distribution is a table which gives the density of each particle for each radius of

particle.

Log normal distribution is described as following with S as standard deviation and r0 as mean

radius.

Dye Editor

Dye Editor is only available for fluorescent material.

You can create, open or save a pigment. In this case you can save your pigment as a .dye file.

Spectrum

You must select two spectra.

Absorption Spectrum

Each dye has an absorption spectrum.

The concentration ratio is used to scale this absorption spectrum to the appropriate value for the

simulation.

Maxwell's free path length formula is used to demonstrate the validity of this operation:

With:

L the mean free path length

r the particles radius

n the concentration.

Absorption is proportional to the concentration.


When propagating a photon, we compute a random distance according to the dye's absorption.

Then the photon has a probability equal to the quantum efficiency to be re-emitted with a new

wavelength.

This new wavelength is chosen randomly using the dye's emission spectrum.

Finally, we compute a new random direction for the photon.

Note that for the computation the photon's direction generated by florescence does not depend on the

photon's direction which has been absorbed. It is emitted again in an isotrope way, all directions are

equiprobable.

Then we propagate the photon to the next interaction.

Absorption spectrum has to be defined in mm-1.

You can click Spectrum to edit a spectrum or browse an existing spectrum. For more details, you

can view Spectrum Editor see page 49.

Efficiency Spectrum

The efficiency value is spectral. The related spectrum has to be written in percentage.



Excitance Spectrum

Excitance spectrum is obtained by multiplying the absorption spectrum by the efficiency spectrum.



Emission Spectrum



Scattering Properties

For more details, you can view Scattering properties see page 56.

Particle: Refractive Index and Size

Particle: refractive index and size is available when Give particles specifications: Optical

properties of the medium will be evaluated using MIE theory from Scattering properties tab

has been selected.

With Particle: refractive index and size tab, you can select a .material file containing the pigment

refraction index. In this case the material absorption, diffusion and fluorescence parameters are not

taking into account.

Emission Distribution Type

Emission distribution type tab is available when Unscattering material from Scattering

properties tab has not been selected.

You can select the Emission distribution changes according to the wavelength check box to

define an emission function by wavelength.

When no selecting Isotropic emission distribution, you can edit the Emission distribution.

Theta is the angle between the incident photon angle on the pigment and the direction of the photon

emitted by pigment's fluorescence.


Material Color

Editing Material Color

With Material Color, you can display the resulting color if the light comes from a black body (3200°K)

through 1 mm, or the material preview of the material color giving the light source's spectrum and

material thickness.

1. Click Tools, Colorimetric Data... .

A window appears.


Parameters of Material Color

Light Source

In Light Source group box, you can select User Spectrum or Blackbody spectrum.

If selecting User Spectrum, you must browse a spectrum file.

You can click Edit to edit the spectrum file. For more details, you can view Spectrum Editor see page

49.

If selecting Blackbody spectrum, you can change the temperature in Kelvin.

Material Thickness

In Material Thickness group box, you must set the material thickness value in millimeters.


Tool see page 44.

Parameters of Chromaticity Coordinates Tool

With Chromaticity coordinates tool, you can view colorimetric data at the point on which the cursor is

located.

The white curve indicates the color of a black body source in respect of the temperature.

The triangle indicates the domain where your screen displays real color.

With the first list of values, you can choose the units you want in the chromaticity diagram.

The link between xyY and u'v'Y coordinates systems is given by:

u' = 4.x / (-2.x+12.y+3)

v' = 9.y / (-2.x+12.y + 3)

Current Color

On the chromaticity diagram, you can zoom by drawing a rectangle.

You can view the temperature of the color in the status bar.

The temperature is automatically updated when moving the mouse over the map. This temperature

depends of the spectrum.

Ra value is also displayed in the status bar. You must resize the window to see the value. For more

details, you can view Parameters of the Color Rendering Index see page 51.

Reference Color

You can select the Reference color check box to set a reference color and to calculate the DeltaE

between reference color and selected color.


CLS File

By right-clicking on the diagram, you can display contextual menu and choose to display some

information.

By clicking Standard, Select standard..., you can display Colorimetric Standard File (*.cls) box.

By double-clicking on directories, you can select a .cls file.

The definition of a standard is stored in a .cls file. The installation creates some .cls files in

...\OPTIS\Standards\Colorimetry directory.

You can define or add your own standard by adding .cls files into this directory.

You can define the default standard used by Standard, Draw standard. For more details, you can

view Colorimetry see page 195.

CLS File format is the following for a definition with line equations.

Line 1



Line 2


SAE J578 June 27th

Line 3

This line is the definition with line equations.

0

Line 4


7

Line 5


Selective Yellow

Line 6


1

Line 7

The line is the number of lines without limits given by the colorimetric diagram.

3

Line 8, 9, 10

The lines are operators a and b.

Operators a and b correspond to the line equation y= ax+b.

Operators < and > give the position of the area regarding the line.

Use = for x = constant, for example = 0.5 0 for x=0.5.

> 0.58 0.14

> -1 0.97

>1.29 -0.1

N Lines

Next lines are for the next area as described from lines 5 to 10.

CLS File format is the following for a definition with list of vertexes.


Line 1



Line 2


MIL-S-22885/101C

Line 3

This line is the definition with with list of vertexes.

1

Line 4


7

Line 5


Red

Line 6


1

Line 7

The line is the number of vertexes.

4

Line 8

The line is the (x,y) of first vertex.

0.665 0.334

Line 9

The line is the (x,y) of second vertex.

0.659 0.335

N Lines

Next lines are for the (x,y) of the next vertex and then lines for the next area as described from lines 5

to 9.



A window appears.



LABS

Photometric Calc

With Photometric Calc, you can make operations on map.

Using Photometric Calc

1. From Start menu, click All Programs, OPTIS, OPTIS Labs, Labs, Photometric Calc.

-Or-

1. Click Photometric Calc .

A window appears.


3. Click Close.

Parameters of Photometric Calc

Source Files

In Source Files group box, you have to select one or two maps depending on the type of operation.

In Operation box, you must select the operations in the operation list.

MAP ADDITION map1 + map2

MAP SUBTRACTION map1 - map2

VALUE MULTIPLICATION map1 * value

MAP MULTIPLICATION map1 * map2

MAP DIVISION map1 / map2

This operation does not work with spectral maps.

VERTICAL AXIS SYMMETRY This operation makes a vertical axis symmetry on the data of

map1.

HORIZONTAL AXIS SYMMETRY This operation makes an horizontal axis symmetry on the data of

map1.

VERTICAL AXIS MIRROR This operation makes a vertical mirror on the data of map1.

HORIZONTAL AXIS MIRROR This operation makes an horizontal mirror on the data of map1.

ROTATION This operation rotates map1 with an angle.

You must type the angle value in degrees.

MERGE RESULTS This operation makes an addition of map1 and map2 taking into

account number of integrated rays of each one.

It is possible to merge xmp spectral maps which do not have

same wavelength sampling, only in case spectral data are not

saved in the XMP. If the sampling is not the same and spectral

data are saved, you can read a message suggesting to export the

XMP without spectral data.

MAP UNION (COMBINE TWO MAPS IN ONE)

This operation creates a spectral or an extended map with N1+N2

layers.

N1 is the number of layers of map1.

N2 is the number of layers of map2.

SPECTRUM MULTIPLICATION This operation makes the multiplication of a basic or a spectral

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MAP ADDITION map1 + map2

map by a .spectrum file.

SIGNAL TO NOISE RATIO The division is not made source by source but on the complete

map with the possibility to visualize the contribution to the signal

to noise ratio from each source. Signal Noise Ratio = Luminance

map1/Luminance map2.

This operation works with basic, extended and spectral maps.

ABSOLUTE VALUE

Operations are available on all types of maps.

Result

In Result box, you have to select one map for result.

Virtual 3D Photometric Lab

With Virtual 3D Photometric Lab, you can view photometric or radiometric information as reflection,

transmission, absorption or irradiance directly on your 3D model.

Using Virtual 3D Photometric Lab

1. From Start menu, click All Programs, OPTIS, OPTIS Labs, Labs, Virtual 3D Photometric Lab.

-Or-

1. Click Virtual 3D Photometric Lab .

A window appears.

2. Click File, Open ....

-Or

Click .

3. Select a SPEOS 3D map file.

SPEOS 3D map file is a .xm3 format.

You can save a 3D map file. In this case you can save your 3D map as a .xm3 file.

By clicking , you can export a 3D map in a .txt file format. You can then open it with Excel

software and find hot spots.

This .txt file includes x, y, z coordinates of each vertex, value of each layer (Transmission,

Reflection...) and for 3D map including color, the X, Y and Z colorimetric coordinates.

You can click File, Info to get file information as number of nodes, number of cells, generated

photons, emitted photons, absorbed photons, radiometric or photometric power.

You can click to choose color level display.

You can manage display see page 66.

You can do post-processing see page 66.

You can make surface and section analysis see page 67.


By clicking Filtering, XM3 Filtering..., you can set a standard filtering.

It only uses neighbors without any considerations regarding values of these neighbors.

In Pass number box, you must type the number of times the filtering algorithm is called. 0 value

means there is no filtering.


The level of filtering is displayed in the status bar of the viewer. By clicking the filter value in the

status bar, you can open the filtering box.

Managing the Display

Display




By selecting the Mesh limit check box, you can display the mesh limit.

By selecting the Legend check box, you can display the legend.

By selecting the Axis check box, you can display the axis.

By selecting the Clip plane check box, you can display the clip plane.

By selecting the Contour check box, you can display the contour.

You can select the Colored check box to color contour.

You can select the Annotation check box to display value of each contour line.

You can select a value in the both level lists.

Transparent

In Transparent box, you can move the slider to set the transparency.

In Max and Min boxes, you can change the maximal and minimal level of colors on the map.

By clicking Default values, you can save values as default values.

3D Map Post-Processing

Doing 3D Map Post-Processing

With 3D map Post-Processing, you can compute illuminance or luminance directly on a 3D geometry.

You must have opened a 3D map resulting from a direct simulation.

Illuminance post-processing gives same result than standard simulation result except that it can be

displayed in false or true color.

Luminance post-processing gives same result than a 2D XMP map luminance post-processing except

that result is in 3D instead of 2D. This avoids blurred results on curved geometry.

1. Click Post-processing, Irradiance/Illuminance from ray file....

-Or-

1. Click Post-processing, Radiance/Luminance from ray file....

A box appears.


3. Click to launch the post-processing.

A progress bar appears.

An illuminance or luminance 3D map appears.

If you want to select a false or true color display, use the color list.

If you want to change the unit display, use the unit list. Radiometric unit is displayed in W/(m².sr),

and photometric unit in cd/m².

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Parameters of 3D Map Post-Processing

Initial Ray File

In File box, you must click and browse a .ray file.

You can read Ray file size, Radiant flux, Ray file data and Number of rays values.

If needed, you can select the Luminous flux check box to display the luminous flux value in lumens.

Parameter

In Wavelength group box, you can change Wavelength parameters.

In Wmin box, you can type the minimal wavelength value in nanometers.

In Wmax box, you can type the maximal wavelength value in nanometers.

In Nb W box, you can type the number of wavelength.

For luminance post-processing, in Integration angle box you can change the value.

Surface and Section Analysis

Making Surface and Section Analysis

With Surface and Section Analysis tool, you can use the 3D axis to make measurements.

1. Click Tools, Surface...

A box appears and axis appear on your map.


Close the window.

Parameters of Surface and Section Analysis

Units are automatically set depending on the type of map (luminance, illuminance...).

If needed, you can use the mouse to change values.

Shape

You must select a type of shape as Rectangle or Ellipse to define the analysis surface.

Center

In Center group box, you must type values to define the position of the object which is the

intersection of the three axes.

Direction

In Direction group box, you must type values to define the direction of the analysis surface.

The direction is from the blue cube toward the center of the object.

Phi is the available rotation at 360 degrees around the blue axis.

Dimension

In Dimension group box, you must type values to define the dimension of the analysis surface.

Section

You can select User line to enable the analysis section.


Sampling

In Sampling box, you can change the sampling value.

Sampling is the number of point for the measurement.

Maximum / Minimum

You can read maximum and minimum values of the analysis surface.

Average

You can read average value for the shape or section belong to the following formula.

V is the value in one pixel.

W is the weight of V, ratio between the pixel surface in the calculation area and the total surface of the

pixel.

N is the number of measurement points.

Flux

You can read flux value in the shape belong to the following formula.

S is the surface of the calculation area.

Sp is the surface of one pixel.

Sigma

You can read sigma value belong to the following formula.

Contrast

You can read contrast value belong to the following formula.

RMS Contrast

You can read RMS contrast value belong to the following formula.

You can click Threshold... to set maximum and minimum threshold values, and then click OK.

You can select the Automatic update check box to compute data in real time.

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A window appears.


Virtual Human Vision Lab

The human eye has a great dynamic to detect levels of luminance going from 10-6 cd/m² to 108 cd/m².

Unfortunately most of media used to display luminance map obtained using OPTIS software do not

have such a dynamic. As an example, a monitor has a dynamic lower than one hundred.

With Virtual Human Vision Lab, you can reproduce visual appearance of modeled scenes on this media.

Virtual Human Vision Lab restores contrasts perceived by an observer placed in the scene.

All luminance map fields having luminance lower than the detection threshold of the human eye are

not displayed.

This threshold depends on the luminance to which the eye is adapted. It takes into account properties

of the various eye photoreceptors.

Those can be classified in two families:

The first one is called cone and intervenes in the process of colors perception.

The second called rod is much more sensitive and with it you can perceive luminance lower than

0.001 cd/m² for which cone sensitivity is insignificant.

Under this condition, this is the case of a scotopic vision for which you do not have colors

perception.

When luminance becomes higher than approximately 5 cd/m², the rods are subjected to a

phenomenon of saturation. This vision only results in the cones and is called the photopic vision.

When the luminance of adaptation is between 0.005 cd/m² and 5 cd/m², cones and rods intervene

in the vision process. One is then in mesopic vision.

In order to restore the perception of contrasts as well as possible, Virtual Human Vision Lab takes into

account the luminance of the used screen to display the luminance map.

White Point Luminance value has to be the maximum luminance of a white zone displayed by the

used screen. For more details, you can view Monitor see page 194.

Using Virtual Human Vision Lab

1. From Start menu, click All Programs, OPTIS, OPTIS Labs, Labs, Virtual Human Vision Lab.

-Or-

1. Click Virtual Human Vision Lab .

A window appears.


-Or-

Click .

3. Browse a .xmp file.


You can save the xmp file. In this case you can save your xmp map as a .xmp file.

You can print the xmp map file.

You can import see page 70 or export see page 70 a file.

You can display results, manage display options see page 74.

By clicking View, Map information, you can read map properties. For more details about

precision, you can view Reading Precision see page 76.

You can analyze colorimetric data see page 76.

You can do color management see page 77.

You can use Look at see page 79.

You can set vision parameters see page 81.

You can use the glare effect see page 86.

By clicking Tools, Time adaptation ..., you can do time adaptation see page 87.

You can do analysis see page 87.

You can use legibility/visibility tools see page 89.

You can use sun glasses / colored filter see page 92.

You can use night vision goggles see page 94.


You can use the virtual lighting controller see page 98.


Importing an Image

1. Click File, Import ....

A window appears.

2. Browse an image.

The imported image is Technoteam color image file with .cos format.

Files data have to be in the XYZ format.

3. Click Open .

Exporting

Exporting an Image

You must open an image first.

1. Click File, Export ....

A window appears.

2. Type a file name and select a format.

The image can have one of the following formats.

FILES EXTENSIONS

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FILES EXTENSIONS

XMP map .xmp

Bitmap .bmp

JPeg .jpg

PNG .png

Tiff .tiff

OpenEXR .exr

RGBE .hdr

For more details about .hdr files, you can view HDRI File Format see page 71.

OpenEXR and RGBE are only enable in case of spectral maps.

3. Click Save .

4. In case of a .xmp file export, a box appears. Set the parameters see page 74 and click OK.

HDRI File Format

High Dynamic Range Image (HDRI) is a generic name for an image format which improve the classical

bitmap representation.

Classical bitmaps are coding RGB colors using three 8bits or 16bits integer values (.bmp, .jpg, .tiff...).

The dynamic range of the picture is much more limited than what the eye is able to see in the real

world.

HDRI enables to overcome this problem by using a much wider dynamic range.

Moreover, the color quantization steps are smaller with HDRI. This provides a better colorimetric

accuracy especially when using a wide gamut.

When exporting or importing HDRI for bitmap emission with a better dynamic range, you can not only

simulate displays but also real background illumination.

Today, HDRI are supported by most rendering programs to export the rendering results but also to

import environment map. Environment maps enable to achieve very realistic illuminations. OPTIS

software are able to use environment maps (cube or sphere HDRI maps) to achieve comparable result

and even better result thanks to its physics based calculation.

You can generate good environment HDRI maps using digital cameras and a software tool like

HDRShop.

Supported Formats

RGBE and OpenEXR are supported formats.

RGBE is the native Radiance format. This is the most wide used format today.

ILM 's OpenEXR is the most powerful format to date.

XMPs are even better than HDRI, including spectral data, source separation...

When exporting XMP to HDRI your are able to address the full dynamic provided by HDRI which is not

possible when exporting a BMP to HDRI with a classical rendering software.

XMP export to HDRI: 16 bits to 16 bits

BMP export to HDRI: 8 bits to 16 bits


HDRI/Classical Bitmap Comparison

Here is a picture having levels divided by two at each step from the left to the right.

Only the left most columns are visible, the other are too dark to be seen. To see the rest of the picture,

one has to saturate the visible part by changing the exposure.

Let us compare what happen if the picture is HDRI (on the right) and if the picture is a classical bitmap

(on the left).

When the exposition increases only slightly, no difference is noticeable

Both formats still look the same

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The classical bitmap starts to show its limits

The difference is clear now

The HDRI is able to display the entire picture

As the classical bitmap only has 256 grey levels, all levels inferior to the darker possible grey level are

coded black. This is why they are unrecoverable.

XMP Emission

Now if we compare XMP emission, the XMP is seen through a transparent sphere.

The same simulation was achieved using a HDRI import generated XMP (left column) and a classical

bitmap import generated XMP (right column).

The Virtual Photometric Lab level indicates the light level that is displayed saturated.


Virtual Photometric Lab level = 2 500 cd/m²


Parameters of XMP Export

The xmp Export is like a Save As except that the export includes options.

These options help to reduce the file's size on the disk.

If you do not need to analyze the spectrum on each pixel of the map and if you do not need to

analyze the data for each wavelength, you can select Include spectral data check box.

If you want to group some sources data of the map, you can select Merge active layer(s) check

box.

If you want to have filtered or original data in the exported file, you can select Export filtered

data check box.

If you want to export a spectral map to convert it into an extended map, you can select

Conversion to extended map check box.

You can select Intensity normalized as luminance check box and set a value for the Surface

box in square millimeters.


All display's options as filtering level, Surface/Section parameters or layers' configurations are saved

within the Virtual Human Vision map when saving the file.

If you want to move the map, left-click and move the mouse at the same time.

If you want to use the zoom, rotate the IntelliMouse wheel, click Edit, Activate Zoom or click

and then left-click or right-click.

Click to display the original size.

When moving the mouse over the map, values at the position are displayed in the status bar.

The displayed value is interpolated with the value of many pixels. By clicking View, Interpolate

values, you can activate or deactivate the interpolation.

If you want to view spectrum curve at the mouse position, click .

Status bar provides Angle, Depth, Luminance or Relative brightness, Vision Mode, Filter

values.

Angle is the angle between fixation point and the map field pointed by mouse.

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Depth is the distance between the observer and the 3D scenery's point pointed by mouse.

Vision Mode can be Photopic, Mesopic or Scotopic. It is estimated to starting from the values of

the displayed luminance map.

Images below show the results when one changes the level of luminance of a simulation of a set of

colored translucent plastics.

With Virtual Photometric Lab

Maximum luminance of the map: 0.7 cd/m²

With Virtual Human Vision Lab, mesopic

vision


Following images were obtained with Photometric Calc by multiplying luminance value of the initial

map.

In case of scotopic vision, there is a very poor colors perception because cone sensitivity is

insignificant. Cones are responsible of color perception.

In case of mesopic vision, as the map luminance increases, one starts to perceive some colors:

first red color, then orange, green and last blue.

With Virtual Human Vision Lab, mesopic

vision


With Virtual Human Vision Lab, scotopic vision


If you want to modify the number format, right-click on the status bar.

The number format is the number of decimal per value.

If you want to switch between luminance unit and relative brightness, click View, Relative

brightness.

Brightness is a subjective attribute of light to which humans assign a label between very dim and

very bright.

Brightness is perceived but not measured.

The sensitivity of the eye to luminance is non-linear and complex that's why brightness notion is

used.


The most brilliant point of the map has a relative brightness of 100.

If you want to modify the axis unit of displayed values, right-click on the status bar.

If you want to display grids and other options, right-click on the map to select tools.

As an example you can show ruler, set ruler parameters, show axis on cross, snap cross to grid,

show tooltip, show gray around the map, fill shape, show primary or secondary graduations, set

graduations parameters, show primary or secondary grids, set grid parameters.

Reading Precision

Precision Value

In direct simulation, the displayed precision value corresponds to the pixel having the highest number

of integrated rays.

Precision formula is the following.

Precision = 1/sqrt(N)

With N the number of rays integrated by the pixel.

When no rays are integrated on a pixel, the error is infinite. The precision value is one hundred

percent.

In direct simulation using radiance luminance sensor with activated gathering, precision does not have

any meaning. Precision value is also one hundred percent.

In inverse simulation using the Monte-Carlo algorithm, a number of pass has to be specified as 100

passes = 100 rays per pixel (not necessary effective rays).



With N the number of passes.

In inverse simulation using determinist or photon map algorithms, precision does not have any

meaning. Precision value is also one hundred percent.

Higher is the precision percent, lower is the image quality.

Be aware that one pixel which has not received any rays or which has received only one has a one

hundred percent precision.

More rays or passes there are, lower is the statistical noise. A direct correlation between this number

and the error (or variance, standard deviation) is not possible.

For systems under weighted Monte-Carlo algorithms, the only way to compute error (variance) is to

launch the same simulation several times and to calculate the standard deviation of specific pixels.

The statistical error is always less important for pixels with more integrated rays.

Precision Map

For direct simulation, you can click Tools, Precision map... to display the precision map.

The precision map is only validate for all sources set at one hundred percent when there is no any

separation by sources.

The precision is displayed in percent and is saved in rays number in the map. You can then generate

precision calculation with the surface / section analysis tool.

Analyzing Colorimetric Data

Three tools are available to analyze colorimetric data.

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If you want to see colorimetric data at a specific pixel location, you can click Tools, Colorimetric

data... or .

For more details, you can view Parameters of Chromaticity Coordinates Tool see page 44.

If you want to analyze the error between the color displayed by the screen and the reality for all

points of the map, you can click Tools, Colorimetric error....

The true color luminance map is replaced by a colorimetric error map displayed in false color.

When the dynamic of the luminance map is higher than the one of the screen, the Lab compresses

the luminance using a linear relation.

With colorimetric error tool, you can analyze the error between the color after compression and the

color really displayed by the screen.

The colorimetric error is calculated using the CIE94 (1 :1 :1) formula (CIE 116-1995).

When the dynamic of the luminance map is lower than the one of the display, there is no

luminance compression. In this case the displayed error is the one between the color contained in

the luminance map and the one really displayed.

If you want to have all information about the spectrum for all points of the map, you can click

Tools, Spectrum... or .


If you want to read the color rendering index values, you can click Tools, Color Rendering Index

(CRI) ....

For more details, you can view Parameters of the Color Rendering Index see page 51.

Doing Color Management

A number of color are physically not reproducible by a display.

We say that colors are outside of the gamut of the display.

The color management is to ensure a good correspondence of color appearance between the luminance

map and the display.

The Image Color Management, also called ICM, is a standard color management method available

in Windows.

The Color space conversion is an OPTIS specific color management method.

ICM Profiles

By clicking Tools, Color Management, ICM profiles ..., you can display the Color Management

window.

You must select the Enable Color Management check box, and select Basic color management or

Proofing.

In Rendering Intent box, you can select one of the four standard methods for the color conversion of

the XMP image.

When saving the XMP image to a JPeg file, if the ICM color management is enabled, the ICM profile is

saved in the JPeg file.

Details about the ICM can be found here (http://www.color.org).

Color Space Conversion

By clicking Tools, Color Management, Color Space conversion, you can select how to assign colors

from the reproduction medium to colors from the luminance map.

When selecting Gamut clipping, colors outside of the gamut of the display are clipped along lines

towards the center of the lightness axis.

http://www.color.org/


Gamut clipping

Maintain lightness and hue and Maintain hue methods intend to map perceptual attributes separately.

When selecting Maintain lightness and hue, it keeps the lightness and hue of color outside of the

monitor gamut and changes the chromaticity until the color can be displayed by the display.

Maintain lightness and hue

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When selecting Maintain hue, it keeps the hue of color outside of the monitor gamut and changes the

chromaticity until the color can be displayed.

Maintain hue

Look At

Using Look At

With Look at, you can display vision area on the luminance map.

1. Click Tools, Look at.

-Or-

1. Click .

Areas see page 80 are displayed.


Areas of Look At

Fovea

The fovea is at the center of the area. It is the central part of the retina known as the macula by

ophthalmologists.

Fovea area has a very high concentration of cones also called photoreceptors, and thus the maximum

acuity.

With these cones, you can appreciate color.

For photopic vision mode, it is the most sensitive area to light.

This very small area is responsible for our central, sharpest vision. It is used for reading, driving, and

other activities that require the ability to see details.

Attention Field

The attention field corresponds to the parafovea area.

It is the zone in which some pre-processing of visual inputs, like reading, occurs.

Motion Detection

The rest of the visual field is called peripheral.

This area is less sensitive to light and it is weak especially at distinguish color and shape.

But with an important part of this area, you can detect motion and see though less clearly, objects off

to the side or above or below straight-ahead vision.

Blind Spot

The human eye has a blind spot in its field of vision. It is located where the optic nerve meets the eye.

The retina has no photoreceptors at this point, and so a small object in the field of vision's blind spot

becomes invisible.

This blind spot is symbolized by a dark circle in the Lab.

All these areas are given for a mean young observer.

They are given in an informative way, because measurement of these areas has shown a significant

modification in function of tested people.

Moreover, numbers of reports have shown a change in the size of the visual field in function of age.

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Vision Parameters

Using Vision Parameters

With Vision Parameters, you can change the map point fixed by the observer or the physical

characteristics of the eye.

1. Click Tools, Vision parameters ....

-Or-

1. Click .

A window appears.


3. Click OK.


4. Click Close.

Parameters of Vision Parameters

Modelisation Parameters

In Modelisation parameters group box, you can select physical phenomena that can be taken into

account in the luminance map display.

By selecting the Depth of field check box, you can simulate the depth of field.

This model takes into account physical properties of the eye, like focal length and pupil diameter,

and accommodation distance.

Accommodation distance corresponds to the distance between the observer and the object that the

observer is looking at.

Following images are a scene made up of two tests of vision separated by a distance from two

meters. The observer is placed at one meter of the nearest test.


Accommodation distance = 10 m Accommodation distance = 5 m

Accommodation distance = 3 m Accommodation distance = 1 m

The pupil size is given in an automatic way, starting from the average luminance of the luminance

map. This can be modified.

For post-processing, the diameter of the pupil is three millimeters.

By selecting the Visual acuity check box, you can model the acuity according to the level of

luminance.

Visual acuity diminishes when the luminance decreases.

Visual acuity is computed according to the level of light for each fovea area.

For more details about fovea, you can view Areas of Look At see page 80.

Dark area are displayed with a worst resolution than bright area to reflect the loss of acuity of the

fovea area when luminance decreases.

With visual acuity Without visual acuity

Visual acuity depends directly on the average level of luminance of the simulated scene. Indeed,

cones density and distribution on the retina are not similar to rods one.

Thus, there is a significant modification of visual acuity when one passes from the photopic

conditions of observation in the mesopic conditions.

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Average luminance of the map = 20 cd/m² Average luminance of the map = 0.05

cd/m²

In order that this filtering has perceptible effects, it is necessary to have a luminance map with

significant angular resolutions (relationship between the number of pixel and the angle of view).

By selecting the Peripheral acuity check box, the loss of the eye space resolution according to

the image's position on the retina is taking into account.

In this case, fovea acuity is only computed for the vision center.

The distribution of the cones on the retina decreases from the center of the retina towards the

periphery.

It results in a variation of the visual acuity according to the position on the retina.

The following images show results obtained when one takes into account the distribution and the

density of the cones on the retina.

The luminance maps used are the same than in the Depth of field example.

For left and middle images, the central point of vision is the center of the luminance map. This can

be modified and it is possible to indicate any points of the map as being the new fixation point.

On the right image, the fixation point corresponds to the letter T.

In following images, you can see the fixation point displacement.

Note that the luminosity of the images is high to better visualize the effects of acuity loss.

The maximum map luminance is of approximately 1.e-3 cd/m².


By selecting the Glare effect check box, you can activate the glare effect.

For more details about the glare effect, you can view Glare Effect Overview see page 86.

You must select Vos, 1984 or Holladay, 1926.

Vos,1984 is partly based on Vos, J. Disability glare - a state of the art report. C.I.E. Journal 3, 2

(1984), 39-53.

Vos,1984 takes into account the light scattering into the cornea, the lens and the retina of the eye

responsible for the veil of luminance.

It also simulates the lenticular halo and the ciliary corona essentially caused by the lens.

Holladay,1926 is partly based on the work described in Holladay,Journal of the Optical Society of

America, 12, 271 (1926) and P. Moon, D. Spencer, The Visual Effect of Non-Uniform Surrounds,

Journal of the Optical Society of America, vol. 35, No. 3, pp. 233-248 (1945).

Holladay,1926 takes only into account scattering into the cornea, the lens and the retina.

Without glare effect Vos,1984 Holladay,1926

Eye Adaptation

In Adaptation type box, you can select Local adaptation or Dynamic adaptation.

With Local adaptation, the accommodation is on a fixed point of the luminance map.

You can change the luminance value of this point in Cd/m². When you open a luminance map, this

value is equal to the average luminance of the map.

You can click Default to restore this value.

With Dynamic adaptation, you can model spatial adaptation of the human eye.

This model is equivalent to the fact that the eye adapts locally as the viewer scan the different regions

of the luminance map.

Dynamic adaptation method can be significantly more expensive than local adaptation techniques.

When selecting Dynamic adaptation, you can modify the condition of observation of the scene.

You can click Default to restore initial values.

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Condition of Observation of the Scene

In Condition of observation of the scene group box, you can take into account the fact that it takes

some times for the observer to adapt to the average luminance of the current luminance map when the

observer is adapted to a luminance L0.

In Previous adaptation luminance box, you can change the luminance L0 value in Cd/m² at which

the observer is adapted before seeing the current luminance map.

In Observation time box, you can change the time value in seconds during which the observer sees

the current luminance map.

In Age of the observer box, you can change the age of the observer in years which is taking into

account to evaluate contrast sensitivity, glare and time adaptation.

You can click Default to restore initial values.

The default Previous adaptation luminance value is the mean luminance of the map and the default

Observation time value is a very long time equal to three thousands seconds.

Here the observer is fully adapted to the current luminance map.

Vision Mode Evaluation is Based on

In Vision mode evaluation is based on group box, you can define how the vision mode photopic,

mesopic, or scotopic is estimated.

Vision mode defines the photoreceptors sensitivity. As an example for photopic vision, rods are fully

saturated.

By selecting Average value of the xmp, vision mode is computed using the mean luminance value of

the map.

The rods saturation state is supposed to be the same for all the point of the luminance map.

By selecting Maximum value of the xmp, vision mode is computed using the maximum luminance

value of the map.

The rods saturation state is supposed to be the same for all the point of the luminance map.

By selecting Each point of the xmp, vision mode is computed using the mean luminance value of the

map and the result displayed in the status bar.

But in each point of the luminance map, rod saturation state is computed using the luminance value of

the pixel.

Eye Parameters

In the Eye parameters group box, you can click to clear the Automatic evaluation check box.

In the Aperture box, you can type the pupil diameter value in millimeters.

In the Focal length box, you can type the value of the equivalent focal distance from the eye in

millimeters.

By selecting the Automatic evaluation check box, it automatically calculates eye parameters.

The pupil diameter is estimated from the displayed map luminance and a focal distance is defined from

an average eye.

Vision Center

In Vision center group box, you can define the point of the map fixed by the observer.

In Point at box, the value refers to the fixed point compared to the center of the luminance map.

In Accommodation distance box, you can enter accommodation distance value in millimeters.

You can click to select a pixel in the map. It updates the accommodation distance value.


Glare Effect

Glare Effect Overview

Glare is the contrast lowering effect of stray light in a visual scene.

Glare forms a veil of luminance which reduces the contrast and thus the visibility of a target is

decreased.

Glare effect is due to the fact that light sources located in periphery of the visual field are diffused by

various diopters constituting the human eye, like by the aqueous humor, which results in darkening the

central zone of vision, the fovea.

Without glare effect

With glare effect

Using the Glare Effect

1. Click Tools, Glare effect.

-Or-

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1. Click .

-Or-

1. From the Vision parameters window, select the Glare Effect check box .

For more details about Vision parameters window, you can view Using Vision Parameters see

page 81.

Doing Time Adaptation

With Time adaptation, you can generate an AVI file which includes successive images seen by a human

adapted to a specified luminance level L0 and seeing the current luminance map.

If the difference between the luminance L0 and the mean luminance of the map is very high, it takes

some time for the observer to adapt to the new luminance.

The AVI file shows the image variation perceived by the observer during this time.

Previous Adaptation Luminance

In Previous adaptation luminance box, you must type the luminance value of the time adaptation

area with L0 luminance in Cd/m².

Filename

In Filename box, you must browse the path and type the name of the AVI file.

If needed, you can select the Flip vertically check box.

Adaptation

You must click Adaptation to generate the AVI file.

If the observer is adapted at a very high luminance and observes a luminance map with a very low

mean luminance, the time adaptation is called dark adaptation and the adaptation can take until

thirty minutes. That’s why the time of the AVI file is compressed , the real time is displayed in the

left top of the AVI.

If the observer is adapted to a very low luminance and observe a luminance map with a very high

luminance the time adaptation is called light adaptation and takes few seconds.

The first image of the AVI file shows the previous luminance adaptation state and the mean

luminance value of the current luminance map.

The AVI stops when the observer is totally adapted to the luminance map.

Time adaptation only uses the dynamic adaptation mode.

Doing Analysis

The human eye has a high range of luminance detection. It is able to detect luminance level from 10-6

cd/m² to 108 cd/m².

Displays do not have such a high dynamic.


The Virtual Human Vision Lab includes specific functions able to display the final image as if the scene

is seen by a human. The luminance map compression is required.

With Analysis tools, you can have information on the luminance distribution of the map, and on the

level of compression.

Click Tools, Analysis... to display the Analysis tools window.

Analysis tools depends on the eye adaptation.

For more details about eye adaptation, you can view Parameters of Vision Parameters see page 81.

The fovea luminance histogram shows the distribution of luminance for the current XMP file.

For more details about fovea, you can view Areas of Look At see page 80.

The fovea luminance is computed into a solid angle of about 1°, so the luminance map is

subdivided into solid angle of 1°.

The histogram shows for each luminance value, the number of fovea area of the map having this

luminance.

The Display luminance according to scene luminance diagram shows the relationship between the

map luminance and the display luminance.

If it is a dynamic adaptation, the diagram depends on the fovea luminance histogram.

Here the compression of the luminance map is made to take into account human vision properties,

and to allocate the maximum of display dynamic for luminance area with a high number of areas.

For luminance value for which histogram contains a lot of values, the curve slope of the diagram is

very high.

Dynamic adaptation

If it is a local adaptation, the diagram only depends on the adaptation luminance.

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For more details about adaptation luminance, you can view Parameters of Vision Parameters see

page 81.

Local adaptation

Legibility and Visibility Analysis

Using Legibility and Visibility Tools

1. Click Tools, Legibility/Visibility tools ....

A window appears.



Parameters of Legibility and Visibility Tools

Legibility and Visibility Tools give additional information regarding results.

Legibility (CIE 145:2002 standard)

Legibility (CIE 145:2002 standard) tab gives the relative visual performance of an observer according

to different parameters.

With Legibility (CIE 145:2002 standard) tab, you can indicate if a letter selected in a luminance map

can be read.


Legibility (CIE 145:2002 standard) tab applies the CIE 145: 2002 The correlation of models for vision

and visual performance standard.

Letter Luminance

In Letter luminance box, you can type the luminance value of the letter in cd/m².

If needed, you can click to select a pixel in the map.

If needed, you can click to clear the previous selection.

Background Luminance

In Background luminance box, you can type the luminance value of the background in Cd/m².



If needed, you can click to display colorimetric coordinates when using .

Current color is related to the letter coordinates described by a black cross on the diagram.

Reference color is related to the background coordinates described by a red cross on the diagram.

DeltaE indicates colorimetric gap between letter and background. DeltaE value should be higher than

100 to get good legibility.

Colorimetric gap between target and background is low message appears when the DeltaE value

is inferior to one hundred value using the DeltaE Luv formula.

This value is defined to have a good readability of the letter using the MILSTD1472F norm, 5.2.1.5.6.4

paragraph.

For more details about colorimetric data, you can view Parameters of Chromaticity Coordinates Tool

see page 44.

If needed, you can select the Automatic update check box to update luminance each time the

luminance map is modified.

Size of the Critical Detail

In Size of the critical detail box, you can set the size of the letter by typing the angle subtended by

the critical detail of the letter in minutes of arc.

As an example, critical detail of the letter can be the stroke widths.

The CIE regulation recommends measuring the letter height or stroke width.

Size is calculated using the observer position and the map size.

If needed, you can click to evaluate the size of the critical detail.

A line is displayed in the luminance map to adjust the extreme points.

Observer Age

In Observer age box, you can type the age of the observer in years.

Contrast

In Contrast box, you can read the contrast value calculated from the formula recommended by the

CIE 145:2002 regulation.

Contrast = (Luminance of the background- Luminance of the letter)/ Luminance of the background

Relative Visual Performance

In Relative visual performance box, you can read the relative visual performance value.

Relative visual performance is also called RVP.

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Relative visual performance is measured using the size of the critical detail and the observer age.

The value is between 0 and 1.

RVP = 1 is normalized to the performance level of an adult of twenty years old reading critical detail

sizes of 4.5 minutes of arc with an average luminance of 1000 cd/m².

The relative visual performance is defined as a proportional measure of visual performance potential

expressed in terms of the maximum value achievable.

Curve Options

In Curve options group box, you can select the option to display the Relative visual performance

diagram according to the observer age, the background luminance, the letter luminance, the letter size

or the contrast.

When selecting Contrast, you can select Background luminance is constant or Letter luminance

is constant.

Surface Tool

In Surface tool box, you can click to select a letter using a displayed rectangle in the luminance

map.

You must click or to select if your text is in positive or negative contrast.

If needed, you can click Update to computed letter luminance, background luminance and letter size.

You can select the Automatic update check box to computed data in real time.

Visibility

With Visibility tab, you can evaluate the visibility of an object having an angular size superior to 4

degrees.

The object can be as an example a reflection into a windshield.

This evaluation is partly based on the work done by Blackwell. References are Blackwell, H.R. Contrast

threshold of the human eye, Journal of the optical society of America 1946, 36, 624-643.

Previous Adaptation Luminance

In Previous adaptation luminance box, you can type the luminance (L0) value at which the

observer is adapted before seeing the current object. Value is in cd/m².

Observation Time

In Observation time box, you can type the time during which the observer has been adapted to the

luminance L0. Value is in seconds.

Observer Age

In Observer age box, you can type the age of the observer in years.

Background Luminance

In Background luminance box, you can type the luminance value of the background around the

target in cd/m².



Target Luminance

In Target luminance box, you can type the luminance value of the object for which you want to

analyze visibility in cd/m².




Curve Options

In Curve options group box, you can select the option to display the visibility diagram with delta

luminance in cd/m² in function of the background luminance in cd/m².

Delta luminance is equal to the difference between background luminance and target luminance.

Visibility state box gives information if the target is visible.

Using Sun Glasses / Colored Filter

You must have a spectral xmp map to use Sun glasses or Colored filter.

With Sun glasses or Colored filter, you can select sun glasses spectrum or colored filter.

The transmission values contained in the file are in percent.

1. Click Tools, Sun glasses or Colored filter ....

A box appears.

2. Select the Activate check box.

3. Click to browse a .spectrum or .spe file.

If needed, you can click to display the spectrum.

4. Click Apply.

5. Close the box.

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Sunglasses spectrum

Without glasses


With sunglasses - Category 3

Night Vision Goggles

Using Night Vision Goggles

You must have a spectral xmp map to use Night vision goggles.

1. Click Tools, Night vision goggles ....

A box appears.



You can open or save a file containing night vision goggles data. In this case you can save your

data as a .nvg file.

4. Click Apply.

Calculation time can be quite long because of the spectral data's treatment.

Parameters of Night Vision Goggles

Technology

In Technology box, you can select night vision goggles of generation II (Gen II) or generation III

(Gen III).

With Gen III class A, B or C, you can define a NVG of generation III with a filter in the objective lens to

restrict the response in the visible range.

Class A defines a 625nm minus blue filter.

Class B defines a 665nm minus blue filter.

Class C defines a leaky green filter.

Field of View

In Field of view, you must set the field of view value in degrees.

The field of view is the spatial angle of the outside scene that can be viewed through night vision

goggles.

System Resolution

In System Resolution box, you must set the resolution value in cycles per milliradians.

The system resolution at the center of the image is the ability of night vision goggles to distinguish

between objects close together.

Image intensifier resolution is measured in line pairs per millimeter (lp/mm) while system resolution is

measured in cycles per milliradian (cy/mr).

For any particular night vision system, the image intensifier resolution remains constant while the

system resolution can be affected by altering the objective or eyepiece optics by adding magnification

or relay lenses.

Signal to Noise Ratio

In Signal to noise ratio box, you must type a ratio value.

Signal to Noise Ratio is also called SNR.

A measure of the light signal reaching the eye divided by the perceived noise as seen by the eye.

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A tube's SNR determines the low light resolution of the image tube. Therefore higher is the SNR, better

is the ability of the tube to resolve objects with good contrast under low light conditions.

System Luminance Gain

In System luminance gain box, you must type the luminance gain value.

System luminance gain is the ratio of NVG output's luminance to input's luminance. Units are in foot-

lamberts.

A typical value for a GEN III tube is 5,000 fL/fL.

Max. Average Output Luminance

In Max. average output luminance box, you must type the maximal average output luminance

value in foot-lamberts.

Maximal average output luminance is the maximal output luminance averaged across the full field of

view.

When observed luminance increases, the luminance system gain is reduced to keep average luminance

of the phosphor screen below this value.

Phosphor Screen Spectrum

In Phosphor screen spectrum box, you must click to browse a .spectrum or .spe file to define

the spectrum of the phosphor screen.


Additional Filter

In Additional filter box, you must click to browse a .spectrum or .spe file to simulate a filter

used in the input of the night vision goggle.




With Surface and Section Analysis tool, you can have several information as total flux, contrast,

average luminance or brightness inside a surface which can be a rectangle, a polygon or an ellipse. You

can also display image section.


-Or-

1. Click .

A box appears and a shape appears on your map.


Close the window.


Units are automatically set depending on the type of map: luminance (cd/m²) or relative brightness.

Shape

You must select a type of shape as Rectangle, Ellipse or Polygon to define the analysis surface.


You can select the Surface 3D check box to enable the 3D view display of the image.

When right-clicking, the 3D Chart Control Properties box appears.

You can click ChartGroup to configure display options.

You can click Axes to configure axes and add grid lines by clicking GridLines.

You can click Levels to change levels and colors.

You can click Control, Save... to save values.

In case of a spectral map, you can view spectrum data , colorimetric data or color rendering

index .

Center

In Center group box, you must type values to define the position of the analysis surface.

Note that you can use the mouse to set center values.

Dimensions

In Dimensions group box, you must type values to define the dimension of the analysis surface.

Note that you can use the mouse to set dimensions values.

Section

You can enable the analysis section. A line is drawn on the map and a box opens to display the curve.

From the map display, you can move horizontal, vertical or user lines.

Data over a line can be exported to a .txt file by clicking Export....

Maximum / Minimum


Average




pixel.


Barycenter X / Barycenter Y

You can read barycenter X and barycenter Y values belong to the following formula.

x and y are the pixel coordinates.

Eye Illuminance

You can read the eye illuminance value.

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Eye illuminance is the illuminance at the map's observer point due to the light of the map enclosed in

the surface tool.

E is the Eye illuminance.

is both the map normal and the virtual eye illuminance sensor's normal.

is one direction in the solid angle domain defined by the viewer's surface tool.

is the map luminance in the direction.

is the elementary solid angle associated with the direction.

Sigma X / Sigma Y

You can read sigma X and sigma Y values belong to the following formula.

Sigma


Contrast


You can compare luminance contrast and brightness contrast.

If the luminance value of a map is multiplied by 100, the luminance contrast does not change but

brightness contrast evolves.

This is due to the fact that it is more difficulty to distinguish contrast when light intensity decreases.

RMS Contrast




You can click Update to compute data manually.

Export

You can click Export... to export Surface / Section data in .txt or .xmp file.

When exporting in .xmp file, you can generate a XMP corresponding to the selected area. It can be

useful to resize an XMP or to select a small area from a big size XMP.


You can then export as a .txt file.

For an extended map (data separated by source or surface) or a spectral map (data separated by

wavelength), the exported file includes one line for each source (or surface) or wavelength.

The format of the exported file is:

The same header as when you export the XMP map in a TXT file,

A line for the surface or the line definition:

Surface=Rectangle Left=value Top=value Right=value Bottom=value

-Or-

Surface=Ellipse CenterX=value CenterY=value RayX=value RayY=value

-Or-

Surface=Polygon PtNumber=n Pt0_X=value Pt0_Y=value... Ptn_X=value Ptn_Y=value

-Or-

Line Pt0_X=value Pt0_Y=value Pt1_X=value Pt1_Y=value Sampling=value

A column header:

(Source) (Wavelength) XMax YMax Max XMin YMin Min Average Contrast Sigma Flux BarycentreX

BarycentreY SigmaX SigmaY

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(Source) (Wavelength) XMax YMax Max XMin YMin Min Average Contrast Sigma

The data:

Basic map: One line

Extended map:

line 1 => User

line 2 => All

line 3 => Data for source 0


...

Spectral map:

line 1 => All

line 2 => Data for wavelength 0



...

Virtual Lighting Controller

Using the Virtual Lighting Controller

To use Virtual Lighting Controller, you must have a map with data separated by source, by surface or

sequence (extended or spectral).

With Virtual Lighting Controller, you can change contribution of layers without running new simulation.

Layers can be sources, surfaces or sequence.

1. Click Tools, Virtual Lighting Controller ...

-Or-

1. Click .

A box appears.


3. Close the box.

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Parameters of the Virtual Lighting Controller

If needed, you can change layers' name.



You can click Select all or Unselect all to respectively select or unselect all the layers.

If needed, you can add or delete a new sliders configuration.

When it is enabled, you can select Power to display power instead of ratio.

In case of spectral map, you can change units using the View menu.

For spectral maps, you can click to display a layer's spectrum.

The option is not available for ambient sources, LCD sources and set of sources including sources

which do not have the same spectrum.

The spectrum change has to be used carefully in case of fluorescent surface.

Vertical lines correspond to the spectral sampling of the xmp.

Click to define a new light source spectrum.

The spectrum of the new source is normalized to get the same power than the initial source. Unit is

photometric or radiometric depending on the one defined in the View menu.

Initial xmp Result after the spectrum change

With , you can delete a spectrum.

This function is only available in the Virtual Photometric Lab, Virtual Human Vision Lab and 3D

Energy Density Lab.

With , you get information a new spectrum has been added.

With , you can get back previous spectrum.

With , you get information a spectral data has not been saved in xmp map.

The spectral sampling of the xmp should be sufficient to cover spectrum of the new layer.

Spectrum of the initial layer should not be null within all spectral zone on each the new spectrum is

not null.

Spectrum changes can take a lot of time because calculations have been made directly on spectral

data of xmp map. When you change a spectrum for the first time, all spectral data are downloaded

in the memory and all modified calculations of layers powers are made on the spectral data. This

can take more time than usual. To avoid this when you do not need any new spectrum change but

only power change, you can clear the View, Load spectral data option.



1. Click Tools, Preferences....

-Or-

1. Click .

A window appears.


Virtual Photometric Lab

With Virtual Photometric Lab, you can visualize spectral luminance maps and display an image for each

wavelength.

Using the Virtual Photometric Lab

Virtual Photometric Lab is compatible with OLE Automation standard so that you can use a language

like VBScript to get information stored into XMP maps.

For more details, you can view Virtual Photometric Lab.

1. From Start menu, click All Programs, OPTIS, OPTIS Labs, Labs, Virtual Photometric Lab.

-Or-

1. Click Virtual Photometric Lab .

A window appears.

You can open or save a XMP map file. In this case you can save your XMP map as a .xmp file.

You can print the XMP map file.

You can import see page 101 or export see page 103 a file.

You can also import a BMP mask see page 101.

You can display results, manage display options see page 110.

Click to read map properties. For more details about precision, you can view Reading Precision

see page 111.

You can analyze colorimetric data see page 76.


Click Tools, Pick value.... to get value at a specific position.

Click or Tools, Zernike to display Zernike coefficients.

You can use the Virtual Lighting Controller see page 115.

For spectral xmp maps, you can use sun glasses or colored filter see page 117 and you can use

Night Vision Goggles see page 94.


You can manage the filtering see page 119.

All following operations are multi threaded: Open, Standard filtering, Remove highest peaks

filtering, Map addition and multiplication by a value (Photometric Calc and Distributed Computing),

Surface/Section calculations and Display update.

The threads number used for these operations is the number of processors (including cores) of the

computer.

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Importing and Exporting

Importing

Importing an Image

1. Click File, Import....

A window appears.

2. Browse an image.


FILES EXTENSIONS

Bitmap .bmp

Text .txt

Technoteam luminance image .pf

Technoteam color image .cos

OpenEXR .exr

RGBE .hdr, .pic

For more details about .txt files, you can view TXT File Format see page 104.


Files data have to be in the XYZ format.

If the Operation not supported message appears, the colorimetric space in the technoteam

software has to be set on XYZ.

If the imported map is uniform, the regional preferences of windows have to be set to have point

instead of comma.

3. Click Open .

4. If the image is a .bmp, .hdr or.pic file, a window appears. Set the parameters see page 101 and

click OK.

5. If the image is a .pf file, a window appears. Set the parameters see page 103 and click OK.

Importing a BMP Mask

1. Click File, BMP mask import....

A box appears.

2. Browse a .bmp file.

3. Click Open .

A window appears.


5. Click OK.

Parameters of Bitmap or RGBE Import

When importing bitmap file and converting it as map, the map can be used as emittance for source

definition.

The emittance of a source describes how each point of a surface emits rays.

For a source definition, the emittance can be uniform or described by a basic or a spectral map.

In the case of a basic map you have to supply a spectrum for the source and this spectrum is the same


for each point of the source.

In the case of a spectral map, the spectrum for the source is generated from the color of each pixel of

the bitmap.

Importing bitmap file is very useful to define an environment around your system for a real rendering

(luminance simulation).

There is an infinite possible spectrum for one color and the bitmap file import only provides a solution

with three Gaussian spectrum centered on red, green and blue. In most cases, default options gives a

good resulting XMP map.

Bitmap File

In Bitmap file box, you can change the bitmap file.

Map Type

In Map type group box, you must select the map type.

With Basic map, you can convert the selected bitmap into a basic xmp map.

With Laser map, you can convert the selected bitmap into a basic laser xmp map. You can then select

Amplitude check box. If needed you can select Phase check box and browse a .bmp file. In

Wavelength box, you must set the wavelength value in nanometers.

With Spectral map, you can convert the selected bitmap into a spectral xmp map. In Wavelength

minimum, Wavelength maximum, Wavelength Nb and Wavelength Step boxes, you must set

values to define the wavelength's sampling for converting a color bitmap into a spectral map. In Red

spectrum, Green spectrum and Blue spectrum boxes, you must browse to select spectrum files for

converting a color bitmap into a spectral map.

Dimensions

In Dimensions group box, you must set the width and height of the converted xmp map in

millimeters.

You can select the Respect ratio check box to keep ratio between width and height.

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Parameters of Technoteam PF File Import

Technoteam luminance images are generated from Technoteam photometric camera.

These files contain a luminance image.

Dimensions

In Dimensions group box, you must set the width and height of the image in millimeters.

This information could be found using Technoteam software delivered with the photometric camera.

You can select the Respect ratio check box to keep ratio between width and height.

Exporting

Exporting an Image

You must open an image first.

1. Click File, Export....

A window appears.

2. Type a file name and select a format.


FILES EXTENSIONS

Xmp map .xmp

Bitmap .bmp

JPeg .jpg

PNG .png

Tiff .tiff

Text .txt

Technoteam luminance image .pf

Excel .xls


FILES EXTENSIONS

OpenEXR .exr

RGBE .hdr

For more details about .txt files, you can view TXT File Format see page 104.


OpenEXR and RGBE are only enable in case of spectral maps.

3. Click Save .

4. In case of a .xmp file export, a box appears. Set the parameters see page 74 and click OK.

5. In case of a .txt file export, a box appears. Select Export data by layer or Merge active

layer(s). Click OK.

For more details, you can view Extended Map Format see page 105.

Parameters of XMP Export

The xmp Export is like a Save As except that the export includes options.

These options help to reduce the file's size on the disk.

If you do not need to analyze the spectrum on each pixel of the map and if you do not need to

analyze the data for each wavelength, you can select Include spectral data check box.

If you want to group some sources data of the map, you can select Merge active layer(s) check

box.

If you want to have filtered or original data in the exported file, you can select Export filtered

data check box.

If you want to export a spectral map to convert it into an extended map, you can select

Conversion to extended map check box.

You can select Intensity normalized as luminance check box and set a value for the Surface

box in square millimeters.

TXT File Format

With TXT file import, you can precisely define the emittance of any sources. As an example, TXT file

can be generated with a camera.

The format of the ASCII file is the same for import and export.

MapType

ValueType Intensitytype

UnitType

AxisUnit

XMin XMax YMin YMax

NbX NbY

WMin WMax NbW (Spectral map)

SourceNb Ratio0 Ratio1... RatioNb (Extended map)

x0y0 x1y0 x2y0 ... xny0

x0y1 x1y1 x2y1 ... xny1

x0y2 x1y2 x2y2 ... xny2

...

x0yn x1yn x2yn ... xnyn

Option preceding by // are not supported at that time.

MapType can have one of the following values.

OptisMapTypeBasic = 0

//OptisMapTypeLaser = 1

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OptisMapTypeSpectral = 2

OptisMapTypeExtended = 3

//OptisMapTypeUnknown = 4

//OptisMapTypeGainMatrix = 5

ValueType can have one of the following values.

OptisValueTypeIrradiance = 0

OptisValueTypeIntensity = 1

OptisValueTypeRadiance = 2

//OptisValueTypeSel = 3

//OptisValueTypeLaserPhase = 4

//OptisValueTypeLaserPhasePlane = 5

//OptisValueTypeDirectionalIrradiance = 6

//OptisValueTypeGain = 7

Intensitytype can have one of the following values.

OptisIntensityOptis = 0

OptisIntensitySAETypeA = 1

OptisIntensitySAETypeB = 2

OptisIntensityConoscopic = 3

If ValueType is not equal to 1, the IntensityType value is not taken into account.

For Intensity Conoscopic format, you must be aware that transformation takes into account following

formulas.

TetaX = Teta.cos Phi

TetaY = Teta.sin Phi

UnitType can have one of the following values.

OptisUnitTypeRadiometric = 0

OptisUnitTypePhotometric = 1

//OptisUnitTypeGain = 2

//OptisUnitTypeUnknown = 3

AxisUnit can have one of the following values.

//OptisUnitDefault = 0

OptisUnitMillimeter = 1

OptisUnitDegree = 2

OptisUnitRadian = 3

OptisUnitFeet = 4

//OptisUnitMicrons = 5

//OptisUnitNanometer = 6

//OptisUnitMeter = 7

For intensity maps, XMin XMax YMin YMax has to be replaced by ThetaXMin ThetaXMax

ThetaYMin ThetaYMax.

Extended Map Format

When exporting TXT file format, it is possible to merge enable sources.

MapType (3 for an extended map)

ValueType

UnitType

AxisUnit

XMin XMax YMin YMax (For an intensity map: ThetaXMin ThetaXMax ThetaYMin ThetaYMax)

NbX NbY

In case of extended map with no merged sources, the format is as following.

LayerNb LayerInitialPower0 LayerInitialPower1... LayerInitialPowerNb

Source_Name_1

x0y0s1 x1y0s1 x2y0s1 ... xny0s1




Source_Name_2




In case of extended map with merged sources, the format is as following.

-1 LayerNb LayerInitialPower0 LayerInitialPower1... LayerInitialPowerNb

SourceRatio1 SourceRatio2 ... SourceRatioN

x0y0 x1y0 x2y0 ... xny0

x0y1 x1y1 x2y1 ... xny1

x0y2 x1y2 x2y2 ... xny2

With -1 value before LayerN, you can know if the extended map has been included in an enable

sources's merge.

If sources are not merged, you do not have to enter any values. In this case, sources power and their

ratio are not taking into account. You must not use it for the import because it means there is only one

enable source and you can not use a basic map. This parameter is useful as information when

exporting an extended map with a merge of enable sources.

In case of spectral map with merged sources, the format is as following.

WMin WMax NbW

SeparatedByLayer SourceRatio1 SourceRatio2 ... SourceRatioN

Layer_Name

x0y0w0 x1y0w0 x2y0w0 ... xny0w0






...

x0y0wN x1y0wN x2y0wN ... xny0wN



In case of spectral map with no merged sources, the format is as following.

WMin WMax NbW

SeparatedByLayer LayerNb RadiometricPowerofSource1 PhotometricPowerofSource1 ...

RadiometricPowerofSourceN PhotometricPowerofSourceN

Layer_Name_1







...




Layer_Name_2







...




...

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Layer_Name_1




Layer_Name_2




The values at the end of the file correspond to the integral over all wavelengths per pixel per layer.

In case of spectral map without spectral data and with merged sources, the format is as following.

-1

SeparatedByLayer SourceRatio1 SourceRatio2 ... SourceRatioN

Layer_Name

x0y0ColorX x0y0ColorY x0y0ColorY2 x0y0ColorZ ... xny0ColorX xny0ColorY xny0ColorY2

xny0ColorZ


xny1ColorZ

...

x0ynColorX x0ynColorY x0ynColorY2 x0ynColorZ ... xnynColorX xnynColorY xnynColorY2

xnynColorZ

Spectral map without spectral date and with sources not merged:

-1

SeparatedByLayer LayerNb RadiometricPowerofSource1 PhotometricPowerofSource1 ...

RadiometricPowerofSourceN PhotometricPowerofSourceN

Layer_Name_1


xny0ColorZ


xny1ColorZ

...


xnynColorZ

Layer_Name_2


xny0ColorZ


xny1ColorZ

...


xnynColorZ

ColorX, ColorY and ColorZ correspond to colorimetric coordinates.

ColorY corresponds to the luminance and ColorY2 to the radiance.

HDRI File Format

High Dynamic Range Image (HDRI) is a generic name for an image format which improve the classical

bitmap representation.

Classical bitmaps are coding RGB colors using three 8bits or 16bits integer values (.bmp, .jpg, .tiff...).

The dynamic range of the picture is much more limited than what the eye is able to see in the real

world.

HDRI enables to overcome this problem by using a much wider dynamic range.

Moreover, the color quantization steps are smaller with HDRI. This provides a better colorimetric

accuracy especially when using a wide gamut.

When exporting or importing HDRI for bitmap emission with a better dynamic range, you can not only

simulate displays but also real background illumination.


Today, HDRI are supported by most rendering programs to export the rendering results but also to

import environment map. Environment maps enable to achieve very realistic illuminations. OPTIS

software are able to use environment maps (cube or sphere HDRI maps) to achieve comparable result

and even better result thanks to its physics based calculation.

You can generate good environment HDRI maps using digital cameras and a software tool like

HDRShop.

Supported Formats

RGBE and OpenEXR are supported formats.

RGBE is the native Radiance format. This is the most wide used format today.

ILM 's OpenEXR is the most powerful format to date.

XMPs are even better than HDRI, including spectral data, source separation...

When exporting XMP to HDRI your are able to address the full dynamic provided by HDRI which is not

possible when exporting a BMP to HDRI with a classical rendering software.

XMP export to HDRI: 16 bits to 16 bits

BMP export to HDRI: 8 bits to 16 bits

HDRI/Classical Bitmap Comparison

Here is a picture having levels divided by two at each step from the left to the right.

Only the left most columns are visible, the other are too dark to be seen. To see the rest of the picture,

one has to saturate the visible part by changing the exposure.

Let us compare what happen if the picture is HDRI (on the right) and if the picture is a classical bitmap

(on the left).

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When the exposition increases only slightly, no difference is noticeable

Both formats still look the same

The classical bitmap starts to show its limits

The difference is clear now

The HDRI is able to display the entire picture

As the classical bitmap only has 256 grey levels, all levels inferior to the darker possible grey level are

coded black. This is why they are unrecoverable.

XMP Emission

Now if we compare XMP emission, the XMP is seen through a transparent sphere.

The same simulation was achieved using a HDRI import generated XMP (left column) and a classical

bitmap import generated XMP (right column).


The Virtual Photometric Lab level indicates the light level that is displayed saturated.




All display's options as filtering level, Surface/Section parameters or layers' configurations are saved

within the Virtual Photometric map when saving the file.


If you want to make a vertical or horizontal symmetry of the map, click Operation, Vertical axis

symmetry or Horizontal axis symmetry.

If you want to use the zoom, rotate the mouse wheel, click Edit, Activate Zoom or click and

then left-click or right-click.

Click to display the original size.


The displayed value is interpolated with the value of many pixels. Click View, Interpolate values to

activate or deactivate the interpolation.

If you want to view spectrum curve at the mouse position, click .

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If you want to modify the unit belong to the map type, click View, Photometric units or

Radiometric units.


If you want to change displayed colors, use the color list.

Iso levels displays the image with ISO curves or surfaces.

If you want to display Wavefront Error or FFT MTF or PSF, use the Wavefront Error list.

If you to change displayed field, use the field list.

If you want to display one single wavelength, use the wavelength list.

If you want to display grids and other options, right-click on the map to select tools.

As an example you can show ruler, set ruler parameters, show axis on cross, snap cross to grid,

show tooltip, show gray around the map, fill shape, show primary or secondary graduations, set

graduations parameters, show primary or secondary grids, set grid parameters.

If you want to modify display's parameters, click Tools, Level... or .

You can select a level to modify the value. Press Enter to validate the change.

You can right-click and select Copy to clipboard.

When modifying minimum or maximum value, you can select the Intermediate levels auto-

update check box to compute all intermediate values.

If needed, you can add or delete a color level.

You can click Default to cancel all modifications.

Select the IsoCurve and Filled check boxes, to display the image with or without ISO curves.

Click Linear or Log to switch between a linear or logarithmic scale.

Click Load Scale or Save Scale to load or save parameters in an OPTIS scale file. Format is .scl.

When Iso levels is selected in the color list, you can change the color between two levels clicking

.

Reading Precision

Precision Value

In direct simulation, the displayed precision value corresponds to the pixel having the highest number

of integrated rays.



With N the number of rays integrated by the pixel.

When no rays are integrated on a pixel, the error is infinite. The precision value is one hundred

percent.

In direct simulation using radiance luminance sensor with activated gathering, precision does not have

any meaning. Precision value is also one hundred percent.

In inverse simulation using the Monte-Carlo algorithm, a number of pass has to be specified as 100

passes = 100 rays per pixel (not necessary effective rays).



With N the number of passes.

In inverse simulation using determinist or photon map algorithms, precision does not have any

meaning. Precision value is also one hundred percent.


Higher is the precision percent, lower is the image quality.

Be aware that one pixel which has not received any rays or which has received only one has a one

hundred percent precision.

More rays or passes there are, lower is the statistical noise. A direct correlation between this number

and the error (or variance, standard deviation) is not possible.

For systems under weighted Monte-Carlo algorithms, the only way to compute error (variance) is to

launch the same simulation several times and to calculate the standard deviation of specific pixels.

The statistical error is always less important for pixels with more integrated rays.

Precision Map

For direct simulation, you can click Tools, Precision map... to display the precision map.

The precision map is only validate for all sources set at one hundred percent when there is no any

separation by sources.

The precision is displayed in percent and is saved in rays number in the map. You can then generate

precision calculation with the surface / section analysis tool.

Analyzing Colorimetric Data

Three tools are available to analyze colorimetric data.

If you want to see colorimetric data at a specific pixel location, you can click Tools, Colorimetric

data... or .

For more details, you can view Parameters of Chromaticity Coordinates Tool see page 44.

If you want to analyze the error between the color displayed by the screen and the reality for all

points of the map, you can click Tools, Colorimetric error....

The true color luminance map is replaced by a colorimetric error map displayed in false color.

When the dynamic of the luminance map is higher than the one of the screen, the Lab compresses

the luminance using a linear relation.

With colorimetric error tool, you can analyze the error between the color after compression and the

color really displayed by the screen.

The colorimetric error is calculated using the CIE94 (1 :1 :1) formula (CIE 116-1995).

When the dynamic of the luminance map is lower than the one of the display, there is no

luminance compression. In this case the displayed error is the one between the color contained in

the luminance map and the one really displayed.

If you want to have all information about the spectrum for all points of the map, you can click

Tools, Spectrum... or .


If you want to read the color rendering index values, you can click Tools, Color Rendering Index

(CRI) ....

For more details, you can view Parameters of the Color Rendering Index see page 51.



With Surface and Section Analysis tool, you can have several information as total flux, contrast,

average inside a surface which can be a rectangle, a polygon or an ellipse. You can also display image

section.

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-Or-

1. Click .





Units are automatically set depending on the type of map (luminance, illuminance...).

Shape

You must select a type of shape as Rectangle, Ellipse or Polygon to define the analysis surface.

You can select the Surface 3D check box to enable the 3D view display of the image.

When right-clicking, the 3D Chart Control Properties box appears.

You can click ChartGroup to configure display options.

You can click Axes to configure axes and add grid lines by clicking GridLines.

You can click Levels to change levels and colors.

You can click Control, Save... to save values.

In case of a spectral map, you can view spectrum data , colorimetric data or color rendering

index .

Center

In Center group box, you must type values to define the position of the analysis surface.


Dimensions

In Dimensions group box, you must type values to define the dimension of the analysis surface.


Section

You can enable the analysis section. A line is drawn on the map and a box opens to display the curve.

From the map display, you can move horizontal, vertical or user lines.

Data over a line can be exported to a .txt file by clicking Export....

Maximum / Minimum


Average





pixel.


Flux

You can read flux value in the shape belong to the following formula.

S is the surface of the calculation area.

Sp is the surface of one pixel.

Barycenter X / Barycenter Y

Barycenter X and Y values are not useful for conoscopic maps.

You can read barycenter X and barycenter Y values belong to the following formula.

x and y are the pixel coordinates.

Sigma X / Sigma Y

You can read sigma X and sigma Y values belong to the following formula.

Sigma


Contrast


RMS Contrast





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Export

You can click Export... to export Surface / Section data in .txt or .xmp file.

When exporting in .xmp file, you can generate a XMP corresponding to the selected area. It can be

useful to resize an XMP or to select a small area from a big size XMP.

You can then export as a .txt file.

For an extended map (data separated by source or surface) or a spectral map (data separated by

wavelength), the exported file includes one line for each source (or surface) or wavelength.

The format of the exported file is:

The same header as when you export the XMP map in a TXT file,

A line for the surface or the line definition:

Surface=Rectangle Left=value Top=value Right=value Bottom=value

-Or-

Surface=Ellipse CenterX=value CenterY=value RayX=value RayY=value

-Or-

Surface=Polygon PtNumber=n Pt0_X=value Pt0_Y=value... Ptn_X=value Ptn_Y=value

-Or-

Line Pt0_X=value Pt0_Y=value Pt1_X=value Pt1_Y=value Sampling=value

A column header:

(Source) (Wavelength) XMax YMax Max XMin YMin Min Average Contrast Sigma Flux BarycentreX

BarycentreY SigmaX SigmaY

-Or-

(Source) (Wavelength) XMax YMax Max XMin YMin Min Average Contrast Sigma

The data:

Basic map: One line

Extended map:

line 1 => User

line 2 => All



...

Spectral map:

line 1 => All




...









-Or-

1. Click .

A box appears.


3. Close the box.




















Energy Density Lab.


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Using Sun Glasses or Colored Filter

You must have a spectral xmp map to use Sun glasses or Colored filter.

With Sun glasses or Colored filter, you can select sun glasses spectrum or colored filter.

The transmission values contained in the file are in percent.

1. Click Tools, Sun glasses or Colored filter ....

A box appears.


3. Click to browse a .spectrum or .spe file.


4. Click Apply.

5. Close the box.

Night Vision Goggles

Using Night Vision Goggles

You must have a spectral xmp map to use Night vision goggles.

1. Click Tools, Night vision goggles ....

A box appears.



You can open or save a file containing night vision goggles data. In this case you can save your

data as a .nvg file.

4. Click Apply.

Calculation time can be quite long because of the spectral data's treatment.

Parameters of Night Vision Goggles

Technology

In Technology box, you can select night vision goggles of generation II (Gen II) or generation III

(Gen III).


With Gen III class A, B or C, you can define a NVG of generation III with a filter in the objective lens to

restrict the response in the visible range.

Class A defines a 625nm minus blue filter.

Class B defines a 665nm minus blue filter.

Class C defines a leaky green filter.

Field of View

In Field of view, you must set the field of view value in degrees.

The field of view is the spatial angle of the outside scene that can be viewed through night vision

goggles.

System Resolution

In System Resolution box, you must set the resolution value in cycles per milliradians.

The system resolution at the center of the image is the ability of night vision goggles to distinguish

between objects close together.

Image intensifier resolution is measured in line pairs per millimeter (lp/mm) while system resolution is

measured in cycles per milliradian (cy/mr).

For any particular night vision system, the image intensifier resolution remains constant while the

system resolution can be affected by altering the objective or eyepiece optics by adding magnification

or relay lenses.

Signal to Noise Ratio

In Signal to noise ratio box, you must type a ratio value.

Signal to Noise Ratio is also called SNR.

A measure of the light signal reaching the eye divided by the perceived noise as seen by the eye.

A tube's SNR determines the low light resolution of the image tube. Therefore higher is the SNR, better

is the ability of the tube to resolve objects with good contrast under low light conditions.

System Luminance Gain

In System luminance gain box, you must type the luminance gain value.

System luminance gain is the ratio of NVG output's luminance to input's luminance. Units are in foot-

lamberts.

A typical value for a GEN III tube is 5,000 fL/fL.

Max. Average Output Luminance

In Max. average output luminance box, you must type the maximal average output luminance

value in foot-lamberts.

Maximal average output luminance is the maximal output luminance averaged across the full field of

view.

When observed luminance increases, the luminance system gain is reduced to keep average luminance

of the phosphor screen below this value.

Phosphor Screen Spectrum

In Phosphor screen spectrum box, you must click to browse a .spectrum or .spe file to define

the spectrum of the phosphor screen.


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Additional Filter

In Additional filter box, you must click to browse a .spectrum or .spe file to simulate a filter

used in the input of the night vision goggle.




A window appears.


Managing the Filtering

With Filtering, you can smooth the map and use several analysis tools.

Using the XMP Filtering

By clicking Filtering, XMP Filtering, you can modify the map data by applying a filtering on the data.

The filtering algorithm modifies the value of each pixel with the values of its neighbors.

Depending on the map type, different types of XMP filtering are available.

When selecting Standard, you can do XMP filtering for basic or extended maps. It only uses

neighbors without any considerations regarding values of these neighbors.

When selecting Remove highest peaks, you can do XMP filtering for spectral maps. It removes very

high values which could appear in a very noisy map.

In Threshold box, you must type the threshold value.

If the pixel value is threshold times higher or lower than the average value of its neighbors, a

median filtering is applied to the pixel.

When selecting Anisotropic, it uses neighbors taking into account the values of these neighbors and

it diffuses modifications.

Anisotropic filtering is used to filter low dynamic images. Using high dynamic images can generate

problems and change colors.

Anisotropic filtering is a filter algorithm that keeps objects edge in the image to avoid blur. It

computes the mean of neighboring pixels according an edge detection criteria.

It acts as if the pixels influence spreads on its neighbors circularly in uniform regions, and

elliptically in edge regions in order to keep borders.

Filter shape when arriving near an image's border

At each diffusion pass, a diffusion step is applied in two directions.


In Min Diffusion box, you must type the minimal diffusion value. Minimal diffusion indicates the

relative size of the smallest ellipse axis in the edge direction.

In Max Diffusion box, you must type the maximal diffusion value. Maximal diffusion indicates the

relative size of the tallest ellipse axis in the orthogonal edge direction.

In Time step box, you must type the time step value. Time step is proportional to the number of

pixels taken into account during filtering in each ellipse direction. It is according ellipse shape given

by minimal and maximal diffusion.

In Pass number box, you must type the number of times the XMP filtering algorithm is called. 0

value means there is no filtering.

The level of filtering is displayed in the status bar of the viewer. By clicking the filter value in the status

bar, you can open the filtering box.

Using Other Filterings

All following filters only modify the image.

By clicking Filtering, Averaging filters, you can click Smooth, Medium or Hard to choose the

size of the matrix.

The Averaging filters gives to a pixel the average value of a matrix around it.

Smooth is 3x3 pixels, Medium is 5x5 pixels and Hard is 7x7 pixels.

By clicking Filtering, Median filter, you can click Smooth, Medium or Hard to choose the size of

the matrix.

With Median filter, you can make the details stand out.

Smooth is 3x3 pixels, Medium is 5x5 pixels and Hard is 7x7 pixels.

By clicking Filtering, User smoothing, you have same filter than Median filter but with the

possibility to set parameters.

More level parameter there are, more details stand out.

In Pass number box, you must type the number of times the filter is called.

In Pixel number box, you must type the size of the filter. Note that a filter is always square.

In Mask pixel number box, you must type the mask pixel number. This number do not impact

the filtering which is not used.

In Mask level number box, you must type the coefficient to improve edges detection.

Using Filtering Tools

You can use analysis tools by clicking Filtering, Log, Edge detector, Threshold... or Log2.

In Threshold parameter box, you must type the threshold value.

Note that Log2 is a little more important than Log.

You can use contrast and brightness tools by clicking Filtering, Contrast, or Brightness.

Original image Level filtered image

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Contrast filtered image Brightness filtered image

For more details about the level tool, you can view Managing the Display see page 110.

Virtual Reality Lab

With Virtual Reality Lab, you can read natively OpenEXR/HDR and XMP spectral picture and OPTIS

environment map (OptisVR).

You can visualize a HDR environment map and create it with six pictures of your simulation (HDR or

XMP spectral).

Moreover, you can use the virtual lighting controller to change source level of lights on picture and

environment map.

Finally, with Virtual Reality Lab, you can export the result to HDR/EXR/OptisVR and QTVR formats.

Virtual Reality Lab Icons

You can open a file (EXR, HDR, XMP (only spectral format) and OptisVR).

You can save the current file.

You can use the Virtual Lighting Controller.

For more details, you can view Using Virtual Lighting Controller see page 123.

With Maximal Level Controller, you can change the maximal level of the

picture or environment map.

Colorimetric Data.

Human Vision.

Vision Parameters.


Preferences. For more details, you can view Monitor see page 194.

With View true picture size, you can visualize picture with 100% zoom level.

With Fit picture to window, you can fit picture to screen keeping the picture's

proportion.

Visualization of left eye's environment map only.

Visualization of right eye's environment map only.

Active stereo vision.

With View Front, View Top, View Bottom, View Left, View Right and View

Back, you can change camera orientation.

With View Picture, you can view OptisVR as a plan picture.

With View OptisVR, you can view OptisVR as an environment map or

generate an environment map with a picture file.

With Create a Stereo OptisVR. , you can create a Stereo environment map

see page 126 with two OptisVR file.

With Create an Immersive View, you can create an environment map see

page 124 with six pictures (EXR, HDR, XMP spectral format supported).

With Create an Observer View, you can create an Observer View see page

129.

You can launch Help.

Using Virtual Reality Lab

The first launch of Virtual Reality Lab can take a while, in this case please wait.

1. Click Virtual Reality Lab .

The window appears.

The Devices preferences window appears at the first use. For more details, you can view Devices

preferences see page 199.

2. Click File, Open to select a picture file.

The picture appears.

Format can be .OptisVR, .xmp, .exr, .pic or .hdr.

For an image, rotate the mouse wheel to zoom in or out, click the mouse left button to translate

the picture, and click the + or - button to change maximum level of picture.

For an OptisVR, rotate the mouse wheel to open or close the aperture camera, click the mouse left

button to rotate the camera, and click the + or - button to change maximum level of environment

map.

Use the Up/Down page keyboard shortcuts to change the mode of the used colors.

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1. Click Edit, Virtual Lighting Controller ...

-Or-

1. Click .

A box appears.


3. Close the box.

Parameters of the Virtual Lighting Controller VRL




















Energy Density Lab.






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Creating an Immersive View

Immersive View is when the eyes are looking around them.

Immersive view is an environment map with six pictures.

Immersive view's format is Optis VR.

1. Click Create an Immersive View .

-Or-

1. Click the Creation menu, Create an Immersive View.

A window appears.

2. Select the wanted picture, and then double-left-click.

3. Browse a picture file.

The first loaded picture configures the environment map (size of picture, format and number of

sources).

Only one picture has to be uploaded.

The environment map with six pictures appears.

If you want to rotate a picture, you can use the rotation menu.

You can change the Maximal Level.

4. Click OK.

5. Save the Immersive View.

The Immersive View appears.

Human Vision

Using Human Vision

1. Click Edit, Human Vision...

-Or-

2. Click .

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The Human vision is now enabled.

3. Click Edit, Human Vision Parameters...

-Or-

4. Click .

A box appears.


Parameters of Human Vision

You can select an Adaptation type from the list.

Select Local adaptation so that the accommodation is on a fixed point of the luminance map.

Use the slider in the Local Adaptation Properties box to change the luminance value of this

point in Cd/m² . When you open a luminance map, this value is equal to the average luminance

of the map.

You can click Default to reset adaptation luminance.

Select Dynamic adaptation to enable the spatial adaptation of the human eye.

This models the fact that the eye adapts locally as the viewer scans the different areas of the

luminance map.

You can select the Automatic update check box to compute automatically the ideal adapted

luminance for the scene.

This option is automatically activated for Dynamic Adaptation. It disables the Local Adaptation

Properties box for the Local Adaptation type.

You can select the Temporal adaptation check box to enable human eye time adaptation which

occurs on scene luminance changes.

This option is available only for Dynamic Adaptation.

Example of Temporal adaptation (in mm:ss)

You can select a Mesopic calculation mode from the list to define how the photopic, mesopic or

scotopic vision mode is estimated.

This defines the photoreceptors sensitivity.

As an example for photopic vision rods are fully saturated.

You can select Maximum. With this parameter the vision mode is computed using the

maximum luminance value of the scene. Rods saturation state is supposed to be the same for

all points of the luminance map.


You can select Average. With this parameter vision mode is computed using the mean value of

the scene. Rods saturation state is supposed to be the same for all points of the luminance map.

You can select the Glare Effect (Vos 1984) check box to activate the glare effect.

Vos 1984 is partly based on Vos, J. Disability glare – a state of the art report. C.I.E Journal 3,

2(1984), 39-53.

Vos 1984 takes into account the light scattering into the cornea, the lens and the retina of the eye

responsible for the veil of luminance.

It also simulates the lenticular halo and the ciliary corona essentially caused by the lens.

Without glare effect Vos, 1984

You can edit the Age of the observer group box to change the observer’s age in years.

This option is available only when Dynamic Temporal Adaption or Glare Effect are enabled.

Stereo OptisVR

Creating a Stereo OptisVR

Stereo OptisVR is saved in .OptisVR format.

1. Click Create a Stereo OptisVR .

-Or-

2. Click Creation, Create a Stereo OptisVR.

A window appears.

3. Browse a left .OptisVR file.

4. Browse a right .OptisVR file.

Files must have same dimensions and sources' number.

5. Click OK.

6. Save the Stereo OptisVR.

The Stereo OptisVR appears.

You can use the + and - buttons to optimize the rendering.

You can click View left eye or View right eye to switch between left and right eye's

environment map.

You can click View in 3D Stereo to activate the stereo mode.

This option is only enabled when using a graphics card supporting the active stereo (for example

QUADRO model for NVIDIA).

Active Stereoscopy (Frame sequential mode)

One projector displays right and left images in frame sequential mode.

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The end-user wears shutter glasses that occult each eye after the other according to the display

framerate.

Passive Stereoscopy

Passive view can be used in one or several screens. When using one screen, a graphic card with two

output LCD projectors is needed (not available for LCD screen).

When using several screens, two projectors equipped with special filters displaying right and left

images are needed. End-user wears passive stereo glasses and look at screens.

1. Open the Multiscreen tool.

2. Set one Display, one Window, two Areas and two Eyes for the Avatar.

3. Save.

4. Click Run.


5. Select a stereo OptisVR file.

Using the Stereo Immersive View Correction

This tool can only be used with an Immersive View see page 124.

By default, the focal plane is at the infinite.

With Stereo Immersive View Correction, you can set the stereo focus distance to optimize the

visualization.

1. Click File, Open or click Open to launch a Stereo OptisVR file.

2. In case of the active stereoscopy, click View in 3D Stereo to activate the stereo mode.

3. In case of the passive stereoscopy, use the Multiscreen to activate the stereo mode.

4. Click View, Set Focal plane.

A window appears.

5. Move the slider to align an area.

This sets the focal plane at this location.

Focal Plane on the acronym Focal Plane on the rear-view mirror

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Switching between Stereo and Normal Mode

It is possible to switch between Stereo and Normal Mode in Full Screen mode.

To do it, you can use the following shortcuts:

r Right eye

l Left eye

s Stereo mode

Creating an Observer View

Observer View is when eyes are turning around the object.

In the simulation several cameras should have been placed around the object and should look at the

same point.

Result of the simulation has to be a list of images using the XMP format.

Images should have same dimensions and same number of sources.

1. Click Create an Observer View .

-Or-

2. Click Creation, Create an Observer View.

3. Click Open and then select a list of .xmp files.

The number of selected images can be limited by the computer memory.

4. Click OK.

5. Save the view as an .OptisVR file.

The Observer View appears.

You can use the + and - buttons to optimize the rendering.

You can turn the view with the mouse.

Virtual Reality Lab Management

Switching Between HDRI Picture and Immersive View

Converting HDRI Picture to Immersive View

If you load a picture with 4:3, 3:4, 1:6 proportion, you can transform this picture to Immersive View.

1. Click View Immersive .

The picture changes.

This option is only enabled if the conversion is possible.

A picture with 4:3, 3:4, 1:6 proportion is not necessarily a valid cubemap.

Converting Immersive View to HDRI Picture

1. Click View Picture .

The picture changes.


Using the Filtering

The Filtering option is used to reduce noise of the picture.

1. Click Edit, Filtering.

Saving Results

Save As

OPENING FORMAT SAVING FORMAT

PICTURE

EXR

HDR

XMP (spectral)

EXR

HDR

OptisVR

OPTISVR/OPTISVR

OptisVR Environment map

mode

OptisVR

Picture mode EXR HDR

OptisVR Stereo OptisVR Stereo

Export to QTVR

Save OptisVR to Quicktime VR format (.mov).

This function is only enabled with Virtual Reality Lab 32bits.

MultiScreen

The Master Mode manages the simulation and the Slave Mode executes the orders.

The slave is always used on a separated computer.

A directory including .OptisVR files has to be shared between Master and Slave. Used path has to go

through the Network.

Slaves must have the required rights to connect to this shared directory. This means that the slave

does no have to connect to the directory with a login and password.

System VR Configuration

System VR Configuration Overview

System VR Configuration is composed of Windows, Areas and SystemDisplay itself composed of

Displays and Avatars.

Real World Virtual World

Cave SystemDisplay

Cave's wall Display

Human/Machine

in the Cave Avatar

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Axis System

Axis system has to be defined for each SystemDisplay, for each Display and for Avatar's head.

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SystemDisplay

Creating a System Display

1. Click the Multiscreen menu, Launch Multiscreen.

A window appears.

2. Click Master Mode.

A window appears.

3. Right-click SystemDisplay and then click Add.

This is the step to define the system in the world.

A window appears.


Default values are often kept for the SystemDisplay axis system.

5. Click OK.

The System VR Configuration is updated.

Parameters of a SystemDisplay

The SystemDisplay axis system has to be located in respect of the World axis system.

Position

X, Y and Z positions define the axis system.

Direction

X, Y, Z and Phi directions define the locked direction of the axis system.

Phi is the rotation angle around the defined direction axis.

Display

Creating a Display

A SystemDisplay must be created first.


A window appears.


A window appears.

3. Right-click on All Display and then click Add Display.

A window appears.


5. Click OK.


A mouse move on the icon displays parameters.

Parameters of a Display

The Display axis system has to be located in respect of the SystemDisplay axis system.

Dimension

Xmin, Xmax, Ymin and Ymax dimensions define the size of the Display.

Dimensions of the screen define the center of the screen.


Position


It is very important to set an offset to the Display in respect of the SystemDisplay axis system.

Default values should be X=0, Y=0 and Z=-1.

Direction


Phi is the rotation angle around the defined direction axis.

The normal of the display is always looking at the center of the SystemDisplay.

Avatar

Creating an Avatar

A SystemDisplay must be created first.


A window appears.


A window appears.

3. Right-click All Avatars and then click Add Avatar.

A window appears.

4. Click AvatarX, Default head and New EyeX to set the parameters see page 134.

Avatar corresponds to the feet position.

5. Click OK.


Parameters of an Avatar

The axis system of Avatar's head has to be located in respect of the SystemDisplay axis system.

Direction


Position


Avatar's head system has to be offset in respect of the SystemDisplay system.

Window

It is strongly recommended to have one window and several areas to improve calculation

performances.

Creating a Window

You must first define where the zero reference see page 135 is located on your computer screens.


A window appears.


A window appears.

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3. Right-click on Windows and then click Add.

A window appears.


5. Click OK.


Parameters of a Window

Definition

X and Y define the window dimensions.

Position

X and Y define the position in reference to your system's origin.

Defining the zero reference

1. Go to Control Panel, Display, Change display settings.

2. Click on the top left corner to check the references.

The zero reference (0,0) is at the top left corner of your main display.

3. Define your system.

Area

An area is included in a window.

Areas and related Display must have the same ratio for the dimensions to avoid image distortion.

All Areas defined from a same computer must have the same dimensions.

In case of several same size Areas, one will be the master Area.

Creating an Area


A window appears.


A window appears.

3. Right-click on Drawing Area and then click Add.

A window appears.


5. Click OK.



6. Save your complete configuration using the .xml format.

Parameters of an Area

Definition

X and Y define the area dimensions.

Position

X and Y define the position in reference to Windows's origin.

Rendering definition

X and Y define the resolution of the area.

Rendering can not be bigger than the Window dimension.

Less pixels you have, faster the calculation is.

Network Management

Network management has to be set between Master and Slave machines.

Configuring the Network Management

Following steps must be done on master and slaves computers.


A window appears.

2. Click Network management.

A window appears.


4. Click OK.

The configuration is saved in the MultiScreen.cfg file located in the

C:\ProgramData\OPTIS\MultiScreen directory.

To avoid the same modification on all the slaves computers, you can copy this file from the Master

computer to all the Slaves computers at the same location.

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Parameters of Network Management

The port configuration must be identical for all the PCs used in the network configuration.

Multiscreen Options > Synchronization

Without Sync

Master and Slaves display the rendering as they have finished the calculation. There is no software

synchronization.

If the hardware used is not powerful enough, there may be rendering problems, as the display of

different points of view, between the screens.

Soft Lock

This is a software synchronization. The softlock mode guarantees a synchronized rendering on all

screens. The Master gives instructions to all Slaves. Slaves are calculating the rendering in an

internal memory. When calculation is over, the Master is going to ask for the copy of the data on the

screens.

Multicast

Multicast IP

The range of the Multicast is between 224.0.0.1 and 239.255.255.255.

Incoming Port

Enter the port number.

Display Socket

Incoming Port

Enter the port number.

Port numbers have to be different. They are already set by default.

Automatic Start

Detection port

Enter the Detection port number.


Configuring the Windows Firewall

To enable network communications before using multiscreen with Virtual Reality Lab, configure the

Windows firewall.

1. From the Windows Start menu, select Control Panel.

2. Select Windows Firewall.

3. Click Allow a program or feature through Windows Firewall.

4. Click Allow another program...

5. Click Browse and select OPTIS Daemon.

6. Click Open.

7. Click Network Location Type.

8. Select the the Domain and Home/network (Private) check boxes

9. Click Add.

10. Click Browse and select VRLab.

11. Click Open.

12. Click Network Location type.

13. Select the the Domain and Home/network (Private) check boxes

14. Click Add.

15. Click OK.

Network communications are now fully allowed.

This settings are valid for a basic Windows configuration. If you are encountering further network

communications problems, check you additional firewall and/or antivirus programs.

Cluster

The cluster is for the current machine.

Cluster has to contain at least one Display.

In case of one Avatar with one eye, the eye is defined by default.

It is not possible to overlap windows.

Setting the Cluster for the Master

You must set the network management see page 136 first.

You must have defined a complete configuration see page 130 first.



3. Browse your configuration file.

Cluster window is going to be configured.

If needed, right-click on the Master to Change OpenCL platform.

4. Drag and drop a Window from System VR Configuration window to the Cluster window.

5. Drag and drop an Area from System VR Configuration window to the Cluster window.

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6. Drag and drop a Display to [Unlink Display] and Avatar's eyes to [Unlink avatar's eyes].

7. Right-click on Unlink Device and click Link Device.

8. Select the device and click OK.

9. Redo steps for each Area.

10. Save the configuration.

Adding Slaves to the Configuration

In the Multiscreen Distribution window,

1. Click Find slaves.

2. Click Add..., select a computer and click OK.

-Or-

Type a computer name and click Add....

3. Redo previous step for all the slaves you want to add.

If needed you can click Remove to remove a slave computer from the list.

4. Click Find.

Connection can take some time.

New slaves appear in the Cluster area.

5. For each slave computer,

1. Drag and drop a Window from System VR Configuration window to the slave.

2. Drag and drop an Area from System VR Configuration window to the slave.

3. Drag and drop a Display to [Unlink Display] and Avatar's eyes to [Unlink avatar's eyes].

4. Right-click on Unlink Device and click Link Device.

5. Select the platform and click OK.

You can right-click on a slave and click Remove computer to remove a slave from the cluster.

6. Save the configuration.

Starting the MultiScreen Mode

You must have set the cluster for the master see page 138 and the slaves see page 139 first.

1. Click Run.

If you did not save the configuration yet, a message prompts you to save.

A black window appears on each computer of the cluster.

2. From the master, click Open to launch an .OptisVR file.

After a few seconds, the black window on each computer is updated with the .OptisVR image

corresponding to the point of view defined in its configuration.

The download can take some time.

The application automatically runs on slave computers.

In the case there is a distortion of the image you can use a second computer to display it.

From the master, the rendering can be changed to see the effect on slaves.

You can move the mouse to navigate inside the pictures.

3. From the Multiscreen menu, you can click Stop Multiscreen to exit the multiScreen mode.


Using the Multiscreen Autostart

When you select the Multiscreen Autostart option, the last valid configuration you created is

automatically loaded the next time you launch Virtual Reality Lab.

1. Click the Multiscreen menu.

2. Select Multiscreen Autostart.

The Multiscreen Autostart option is activated.

Using the SIM2 HDR Monitor

You must have a standard monitor for interface and a SIM2 HDR monitor for rendering.

1. From the standard monitor, click Virtual Reality Lab .

The window appears.

The first launch of Virtual Reality Lab can take a while, in this case please wait.

If it is the first time you launch Virtual Reality Lab, the Devices preferences window appears. For

more details, you can view Devices preferences see page 199.

2. Set the Display Monitor see page 194 parameters.

3. Connect the SIM2 HDR monitor using the High Dynamic Range DVI signal connector.

4. From the standard monitor, open the Start menu, click Control Panel, Display, and then select

the Change display settings tab.

1. Select the screen you just added and select the Make this my main display check box.

2. In Multiple displays group box, select Extend these displays.

3. Click OK.

5. In Virtual Reality Lab, click MultiScreen, Launch MultiScreen, then Master Mode.

A window appears.

6. Create the rendering zone on the SIM2 HDR monitor.

To do it, you must create SystemDisplay, Display, Avatar, Window, Area and a Cluster. For

more details, you can view Using Master Mode.

You can start from this .xml (../Common/LAB_OPTIS.zip) file example and personalize it.

You can view the video (../Common/LAB_VRLab_SIM2HDR.zip) if you need more help.

Virtual Reality Peripheral Network

Using Virtual Reality Peripheral Network

1. Click MultiScreen, Launch MultiScreen, then Master Mode.

A window appears.

2. Create the rendering zone.

To do it, you must create SystemDisplay, Display, Avatar, Window, Area and a Cluster. For

more details, you can view Using Master Mode.

You can start from this .xml (../Common/LAB_OPTIS.zip) file example and personalize it.

3. Click Run.

4. Check your VRPN server is connected.

5. Click File, Open or click Open to launch an .OptisVR file.

../Common/LAB_OPTIS.zip

../Common/LAB_VRLab_SIM2HDR.zip

../Common/LAB_OPTIS.zip

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6. Click MultiScreen, VRPN Configuration.

A window appears.

7. If needed, set your Server Name and Tracker Label.

Server Name can be a name or an IP address.

Tracker Label is your peripheral's name used by your VRPN server.

8. Click MultiScreen, Launch VRPN.

Tracker can be used.

9. Click MultiScreen, Stop VRPN.

Using the Virtual Reality Peripheral Network Autostart

When you select the VRPN Autostart option, the Virtual Reality Peripheral Network is automatically

loaded when you launch Virtual Reality Lab.

1. Click the Multiscreen menu.

2. Select VRPN Autostart.

The VRPN Autostart option is activated.

3D Energy Density Lab

Using 3D Energy Density Lab

1. From Start menu, click All Programs, OPTIS, OPTIS Labs, Labs, 3D Energy Density Lab.

-Or-

1. Click 3D Energy Density Lab .

A window appears.


-Or-

Click .

3. Browse a .vmp file.

You can save the VMP map file. In this case you can save your VMP map as a .vmp file.

You can import from txt or export to txt.

You can manage the display see page 142.

Click View, Properties, or , to view properties.

By clicking Filtering, VMP Filtering, you can set a standard filtering.


In Pass number box, you must type the number of times the filtering algorithm is called. 0 value

means there is no filtering.

The level of filtering is displayed in the status bar of the viewer. By clicking the filter value in the

status bar, you can open the filtering box.

You can make volume and section analysis see page 143.

You can use the Virtual Lighting Controller see page 144.









If you want to change displayed colors, use the color list.

Iso levels displays the image with ISO curves or surfaces.

If you want to modify display's parameters, click Tools, Level... or .

You can select a level to modify the value. Press Enter to validate the change.

You can right-click and select Copy to clipboard.

When modifying minimum or maximum value, you can select the Intermediate levels auto-

update check box to compute all intermediate values.

If needed, you can add or delete a color level.

You can click Default to cancel all modifications.

Select the IsoCurve and Filled check boxes, to display the image with or without ISO curves.

Click Linear or Log to switch between a linear or logarithmic scale.

Click Load Scale or Save Scale to load or save parameters in an OPTIS scale file. Format is .scl.

When Iso levels is selected in the color list, you can change the color between two levels clicking

.

Properties

You can select the Decoration check box to display the 3D view tool.


You can select the Axis check box, you can display the axis.

You can select the Cutting views check box to display the cutting views.

You can then select the Show Manipulator check box.

Left-click on the axis and move to make a movement.

Left-click on the axis, press Ctrl and move to make a rotation.

Click Up or Down page to change the mode of the used colors.

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Volume and Section Analysis

Making Volume and Section Analysis

With Volume and Section Analysis tool, you can have several information inside a volume. You can also

display image section.

1. Click View, Volume....

-Or-

1. Click .




Parameters of Volume and Section Analysis

Shape

You can select the Parallelepiped type of shape to define the analysis volume.

Center

In Center group box, you must type values to define the position of the analysis volume.


Direction

In Direction group box, you must type values to define the direction of the analysis volume.


Dimension

In Dimensions group box, you must type values to define the dimension of the analysis volume.


Section

You can enable the analysis section. A axis plane is drawn on the map.

If you want to export the map rendering into a XMP file, click Export to XMP.

Sampling

You can change the sampling value.

The sampling is used to improve the definition of the final picture.

Maximum / Minimum

You can read maximum and minimum values of the analysis volume.



You can click Export ... to export in TXT file.









-Or-

1. Click .

A box appears.


3. Close the box.

















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Energy Density Lab.






not null.








A window appears.



VIEWERS

Intensity Viewers

Eulumdat Viewer

With Eulumdat Viewer, you can process intensity data stored in Eulumdat file.

Using the Eulumdat Viewer

1. From Start menu, click All Programs, OPTIS, OPTIS Labs, Viewers, Intensity Viewers,

Eulumdat Viewer.

-Or-

1. Click Eulumdat .

A window appears.

You can create, open or save an Eulumdat file. In this case you can save your file as a .ldt file.

When creating an Eulumdat file, you must select the symmetry type.


By clicking File, Export ..., you can export an Eulumdat file as a XMP map file. For more details

about XMP map file, you can view Virtual Photometric Lab see page 100.

You can view isolux curves see page 150.

You can display Eulumdat file in two dimensions see page 151.

You can display Eulumdat file in three dimensions see page 151.

You can display Sollner curves see page 152.

Parameters of the Eulumdat Viewer

From General tab, you can set general information about the luminaire.

From Miscellaneous tab, you can set photometric parameters about the luminaire.

Light Output Ratio Luminaire is called LORL.

LORL = Output Flux / Lamp Flux

From Dimensions tab, you can set parameters about luminaire dimensions.

From Symmetry tab, you can set parameters about luminaire symmetry.

It is possible to choose symmetry properties when creating an intensity diagram or to add them on

an existing intensity diagram.

From Lamps tab, you can set lamps that can be used with the luminaire.

When editing the Total Luminous Flux value, the Do you want to preserve (cd/klm) values?

message appears.

The cd/klm unit is used in the Intensity tab.

LORL = Output Flux / Lamp Flux

R = Intensity / Lamp Flux

If clicking Yes, R is constant. If you change the Lamp Flux, the intensity changes proportionally.

LORL is constant. The intensity table and the LORL are not modified.

If clicking No, R is not constant and you keep a constant intensity. If you change the Lamp Flux,

the LORL changes. The intensity table and the LORL are modified.

From Direct ratios tab, you can set direct ratios values for the luminaire.

From Sampling tab, you can read sampling values of C planes and G angles.

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From Intensity tab, you can change intensity values in cd/klm for each sample.

From Luminance tab, you can change luminance values in cd/m².

From Edition tab, you can change options for printing the photometric report.

IESNA LM-63 Viewer

With IESNA LM-63 Viewer, you can process intensity data stored in IES file.

It can be used for all IES formats following the LM - 63 - 95 and previous standards.

Using the IESNA LM-63 Viewer


IESNA LM-63 Viewer.

-Or-

1. Click Iesna - LM63 .

A window appears.

You can create, open or save an IES file. In this case you can save your file as an .ies file.

When creating an IES file, you must select the photometric type, the horizontal symmetry and the

vertical angles.


By clicking File, Export ..., you can export an IES file as a XMP map file. For more details about

XMP map file, you can view Virtual Photometric Lab see page 100.


You can display IES file in two dimensions see page 151.

You can display IES file in three dimensions see page 151.

You can display Sollner curves see page 152.

Parameters of the IESNA LM-63 Viewer

From General tab, you can set general information about the luminaire.

From Tilt tab, you can set information about lamp position and its influence.

If selecting None, tilt has no influence on the lamp output.

If selecting Include, the lamp output varies as a function of the luminaire tilt angle.

You can Add Tilt Angle or Delete Tilt Angle .

In the Lamp to luminaire geometry box, you can select the lamp position in the luminaire.

From Miscellaneous tab, you can set photometric parameters about the luminaire.

In Number of Lamps box, you can type the number of lamps value in the luminaire.

In Lumen per lamp box, you can type the power value of the lamp.

This value is obtained from the manufacturer's technical data. It does not represent the lumens

emitted by the test lamp.

In Candela Multiplier box, you can type the multiplying factor to be applied to all Candela

values in the photometric data file.

In Input Watts box, you can type the consumption value of the lamp.

In Ballast factor box, you can type the Ballast factor value.


In Futur Use / Ballast lamp photometric factor box, you can type the futur use of the

Ballast lamp photometric factor value.

In the Photometry Type box, you can read the photometric type.

Type C is most of the time used for architecture and roadway. The polar axis coincide with the

vertical axis of the luminaire, and the 0-180° plane contains the luminaire major axis, the length.

Type B is used for adjustable outdoor area and sports lighting luminaire. The polar axis of the

luminaire coincide with the minor axis, the width of the luminaire, and the 0-180 degree

photometric plane coincides with the vertical axis of the luminaire.

Type A, not yet available, is used for automotive headlights. The polar axis coincide with the major

axis, the length of the luminaire., and the 0-180 photometric plane coincide with the vertical axis

of the luminaire.

From Dimensions tab, you can set parameters about luminaire dimensions.

Negative and null parameters give information about the shape.

In Luminous dimensions box, you can change luminous opening dimensions.

In Width box, you can type the distance value in feets across the luminous opening of the

luminaire as measured along the 90-270 axis.

In Length box, you can type the distance value across the luminous opening of the luminaire as

measured along the 0-180 axis.

In Height box, you can type the distance value across the luminous opening of the luminaire as

measured along the vertical axis.

In Units box, you can select Feet to use english units or Meters to use metric units.

In Luminous Shape box, you can read codes about luminous opening shapes (IESNA LM-63-

95):

WIDTH (W) LENGTH

(L) HEIGHT

(H) LUMINOUS SHAPE

0 0 0 Point

w l h Rectangular (default)

-d 0 0 Circular (d = diameter of circle)

-d 0 -d Sphere (d = diameter of sphere)

-d 0 h Vertical cylinder (d = diameter of cylinder)

0 l -d Horizontal cylinder oriented along luminaire

length

w 0 -d Horizontal cylinder oriented along luminaire

width

-w l h Ellipse oriented along luminaire length

w -l h Ellipse oriented along luminaire width

-w l -h Ellipsoid oriented along luminaire length

w -l -h Ellipsoid oriented along luminaire width

From Symmetry tab, you can read parameters about luminaire symmetry.

It is possible to choose symmetry properties when creating a new IES file.

From Data tab, you can set intensity data given in Candela for each sample.

You can Add Vertical Angle , Add Horizontal Angle , Delete Vertical Angle ,

Delete Horizontal Angle .

In Result tab, you can read maximum values for IES files.

Global Maximum is given with its position and Local Maximum for a given horizontal angle.

The IESNA LM-63 viewer gives you its position.

From Luminance tab, you can change luminance values in cd/m² or cd/ft² for each sample.

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OPTIS Intensity Viewer

With OPTIS Intensity Viewer, you can process intensity data stored in Optis intensity file and also

visualize Spectral intensity files in 3D.

Using the OPTIS Intensity Viewer


OPTIS Intensity Viewer.

-Or-

1. Click Optis Intensity .

You can create, open, save or import an Optis Intensity file

You can open, save or import a Spectral Intensity file.

When creating an Optis Intensity file, you must select the symmetry.

When opening a file, you can select an Optis intensity file in the .intensity or .int format, or a

Spectral Intensity file in the .spid format.

When saving an Optis Intensity file, you can save your file as a .intensity or .int file.

When importing an Optis Intensity file, you can select a SETFOS file. According to its content, the

SETFOS file is imported as a .intensity or.spid file.


By clicking File, Export ..., you can export an Optis Intensity file as a XMP map file. For more

details about XMP map file, you can view Virtual Photometric Lab see page 100.


You can display Optis Intensity file in two dimensions see page 151.

You can display Optis Intensity file in three dimensions see page 151.

Parameters of the OPTIS Intensity Viewer

When you open a Spectral Intensity file, you do not have to set theses parameters.

From General tab, you can set a luminaire description.

In Unit box, you must select the photometric or radiometric unit.

In the OPTIS intensity file, the third line corresponds to the unit type.

1 is for photometric units and 0 is for radiometric units.

From Symmetry tab, you can read parameters about luminaire symmetry.

In the OPTIS Intensity file, the fourth line corresponds to the symmetry used in the file:

0: no symmetry,

1: revolution symmetry,

2: symmetry about xOz plane,

3: symmetry about yOz plane,

4: symmetry both about xOz and yOz planes (symmetry in each quadrant).

From Data tab, you can set intensity data given in Candela for each sample.

You can Add Vertical Angle , Add Horizontal Angle , Delete Vertical Angle ,

Delete Horizontal Angle .



Curves

Isolux Curves

Displaying Isolux Curves

With Isolux Curve, you can view illuminance on a map for a light at a specified height, and isolux

curves at a specified height on a plane.

1. Click View, Isolux Curves.

-Or-

1. Click .

A window appears.

2. Se the parameters see page 150.

By clicking , you can export the isolux curve as a XMP map.

3. Click OK.

Parameters of Isolux Curves

Illuminance Unit gives the result unit.

In Distance box, you can type the distance value in meters between the lamp and the plane or use

the arrows to change it.

In Half map width box, you can type the map size value in meters or use the arrows to change it.

In Levels box, you can type the number of colors in the display or use the arrows to change it.

In Nb of points box, you can type the sampling value or use the arrows to change it.

In Unit group box, you must select the International or the US unit system.

In Display group box, you can select the Grid check box to display the grid.

You must select 2 D to give results as a map, or 3 D to gives results as a 3D shape.

From the Map along list, you must select the plane position.

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Polar Curves

Displaying Polar Curves

With Polar Curves, you can display the intensity data in two dimensions.

1. Click View, Polar Curves.

-Or-

1. Click .

A window appears.


3. Click OK.

Parameters of Polar Curves

With Polar Curves, you can display the intensity data in a plane containing the Oz axis, making a

defined C-angle with the xOz plane (C-angle).

In Series group box, you can select Fill check boxes to fill colored curves.

You can select View check boxes to display red or yellow curves that are at +90°.

With the top slider, you can modify the C-angle value for the blue curve of the first series.

With the bottom slider, you can modify the C-angle value for the green curve of the second series.

In Scale group box, you can select the Graduations check box to display graduations.

You can select the Auto scale check box to fit the display.

In Step box, you can type the graduation's sampling value in degrees.

From the Mode list, you must select a polar, cartesian or hybrid display.

From the Unit list, you must select the unit between Candela (cd) or Candela per kilo Lumens

(cd/klm).

You can select the Invert check box to create a top-bottom inversion of the display.

You can select the Link sliders check box to link sliders.

You can select Other distribution to change the distribution with Intensity, IES, Eulumdat, Optis

intensity or TL files.

3D Curve

Displaying 3D Curve

With 3D Curves, you can display the intensity data in three dimensions.

1. Click View, 3D Curve.

-Or-

1. Click .

A window appears.


3. Click OK.

Parameters of 3D Curve

You can rotate the image, translate zoom, display a wireframe view.


Display

You can select the View Shading check box to display a shading view of the intensity envelope.

You can select the View Mesh check box to display the intensity envelope with wireframe.

You can select the Decorations check box to display the 3D view tool.


You can select the Axis check box to display the axis.

You can select the Grid OXY, Grid OXZ or Grid OYZ check box to display standard planes grid.

You can select Shape to display the shape.

You can select Color to color.

You can click to display the level.

You can click to set 3D view preferences.

For more details, you can view 3D view see page 196.

Wavelength (nm)

When you open a Spectral Intensity file, the Wavelength (nm) group box appears.

You can use the slider to change the wavelength.

Displaying Sollner Curves

1. Click View, Sollner Curves.

-Or-

1. Click .

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A window appears.


Optical Design Viewers

Coupling Efficiency Viewer

The calculation model evaluates the coupling efficiency of a spatial coherent laser beam into a single

mode optical fiber.

This calculation model is included in the laser propagation module within OptisWorks software.

With Coupling Efficiency Viewer, you can evaluate the coupling efficiency by computing the deformation

of the laser beam in phase and amplitude.

This involves to model the real propagation of the electromagnetic field from the laser source to the

fiber, and to compute the overlap integral between the laser input beam and the fiber propagation

field.

The calculation of the incident electromagnetic field in the entrance plane of the fiber is given by the

laser propagation simulation.

An electromagnetic field in form of a sampling matrix of complex numbers is given. For more details,

you can view the OptisWorks User Guide.

Note that the calculation of the electromagnetic field is done in a perpendicular plane to the optical

axis, and this at the observation plane defined by the irradiance sensor.

Using Coupling Efficiency Viewer

1. From Start menu, click All Programs, OPTIS, OPTIS Labs, Viewers, Optical Design Viewers,

Coupling Efficiency Viewer.

A window appears.

2. Click .

A window appears.

3. Set the calculation parameters see page 153.

4. Click OK.

5. Set the parameters to calculate the coupling efficiency see page 155.

You can print the simulation results.

Calculation Parameters

With Calculation Parameters, you can evaluate the fiber mode.

The fiber mode is the transverse distribution function of the electromagnetic field guided by the optical

fiber.

The fiber mode can be defined from each point of the core and the cladding in a given transverse

section.

The field distribution in a transverse section is related to any other transverse sections by a simple

phase shift which depends on the propagation time.

The phase shift factor is

i is the field propagation constant in the optical fiber,

d is the distance between the two transverse sections.


The mode can be defined as a constant with an undetermined phase.

This undetermined phase does not step in the coupling efficiency but only in the phase shift of the

coupled field.

M(x,y) is the fiber mode in cartesian coordinates.

In Fiber parameters group box, you must select the fiber type.

The fiber mode is automatically calculated.

If selecting Gaussian Fiber, you must type the core index value and the radius value of the

fiber mode in microns.

Radius value is the radius value at 1/e² of energy distribution, or 1/e for the amplitude.

The fiber mode is supposed to be similar to a Gaussian function with a constant phase, equal to

zero.

The gaussian mode can be described by:

Most of the optical fibers respond well to this type of mode.

If selecting Step Index Fiber, you must type the core index value, the cladding index and the

core radius in microns.

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The fiber is defined by step index profile with a symmetric revolution. The step index fiber mode is

defined by the diameter of the core, the core index nc and the cladding index ng.

With these data, you can calculate correctly the fiber mode for the wavelength, under the condition

that such a mode exists.

The mode is determined from the resolution of the Helmotz equation. The result is given by the

following publication.

For more details, you can read Weakly Guiding Fibers : D. Glodge-APPLIED OPTICS/vol10, No

10/October 1971.

Following formula are defined:

a is the radius of the core

k = 2/. is the field propagation constant of the fiber

with nc>>ng

The Helmholtz solutions of the inner and outer field distributions of the core are:

J1 et K1 are the Bessel and Hankel functions of order 1 in cylindrical coordinates

In XMP File box, you can browse the XMP file used for the calculation.

Parameters of Coupling Efficiency Viewer

The calculation of the coupling efficiency needs the correct evaluation of the fiber mode.s

Data

In Data group box, you can type cleavage, tilt and offset values.

Result

In the Efficiency box, you can read the coupling efficiency value in percent.

When calculating the coupling efficiency:

M(x,y) is the fiber mode in cartesian coordinates.


E(x,y) is the incident electromagnetic field.

The coupling efficiency is the normalized overlap integral of these two functions or, in another way the

normalized scalar product of these two functions.

The M(x,y) and E(x,y) functions are known by the program in form of a matrix of sampled elements.

The form of the numerical approximation of coupling efficiency is given by:

(XF, YF) are the coordinates of the sampled field element (i,j) referred to the center of the fiber.

In Result group box, you must select the calculation mode to calculate the coupling efficiency.

When selecting Fiber / Source, the global coupling efficiency takes into account the

transmission of the optical system.

When selecting Fiber / Beam, the coupling efficiency is the one between the electromagnetic

field of the image space and the fiber mode.

It does not take into account the loss by diffraction, obturation or absorption in the optical system

In Unit box, you must select the unit between Percent and dB.

In Graph group box, you can select a graph.

You can save graphs as .txt or .xls files.

When selecting Tilt X or Tilt Y, you can display the coupling efficiency in function of the tilt

value for the X or Y direction.

The tilt of the fiber is equivalent to a change of the incident angle between the electromagnetic

field and the fiber.

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The incident field of the entrance plane of the fiber is multiplied by the following function:

l and m are the direction cosines in the sense of the x and y axis.

XF and YF are the coordinates in the entrance plane of the fiber.

The tilt of the fiber is a linear phase shift in the incident plane.

When selecting Offset X, Offset Y or Offset Z, you can display the coupling efficiency in

function of the offset value for X, Y or Z direction.

A transverse offset of the fiber in the x or y direction is equivalent to a transverse translation of the

fiber mode of the same quantity, but in the opposite direction.

When selecting Cleavage, you can display the coupling efficiency in function of the distance

from the exit surface to the observation plane.

The display of the graph can take some times because the wave front must be propagated.

The cleavage of the fiber means that the entrance surface of the fiber is not orthogonal to the fiber

axis.

As the same as for the tilt, the cleavage can be expressed by a simple phase shift of the

electromagnetic field.

You can find the field in the plane parallel to the entrance surface.

The phase shift factor is:

nc = core index

The cleavage of the fiber can be compensated by a tilt of the fiber, if the product of the two phase

shift functions is equal to 1.


By clicking Range, you can type the step number value and the range values used for each

calculation.

Gaussian Propagation Viewer

Using Gaussian Propagation Viewer


Gaussian Propagation Viewer.

A window appears.

2. Open a .txt file.

The simulation results appear see page 158.


-Or-

1. From the OptisWorks tree, double-click Result manager, Laser results, Gaussian propagation,

and then double-click a .txt file.



Parameters of Gaussian Propagation Viewer

You can read parameters of the Gaussian propagation for the source and for the result.

COLUMN DESCRIPTION

W0 (m) Gives the image beam waist diameter at 1/e². The image space is referred as the

space following the refracting surface of this line.

theta (rd) Gives the total beam divergence defined in the current surface material.

rel. pos.

(m)

Gives the position of the "Waist" defined in the current surface material. The

positive direction is the propagation direction of the light.

zr (m) Gives the actual Rayleigh length defined in the current surface material.

E (W) Gives the energy of the beam during the propagation.

F max

(W/m2)

Gives the irradiance in the intermediate material after the surface. It is the power

density in the waist, supposing a global emitted power of 1Watt. The power

density is given in Watts/m². This value has a great importance for the

propagation of a high energy laser beam.

Glass Map Viewer

With Glass Map Viewer, you can apply a particular glass coming from a manufacturer.

Materials contained in the Glass catalog data are available in the manufacturer catalogs.

Using Glass Map Viewer


Glass Map Viewer.

-Or-

1. Click .

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A window appears.


3. Click OK.

Parameters of Glass Map Viewer

In the Manufacturer list, you must select a manufacturer name from the list.

Available catalogs are ARCHER, CORNING, HOYA, OHARA, SCHOTT and SUMITA.

In the Glass box, you can select a material coming from glass manufacturers and corresponding

graphs appear.

The red curve is the index in function of the wavelength.

The blue curve is the dispersion in function of the wavelength.

Index is calculated with Sellmeier or Kettler - Helmotz equations belong to the manufacturer.

Sellmeier equation is the following:

Kettler-Helmotz equation is the following:

You can read constringence and dispersion values.

By clicking , you can display the index curve in function of the constringence.

Constringence values are given by the following formula:

nd: material index at 587.6 nm

nc: material index at 656.3 nm

nf: material index at 486.1 nm

By clicking Diagram, Secondary spectrum, or , you can display the dispersion curve in

function of the constringence.

Dispersion values are given by the following formula:

ng: material index at 435.8 nm

nf: material index at 486.1 nm

nc: material index at 656.3 nm

The ABBE line defines normal glass.

Glasses which are not on this line are very interesting to correct chromatism.

By clicking Diagram, Glass Map, or , you can display back the index curve in function of the

constringence

From the Manufacturers box, you can click to clear some manufacturers check boxes.

Only curves corresponding to selected manufacturers are displayed.

By clicking on a specific point, you can view the related values in the Current glass

characteristics box.

If you want to use the zoom, rotate the mouse wheel, click View, Activate zoom or click

and then click on the graph.


Clicking displays the original size.

When using a large zoom, the glass name is displayed near the point.

Paraxial Data Viewer

Overview

Paraxial Approximation at First Order

Compute paraxial characteristic of an optical system is the first step of optical design to understand

functioning of system and have rough idea of optical performance. Paraxial approximation is a way to

easily and quickly characterize Optical system.

Assumption

Paraxial assumption consists to propagate rays, which remains near optical axis. This assumption

means slope angle, angle of incidence and refraction angle in system approach to zero. Then angle

may be set equal their sines or tangents (first term of Taylor polynomial development):

in radian

One major consequences of this assumption is that trigonometric relation are conveniently transformed

in linear relationship. Rays are fully define by two parameters:

1. slope angle (angle between optical axis and ray),

2. height from optical axis to impact point on surface.

Aperture and Field Ray

This means for optical engineer that every ray passing through diopter has a behavior predictable from

a single linear combination of the two fundamental rays:

1. The aperture ray (AR) (also called marginal ray) starts from the point where object plane intersect

the optical axis (A) and goes through the entrance pupil at on its edge (P), defined by angle u and

height h.

2. The field ray (FR) (also called chief ray or principal ray) starts at the edge of the object-field (B)

and goes through entrance pupil at its center (Q), defined by angle v and height k.

Two cases can be differentiated to set initial aperture and field ray parameters:

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object finite,

Aperture Ray h= 0

u= 1/2 * total angular spread of beam

Field Ray

k= y (height of object)

v= y/x (ratio height of object on distance object

aperture)

object source infinite.

Aperture Ray h= (aperture radius)

u= 0

Field Ray k= 0

v= 1/2 * total field angle

Ray Tracing

The assumption at first order of paraxial rays simplifies greatly any tracing, due to the lack of

trigonometric formula. Any ray (H,U) crossing optical system can be considered as a linear combination

of aperture and field ray.

A coefficient is related to the weight of ray in object field, and B coefficient is related to the weight of

ray in pupil plan.

Knowing this relation, we are able to compute any ray in system, and also to determine by choosing

some specific ray parameters of system, as focal length, image, aperture and focal point localization,

usable pupils diameter.

An abundant literature covers question of paraxial optics and how to compute these paraxials figures.

Paraxial Table

To compute paraxial table is most of optical design first step, due to easiness to fully characterize an

optical system. In this kind of table, quantity h, u', k, v' are computed for each diopter.


From those first step, other figures are computing as third order aberration.

Primary or Third Order Aberration

Primary aberration is an extension of paraxial theory to higher order of polynomial development. Those

aberrations are related to polynomes of 3rd power. Study of these aberrations provide a first idea of

aberration in system, and can be evaluated with analytical equation.

Then primary aberration has the speed of computation for them, but must be complete with more

accurate aberration study method.

Assumption of Theory

For evaluation of third order aberration, only optical system with a revolution along optical axis are

considered.

We consider an optical system, with an object (AB), with a height of y. We consider ray coming outer

point of object (B), passing through optical aperture (s, and forming an image A'B'. Then aberration

of system can be described as a polynomial development:

This polynomial sum can be greatly simplified by considering assumption made on system:

Ray from object point on axis passing through optical point of lens (intersection of principal plan of

lens and the optical axis) has its image formed along optical axis. Then aberration A0 and B0 terms

are null.

Aberration polynomial of first order are also null, if we consider A'B' as paraxial image. Then linear

terms are just magnification of optical system.

In an axially symmetrical system, it can not have even order polynomial aberration, only odd order.

Then aberration development can be re-written as:

First aberrations, to appear in an axially symmetrical system, have power of third order. Then this

aberrations are named primary aberration or Third-order aberration.

In polynomial decomposition of aberration, higher the order of aberration is and smaller its effect will

be. Then to optimize an optical system, always smaller order must be minimized first.

Primary Aberration

Primary aberrations have been studied and classified for monochromatic light, by Ludwig Von Seidel

(1821-1896) in the 1850th. He determined that it exists only five primary aberrations and that they

could be computed with a combination of five polynomials :

Spherical aberration can be defined as focus variation with system aperture. This aberration

come from that an axial ray on edge of pupil are brought to focus faster than paraxial focus.

It exist the longitudinal (or axial) spheric aberration, which characterizes distance between paraxial

focus to an axial ray focus.

Spheric aberration can be described by its transverse magnitude. This value is called transverse.

This is distance, of an axial ray focus position from optical axis at paraxial focus plan position.

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In order to characterize maximum incidence on image of spherical aberration, transverse and

longitudinal aberration are given for margin ray of optical system.

Coma can be defined as magnification variation with system aperture.

Tangential coma is distance between point image of ray through the center of lens to point image

of upper and lower ray.

Image of point has appearance of a comet shape flare. Aberration names comes from this

particular shape.

Coma as far as it depends of field incident angle, coma aberration are evaluated at maximum

incident angle.

Curvature aberration can be defined as curvature of plan in order to have best focus point (or

least diffusion circle).

Curvature as far as it depends of field incident angle, curvature is estimated with maximum

incident angle.

Astigmatism aberration can be defined as best focus variation in function ray position on sagital

and tangential axis.

Astigmatism tangential or sagital is distance between least diffusion circle position and respectively

tangential or sagital focus point.


Astigmatisms are related to incident angle, then tangential and sagital astigmatism are computed

for maximum incident angle.

Distortion (D) can be defined as magnitude as displacement of image compared expected image

with paraxial calculation.

A regular square grid is deformed in pincushion when distortion has a value positive and barrel

when distortion has a negative value.

On left, image has a positive distortion (or pincushion), and right picture represents its opposite: a

negative distortion (or barrel).

Using Paraxial Data Viewer


Paraxial Data Viewer.

A window appears.


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-Or-

1. From the OptisWorks tree, double-click Result manager, Optical results, Paraxial, and then

double-click a .txt file.



You can click to calculate a Seidel sums.

Parameters of Paraxial Data Viewer

Wavelength

On Wavelength list, you can choose wavelength according to wavelength chosen in optical source.

Be careful to set correctly wavelength. Results in Paraxial table and Aberration of third order results

depends of wavelength considered.

Paraxial Table (First-order propagation)

Focal Length

Focal length value is computed by considering propagation of an input parallel ray to optical axis

(H=1, U=0), through diopters. Focal Length is distance between image principal plane and image

focal plane.

Focal length, in paraxial table, is given for an output surface (index i). Focal Length index i is the

effective focal length of the optical system from the its first diopter to its surfaces index i.

HeightA, AngleA,

These values refer to aperture ray traced through optical system from its first diopter and up to surface

index i.

HeightA is the height of aperture ray on surface i.

AngleA is the output angle of aperture ray on surface i.

HeightF, AngleF

These values refer to field ray (chief ray) traced through optical system from its first diopter and up to

surface index i.

HeightF is the height of chief ray on surface i.

AngleF is the output angle of chief ray on surface i.

Back Focal Length (BFL)

Back Focal Length (BFL) of an optical system is distance between the output surface of system to

focal point of system.

Back Focal Length, in paraxial table, is given for an output surface index i of system. Then BFL is

distance from output surface index i to focal point of optical system build considering diopter up to i

surface.

Seidel Coefficient

Click to display Seidel coefficients.

Coefficient display in Seidel windows are:


The fifth Seidel polynomials,

The contribution of the fifth primary aberration.

General expression of primary aberration is:

Primary aberrations are computed with Seidel polynomials. These relations are called Nijboer relations.

Lateral Spherical Aberration (S.A. lateral)

The lateral (or transversal) spherical aberration is computed with the first Seidel sum, according to

relation:

Axial Spherical Aberration (S.A. axial)

The axial (or longitudinal) spherical aberration is computed with the first Seidel sum, according to

relation:

Coma

Coma radius is related to second Seidel term.

Sagital Astigmatism (Delta Sag.)

Given by equation :

Tangential Astigmatism (Delta Tan.)

Given by equation :

Distortion

where SIII and SIV are the third and fourth sums of SEIDEL.

The displacement of the size of the image:

Distortion is displacement of image, related :

The distortion is in %:

l is the invariant of Lagrange.

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Real Aberrations Coefficients Viewer

Using Real Aberrations Coefficients Viewer


Real Aberrations Coefficients Viewer.

A window appears.




-Or-

1. From the OptisWorks tree, double-click Result manager, Optical results, Aberrations,

Aberrations coefficients, and then double-click a .txt file.



Parameters of an Aberration Coefficient Calculation

The real aberrations tab represents the same information than real aberrations graph.

For more details, you can view Real Aberrations Viewer.

The numerical aberration values are displayed in millimeters.

Eight families appear:

TRANSVERSAL COMA ASYMMETRY SYMMETRY

SAGITTAL CURVATURE ASTIGMATIS

M

DISTORTIO

N

Each function is characterized by the object position in the field and the intersection point in the

entrance pupil plane.

All the positions are expressed as normalized fractions of the total field and the total aperture:

central 0.0 the object point is situated on the optical axis

zonal 0.7 the object point is fixed at 0.7 of the total

field-of-view

marginal 1.0 the object point is fixed at the edge of the

field-of-view.

Knowing the significance ofzonal(Z) and ofmarginal(M) simplifies the association between the

aberration and its abbreviation.

Transverse aberrations TAM and TAZ.

y' is the intersection point of the ray in the image plane.

y'0 is the height of the ray passing through the center of the entrance pupil.

y'1 is the height of the ray passing through the entrance pupil at 0.7 of the pupil height.


y'2 is the height of the ray passing through the entrance pupil at the edge.

We use these points to define the following functions:

TAM = y'2 - y'0 TAZ = y'1 - y'0

Coma near the optical axes, COMAM and COMAZ.

y' is the paraxial image height of an object of height y. y'1 is the height of the ray from the object

centre to the edge of the pupil.

y''1 is the height of the ray from y passing the edge of the pupil.

We use these points to define the following functions.

The COMAZ function is exactly the same as COMAM with the ray passing at 0.7 of the pupil height.

Asymmetry and Symmetry

Ray at the Edge of the Pupil

Given the three rays from the point in the field passing through the centre and two edges of the pupil

we obtain the three intersections y'0, y'1 and y'3.

At the Field Edge: AEM and SEM

The asymmetry of the field is termed AEM and is defined as: AEM =

The symmetry at the field edge SEM is defined as: SEM =

At 0.7 of the Field (Zonal Field) AZM and SZM

The definition of AZM and SZM follow the same principle as the previous aberration but the rays start

from 0.7 of the total field. The asymmetry in the zonal field is termed AZM and is defined as: AZM =

Similarly we define the symmetry in the zonal field (SZM) as: SZM =

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Ray at 0.7 of the Pupil Height

Given three rays defined by the starting point in the field and passing the center of the pupil and the +

and - 0.7 pupil heights, we obtain the three impact points y'0, y'3 and y'4.

At Edge of Field: AEZ and SEZ

The asymmetry at the edge of the field is termed AEZ and is defined as: AEZ =

Then we define the symmetry at the edge of the field by the function SEZ: SEZ =

At 0.7 of the Field (Zonal Field) AZZ and SZZ

The AZZ and SZZ functions are exactly the same as AEZ and SEZ with the ray starting from 0.7 of the

total field. The asymmetry in the zonal field is termed AZZ and is defined as: AZZ =

Then we define the symmetry in the zonal field as: SZZ =

Sagittal Aberrations

The Sagittal aberrations are defined by moving the object from the y axis and also moving the

intersection point in the pupil from the x axis.

We obtain an intersection point with the coordinates (x',y').

The x' value allows us to define the following functions: XEM = x' for the edge of the field and the edge

of the pupil XEZ = x' for the edge of the field and 0.7 of the pupil height. for the zonal filed and the

pupil edge XZZ = x' XZM = x' for the zonal field and 0.7 of the pupil height.

Distortion

y' is the image of the paraxial object y.

y' is the intersection of the field ray with the image plane.


Distortion values are : Marginal Distortion: for DISTM = y'1-y the total field Zonal Distortion: for DISTZ

= y'1-y 0.7 of the total field.

Astigmatism and Curvature

Astigmatism and curvature functions are defined by variations of the field ray. The variations are made

at the pupil. Variations in dy give the tangential functions and variations in dx give the sagittal

functions.

Tangential Field Curvature

This is defined by a variation dy across the pupil. These functions are defined by:

Edge of field: TFCM =

At 0.7 of field height: TFCZ =

Sagittal Field Curvature

This is defined by a variation in dx across the pupil. The functions are defined as:

Edge of field: SFCM =

At 0.7 of the field: SFCZ =

Astigmatism

The astigmatism functions are defined by the difference of TFC and SFC. We obtain the expression:

ASTM = TFCM - SFCM ASTZ = TFCZ - SFCZ

Conclusion

Each of the these functions gives important information about the optical system quality based on the

specified criteria. These definitions are essential to evaluate the performances of the optical system.

Real Aberrations Viewer

Using Real Aberrations Viewer


Real Aberrations Viewer.

A window appears.




-Or-

Viewers of 207

1. From the OptisWorks tree, double-click Result manager, Optical results, Aberrations,

Aberrations, and then double-click a .txt file.



Parameters of Transverse Ray Aberrations Viewer

Overview

Transverse ray aberration viewer shows ray aberration as function of pupil coordinate.

X' component of transverse ray aberration in function of X position on pupil are build by launching a

fan ray along X-axis (sagital ray). Y’ transverse aberration contribution are computed by launching a

ray fan along Y-axis.

The plotted data is the distance between the ray intercept coordinate and the chief ray intercept

coordinate. Plotted data in graph are function of ray position pupil. If many wavelengths are selected,

then each plot is referenced to their chief ray position.

Axis definition :

The horizontal axis for each graph represents the normalized and oriented entrance of pupil

coordinate (1 represents the total radius of the pupil).

The vertical axis scale is given at the right side of viewer, and are expressed in µm.

Field

Field list allows to select the percentage of field from which the plotted data are calculated.

Automatic Window Size

Diagram is auto-scale in order to visualize fully plotted data, no matter what the selected field is. An

option is provided in order to scale manually spot diagram:

1. Click to clear Automatic window size.

2. Enter the scale in microns of the plot (Value max - value min) in the scale box.

3. Click Update to apply new scale.


Spot Diagram Viewer

Using Spot Diagram Viewer


Spot Diagram Viewer.

A window appears.

2. Open a .ray file.



-Or-

1. From the OptisWorks tree, double-click Result manager, Optical results, Spot Diagram, and

then double-click a .ray file.



Parameters of Spot Diagram Viewer

The spot diagram gives the position (x, y) of the various ray impacts in an analysis plane defined by its

position z on propagation axis.

Wavelength

In the Wavelength list, you can select or unselect Wavelength ALL to see the impacts of the image

spot or just the impacts from one selected wavelength, which expressed in nanometers (nm).

Field

With the Field list, you can center spot diagram on image spot of selected percentage field.

Automatic Window Size

Diagram is auto-scale in order to visualize all ray impact of selected field in same window.

An option is provided in order to scale manually spot diagram.

You must click to clear the Automatic window size check box, in the Scale box, you must type the

amplitude value in µm spot of diagram full scale (Value Max. -Value Min.), and then you must click

Update to apply new scale.

Best Focus

Energy

The proportion of ray impacts to consider best focus search.

100% means that all ray are taken into account.

80% means that calculus take in account 80 % impacts ray from all, which have the smaller radius.

RMS /GEO

With the RMS/GEO list, you can set method used in order to look for best focus.

If you click RMS, the best focus radius is evaluated with the root mean square of all impact radius

from middle point.

If you click GEO, the best focus radius is evaluated with the average of impact radius. In this

method only impacts with smaller impact radius is taken into account. Proportion of impacts to take

in account is set in field Energy.

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Local Best Focus

If you click Local Best Focus, the viewer looks for position on propagation axis which minimizes spot

radius for selected field.

In case of a multi-wavelength spot diagram, if Wavelength ALL is selected, Local Best Focus is

equal to the barycenter of the Local Best Focus from each wavelengths regarding the wavelengths’

weights from the optical source definition.

Spot diagram is updated in order to display the best local spot. Then analysis plan position is offset

along optical axis according to distance find with Local Best Focus algorithm.

Global Best Focus

If you click Global Best Focus, the viewer looks for position on propagation axis and considering all

fields. Global Best Focus is equal of barycenter of the Local Best Focus from each fields regarding the

fields’ weights from the optical source definition and taking the same selected wavelengthIn case of a

multi-wavelength spot diagram, Global Best Focus minimizes spot diagram radius without taking into

account wavelength. All spot impact are bundle, without prior consideration of wavelength.

Spot diagram is updated in order to display the best global spot. Then analysis plan position is offset

along optical axis according to distance find with Global Best Focus algorithm.

Sensor Offset

Position

Position value is the offset applied to analysis plan position from initial detector position set in CAD,

along propagation axis of the system.

Step

You can check evolution of spot diagram along propagation axis. Step value is the offset applied from

previous position for each click.

Upper arrow shifts sensor of Step value toward higher Z position value (detector goes further from

optical system).

Bottom arrow shifts sensor of Step value toward lower Z position value (detector comes further

from optical system)

Spot Data

Center X

It is x coordinate of spot diagram middle point. Middle point is the mean of x-coordinate maximum and

x-coordinate minimum. If you selected Wavelength ALL, all impacts without wavelength restriction,

are considered to calculate Center X.

This value is used to center spot diagram.

Center Y

It is y coordinate of spot diagram middle point. Middle point is the mean of y-coordinate maximum and

y-coordinate minimum. If you selected Wavelength ALL, all impacts without wavelength restriction,

are considered to calculate Center Y.

This value is used to center spot diagram.

RMS radius

RMS radius is the root of mean of the square radius of all ray impact for selected field. RMS radius is

computed by considering a circle centered on middle point. If you selected Wavelength ALL, all

impacts without wavelength restriction, are considered to calculate RMS radius.

GEO radius

This value is radius in order to encircled of all ray impact for selected field. GEO radius is computed by

considering a circle centered on middle point. If you selected Wavelength ALL, all impacts without

wavelength restriction, are considered to calculate GEO radius.


Airy Radius

This value is the radius of diffraction spot. This is the minimal spot radius that we can reach in an

optical system.

If you selected Wavelength ALL, this value is computed for the barycenter of the wavelengths

regarding their weights from the optical source definition.

Geometric MTF

Frequency X

Frequency X is the spatial frequency in which Geometric MTF drops to 20% for first time along X-axis.

Frequency Y

Frequency Y is the spatial frequency in which Geometric MTF drops to 20% for first time along Y-axis.

GEO Radius VS Disfocusing Viewer

Click to display GEO Radius VS Disfocusing curve.

This is the radius computed which is encircled 100% along optical propagation axis.

Axis definition:

X-axis : offset of sensor position from current position displayed in spot diagram. Then zero

position correspond to current sensor position in spot diagram. Sensor position is express in

millimeters.

Y-axis : GEO Radius displayed in µm.

GEO radius is computed with middle point of Spot and considering number of ray impact.

If you selected Wavelength ALL, all impacts are bundle, without prior consideration of

wavelength.

Encircled Energy Viewer

Click to display Encircled Energy curve.

This viewer displays radius in function of encircled energy proportion considered. For example, in curve

below, there is 80% of Energy in a circle with a radius about 130µm.

Axis definition:

X-axis : Proportion of Encircled Energy.

Y-axis : Radius in which proportion of energy is encircled.

Radius of Encircled Energy is computed with middle point of Spot and considering number of ray

impact.

If you selected Wavelength ALL, all impacts are bundle, without prior consideration of

wavelength.

Viewers of 207

Geometric MTF viewer

Click to display Geometric Viewer.

The Modulation Transfer Function MTF is image contrast of light and dark bars test chart in function

of object spatial frequency. This test chart is composed by equally spaced light and dark bars, which

follow a sines relation. Pitch (or spatial frequency) between light and dark bars is expressed a certain

number of lines per millimeter.

MTF gives contrast response against frequency to a spatial stimulation . As far as optical systems have

aberrations, line image will tend to mix with the other nearest lines images. Then lines images will tend

to blur according to pitch between them. This function then allow to discern limit of resolution.

MTF is time to time referred as frequency response or sine wave response or contrast transfer

function.

MTF plot against frequency is thus an universal measurement of optical performance, which could be

applied on a great amount of optical systems: image-forming, lenses, films, camera... One convenient

characteristic of MTF is that MTF of optical combination can be calculated by multiplying MTF of each

component.

As far as you use geometrical ray propagation to compute MTF, GEO MTF is only valid is if spot radius

is bigger to 10 times of the Airy radius.

Axis definition:

X-axis : spatial frequency expressed in number of lines per millimeter.

Y-axis : Contrast figure.

Curves legend:

Curve with blue cross is the MTF computed by considering only diffraction aberration. This curve

is the theorical performance of an optical system. On example above, this curve is on top of graph.

Curve with green dots is MTF computed with spot spread function along X-axis.

Curve with blue dots is MTF computed with spot spread function along Y-axis.

If you selected Wavelength ALL, MTF due to diffraction (curve with blue cross) is evaluated by

taking the barycenter of the wavelengths regarding their weights from the optical source definition.

If you selected Wavelength ALL, each impact is bundled regarding its wavelength’s weight from

the optical source.


RAY FILE TOOLS

Source Generator

With the Source Generator, you can create .ray files for different type of sources.

Using the Source Generator

1. From Start menu, click All Programs, OPTIS, OPTIS Labs, Ray File Tools, Source Generator.

A window appears.

You can edit, load or save a source. In this case you can save your source as a .sou file.

2. Select the source type you want to create.

A window appears.


4. If needed click Position/Orientation.

Some sources, such as the arc lamp, can be translated and rotated.

A window appears.


6. Click OK.

If needed, you can select Save Rays to load light rays (.ray file).

Parameters

Parameters of Optical Fiber

Geometry/Fiber Type

By selecting Step index fiber, a disk with a uniform spatial radiant exitance distribution

approximates the source.

The diameter for the disk is defined as the fiber core diameter.

The angular distribution is a Gaussian distribution.

The half angle q of the divergence at 1/e² is given by: sin(q)=NA

NA is also known as the numeric aperture of the fiber.

By selecting Gradient index fiber (gaussian), a disk approximates the source with a Gaussian

distribution for the radiant exitance.

The diameter at 1/e² is defined as the fiber diameter.

The angular far field distribution is also a Gaussian distribution.

The half angle q of divergence at 1/e² is defined as: sin(q)=NA

NA is also known as the numeric aperture of the fiber.

By selecting Gradient index fiber (quadratic), the source is approximated by a rectangle with a

Gaussian distribution for the radiant exitance.

The definition is similar to the one above.

Emittance

In the Diameter at 1/e² of box, you can type a diameter value in microns.

Ray File Tools of 207

Intensity

In the Sine of half angle of box, you can type a sine value.

Energy

In the Radiant flux in box, you can type the radiant flux value in Watt.

Spectral Range

In Spectral Range group box, you can click Spectrum.

For more details, you can view Parameters of Spectrum see page 183.

Parameters of LED

A disk having an uniform emittance approximates the source.

A Gaussian distribution approximates the intensity distribution.

This model may be used as a first approximation to simulate a LED with a collimating optical system.

But there is also a more accurate way to simulate the LED where a more explicit description of the far

and near fields is needed.

The LED should thus be modeled as a Lambertian emitter and the collimating system can then be

directly entered in the editor.

The example file LED.SOP is an explicit simulation of a Light Emitting Diode by a Lambertian source

with the collimating optical system.

The Lambertian source enables you to take into account the emittance variation of the emitting surface

of the LED.

For more details about the Lambertian source, you can view Parameters of Lambertian Source see

page 178.

The radius and the distance from the Lambertian source to the lens surface can be found in the

technical documentation of the LED.

Emittance

In the Beam Diameter at 1/e² box, you can type a beam diameter value in millimeters.

Intensity

In the Total angle divergence at 1/e² box, you can type a total angle value in degrees.

Energy


Spectral Range




Parameters of Lambertian Source

A Lambertian surface is such that the intensity of the light emitting surface in a given direction is

proportional to the cosine of the normal's angle to the surface.

The brightness (luminance, radiance) of a Lambertian surface is constant regardless of the angle from

which it is viewed.

Geometry

The Lambertian source is a flat source which can have a rectangular or elliptical shape.

In Geometry box, you can select Ellipse or Rectangle.

You must type the Size X and Size Y values in millimeters.

The emittance distribution is uniform. If you want to simulate non uniform emittance distribution, refer

to the user defined sources.

For more details, you can view Parameters of User Defined Source see page 180.

Intensity

The intensity distribution is always Lambertian which means proportional to the cosine of the normal

angle of the surface.

In the Half-angle of emission box, you can type a half-angle of emission value in degrees.

Within the emission angle, rays are emitted and no rays are emitted beyond this limit angle of

emission.

The advantage of the definition of the emission angle is a speed gain in the computation time: why

should a ray be emitted in a direction where they are absorbed in any case.

Energy


The energy value fixes the radiation flux emitted in the cone defined by the emission angle.

Spectral Range




Parameters of Multimodal Laser Diode

Geometry

The source is represented by a flat rectangle which may have different dimensions in the x and y

directions.

In Waist Diameter in X and Waist Diameter in Y boxes, you must type values in millimeters.

Emittance

The emittance distribution is either uniform or Gaussian in the x and y directions.

Both directions may have different distributions.

In Emittance boxes, you must select gaussian or uniform.

Intensity

The angular distribution is always Gaussian.

You must type the total divergence angle values of the Gaussian curve at 1/e² of its maximal intensity

value.

The divergence angle may be different for the x and y directions.

Energy


Spectral Range



Parameters of Black Body

A Black Body is an object which does not reflect any electromagnetic radiations at any wavelength.

The radiance from a black body is the radiance from a system in thermodynamic balance, defined by

its temperature.

This source is a particular case of a Lambertian source and is characterized by its temperature and

shape.

This source model is suitable for most thermal sources.

The black body is totally defined by following parameters concerning its spectral distribution and the

emitted radiation flux.

Geometry

In Geometry group box, you must select ellipse or rectangular, and you must type size values in

millimeters to define the extension in both directions.

Emittance

The emittance is uniform.

Intensity

The intensity distribution is Lambertian.

The half angle of emission fixes the angle in which the rays are emitted


You must type the half angle of emission value in degrees.

Energy

In the Energy group box, you can type the temperature and emissivity values.

The energy emitted by a black body is defined by its temperature and its emissivity. A perfect black

body has an emissivity of 1.

Lambda max is the Lambda maximum of the emitted spectrum.

The wavelength is for which the spectral emittance is maximal.

The wavelength may be calculated by Wien's Displacement Law in the following way:

lmax = k1 / T

with k1 = 2898 mm.K

where T is the temperature in Kelvins

Total power and used power are the radiation emitted in 2p (half space) which is given for the

chosen spectral range and for all wavelengths from the defined black body.

The indicated values take care of the emissivity.

The used power indicates the amount of radiation effectively emitted in the cone defined by the

half angle of emission.

The radiation values are calculated by Plank's Radiation Law and by the Stefan-Boltzmann's Law.

Spectral Range

The spectral distribution is defined only by the temperature.

In Spectral Range group box, you can type the Lambda and number of samples values.

Lambda min is the Lambda min which define the smallest wavelength of the spectral range used for

the simulation.

Lambda maxis the Lambda max which set the longest wavelength of the spectral range.

Number of samples sets the number of samples used for the simulation.

The maximal number of wavelength samples is 100.

Parameters of User Defined Source

Light sources are very often defined by their physical and geometrical characteristics.

The intensity distribution as well as the emittance distribution are defined by a limited number of

general parameters.

With user defined sources, you can define the source characteristics (emittance and intensity

distribution) by numerical distribution.

You can define non-symmetrical sources or sources, which have characteristics, which are not covered

by the other more generally defined sources.

An increase in the computing time is a consequence of the more general definition possibilities.

In order to optimize an optical system for photometric performances, you should use the basic and

faster source models first.

Only the final step in optimization should be done with the user defined source model.

Another possibility is to use the Saved Rays option to save computing time.

Geometry/Emittance

In Geometry/Emittance group box, you must select a geometry for the source, which defines the

near field.

Intensity

In Intensity box, you must select the intensity distribution (the far field) characteristics of the light

source.


Each intensity distribution may be combined with any of the geometries presented here.

Energy


The radiant flux represents the flux which is emitted in the angle defined by the intensity distribution.

Spectral Range



Parameters of Incandescent Lamp

With the incandescent lamp, you can define the same shapes/volumes of extended sources.

An incandescent lamp emits light when an electric current passes through a filament, which is situated

in a vacuum tube.

Rays are emitted from the surface.

The surface emission determines the far and near field characteristics of the lamp according to the

shape of the wire.

The spectral distribution is the distribution of a black body given by the wire temperature.

Geometry

The geometry of the lamp is defined in a special geometry editor.

Emittance

In the Half-angle of emission box, you can type a value in degrees.

The emission angle is the angle between the optical axis and the maximal emission direction of the

rays.

No ray is emitted in a direction outside of the cone defined by the half angle of emission.

Furthermore, the radiation flux is related to this cone: all radiation flux will be emitted in this cone.

Energy


The radiation flux is defined in radiometric units and then automatically translated into photometric

units.

Spectral Range

In Spectral Range group box, you can type the Lambda, number of samples and temperature values.

The spectral distribution is the distribution of a black body at a defined temperature.

The spectral range is then fixed by the maximal and the minimal wavelengths.

The number of samples fixes the sampling rate for the spectral distribution.

The spectral distribution of a black body is only a suggested distribution, which satisfies a huge number

of applications.

Nevertheless, the user can redefine the spectral range as well as the spectral distribution.



Parameters of Fluorescent Lamp

A Fluorescent lamp is for instance, a tube containing mercury vapor and lined with phosphor. When a

current passes through the gas, visible light is emitted from the vapor.

In consequence, the rays are emitted from the volume and not only from the surface, as is the case for

incandescent lamps.

The volume emission determines the emission characteristics of the light source according to the shape

of the tube.

Geometry

The geometry of the lamp is defined in a special geometry editor.

Emittance

In the Half-angle of emission box, you can type a value in degrees.

The emission angle is the angle between the optical axis and the maximal emission direction of the

rays.

No ray is emitted outside of the cone defined by the half angle of emission.

Furthermore, the radiation flux is related to this cone: all radiation flux will be emitted in this cone.

Energy


Spectral Range


The spectral distribution depends on the gas used in the tube.


Parameters of Arc Lamp

With the arc lamp, you can simulate an arc lamp defined by the geometry of the electrode and a single

radiance distribution measurement, assuming that the arc has a revolution symmetry.

The model also takes into account multiple scattering on the electrodes.

As an example of an arc lamp, just load the example lamp called ARCLAMP.SOU.

Geometry

The arc lamp is defined by the geometry of its electrodes and the radiance distribution in a plane

normal to the direction defined by the axes of the revolution symmetry.

The geometry of the electrodes is given by the supplier as well as the radiance distribution of the arc

itself.

In the case where the radiance data are not known, the radiance distribution may be easily found by

the following experiment:

Take a picture of the arc lamp and find the iso-level-curves of the arc. This can be done manually on

the picture itself or, more sophisticatedly, by image processing.

The position and the orientation of the arc lamp can be defined in the general lamp definition dialog

box.

The emittance distribution inside of the arc is calculated from the radiance distribution by a

mathematical transformation, which is accurate under the hypothesis that the arc has a revolution

symmetry.

Energy



Wavelength

In the Wavelength box, you can type the lambda value in nanometers.


Luminance

In the Luminance group box, you can type number of layers value.

Parameters of Spectrum

Spectral Range

In Spectral Range group box, you can type Lambda min and max values in nanometers.

You can type samples value.

Wavelength Distribution

In Wavelength distribution group box, you can select the wavelength distribution.

Parameters

In Temperature box, you can type the temperature value in Kelvins.

You can load or save spectrum data.

Parameters of Position and Orientation

Position of the Source Center

In x and y boxes, you must type values in millimeters to set the center position of the light source x,

y, z, related to the local reference system.

Orientation of the Source

In the l, m and n boxes, you must type values to define the orientation vector.

l = cosa

m = cosb

n = cosg

The angles are the cosine directions of the axis of the light source and the local reference system.


Post-Processing

Intensity Distribution Post-processing

With the intensity distribution post-processing, you can calculate intensity from rays files.

The intensity data are stored in an IES, Eulumdat or OPTIS intensity format file.

Only one simulation has to be ran as it is using rays files.

Using the Intensity Distribution Post-processing

You must have created a ray file using irradiance / illuminance simulation.

1. From Start menu, click All Programs, OPTIS, OPTIS Labs, Ray File Tools, Post-Processing,

Intensity Distribution Post-processing.

A window appears.

2. Load the .ray file used to calculate the intensity.

Rays file size is the size of the rays file.

Number of rays is the number of rays in the rays file.

Radiant flux is the total flux of rays contained in the rays file.

Luminous flux is the total flux of rays contained in the rays file (visual intensity). You can select or

click to clear the Luminous flux check box.

Ray file date is the date creation of the rays file.


4. Click to calculate the intensity file.

A process dialog box appears.

At the end of the calculation, the precision of maximum value in percent appears.


Parameters of the Intensity Distribution Post-processing

Final Intensity Distribution File

In the Final intensity distribution file group box, you must select the export format in which you

want to save intensity data.

You can browse the file.

Sampling

In Sampling group box, you must select the sampling type.

When selecting Uniform, you can type the B-Plane sampling, B-Angle sampling, C-Plane sampling

or G-Angle sampling values.

C-Plane sampling is the number of sample in the C-plane (xOy).

C-Plane step is as following:

G-Angle sampling is the number of sample from the Oz axis.


G-Angle step is as following:

B plane sampling must be an odd value.

When selecting Adaptive, you must browse a .txt file containing C-Plane and G-Angle definitions.

You can view examples in ..\OPTIS\Standards\Photometry\Intensity Distribution.

Export Parameters

In Integration angle box, you can type the integration angle value in degrees.

The flux is calculated as the average flux around the direction in a cone which is defined by the

integration angle.

In Lamp luminous flux, you can type the lamp luminous flux value in lumens.

By default, it is equal to the rays file total flux.

The value is written in the IES file.

XMP Map Post- processing

With XMP Map Post- processing, you can compute irradiance, radiance and Cartesian intensity maps by

using rays files.

The propagation of rays is made only once while rays file is creating.

To help you orientate your map easily, the normal is defined by the center of the map and a second

point outside the map.

Using the XMP Map Post- processing

You must have created a ray file using irradiance simulation.

1. From Start menu, click All Programs, OPTIS, OPTIS Labs, Ray File Tools, Post-Processing,

XMP Map Post-processing.

A window appears.

2. Load a .ray file

Rays file size is the size of the rays file.

Number of rays is the number of rays in the rays file.

Radiant flux is the total flux of rays contained in the rays file.

Luminous flux is the total flux of rays contained in the rays file (visual intensity). You can select or

click to clear the Luminous flux check box.

Ray file date is the date creation of the rays file.

3. Click to edit map properties.

A window appears.

For more details you can view Parameters of the Map Properties see page 185.

4. Validate.

5. In case of a radiance/luminance map, you can type a value in degrees for the integration angle.

For more details you can view Integration Angle see page 187.

6. Click to calculate the intensity file.

A process dialog box appears.

Parameters of the Map Properties

You must select the map type between Basic map and Spectral map.


For more details about precision, you can view Reading Precision see page 111.

From Values list, you must select the map type.

From Unit list, you must select the unit.

For irradiance / illuminance map, you must define the position of the map as well as a second point

which indicates the normal.

For radiance / luminance map, as in any usual luminance simulation, the main parameters are the view

point, the position of the map and its orientation.

For radiant intensity / luminous intensity, only the orientation is important.

In Position group box, you must type the position values of the map in millimeters.

In Axis Theta 0 group box, you must type the axis theta 0 values.

In Orientation group box, you must type the psi angle value in degrees.

Phi angle defines the orientation of the map around its axis.

In Point at group box, you must type the point at values in millimeters.

In Observer group box, you must type the view point values in millimeters.

In Vector Phi 0 group box, you must type the vector phi values.

In Size and sampling group box, you must define the size and the sampling of the map.

In Wavelength group box, you must define the wavelength sampling.

Information about each wavelength sample is stored in the map.

In Intensity type box, you must select the cartesian intensity map type.

Optis type is not limited with orientation.

X As Meridian, Y As Parallel and X As Parallel, Y As Meridian types are adapted for SAE

automotive regulations.

The following images show differences between these maps.

The source is a small disk which emits in a cone.

Each map shows the projection of the cone on the hemisphere.

According to the type of map, you can see some deformation of the projection of the cone on the

map.

OPTIS map type SAE type A map type SAE type B map type

You can select the Data separated by layer check box.

In Filename box, you can define the name and the location for the final XMP map file.


Integration Angle

All the rays of the integration area whose angle with eye direction is smaller than this integration angle

are taken into account.

All of the rays inside this cone are taken into account.

This set of maps is obtained with different integration angle, in order to show the influence of this

parameter on the resulting map.

The integration area radius is maintained constant

Integration angle = 35 Integration angle = 25 Integration angle = 20 Integration angle =

17.5

Integration angle = 15 Integration angle = 10 Integration angle = 5 Integration angle = 2

Integration angle = 1 Integration angle =

0.5

Integration angle =

0.2


You note that the maps could be split in two parts:

From an integration angle of 35° to 15°, maps contain almost no noise, but the average level if

radiance decreases with the value of the integration angle.

From an integration angle of 15° to 1°, maps contain as many noises that the value of the

integration angle is small and the average map level is constant.

These results could be explained by doing an intensity map.

The intensity map shows that the flux is emitted in a 15° degree angle cone, which is conform with the

source parameter defined in the geo file.

When the integration angle is greater than the emission angle all the flux is collected by the virtual

measurement.

If the integration cone decreases, keeping greater than the emission angle, the level of radiance grows

as the flux is constant.

When the integration angle is smaller than the emission angle the collected flux by the virtual

measurement is proportional to the size of the integration cone, so the radiance level is constant.

Moreover, as the number of rays collected is proportional to the integration angle, the map becomes

noisy for very small integration angle.

As a conclusion, there is no absolute law to determine the better value for the integration angle.

It is often obtain after different trials and with your knowledge of the system.

Often an intensity map could be very useful to choice the better integration angle.

Radiance levels strongly depend of the choice of the integration angle. The results of the post-

processing of radiance must be considered with a physical interpretation and never took as is.

Ray File Editor

With Ray File Editor, you can:

View the details of a .ray file.

Modify the power or the spectrum of a .ray file.


Display the spectrum of a .ray file.

Repair an invalid .ray file.

Add two .ray files.

The relative power of ray and the new power of the resulting .ray file are automatically computed.

Mix all the ray in the .ray file.

Invert directions of ray.

Import or export (ASCII format).

Import Radiant and ASAP ASCII .ray file.

Import TechnoTeam source file (.erf files).

Import ASAP DIS ray file (.dis file).

Import a list of .ray files (.rayfileslist file).

To import a set of ray files in one step, you must create a .txt file listing the names of each file to

be imported.

Set the relative energy of each ray to 1.0.

Recompute the relative energy of each ray.

This divides all relative energy by the maximum.

Maximal Ray number value is 72 million rays.

Using the Ray File Editor

1. From Start menu, click All Programs, OPTIS, OPTIS Labs, Ray File Tools, Ray File Editor.

A window appears.

2. Click File, Open..., or to browse a .ray file.

You can import see page 189 or export see page 190 files.

You can use data downloaded from OSRAM Opto Semiconductors see page 190.

By clicking Edit, Repair or , you can repair a ray file.


You must save each .ray file.

You must take care not to overwrite .ray files as you might need the basic one for a different

binning and thus different emission.


Importing and Exporting

Importing a File

1. Click File, Import... or click .

2. Browse to select a file.

FILES EXTENSIONS

Text .txt

Rayset ASCII .asap, .out

Radiant ASCII .radiant

Technoteam Ray .erf

DIS Ray .dis


FILES EXTENSIONS

Ray Files List .raysfileslist

For more details about Radiant ASCII format, you can view Importing Radiant Imaging Files see

page 190.

3. Click Open.

A window appears.

4. Save the file as a .ray file.

5. Click Save.

Importing Radiant Imaging Files

Radiant imaging files have .rs7 or .rs8 extension.

From ProSource you must generate rays in the Lightools rayset format.

You must then export a ray file from ProSource compatible with SPEOS.

A ProSource licence is required to use ProSource or ProSource dlls.

1. Rename the Lightools .ray file as .radiant.

2. From the Ray File Editor, click File, Import... or click .

3. Browse to select a Radiant ASCII file.

RayEditor also imports the power of the Radiant Imaging source as it is included in the .radiant

file.

4. Click Open.

Exporting a File

1. Click File, Export... or click .

2. Type a file name.

3. Select a format.

FILES EXTENSIONS

Text .txt

DIS Ray Files .dis

4. Click Save.

The conversion is processing.

Using Data Downloaded from OSRAM Opto Semiconductors

1. Log on the OSRAM Website.

2. Download the library of OSRAM Ray Files.


In the downloaded Zip, you can find:

The orientation of the .ray file (PDF or JPEG),

The geometry of the optical system (STEP, IGES, SLDPRT) with the same global orientation as the

.ray files,

.ray files with different sizes (100k, 500k, 5M).

Content of the zip – Monochromatic source emission

For white LED, you find a blue and a yellow portion of the final .ray file.

To model correctly the LED emission, these two .ray files need to be prepared separately and then

put together.

Content of the zip – White source emission

3. Define the LED type if you are going to use sources with a narrow, monochromatic spectrum, or a

white light.

In case of using a source with a narrow spectrum, you can directly create a ray file source in the

OPTIS software.

You must use a support geometry as 1 point - 2 lines to create the Ray File Source in the software

respecting the orientation given for the .ray file (PDF or JPEG in the ZIP).

In SPEOS Standalone, you have to create a surface whose vectors I and J give the direction of the

ray file source.

In OptisWorks and SPEOS CAA V5 Based, only two lines are needed.

In case of using white light, it is first necessary to use the Ray File Editor and to prepare the

.ray file that will be used for the .ray file source.

For the white LED, you find two .ray files, one for the blue and one for the yellow emission.

Both have their corresponding spectrum and the typical flux already given.

To create the final .ray file it is necessary to adjust the power of both components.

4. From the Ray File Editor, open one of the yellow .ray files (100k, 500k, 5M).

If needed, you can adjust the power of the single .ray file, each for the blue and the yellow

portion, according to the designated emission (see therefore the PDF provided by OSRAM).


The default value for the power is the standard value given in the PDF of the zip folder. This value

must be adjusted according to the binning that will be used.

Both, blue and yellow part of the final .ray file have already the correct spectrum applied.

Parameters of Ray File Editor

Polarization data is as following:

I: ellipse big axis normalized vector (o, p, q) 3 float ( such as o*o+p*p+q*q=1 )

r: equal to J / I (small axis divided by big axis) 1 float ( 0 <= r <= 1 )

s: right or left polarization 1 float ( 0:right or 1:left )

I is orthogonal to the photon direction (l, m, n): l*o+m*p+n*q=0

J is orthogonal to I and to the photon's direction.

In the .ray files, (o, p, q, r, s) must be added to each ray.

nRs is the number of specular Reflections.

nRd is the number of diffuse Reflections.

nTs is the number of specular Transmissions.

nTd is the number of diffuse Transmissions.

In Power box, you can type the power value and click Update.

You must select the unit.

By clicking Edit, Change spectrum... or , you can select the spectrum type.

By selecting Blackbody, you can type the temperature value in Kelvins.

By selecting Monochromatic, you can type the value in nanometers.

By selecting Sampled, you must browse a Spectrum file.

You click to use the spectrum editor.


By clicking , you can display the spectrum. You must adjust first the wavelength sampling by

typing the number of wavelengths value.


By clicking Edit, Add another ray file... or , you can add a new .ray file.

By clicking Edit, Invert direction of rays or , you can invert the directions of all rays.

By clicking Edit, Mix all rays in the file or , you can mix all the rays.

By clicking , you can change the relative value of each ray in the .ray file.

This is required when importing or creating .ray files. All containing rays have the same, very small

value as for example 1*10–6.

This function is similar to e/emax.

In case of having very small values for each ray and the values are not equally, you can click to

adjust the relative energy of each ray.

This is used to reach better performance for the calculation.

The ray with the highest energy becomes 1 and all the others are multiplied relatively to the first

ray.

The relative energy remains the same.


PREFERENCES

Monitor

The Monitor tab is available from Virtual Photometric Lab see page 100, Virtual Human Vision Lab see

page 69, User Material Editor see page 52, Spectrum Editor see page 49, Advanced Scattering Surface

Editor see page 16, BSDF - BRDF - Anisotropic Surfaces Viewer see page 17, Virtual Reality Lab see

page 121 and Real Time Lab.

With Monitor tab, you can indicate the characteristics of the monitor.

Monitor parameters are used to perform true color rendering especially in Virtual Photometric Lab.

You can improve the spectral maps' display and avoid the color disparity for a given spectral map

according to the monitor.

All parameters are set by default for an average CRT monitor. Details can be found here

(http://www.color.org/sRGB.html).

To obtain these values, you can ask your monitor's manufacturer or you can measure then with a

calibration tool or the spectrometer available for example with SPEOS Standalone.

Display

In Display box, you must select the display type.

When selecting SIM2 HDR display, you can display results on SIM2 HDR screens.

When selecting SIM2 HDR display, other parameters are not available.

When selecting SIM2 HDR display with Virtual Reality Lab, it is not possible to activate Human

Vision functions as Glare.

To avoid any display problems, SIM2 HDR monitor has to be dedicated for rendering and a

standard monitor for interface.

You must use the multiscreen mode to manage both monitors. For more details, you can view

Multiscreen see page 130.

You should not create any immersive view directly from the HDR screen .

When selecting SIM2 HDR display with Real Time Lab,

You must select Screen definition from Window, Full screen definition.

You must click Edit general preferences, enter 100% value for Rendering Definition for

Complete and Partial.

You must always have one pixel of the display window on only one pixel of the HDR screen.

Chromaticity Values

In Chromaticity values table, you can change the chromaticity values x and y of Red, Green, Blue

and White.

Gamma Correction

Details about Gamma correction can be found here (http://www.poynton.com/GammaFAQ.html).

In Correction Type group box, you must select the way to perform gamma correction.

By selecting Sampled Gamma, the gamma correction is performed by using the result of the

monitor calibration with the spectrometer.

By selecting Fitted Gamma, the gamma correction is performed by using the table underneath.

It is possible to define a different value of Gamma and Gain for each primary color but generally

the same value is satisfactory.

Gamma and Gain values can be obtained from your monitor's manufacturer.

http://www.color.org/sRGB.html

http://www.poynton.com/GammaFAQ.html

Preferences of 207

White Point Luminance

In White Point Luminance, you can type the white luminance level which gives the monitor's

dynamic.

White Point Luminance value has to be the maximum luminance of a white zone displayed by the

used screen.

By clicking , you can launch the monitor calibration to get parameters.

Colorimetry

The Colorimetry tab is available from Virtual Photometric Lab see page 100, User Material Editor see

page 52, Spectrum Editor see page 49, Advanced Scattering Surface Editor see page 16, BSDF - BRDF

- Anisotropic Surfaces Viewer see page 17 and Real Time Lab.

With Colorimetry tab, you can select the standard data used for colorimetric calculations.

You can also change the gamma parameter of your monitor to have a more realistic display.

Illuminant

In Illuminant box, you can select the reference illuminant.

Standard Observer Data

In Standard observer data box, you can select the CIE standard and the sampling.

Data are used from the color computation from the spectrum.

Color Standard Description

In Color standard description box, you can browse a .cls file to define the default colorimetric

standard to be displayed on the colorimetric diagram.

For more details about CLS file, you can view Parameters of Chromaticity Coordinates Tool see page

44.

Default Colorimetric System

In Default colorimetric system box, you can select the default colorimetric system to be used for

the colorimetric diagram.

Printing

The Printing tab is available from Virtual Photometric Lab see page 100, Spectrum Editor see page 49

and BSDF - BRDF - Anisotropic Surfaces Viewer see page 17.

With Printing tab, you can define information related to the print.

By selecting Default, you set values are the one that are in your computer, the user's name and

the company.

By selecting User defined, you can browse a .bmp file.

Spectrometer

The Spectrometer tab is available from Advanced Scattering Surface Editor see page 16, Spectrum

Editor see page 49 and User Material Editor see page 52.

You must have connected the OPTIS Software to the spectrometer.

With Spectrometer tab, you can insure the quality of the measurement by calibrating each

spectrometer with the four coefficients.


These coefficient values can be obtained on the calibration form supplied with the spectrometer.

Virtual Photometric Lab

The Virtual Photometric Lab tab is available from Virtual Photometric Lab see page 100.

This tab is only used for OptisWorks and SPEOS Standalone software.

You can set or save options and settings that would be used every time a XMP map is opened.

All XMP results take these options by default.

By selecting the Show rulers check box, you can display rulers.

You can click Ruler parameters....

By selecting the Show primary graduations or Show secondary graduations check box, you

can display primary or secondary graduations.

You can click Graduations parameters....

By selecting the Show primary grid or Show secondary grid check box, you can display primary

or secondary grid.

You can click Grid parameters....

By selecting the Show axis on cross check box, you can display axis on cross.

By selecting the Snap cross to grid check box, you can snap cross to grid.

By selecting the Show tool tip check box, you can display tool tip.

By selecting the Show gray around the map check box, you can display gray around the map.

By selecting the Fill shape check box, you can fill shape.

Directories

The Directories tab is available from the Virtual Photometric Lab see page 100, Virtual 3D Photometric

Lab see page 65, User Material Editor see page 52, Spectrum Editor see page 49, Advanced Scattering

Surface Editor see page 16 and BSDF - BRDF - Anisotropic Surfaces Viewer see page 17.

In Standard Windows directories group box, you can add standard shortcut for Open and Save

dialog boxes.

In User directories box, you can add your own shortcut for Open and Save dialog boxes.

In Exclude file type box, you can exclude some file types from OPTIS Software directory

management.

From the Help list, you can select the documentation language.

In case the language documentation does not still exist, default language is the english.

3D View

The Preferences window is available from the BSDF-BRDF-Anisotropic Surfaces Viewer see page 18,

Intensity Viewers see page 151 and the User Material Editor see page 58.

With Preferences, you can define parameters of the 3D display. This is useful to have a more precise

view to parameterize the meshing.

Preferences of 207

In Radial Mesh Control group box, you can type the regular subdivisions and the adaptative

subdivisions values.

You can click Default Values to restore default values.

In Mesh reference group box, you must select Geosphere or Sphere theta/phi.

With high values, the loading time is bigger.

Within SPEOS Standalone software, the display is different.

By selecting the Antialiasing check box, you can have a better drawing of lines in 3D view by

avoiding notched lines.

By selecting the Phong check box, you can display 3D view without meshing.

Selecting the Phong check box can cause some problems with ellipsoid, which do not appear in

shading view, and with OSB files if normals have wrong orientation.

Without phong With phong

By selecting the Triangle check box, you can have a better way to mesh the object.

If some problems occur when displaying the 3D view, you must click to clear the check box.

By selecting the UV Axis & Normals check box, you can display UV axis of each face used for

texture on OSB faces.

Normals is used to define the orientation convention for BSDF.

In the 3D view, red and green axis of each faces represent the UV system and blue axis the

normal. The system can be direct or indirect.

The blue axis which is displayed gives the emission direction for the emissive surfaces and

indicates the convention for the 180° BSDF.

The direction related to the blue axis is used for the angles with incidence from 0 to 90° of the

BSDF.


If this direction does not fit, on the OSB it is possible to change the selected face orientation with

the Invert normal contextual menu which changes the OSB face topology.

By selecting the UV Isos 0.5 check box, you can display the Isos at U=V=0.5 which correspond to

the blue lines in the 3D view.

In the Number of first pattern to display (TXT texture) and Number of patterns to display

(TXT texture) boxes, you can type values which are used to display a TXT texture.

If the first value is N0 and the second one N, all the patterns in the text file between N0 and

N0+N-1 are displayed.

In the Number of repetitions to display (Brep texture) box, you can type a value which is

used to display a Brep texture.

When defining a system including a huge number of patterns, it is not possible to display all these

patterns in the 3D view.

Using the number of patterns or the number of repetitions, you can display a part of the texture in

order to check visually your texture definition.

Virtual 3D Photometric Lab

The Virtual 3D Photometric Lab tab is available from Virtual 3D Photometric Lab see page 65.

With Virtual 3D Photometric Lab tab, you can set and save display settings that are used every time a

new file is generated from a simulation.

Display




By selecting the Mesh limit check box, you can display the mesh limit.

By selecting the Legend check box, you can display the legend.

By selecting the Axis check box, you can display the axis.

By selecting the Clip plane check box, you can display the clip plane.

By selecting the Contour check box, you can display the contour.

You can select the Colored check box to color contour.

Preferences of 207

You can select the Annotation check box to display value of each contour line.

You can select a value in the both level lists.

Transparent

In Transparent box, you can move the slider to set the transparency.

Maximum Levels Number

In Maximum levels number box, you can define the maximum levels number to display results.

You can use more than 30 color levels.

Xm3 Filtering

By clicking Xm3 filtering..., you can set a standard filtering.


In Pass number box, you must type the number of times the filtering algorithm is called.

0 value means there is no filtering.

Devices Preferences

The Devices Preferences tab is available from Virtual Reality Lab see page 121.

Computer's Devices

The Computer's Devices box is composed of:

Platform

GPU or CPU

Device (Microprocessor or graphic card)

Only one device can be selected unless the Virtual Reality Lab is launched a second time.

Real Time

The Real Time tab is available from Real Time Lab.

Wavelength Resampling

You can edit wavelengths.

Defaults

You can define default attributes of sources and geometries.

TFCalc

With TFCalc tab, you can set parameters that are used by TFCalc.

INDEX

3

3D Curve • 147, 148, 150, 152, 197

3D Energy Density Lab • 142

3D Map Post-Processing • 67

3D View • 18, 59, 153, 197

A

Absorption Variation • 56

Active Stereoscopy (Frame sequential mode) • 127

Adding Slaves to the Configuration • 140

Advanced Scattering Surface Editor • 16, 42, 195, 196, 197

Analyzing Colorimetric Data • 71, 77, 101, 113

Anisotropic BSDF Surface • 17, 19, 25

Anisotropic BSDF Surface Overview • 19

Anisotropic Scattering Surface • 25

Area • 136

Areas of Look At • 80, 81, 83, 89

Auto-calculate Value Option • 27, 49

Autofill • 17, 48

Avatar • 135

Axis System • 133

B

BRDF, BTDF, BSDF, Anisotropic Measurement Models • 7

BSDF - BRDF - Anisotropic Surface Viewer • 17, 195, 196, 197

BSDF180 Overview • 25

BSDF180 Surface • 17, 18, 25

Building BSDF180 Surface • 25

C

Calculation Parameters • 154

Change Reflection or Transmission Spectrum • 26

Changing Reflection or Transmission Spectrum • 26

Cluster • 139

Coated Surface • 17, 27, 42, 50

Coated Surface Curve • 27, 42

Color Rendering Index • 50, 51

Color Selection • 38, 39

Colorimetric Data • 44

Colorimetry • 45, 62, 196

Complete Scattering Surface (BRDF) • 17, 23

Configuring the Network Management • 137, 139

Configuring the Windows Firewall • 139

Coupling Efficiency Viewer • 154

Creating a Display • 134

Creating a Stereo OptisVR • 123, 127

Creating a System Display • 134

Creating a Window • 135

Creating an Area • 136

Creating an Avatar • 135

Creating an Immersive View • 123, 125, 129

Creating an Observer View • 123, 130

Curves • 151

D

Defining the zero reference • 135, 136

Devices Preferences • 123, 141, 200

Directories • 197

Display • 134

Displaying 3D Curve • 152

Displaying Isolux Curves • 151

Displaying Polar Curves • 152

Displaying Sollner Curves • 147, 148, 153

DOE and Thin Lens Surface Editor • 32

DOE and Thin Lens Surface Overview • 32

Doing 3D Map Post-Processing • 66, 67

Doing Analysis • 71, 88

Doing Color Management • 71, 78

Doing Time Adaptation • 71, 88

Dye Editor • 55, 60

E

Editing Coated Surface Curve • 42

Editing Lab/Gloss Surface Properties • 38, 47

Editing Material Color • 53, 61

Editing Scattering Surface Curve • 43

Editing Surface Properties • 15, 17, 18, 27, 38, 41, 44

Editing the Color Rendering Index Value • 51

Editing the Preferences • 15, 17, 18, 27, 38, 41, 48, 50, 53, 64, 66, 70, 71, 101, 120, 142, 146

Eulumdat Viewer • 147

Example of Polarizers • 9

Exporting • 71, 101, 104

Exporting a File • 190, 191

Exporting an Image • 71, 104

Exporting to Conoscopic Map • 18, 26

Extended Map Format • 105, 106

F

Fluorescent Surface Editor • 37, 42

G

Gaussian Propagation Viewer • 159

General • 53

Generating a Spectrum • 50, 52

Glare Effect • 87

Glare Effect Overview • 85, 87

Glass Map Viewer • 159

Grating Surface Editor • 36

H

HDRI File Format • 72, 102, 105, 108

Human Vision • 125

I

IESNA LM-63 Viewer • 148

Importing • 101, 102

Importing a BMP Mask • 101, 102

Importing a File • 190

Importing an Image • 71, 102

Importing and Exporting • 102, 190

Importing Radiant Imaging Files • 191

Index Variation • 55

Integration Angle • 186, 188

Intensity Distribution Post-processing • 185

Intensity Viewers • 147

Isolux Curves • 147, 148, 150, 151

J

Jones Matrix Examples • 29

L

Lab/Gloss Surface Definition • 47

LABS • 65

LCD Surface • 39, 42

Legibility (CIE 145

2002 standard) • 90

Legibility and Visibility Analysis • 90

Light Behavior Models • 6

Look At • 80

M

Making Surface and Section Analysis • 66, 68, 71, 96, 101, 113

Making Volume and Section Analysis • 142, 144

Managing the Display • 66, 67, 71, 75, 101, 111, 122, 142, 143

Managing the Filtering • 101, 120

Material Color • 61

Monitor • 70, 123, 141, 195

MultiScreen • 131, 139, 195

N

Network Management • 137

Night Vision Goggles • 95, 118

O

Optical Design Viewers • 154

Optical Polished Surface • 13

OPTICAL PROPERTY EDITORS • 6

OPTIS Intensity Viewer • 150

Others Options • 49

Overview • 6, 161

P

Parameters • 177

Parameters of 3D Curve • 152

Parameters of 3D Map Post-Processing • 67, 68

Parameters of a Coated Surface • 27

Parameters of a Display • 134

Parameters of a DOE and Thin Lens Surface • 35, 36

Parameters of a Fluorescent Surface • 37

Parameters of a Grating Surface • 36

Parameters of a LCD Surface • 40

Parameters of a Polarizer Surface • 28

Parameters of a Rendering Surface • 38

Parameters of a Retro Reflecting Surface • 31

Parameters of a Rough Mirror Surface • 41

Parameters of a Simple Scattering Surface • 15

Parameters of a Spectrum • 50

Parameters of a SystemDisplay • 134

Parameters of a User Material • 53

Parameters of a Window • 136

Parameters of an Aberration Coefficient Calculation • 168

Parameters of an Advanced Scattering Surface • 17, 38

Parameters of an Area • 137

Parameters of an Avatar • 135

Parameters of Arc Lamp • 183

Parameters of Auto-calculate Value Option • 49

Parameters of Autofill • 48

Parameters of Bitmap or RGBE Import • 102

Parameters of Black Body • 180

Parameters of Chromaticity Coordinates Tool • 44, 48, 50, 52, 62, 78, 91, 113, 196

Parameters of Coated Surface Curve • 42

Parameters of Coupling Efficiency Viewer • 154, 156

Parameters of Fluorescent Lamp • 183

Parameters of Gaussian Propagation Viewer • 159

Parameters of Glass Map Viewer • 160

Parameters of Human Vision • 126

Parameters of Incandescent Lamp • 182

Parameters of Isolux Curves • 151

Parameters of Lab/Gloss Surface Properties • 47

Parameters of Lambertian Source • 178, 179

Parameters of LED • 178

Parameters of Legibility and Visibility Tools • 90

Parameters of Material Color • 61

Parameters of Multimodal Laser Diode • 180

Parameters of Network Management • 137, 138

Parameters of Night Vision Goggles • 95, 118

Parameters of Optical Fiber • 177

Parameters of Paraxial Data Viewer • 166

Parameters of Photometric Calc • 65

Parameters of Polar Curves • 152

Parameters of Polarization Option • 50

Parameters of Position and Orientation • 177, 184

Parameters of Ray File Editor • 190, 193

Parameters of Scattering Surface • 17, 18, 43, 197

Parameters of Spectrum • 178, 179, 180, 182, 183, 184

Parameters of Spectrum Generation • 52, 53

Parameters of Spot Diagram Viewer • 173

Parameters of Surface and Section Analysis • 68, 96, 114

Parameters of Surface Properties • 44

Parameters of Technoteam PF File Import • 102, 104

Parameters of the Color Rendering Index • 45, 52, 62, 78, 113

Parameters of the Eulumdat Viewer • 147

Parameters of the IESNA LM-63 Viewer • 148

Parameters of the Intensity Distribution Post-processing • 185

Parameters of the Map Properties • 186

Parameters of the OPTIS Intensity Viewer • 150

Parameters of the Virtual Lighting Controller • 99, 100, 117, 145

Parameters of the Virtual Lighting Controller VRL • 124

Parameters of Transverse Ray Aberrations Viewer • 171, 172

Parameters of User Defined Source • 179, 181

Parameters of Vision Parameters • 82, 89, 90

Parameters of Volume and Section Analysis • 144

Parameters of XMP Export • 72, 75, 105

Parameters to Change Reflection or Transmission Spectrum • 26

Paraxial Data Viewer • 161

Particles • 57, 58, 59

Passive Stereoscopy • 128

Perfect Mirror Surface • 13

Photometric Calc • 65

Polar Curves • 147, 148, 150, 152

Polarization • 8, 27, 42, 50

Polarizer Surface Editor • 27

Polarizer Surface V1.0 • 28, 29

Polarizer Surface V2.0 • 28, 30

Post-Processing • 185

Preferences • 44, 48, 64, 70, 101, 120, 146

PREFERENCES • 195

Preferences of Scattering Surface Curve • 43, 44

Printing • 196

R

Ray File Editor • 189

RAY FILE TOOLS • 177

Reading Precision • 71, 77, 101, 112, 187

Real Aberrations Coefficients Viewer • 168

Real Aberrations Viewer • 171

Real Time • 200

Rendering Surface Editor • 38

Retro Reflecting Surface Editor • 31, 42

Rough Mirror Surface Editor • 41, 42

S

Saving Results • 131

Scattering Phase Function • 57, 58, 197

Scattering Properties • 56, 61

Scattering Surface Curve • 15, 17, 31, 37, 40, 41, 42

Setting the Cluster for the Master • 139, 140

Simple BSDF Surface • 17, 19

Simple Scattering Surface Editor • 15, 42

Source Generator • 177

Spectrometer • 196

Spectrum Editor • 37, 38, 44, 48, 50, 51, 52, 60, 61, 62, 78, 113, 193, 195, 196, 197

Spectrum Generation • 52

Specular Constant for Anisotropic BSDF • 22

Spot Diagram Viewer • 173

Starting the MultiScreen Mode • 140

Stereo OptisVR • 127

Structure of Anisotropic BSDF Files • 20

Surface and Section Analysis • 68, 96, 113

Surface Optical Property Editors • 6

Surfaces Overview • 6

Switching Between HDRI Picture and Immersive View • 131

Switching between Stereo and Normal Mode • 130

System VR Configuration • 132

System VR Configuration Overview • 132

SystemDisplay • 134

T

TFCalc • 49, 200

TFCalc Import • 27, 49

Tools • 44

TXT File Format • 102, 105

U

Unpolished Surface • 13, 17

User Material Editor • 53, 195, 196, 197

Using 3D Energy Density Lab • 142

Using Auto-calculate Value Option • 49

Using Autofill • 48

Using Coupling Efficiency Viewer • 154

Using Data Downloaded from OSRAM Opto Semiconductors • 190, 191

Using Filtering Tools • 121

Using Gaussian Propagation Viewer • 159

Using Glass Map Viewer • 159

Using Human Vision • 125

Using Legibility and Visibility Tools • 71, 90

Using Look At • 71, 80

Using Night Vision Goggles • 71, 95, 101, 118

Using Other Filterings • 121

Using Paraxial Data Viewer • 165

Using Photometric Calc • 65

Using Polarization Option • 50

Using Real Aberrations Coefficients Viewer • 168

Using Real Aberrations Viewer • 171

Using Spot Diagram Viewer • 173

Using Sun Glasses / Colored Filter • 71, 93

Using Sun Glasses or Colored Filter • 101, 118

Using the Advanced Scattering Surface Editor • 16

Using the BSDF - BRDF - Anisotropic Surface Viewer • 17

Using the Coated Surface Editor • 27

Using the DOE and Thin Lens Surface Editor • 35

Using the Eulumdat Viewer • 147

Using the Filtering • 131

Using the Fluorescent Surface Editor • 37

Using the Glare Effect • 71, 87

Using the Grating Surface Editor • 36

Using the IESNA LM-63 Viewer • 148

Using the Intensity Distribution Post-processing • 185

Using the LCD Surface Editor • 40

Using the Multiscreen Autostart • 141

Using the OPTIS Intensity Viewer • 150

Using the Polarizer Surface Editor • 28

Using the Ray File Editor • 190

Using the Rendering Surface Editor • 38

Using the Retro Reflecting Surface Editor • 31

Using the Rough Mirror Surface Editor • 41

Using the SIM2 HDR Monitor • 141

Using the Simple Scattering Surface Editor • 15

Using the Source Generator • 177

Using the Spectrum Editor • 50

Using the Stereo Immersive View Correction • 129

Using the User Material Editor • 53

Using the Virtual Lighting Controller • 71, 99, 101, 116, 122, 124, 142, 145

Using the Virtual Photometric Lab • 101

Using the Virtual Reality Peripheral Network Autostart • 142

Using the XMP Filtering • 120

Using the XMP Map Post- processing • 186

Using Virtual 3D Photometric Lab • 66

Using Virtual Human Vision Lab • 70

Using Virtual Reality Lab • 123

Using Virtual Reality Peripheral Network • 141

Using Vision Parameters • 71, 82, 88

V

View • 42

VIEWERS • 147

Virtual 3D Photometric Lab • 66, 197, 199

Virtual Human Vision Lab • 51, 70, 195

Virtual Lighting Controller • 99, 116, 124, 145

Virtual Photometric Lab • 51, 101, 147, 148, 150, 195, 196, 197

Virtual Reality Lab • 122, 195, 200

Virtual Reality Lab Icons • 122

Virtual Reality Lab Management • 131

Virtual Reality Peripheral Network • 141

Visibility • 92

Vision Parameters • 82

Volume and Section Analysis • 144

W

Window • 135

X

XMP Map Post- processing • 186

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