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tutorials:basic-spectral-light-modeling [2025/06/04 07:06] – MHtutorials:basic-spectral-light-modeling [2025/06/04 14:08] (current) – MH
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 <code java> <code java>
 +import de.grogra.gpuflux.scene.experiment.Measurement;
 +
 Measurement spectrum = LM.getAbsorbedPowerMeasurement(x); Measurement spectrum = LM.getAbsorbedPowerMeasurement(x);
 float absorbedPower = spectrum.integrate(); float absorbedPower = spectrum.integrate();
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 <code java> <code java>
 +import de.grogra.gpuflux.imp3d.spectral.SpectralCurve;
 +import de.grogra.gpuflux.imp3d.spectral.IrregularSpectralCurve;
 +
 const float[] WAVELENGTHS = {380, 410, 420, 450, 465, 480, 490, 600, 620, 630, 640, 655, 660, 670, 690, 700, 720}; const float[] WAVELENGTHS = {380, 410, 420, 450, 465, 480, 490, 600, 620, 630, 640, 655, 660, 670, 690, 700, 720};
-const AMPLITUDES = {0.05, 0.1, 0.4, 0.63, 0.25, 0.15, 0.05, 0.01, 0.1, 0.3, 0.4, 0.85, 0.75, 0.95, 0.6, 0.25, 0.1};+const float[] AMPLITUDES = {0.05, 0.1, 0.4, 0.63, 0.25, 0.15, 0.05, 0.01, 0.1, 0.3, 0.4, 0.85, 0.75, 0.95, 0.6, 0.25, 0.1};
  
-const ChannelSPD TEST_SPD = new ChannelSPD(new IrregularSpectralCurve(WAVELENGTHS, AMPLITUDES)); +const SpectralCurve TEST_SPD = new IrregularSpectralCurve(WAVELENGTHS, AMPLITUDES)); 
 </code> </code>
  
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 {{ :tutorials:light_SpectralCurve.png?direct&200 |}} {{ :tutorials:light_SpectralCurve.png?direct&200 |}}
- 
  
 Since these spectral curve classes all implement the same //SpectralCurve// interface, they can be used in the same way and are therefore exchangeable.  Since these spectral curve classes all implement the same //SpectralCurve// interface, they can be used in the same way and are therefore exchangeable.
  
 <code java> <code java>
 +import de.grogra.gpuflux.imp3d.spectral.SpectralCurve;
 +import de.grogra.gpuflux.imp3d.spectral.IrregularSpectralCurve;
 +import de.grogra.gpuflux.imp3d.shading.ChannelSPD; 
 +
 //user defined spectral curve, applied to an IrregularSpectralCurve //user defined spectral curve, applied to an IrregularSpectralCurve
 float[] WAVELENGTHS = {380, 485, 490, 610, 615, 720}; float[] WAVELENGTHS = {380, 485, 490, 610, 615, 720};
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 ChannelSPD REG_SPD = new ChannelSPD(new CIENormSpectralCurve(Attributes.CIE_NORM_D55)); ChannelSPD REG_SPD = new ChannelSPD(new CIENormSpectralCurve(Attributes.CIE_NORM_D55));
  
-// a black body spectral curve with a temperature of 5000K+//a black body spectral curve with a temperature of 5000K
 ChannelSPD REG_SPD = new ChannelSPD(new BlackbodySpectralCurve(5000)); ChannelSPD REG_SPD = new ChannelSPD(new BlackbodySpectralCurve(5000));
 </code> </code>
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 {{ :tutorials:light11.png?direct&600 |}} {{ :tutorials:light11.png?direct&600 |}}
  
-To use the spectral curve as input for a light source, a //SpectralLight// needs to be defined. +To use the spectral curve as input for a light source, a //SpectralLight// needs to be defined. In the example below, a //SpectralLight// is defined as //PointLight// that emitts a user-defined //IrregularSpectralCurve//.
  
 <code java> <code java>
-const float[] WAVELENGTHS = {380,385,...}; +import de.grogra.gpuflux.imp3d.objects.SpectralLight; 
-const float[] AMPLITUDES = {0.000967721, 0.000980455, ...};+import de.grogra.gpuflux.imp3d.spectral.SpectralCurve; 
 +import de.grogra.gpuflux.imp3d.spectral.IrregularSpectralCurve; 
 +  
 +//user defined spectral curve, applied to an IrregularSpectralCurve 
 +const float[] WAVELENGTHS = {380, 485, 490, 610, 615, 720}; 
 +const float[] AMPLITUDES = {0,0,1,1,0,0}; 
 +const SpectralCurve TEST_SPD = new IrregularSpectralCurve(WAVELENGTHS, AMPLITUDES);  
  
 module MyLamp extends LightNode() { module MyLamp extends LightNode() {
     {     {
         setLight(         setLight(
-            new SpectralLight(new IrregularSpectralCurve(WAVELENGTHS, AMPLITUDES)).(+            new SpectralLight(TEST_SPD).(
                 setPower(100), // [W]                 setPower(100), // [W]
                 setLight(new PointLight())                 setLight(new PointLight())
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     }     }
 } }
 +
 +protected void init() [
 + Axiom ==> MyLamp;
 +]
 </code> </code>
  
-**PLD** = **P**physical **L**ight **D**istribution+Note: //ChannelSPD// are the input for shader, while //SpectralCurve// is the expected input data type for //LightNodes// objects.
  
-To complete the definition of a light source, besides the spectral power distribution, the physical light distribution, which defines the light pattern, needs to be defined. This is especially helpful or necessary for any definition of artificial light sources, such as those found in greenhouses, including HPS lamps or modern LED-based light systems, which are usually equiped with a reflector.+Within the //CIENormSpectralCurve// class, a small database of several predefined standard spectral curves is given: 
 + 
 +  * at 1nm resolution [300, 780] 
 +    * A, D65 
 +  * at 5nm resolution [300, 780] 
 +    * A, C, D50, D55, D65, D75 
 +  * at 5nm resolution [380, 780] 
 +    * FL1-12, FL3_1-15, HP1-5 
 + 
 +For instance, to use the predefined CIE NORM D65 for typical sun light within a user defined light module, one could use the following code. 
 + 
 +<code java> 
 +import de.grogra.gpuflux.imp3d.spectral.CIENormSpectralCurve;  
 +import de.grogra.gpuflux.imp3d.objects.SpectralLight; 
 + 
 +//define a light module 
 +module MyLamp extends LightNode { 
 +  { 
 +    setLight( 
 +      new SpectralLight( new CIENormSpectralCurve(Attributes.CIE_NORM_D65) ).( 
 + setPower(100), //[W] 
 + setLight(new PointLight()) 
 +      ) //end SpectralLight 
 +    ); //end setLight 
 +  } 
 +} 
 +</code> 
 + 
 + 
 +Using the SPD, we define the light 'composition' or light quality. 
 + 
 +In the above example, a //PointLight// is used as light source to emit the wanted spectrum. In the next step, we will continue and show how to define and use user-defined light emission pattern. The keyword here is **PLD** = **P**hysical **L**ight **D**istribution. 
 + 
 +This is especially helpful or necessary for any definition of artificial light sources, such as those found in greenhouses, including HPS lamps or modern LED-based light systems, which are usually equiped with a reflector.
  
 The physical light distribution can be defined as a polar distribution diagram (also called polar curve) showing the luminous intensity values with increasing angles from two imaginary axes of the lamp, which is placed in the centre. Red: 0–180◦ plane, blue 90–270◦ plane. On the right of the figure below, a 3D visualisation of the same light source is given. The colour of each point (gradient from black to bright red), as well as the distance to the light source, both indicate the power emitted by the light source in a particular direction per unit solid angle. The physical light distribution can be defined as a polar distribution diagram (also called polar curve) showing the luminous intensity values with increasing angles from two imaginary axes of the lamp, which is placed in the centre. Red: 0–180◦ plane, blue 90–270◦ plane. On the right of the figure below, a 3D visualisation of the same light source is given. The colour of each point (gradient from black to bright red), as well as the distance to the light source, both indicate the power emitted by the light source in a particular direction per unit solid angle.
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 {{ :tutorials:light_visulizedLightSources.png?direct&500 |}} {{ :tutorials:light_visulizedLightSources.png?direct&500 |}}
  
-To see a more realistic light pattern, the scene needs to be rendered using one of the light models. Below is a rendered image of the LampDemo.gsz, as it can be found in the GroIMP internal example gallery. +To see a more realistic light pattern, the scene needs to be rendered using one of the light models. Below is a rendered image of the //LampDemo.gsz//, as it can be found in the GroIMP internal example gallery.
  
 {{ :tutorials:light_lampDemo.png?direct&500 |}} {{ :tutorials:light_lampDemo.png?direct&500 |}}
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 Defining a PLD for a light source can be done in two ways: 1) 'manually' by defining the polar curve as an array of intensities within XL, or 2) by importing a PLD file—as it is provided by most professional light companies for their products. Defining a PLD for a light source can be done in two ways: 1) 'manually' by defining the polar curve as an array of intensities within XL, or 2) by importing a PLD file—as it is provided by most professional light companies for their products.
  
-In any case, instead of one of the predefined light sources, such as //PointLight//, //SpotLight//, or //DirectionalLight//, a so-called //PhysicalLight// needs to be defined. The //PhysicalLight// allows us to apply a PLD to it. For the 'manual way,' the PLD is defined as a two-dimensional array (called DISTRIBUTION in the code snippet below) that is then passed as an input parameter to the //PhysicalLight// class.+In any case, instead of one of the predefined light sources, such as //PointLight//, //SpotLight//, or //DirectionalLight//, a so-called **//PhysicalLight//** needs to be defined. The //PhysicalLight// allows us to apply a PLD to it. For the 'manual way,' the PLD is defined as a two-dimensional array (called DISTRIBUTION in the code snippet below) that is then passed as an input parameter to the //PhysicalLight// class.
  
  
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 } }
 </code> </code>
 +
 +
 +A PLD distribution is defined as two-dimensional array, where the values of each row represent the intensities in one direction, starting at 90 degree (above the light source) going down to 270 degree (right below the light source), covering 180 degree. The values given are equally distributed of the 180 degree, e.g., when only three values are given, the first will be associated with 90 degree, the second with zero and the third with 270 degree. The rows on the other hand are equally distributed around the virtual z-axis, around the light source. If only one row is given, this distribution defined within the first row, will be used equally around the whole light source. If two rows are given, the first one will be used at zero degree and the second one at 180 degree. The values in-between are interpolated. The intensities are given in ether in absolute values (in Watt) or in percent in the range or zero to one or zero to 100. They are normalized internally again.
  
  
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 <code java> <code java>
-float[] WAVELENGTHS = {380, 485, 490, 610, 615, 720}; +import de.grogra.gpuflux.imp3d.shading.ChannelSPD; 
-float[] AMPLITUDES = {0,0,1,1,0,0}; +import de.grogra.gpuflux.imp3d.spectral.IrregularSpectralCurve; 
-ChannelSPD GREEN_SPD = new ChannelSPD(new IrregularSpectralCurve(WAVELENGTHS, AMPLITUDES)); +import de.grogra.gpuflux.imp3d.spectral.RGBSpectralCurve; 
 +import de.grogra.gpuflux.imp3d.spectral.ConstantSpectralCurve;
  
-ChannelSPD RED_SPD = new ChannelSPD(new RGBSpectralCurve(0.8,0,0));  +static float[] WAVELENGTHS = {380, 485, 490, 610, 615, 720}; 
-ChannelSPD CONST_SPD = new ChannelSPD(new ConstantSpectralCurve(0.25)); +static float[] AMPLITUDES = {0,0,1,1,0,0}; 
 +static ChannelSPD GREEN_SPD = new ChannelSPD(new IrregularSpectralCurve(WAVELENGTHS, AMPLITUDES)); 
  
-Phong myShader = new Phong(); +static ChannelSPD RED_SPD = new ChannelSPD(new RGBSpectralCurve(0.8,0,0));  
-myShader.setDiffuse(GREEN_SPD); +static ChannelSPD CONST_SPD = new ChannelSPD(new ConstantSpectralCurve(0.25));  
-myShader.setTransparency(RED_SPD);+ 
 +//shader definition as global variable 
 +Phong myShader0 = new Phong(); 
 +static { 
 +  myShader0.setDiffuse(GREEN_SPD); 
 +  myShader0.setTransparency(RED_SPD); 
 +} 
 + 
 +//and use of the global shader within a module that is interpreted as Box 
 +module TestBox ==> { 
 +} Box(0.001,1,1).(setShader(myShader0));
  
  
-//within a module that extends a Box+//or define the shader within a module that extends a Box
 module TestBox extends Box(0.001,1,1) { module TestBox extends Box(0.001,1,1) {
          
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     }     }
 } }
- 
-//as a module that is interpreted as Box 
-module TestBox ==> { 
-    Phong myShader = new Phong(); 
-} Box(0.001,1,1).(setShader(myShader)); 
 </code> </code>
- 
-Within the //CIENormSpectralCurve// class, a small database of several predefined standard spectral curves is given: 
- 
-  * at 1nm resolution [300, 780] 
-    * A, D65 
-  * at 5nm resolution [300, 780] 
-    * A, C, D50, D55, D65, D75 
-  * at 5nm resolution [380, 780] 
-    * FL1-12, FL3_1-15, HP1-5 
- 
-For instance, to use the predefined CIE NORM D65 for typical sun light within a user defined light module, one could use the following code. 
- 
-<code java> 
-import de.grogra.gpuflux.imp3d.spectral.CIENormSpectralCurve;  
-import de.grogra.gpuflux.imp3d.objects.PhysicalLight; 
- 
-//define a light module 
-module MyLamp extends LightNode { 
-  { 
-    setLight( 
-      new SpectralLight( 
-        new CIENormSpectralCurve(Attributes.CIE_NORM_D65) 
-      ).( 
- setPower(100), //[W] 
- setLight( 
-   new PhysicalLight(DISTRIBUTION).( 
-     setVisualize(true), //activate light ray visualization 
-            setNumberofrays(250),  
-            setRaylength(1)// [m] 
-          ) 
-        ) 
-      ) //end SpectralLight 
-    ); //end setLight 
-  } 
-} 
-</code> 
- 
- 
  
 Note: Do NOT mix common RGB shaders (like the //RGBAShader//) and spectral shaders! This applies to having RGB and spectral shaders within the same model but in different objects but also for one (Phong) shader that combines RGB and spectral shaders. The ranges of common RGB shaders will most probably not match the ranges of the other shader and the simulated light spectrum which will inevitably lead to false results. Note: Do NOT mix common RGB shaders (like the //RGBAShader//) and spectral shaders! This applies to having RGB and spectral shaders within the same model but in different objects but also for one (Phong) shader that combines RGB and spectral shaders. The ranges of common RGB shaders will most probably not match the ranges of the other shader and the simulated light spectrum which will inevitably lead to false results.
  
  
-==== Sensor nodes ==== 
- 
-To monitor light distributions with a scene without interfering, GroIMP provides the //SensorNode// class, a sphere that can be placed arbitrarily within the scene. To obtain the sensed spectrum, the //getSensedIrradianceMeasurement()// function needs to be called. 
- 
-Note: The size of the sensor node directly correlates with the probability of got hit by a light ray. For a very small sphere the probability to got hit by a light ray is relatively low, so the number of light rays simulated by the light model needs to be much larger to get repayable results. Therefore, better not to use very small sensor nodes. 
- 
-Note: The colour of the sensor node determines which wavelengths should be observed. The default value is white, what stands for monitor all colours. If, for instance, the sensor colour is set to red, only red spectra will be sensed. 
- 
-Note: The output of a sensor node is normalized to absorbed radiance per square meter, independent of the actual size of the sensor.  
- 
-Note: Sensor nodes can be enabled and disabled for the light model using the LM.setEnableSensors(true/false) function. By default they are disabled, since GroIMP version 2.1.4, before they were enabled by default. Having them disabled speeds up the light computation time for scenarios where not sensor nodes are involved.  
- 
-<code java> 
-// create a 5cm, white sensor node 
-Axiom ==> SensorNode().(setRadius(0.05), setColor(1, 1, 1)); 
- 
-//check what the sensor node has sensed 
-x:SensorNode ::> { 
-    Measurement spectrum = lm.getSensedIrradianceMeasurement(x); 
-    float absorbedPower = spectrum.integrate(); 
-    ... 
-} 
-</code> 
  
  
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 </code> </code>
  
 +GroIMP supports the inport of 'Spectral Distribution Files, *.spd' as input for spectral curves, and 'Luminance Files, *.lum' as well as 'IES Light Distribution Files, *.ies' as inport formats for PLDs.
  
 ==== Example ==== ==== Example ====
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 </code> </code>
  
-The model will run and directly when saved, creates an instance of the light model, set wanted parameters and run it. there will be no output (except the one form the light model itself, stating that it was executed and giving some statistics on the scene). +The model will run and directly when saved, creates an instance of the light model, set wanted parameters and run it. there will be no output (except the one form the light model itself, stating that it was executed and giving some statistics on the scene and further stating that no light sources could be found within the scene). 
  
 If you already get errors here, your system most probably does not support spectral light modelling. If you already get errors here, your system most probably does not support spectral light modelling.
tutorials/basic-spectral-light-modeling.1749013607.txt.gz · Last modified: 2025/06/04 07:06 by MH