#!/usr/bin/env python
# coding: utf-8

# # Colour Temperature & Correlated Colour Temperature

# The [colour temperature](http://en.wikipedia.org/wiki/Color_temperature) noted $T_c$ is the temperature of a Planckian radiator whose radiation has the same chromaticity as that of a given stimulus. <a name="back_reference_1"></a><a href="#reference_1">[1]</a>
# 
# The [correlated colour temperature](http://en.wikipedia.org/wiki/Color_temperature#Correlated_color_temperature) noted $T_{cp}$ and shortened to $CCT$ is the temperature of the Planckian radiator having the chromaticity nearest the chromaticity associated with the given spectral distribution on a diagram where the (CIE 1931 2° Standard Observer based) $u^\prime, \cfrac{2}{3}v^\prime$ coordinates of the Planckian locus and the test stimulus are depicted. <a name="back_reference_2"></a><a href="#reference_2">[2]</a>
# 
# The *CIE Standard Illuminant A*, *CIE Standard Illuminant D65* and *CIE Illuminant E* illuminants plotted in the *CIE 1960 UCS Chromaticity Diagram*:

# In[1]:


import colour

from colour.plotting import *


# In[2]:


colour_style();


# In[3]:


with colour.utilities.suppress_warnings(python_warnings=True):
    plot_planckian_locus_in_chromaticity_diagram_CIE1960UCS(['A', 'D65', 'E']);


# In[4]:


# Zooming into the *Planckian Locus*.
with colour.utilities.suppress_warnings(python_warnings=True):
    plot_planckian_locus_in_chromaticity_diagram_CIE1960UCS(
        ['A', 'D65', 'E'], bounding_box=[0.15, 0.35, 0.25, 0.45]);


# The concept of correlated colour temperature should not be used if the chromaticity of the test source differs more than $\Delta C=5\cdot10^{-2}$ from the Planckian radiator with: <a name="back_reference_2"></a><a href="#reference_2">[2]</a>
# 
# $$
# \Delta C= \Biggl[ \Bigl(u_t^\prime-u_p^\prime\Bigr)^2+\cfrac{4}{9}\Bigl(v_t^\prime-v_p^\prime\Bigr)^2\Biggr]^{1/2}
# $$
# 
# where $u_t^\prime$, $u_p^\prime$ refer to the test source, $v_t^\prime$, $v_p^\prime$ to the Planckian radiator.
# 
# [Colour](https://github.com/colour-science/colour/) implements various methods for correlated colour temperature computation $T_{cp}$ from chromaticity coordinates $xy$ or $uv$ and chomaticity coordinates $xy$ or $uv$ computation from correlated colour temperature:
# 
# * Robertson (1968) correlated colour temperature $T_{cp}$ and $D_{uv}$ computation method by interpolation between isotemperature lines.
# * Ohno (2013) correlated colour temperature $T_{cp}$ and $D_{uv}$ computation method by direct approach and combined triangular and parabolic solutions.
# * McCamy (1992) correlated colour temperature $T_{cp}$ cubic approximation computation method.
# * Hernandez-Andres, Lee and Romero (1999) correlated colour temperature $T_{cp}$ cubic approximation computation method.
# * Krystek (1985) chomaticity coordinates $uv$ polynomial approximation computation method.
# * Kang et al. (2002) chomaticity coordinates $xy$ cubic approximation computation method.
# * *CIE Illuminant D Series* chomaticity coordinates $xy$ computation method.

# ## Robertson (1968) Method

# Robertson (1968) method is based on $T_{cp}$ computation by linear interpolation between two adjacent members of a defined set of 31 isotemperature lines. <a name="back_reference_3"></a><a href="#reference_3">[3]</a>
# 
# In the *CIE 1960 UCS chromaticity diagram* the distance $d_i$ of the chromaticity point of given source ($u_s$, $v_s$) from each of the chromaticity point ($u_i$, $v_i$) through which the $i$th isotemperature line of slope $t_i$ passes is calculated as follows: <a name="back_reference_3"></a><a href="#reference_3">[3]</a>
# 
# $$
# \begin{equation}
# d_i=\cfrac{(v_s-v_i)-t_i(u_s-u_i)}{(1+t_i^2)^{1/2}}
# \end{equation}
# $$
# 
# The chromaticity point ($u_s$, $v_s$) is located between the adjacent isotemperature lines $j$ and $j + 1$ if $d_j/d_{j+1} < 0$
# 
# $$
# \begin{equation}
# T_c=\Biggl[\cfrac{1}{T_j}+\cfrac{\theta_1}{\theta_1+\theta_2}\biggl(\cfrac{1}{T_{j+1}}-\cfrac{1}{T_j}\biggr)\Biggr]^{-1}
# \end{equation}
# $$
# 
# where $\theta_1$ and $\theta_2$ are respectively the angles between the isotemperature lines $T_j$ and $T_{j+1}$ and the line joining ($u_s$, $v_s$) to their intersection. Since the isotemperature lines are narrow spaced $\theta_1$ and $\theta_2$ are small enough that one can set $\theta_1/\theta_2 = \sin\theta_1/\sin\theta_2$. The above equation can then be written:
# 
# $$
# \begin{equation}
# T_c=\Biggl[\cfrac{1}{T_j}+\cfrac{d_j}{d_j-d_{j+1}}\biggl(\cfrac{1}{T_{j+1}}-\cfrac{1}{T_j}\biggr)\Biggr]^{-1}
# \end{equation}
# $$
# 
# The `colour.uv_to_CCT_Robertson1968` definition is used to calculate the correlated colour temperature $T_{cp}$ and distance $D_{uv}$ ($d_i$):

# In[5]:


colour.temperature.uv_to_CCT_Robertson1968((0.19783451566098664, 0.31221744678060825))


# `colour.uv_to_CCT` definition is implemented as a wrapper for various correlated colour temperature computation methods:

# In[6]:


colour.uv_to_CCT((0.19783451566098664, 0.31221744678060825), 'Robertson 1968')


# > Note: `'robertson1968'` is defined as a convenient alias for `'Robertson 1968'`:

# In[7]:


colour.uv_to_CCT((0.19783451566098664, 0.31221744678060825), 'robertson1968')


# Converting from correlated colour temperature $T_{cp}$ and distance $D_{uv}$ to chomaticity coordinates $uv$:

# In[8]:


colour.CCT_to_uv((6503.03994225557, 0.0032556165414977167), 'Robertson 1968')


# In[9]:


colour.CCT_to_uv((6503.03994225557, 0.0032556165414977167), 'robertson1968')


# ## Ohno (2013) Method

# Ohno (2013) presented new practical accurate methods to calculate the correlated colour temperature $T_{cp}$ and distance $D_{uv}$ with an error of 1 $K$ in $T_{cp}$ range from 1000 to 20,000 and $\pm$0.03 in $D_{uv}$. <a name="back_reference_4"></a><a href="#reference_4">[4]</a>

# ### Triangular Solution

# The correlated colour temperature is calculated by searching the closest point on the Planckian locus on the *CIE 1960 UCS chromaticity diagram* but without the complexity of Roberston (1968) method.
# 
# A table of coordinates ($U_i$, $V_i$) of Planckian locus (Planckian ($u$, $v$) table) in the estimated range of correlated colour temperature needed is generated and then the distance $d_i$ from the chromaticity coordinates ($U_x$, $V_x$) of a test light source is calculated.
# 
# The point $i = m$ is the point where $d_i$ is the smallest in the table ensuring that the correlated colour temperature to be obtained lies between $T_{m-1}$ and $T_{m+1}$.
# 
# The previous computation is repeated $n$ times through cascade expansion in order to reduce errors.
# 
# A triangle is then formed by the chromaticity point ($U_x$, $V_x$) of the test light soure and the chromaticity points on Planckian locus at $T_{m-1}$ and $T_{m+1}$. The blackbody temperature $T_x$ for the closest point to the line between $T_{m-1}$ and $T_{m+1}$ is calculated as follows: <a name="back_reference_4"></a><a href="#reference_4">[4]</a>
# 
# $$
# \begin{equation}
# T_x=T_{m-1}+(T_{m+1}-T_{m-1})\cdot\cfrac{x}{l}
# \end{equation}
# $$
# 
# with
# 
# $$
# \begin{equation}
# \begin{aligned}
# x&=\cfrac{d_{m-1}^2-d_{m+1}^2+l^2}{2l}\\
# l&=\sqrt{(u_{m+1}-u_{m-1})^2+(v_{m+1}-v_{m-1})^2}
# \end{aligned}
# \end{equation}
# $$
# 
# $D_{uv}$ is then calculated as follows:
# 
# $$
# \begin{equation}
# D_{uv}=(d_{m-1}^2-x^2)^{1/2}\cdot sgn(v_x-v_{T_x})
# \end{equation}
# $$
# 
# with
# 
# $$
# \begin{equation}
# \begin{aligned}
# v_{T_x}&=v_{m-1}+\{v_{m+1}-v_{m-1}\}\cdot x/l\\
# SIGN(z)&=1\ for\ z \geq0\ and\ SIGN(z)=-1\ for\ z <0
# \end{aligned}
# \end{equation}
# $$
# 
# Errors due to the non linearity of the correlated colour temperature scale on ($u$, $v$) coordinates are reduced by applying the following correction:
# 
# $$
# \begin{equation}
# T_{x,cor}=T_x\times 0.99991
# \end{equation}
# $$
# 
# This correction is not needed for Planckian ($u$, $v$) table with steps of 0.25% or smaller.

# ### Parabolic Solution

# After finding $T_{m-1}$ and $T_{m+1}$ as described in the [triangular solution](#Triangular-Solution) method above, $d_{m−1}$, $d_m$, $d_{m+1}$ are fitted to a parabolic function. The polynomial is derived from $d_{m−1}$, $d_m$, $d_{m+1}$ and $T_{m−1}$, $T_m$, $T_{m+1}$ as: <a name="back_reference_4"></a><a href="#reference_4">[4]</a>
# 
# $$
# \begin{equation}
# d(T)=aT^2+bT+c
# \end{equation}
# $$
# 
# where
# 
# $$
# \begin{equation}
# \begin{aligned}
# a&\ =[T_{m-1}(d_{m+1}-d_m)+T_m(d_{m-1}-d_{m+1})+T_{m+1}(d_m-d_{m-1})]\cdot X^{-1}\\
# b&\ =-[T_{m-1}^2(d_{m+1}-d_m)+T_m^2(d_{m-1}-d_{m+1})+T_{m+1}^2(d_m-d_{m-1})]\cdot X^{-1}\\
# c&\ =-[d_{m-1}(T_{m+1}-T_m)\cdot T_m\cdot T_{m+1}+d_m(T_{m-1}-T_{m+1})\cdot T_{m-1}\cdot T_{m+1}+d_{m+1}(T_m-T_{m-1})\cdot T_{m-1}\cdot T_m]\cdot X^{-1}
# \end{aligned}
# \end{equation}
# $$
# 
# with
# 
# $$
# \begin{equation}
# X=(T_{m+1}-T_m)(T_{m-1}-T_{m+1})(T_m-T_{m-1})
# \end{equation}
# $$
# 
# The correlated colour temperature $T=T_x$ is then obtained as follows:
# 
# $$
# \begin{equation}
# T_X=-\cfrac{b}{2a}\qquad\because d^\prime(T)=2aT_x+b=0
# \end{equation}
# $$
# 
# The correction factor $T_{x,cor}$ for nonlinearity is applied as described in the [triangular solution](#Triangular-Solution) method.
# 
# $D_{uv}$ is then calculated as follows:
# 
# $$
# \begin{equation}
# D_{uv}=SIGN(v_x-v_{T_x})\cdot(aT_{x,cor}^2+bT_{x,cor}+c)
# \end{equation}
# $$
# 
# with
# 
# $$
# \begin{equation}
# SIGN(z)=1\ for\ z \geq0\ and\ SIGN(z)=-1\ for\ z <0
# \end{equation}
# $$

# ### Combined Solution

# The parabolic solution works accurately except in on or near the Planckian locus. Taking triangular solution results for $|D_{uv}| < 0.002$ and the parabolic solution results for other regions solves that problem. <a name="back_reference_4"></a><a href="#reference_4">[4]</a>
# 
# The `colour.uv_to_CCT_Ohno2013` definition is used to calculate the correlated colour temperature $T_{cp}$ and distance $D_{uv}$ ($d_i$):

# In[10]:


colour.temperature.uv_to_CCT_Ohno2013((0.19783451566098664, 0.31221744678060825))


# Precision can be changed by passing a value to the *iterations* argument:

# In[11]:


for i in range(10):
    print(colour.temperature.uv_to_CCT_Ohno2013(
        (0.19783451566098664, 0.31221744678060825), iterations=i + 1))


# Using the `colour.uv_to_CCT` wrapper definition:

# In[12]:


colour.uv_to_CCT((0.19783451566098664, 0.31221744678060825), 'Ohno 2013')


# > Note: `'ohno2013'` is defined as a convenient alias for `'Ohno 2013'`:

# In[13]:


colour.uv_to_CCT((0.19783451566098664, 0.31221744678060825), 'ohno2013')


# Converting from correlated colour temperature $T_{cp}$ and distance $D_{uv}$ to chomaticity coordinates $uv$:

# In[14]:


colour.CCT_to_uv((6503.03994225557, 0.0032556165414977167), 'Ohno 2013')


# In[15]:


colour.CCT_to_uv((6503.03994225557, 0.0032556165414977167), 'Ohno 2013')


# ## McCamy (1992) Method

# McCamy (1992) proposed an equation to compute correlated colour temperature $T_{cp}$ from *CIE 1931 2° Standard Observer* chromaticity coordinates $x$, $y$ by using a chromaticity epicenter ($x_e$, $y_e$) where the isotemperature lines in some of the correlated colour temperature range converge and the inverse slope of the line $n$ that connects it to $x$, $y$. <a name="back_reference_5"></a><a href="#reference_5">[5]</a>
# 
# The cubic approximation equation is defined as follows: <a name="back_reference_5"></a><a href="#reference_5">[5]</a>
# 
# $$
# \begin{equation}
# T_{cp}=-449n^3+3525n^2-6823.3n+5520.33
# \end{equation}
# $$
# 
# where
# 
# $$
# \begin{equation}
# n=\cfrac{x-x_e}{y-ye}\\
# x_e=0.3320\qquad y_e=0.1858
# \end{equation}
# $$
# 
# The `colour.xy_to_CCT_mccamy` definition is used to calculate the correlated colour temperature $T_{cp}$ from *CIE 1931 2° Standard Observer* chromaticity coordinates $x$, $y$:

# In[16]:


colour.temperature.xy_to_CCT_McCamy1992((0.31271, 0.32902))


# The `colour.xy_to_CCT` definition is implemented as a wrapper for various correlated colour temperature computation methods from *CIE 1931 2° Standard Observer* chromaticity coordinates $x$, $y$:

# In[17]:


colour.xy_to_CCT((0.31271, 0.32902), 'McCamy 1992')


# > Note: `'mccamy1992'` is defined as a convenient alias for `'McCamy 1992'`:

# In[18]:


colour.xy_to_CCT((0.31271, 0.32902), 'mccamy1992')


# ## Hernandez-Andres, Lee and Romero (1999) Method

# Hernandez-Andres, Lee and Romero (1999) extended McCamy (1992) work by using a second epicenter to extend the accuracy over a wider correlated colour temperature and chromaticity coordinates range ($3000$–$10^6K$). <a name="back_reference_6"></a><a href="#reference_6">[6]</a>
# 
# The new extended equation to calculate the correlated colour temperature $T_{cp}$ is defined as follows: <a name="back_reference_6"></a><a href="#reference_6">[6]</a>
# 
# $$
# \begin{equation}
# T_{cp}=A_0+A_1exp(-n/t_1)+A_2exp(-n/t_2)+A_3exp(-n/t_3)
# \end{equation}
# $$
# 
# where
# 
# $$
# \begin{equation}
# n=\cfrac{x-x_e}{y-ye}\\
# \end{equation}
# $$
# 
# with
# 
# | Constants | $T_{cp}$ Range ($K$) $3000$-$50,000$ | $T_{cp}$ Range ($K$) $50,000$-$8\times10^5$ |
# |:---------:|:------------------------------------:|:-------------------------------------------:|
# | $A_0$     | $-949.86315$                         | $36284.48953$                               |
# | $A_1$     | $6253.80338$                         | $0.00228$                                   |
# | $t_1$     | $0.92159$                            | $0.07861$                                   |
# | $A_2$     | $28.70599$                           | $5.4535\times10^{-36}$                      |
# | $t_2$     | $0.20039$                            | $0.01543$                                   |
# | $A_3$     | $0.00004$                            |                                             |
# | $t_3$     | $0.07125$                            |                                             |
# | $x_e$     | $0.3366$                             | $0.3356$                                    |
# | $y_e$     | $0.1735$                             | $0.1691$                                    |
# 
# The `colour.xy_to_CCT_hernandez` definition is used to calculate the correlated colour temperature $T_{cp}$ from *CIE 1931 2° Standard Observer* chromaticity coordinates $x$, $y$:

# In[19]:


colour.temperature.xy_to_CCT_Hernandez1999((0.31271, 0.32902))


# Using the `colour.xy_to_CCT` wrapper definition:

# In[20]:


colour.xy_to_CCT((0.31271, 0.32902), 'Hernandez 1999')


# > Note: `'hernandez1999'` is defined as a convenient alias for `'Hernandez 1999'`:

# In[21]:


colour.xy_to_CCT((0.31271, 0.32902), 'hernandez1999')


# ## Krystek (1985) Method

# Krystek (1985) proposed a polynomial approximation valid from $1000K$ to $15000K$. <a name="back_reference_7"></a><a href="#reference_7">[7]</a>
# 
# The *CIE UCS* colourspace chromaticity coordinates $u$, $v$ are given by the following equations: <a name="back_reference_7"></a><a href="#reference_7">[7]</a>
# 
# $$
# \begin{equation}
# \begin{aligned}
# u&\ =\cfrac{0.860117757 + 1.54118254 \times 10^{-4} T + 1.28641212 \times 10^{-7} T^2}{1 + 8.42420235 \times 10^{-4} T + 7.08145163 \times 10^{-7} T^2}\\
# v&\ =\cfrac{0.317398726 + 4.22806245 \times 10^{-5} T + 4.20481691 \times 10^{-8} T^2}{1 - 2.89741816 \times 10^{-5} T + 1.61456053 \times 10^{-7} T^2}
# \end{aligned}
# \end{equation}
# $$
# 
# The `colour.CCT_to_uv_Krystek1985` definition is used to calculate the *CIE UCS* colourspace chromaticity coordinates $u$, $v$ from correlated colour temperature $T_{cp}$:

# In[22]:


colour.temperature.CCT_to_uv_Krystek1985(6504.389383048972)


# Using the `colour.CCT_to_uv` wrapper definition:

# In[23]:


colour.CCT_to_uv(6504.389383048972, 'Krystek 1985')


# ## Kang et al. (2002) Method

# Kang et al. (2002) proposed an advanced colour-temperature control system for HDTV applications in the range from $1667K$ to $25000K$. <a name="back_reference_8"></a><a href="#reference_8">[8]</a>
# 
# The *CIE 1931 2° Standard Observer* chromaticity coordinates $x$, $y$ are given by the following equations: <a name="back_reference_8"></a><a href="#reference_8">[8]</a>
# 
# $$
# \begin{equation}
# \begin{aligned}
# x&\ =\begin{cases}-0.2661239\cfrac{10^9}{T_{cp}^3}-0.2343589\cfrac{10^6}{T_{cp}^2}+0.8776956\cfrac{10^3}{T_{cp}}+0.179910 & for\ 1667K\leq T_{cp}\leq4000k\\
# -3.0258469\cfrac{10^9}{T_{cp}^3}+2.1070379\cfrac{10^6}{T_{cp}^2}+0.2226347\cfrac{10^3}{T_{cp}}+0.24039 & for\ 4000K\leq T_{cp}\leq25000k\end{cases}\\
# y&\ =\begin{cases}-1.1063814x^3-1.34811020x^2+2.18555832x-0.20219683 & for\ 1667K\leq T_{cp}\leq2222k\\
# -0.9549476x^3-1.37418593x^2+2.09137015x-0.16748867 & for\ 2222K\leq T_{cp}\leq4000k\\
# 3.0817580x^3-5.8733867x^2+3.75112997x-0.37001483 & for\ 4000K\leq T_{cp}\leq25000k\end{cases}
# \end{aligned}
# \end{equation}
# $$
# 
# The `colour.CCT_to_xy_kang` definition is used to calculate the *CIE 1931 2° Standard Observer* chromaticity coordinates $x$, $y$ from correlated colour temperature $T_{cp}$:

# In[24]:


colour.temperature.CCT_to_xy_Kang2002(6504.389383048972)


# The `colour.CCT_to_xy` definition is implemented as a wrapper for various *CIE 1931 2° Standard Observer* chromaticity coordinates $x$, $y$ computation from correlated colour temperature:

# In[25]:


colour.CCT_to_xy(6504.389383048972, 'Kang 2002')


# > Note: `'kang2002'` is defined as a convenient alias for `'Kang 2002'`:

# In[26]:


colour.CCT_to_xy(6504.389383048972, 'kang2002')


# ## *CIE Illuminant D Series* Method

# Judd et al. (1964) defined the following equations to calculate the *CIE 1931 2° Standard Observer* chromaticity coordinates $x_D$, $y_D$ of a *CIE Illuminant D Series*: <a name="back_reference_9"></a><a href="#reference_9">[9]</a>
# 
# $$
# \begin{equation}
# \begin{aligned}
# x_D&\ =\begin{cases}-4,6070\cfrac{10^9}{T_{cp}^3}+2.9678\cfrac{10^6}{T_{cp}^2}+0.09911\cfrac{10^3}{T_{cp}}+0.244063 & for\ 4000K\leq T_{cp}\leq7000k\\
# -2.0064\cfrac{10^9}{T_{cp}^3}+1.9018\cfrac{10^6}{T_{cp}^2}+0.24748\cfrac{10^3}{T_{cp}}+0.237040 & for\ 7000K\leq T_{cp}\leq25000k\end{cases}\\
# y_D&\ =-3.000x_D^2+0.2.870x_D-0.275
# \end{aligned}
# \end{equation}
# $$
# 
# The `colour.CCT_to_xy_CIE_D` definition is used to calculate the *CIE 1931 2° Standard Observer* chromaticity coordinates $x$, $y$ of a *CIE Illuminant D Series* from correlated colour temperature $T_{cp}$:

# In[27]:


colour.temperature.CCT_to_xy_CIE_D(6504.389383048972)


# Using the `colour.CCT_to_xy` wrapper definition:

# In[28]:


colour.CCT_to_xy(6504.389383048972, 'CIE Illuminant D Series')


# > Note: `'daylight'` is defined as a convenient alias for `'CIE Illuminant D Series'`:

# In[29]:


colour.CCT_to_xy(6504.389383048972, 'daylight')


# ## Bibliography

# 1. <a href="#back_reference_1">^<a> <a name="reference_1"></a>CIE. (n.d.). 17-231 colour temperature [Tc]. Retrieved from http://eilv.cie.co.at/term/231
# 2. <a href="#back_reference_2">^<a> <a name="reference_2"></a>CIE. (n.d.). 17-258 correlated colour temperature [Tcp]. Retrieved from http://eilv.cie.co.at/term/258
# 3. <a href="#back_reference_3">^<a> <a name="reference_3"></a>Wyszecki, G., & Stiles, W. S. (2000). DISTRIBUTION TEMPERATURE, COLOR TEMPERATURE, AND CORRELATED COLOR TEMPERATURE. In Color Science: Concepts and Methods, Quantitative Data and Formulae (pp. 224–229). Wiley. ISBN:978-0471399186
# 4. <a href="#back_reference_4">^<a> <a name="reference_4"></a>Ohno, Y. (2014). Practical Use and Calculation of CCT and Duv. LEUKOS, 10(1), 47–55. doi:10.1080/15502724.2014.839020
# 5. <a href="#back_reference_5">^<a> <a name="reference_5"></a>Wikipedia. (n.d.). Approximation. Retrieved June 28, 2014, from http://en.wikipedia.org/wiki/Color_temperature#Approximation
# 6. <a href="#back_reference_6">^<a> <a name="reference_6"></a>Hernández-Andrés, J., Lee, R. L., & Romero, J. (1999). Calculating correlated color temperatures across the entire gamut of daylight and skylight chromaticities. Applied Optics, 38(27), 5703–5709. doi:10.1364/AO.38.005703
# 7. <a href="#back_reference_7">^<a> <a name="reference_7"></a>Krystek, M. (1985). An algorithm to calculate correlated colour temperature. Color Research & Application, 10(1), 38–40. doi:10.1002/col.5080100109
# 8. <a href="#back_reference_8">^<a> <a name="reference_8"></a>Kang, B., Moon, O., Hong, C., Lee, H., Cho, B., & Kim, Y. (2002). Design of advanced color: Temperature control system for HDTV applications. Journal of the Korean …, 41(6), 865–871. Retrieved from http://cat.inist.fr/?aModele=afficheN&cpsidt=14448733
# 9. <a href="#back_reference_9">^<a> <a name="reference_9"></a>Wyszecki, G., & Stiles, W. S. (2000). CIE Method of Calculating D-Illuminants. In *Color Science: Concepts and Methods, Quantitative Data and Formulae* (pp. 145–146). Wiley. ISBN:978-0471399186