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Light level examples

The following table gives examples of light levels that are encountered in everyday life.

Situation

Illuminance [lx]

Luminance of 90%

Luminance of 18%

diffuse reflector [nt]

diffuse reflector [nt]

 

 

 

 

Clear, bright sunlight at noon

100 000

30 000

6 000

 

 

 

 

Typical daylight

10 000

3 000

600

 

 

 

 

Overcast daylight sky; TV studio

1 000

300

60

 

 

 

 

Very dark overcast sky; living room

100

30

6

 

 

 

 

Twilight; candle at 33 cm

10

3

0.6

 

 

 

 

Deep twilight; candle at 1 m

1

0.3

0.06

 

 

 

 

Full moon overhead, clear sky

0.1

0.03

0.006

 

 

 

 

Half moon overhead, clear sky

0.01

0.003

0.000 6

 

 

 

 

Starlight + airglow

0.002

 

 

 

 

 

 

Total starlight, overcast night

0.000 1

 

 

 

 

 

 

Sirius (mv = -1.47)

0.000 01

 

 

Vega (mv = 0)

0.000 003

 

 

Table B.2 Light level examples

Michael Brill and Bob Hunt agree that R, G, and B tristimulus values have no units. See Hunt, R.W.G. (1997),“The heights of the CIE colour-matching functions,” in Color Research and Application, 22 (5): 337 (Oct.).

Image science

Absolute luminance has units of cd·m-2, colloquially called nits [nt]. In image science, luminance is usually normalized to a range of 100 (or as I prefer, 1) with respect to a specified or implied white reference, and expressed without units. So normalized, its symbol is Y. The term luminance is often used as shorthand to refer to this pure quantity; however, it is properly called relative luminance. The term luminance factor should be avoided for this quantity, since the latter term refers to a property of a surface or material: Luminance factor is the ratio of luminance of a surface, under specified conditions of light source, incidence, and observation, to the luminance of a perfectly diffusing (“Lambertian”) surface, under the same conditions.

Relative luminance (Y) is one of three distinguished tristimulus values standardized by the CIE; the other two distinguished tristimulus values are X and Z. Other tristimulus values such as [R, G, B] are related to CIE

[X, Y, Z] values by a 3× 3 linear matrix product. Relative luminance (Y) and other tristimulus values such as X, Z, R, G, or B are pure numbers.

578

DIGITAL VIDEO AND HD ALGORITHMS AND INTERFACES

It was inconsistent mixture of US customary (Imperial!) units and SI units that led to the 1998 crash of NASA’s Mars Climate Orbiter. American cinema experts often express luminance in footlamberts; why then do they refer to cinema film as

35 mm instead of 13/8-inch?

106

=

1

10.764

 

0.30482

25.42 122

 

Units

Many bizarre units have been used for illuminance and luminance. I urge you to abandon these, and to adopt the standard SI units. Radiometry and photometry are sufficiently difficult without having to deal with

a plethora of arcane units. If radiometry and photometry are new to you, I believe that your understanding will come more rapidly if you ignore the traditional units – which were deprecated by the scientific community 40 years ago – and adopt the SI units. If you are

a practitioner who learned the science and the craft using the traditional Imperial units, please don't stubbornly stick to them: According to the CIA World Factbook, only three countries – Burma, Liberia, and the United States – have not adopted International System of Units (SI, or metric system) as their official system of weights and measures. I urge you to use SI units. Simply learn to multiply footlamberts by 3.4 to get candelas per meter squared. A movie screen has a typical white luminance of about 14 fL; call this 48 nits. A studio reference display in North America typically has a reference white luminance of about 100 nits (about 33 fL).

To convert illuminance into lux [lx], use Table B.3:

To obtain lm·m–2 [lx],

by

numerically

multiply unit below

 

 

 

lm·ft–2, footcandle, fc

10.764

10.764

metercandle

1

1

 

 

 

Table B.3 Conversion of illuminance into lux

To convert luminance into candelas per meter squared, use Table B.4:

To obtain cd·m–2 [nit, nt],

by

numerically

multiply unit below

 

 

 

lambert, L

10 000 π

3183.1

millilambert, mL

10 π

3.1831

cd·ft–2

10.764

10.764

footlambert, fL

10.764π

3.4263

Table B.4 Conversion of luminance into cd·m–2

APPENDIX B

INTRODUCTION TO RADIOMETRY AND PHOTOMETRY

579

Further reading

Chapter 1 of Ian Ashdown’s book presents a very approachable introduction to measuring light. (The remainder of the book details the computer graphics technique called radiosity.) A version of that chapter is available on the web.

D. Allan Roberts offers a terse summary of the basic quantities of radiometry and photometry, and describes the confusing units. (It is worth seeking out the 1994 edition; sadly, the description of radiometry in the 2006 edition of this handbook is not nearly as lucid.)

Ashdown, Ian (1994), Radiosity: A Programmer’s Perspective

(New York: Wiley).

Ashdown, Ian (2002), Photometry and Radiometry – A Tour Guide for Computer Graphics Enthusiasts,

<http://www.helios32.com/Measuring%20Light.pdf>.

Roberts, D. Allan (1994), “A Guide to Speaking the Language of Radiometry and Photometry,” in Photonics Design and Applications Handbook, 1994 edition, vol. 3, pages H-70 to H-73 (Pittsfield, Mass.: Laurin Publications).

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