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Scatter and Stray Light Analysis

Here is a simple example of a veiling glare calculation.  Veiling glare is defined (in the Photonics Directory) as “diffuse stray light at the image plane of an optical system that results in reduced contrast and resolution.” 

Veiling glare typically results when unwanted light from an out-of-field source enters an optical system. For example, consider the case of a telescope looking up from the earth.  No matter where in the sky the telescope is aimed, some light from the sun (or moon, or other bright "out-of-field" object) may strike the front of the telescope and then scatter around inside, eventually ending up at the telescope’s focal plane.

A telescope’s designer must take this extraneous light – the veiling glare – into account.  A good way to measure and compare the amount of veiling glare in different optical systems is to calculate the Normalized Detector Irradiance (NDI).  From “Stray Light Performance Optimization through System Design,” by Francis Reininger (SPIE Vol.2260, p.21; 1994):

The Normalized Detector Irradiance (NDI) is the standard figure of merit for evaluating a system’s stray radiation performance as a function of off-axis point source angles.  The NDI is the ratio of the stray light irradiance at the detector to the stray light source irradiance at the entrance port when evaluated for a plane normal to the line of sight to the source point.  Because it is a ratio of irradiance rather than power, the NDI can be used to compare the stray light suppression capability of instruments of various sizes without the need for scaling.

The images below show a telescope system before and after interior stray light baffles are introduced.  For each of the two systems (one with, and the other without, interior baffles) we have set up ZEMAX to perform dozens of stray light calculations for various stray light source angles and then automatically calculate the NDI as a function of angle.  Using the ZEMAX Programming Language (ZPL) we have created customized NDI plots, the comparison of which clearly shows the value added by including the interior baffles.

No Scatter

Telescope without Baffles, no Scatter Present

ABg Graph

BRDF Graph for the Mirrors (Large FIle)

Telescope without Baffles, with Scatter Present

NDI 1.0

NDI of simple telescope without baffles

With Baffles

Telescope with Added Baffles

NDI2

NDI of simple telescope with baffles

 

In this simple example, we have shown how the addition of two interior baffles can decrease the amount of veiling glare in our simple telescope by about two orders of magnitude – that is, we have reduced the amount of veiling glare by a factor of 100X.

More examples below...

Optical Design and Analysis Examples


Custom Lens Design

Eye
Modeling of the Human Eye
Scatter
Scatter / Stray Light Analysis
Fringe
Wavefront Correction

Freeform Illumination

ZEMAX Macros and DDEs
 
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