Attachment_D_-_NIST_SP250-37-1997.pdf

NIST Special Publication 250-37

NIST MEASUREMENT SERVICES:

PHOTOMETRIC CALIBRATIONS

Yoshihiro Ohno

Optical Technology Division Physics Laboratory National Institute of Standards and Technology Gaithersburg, MD 20899

Supersedes SP250-15

Reprint with changes

July 1997

U.S. DEPARTMENT OF COMMERCE

William M. Daley, Secretary

Technology Administration Gary R. Bachula, Acting Under Secretary for Technology

National Institute of Standards and Technology Robert E. Hebner, Acting Director

RFQ SB1341-16-RQ-0527 - Attachment D - NIST SP250-37-1997

PREFACE

The calibration and related measurement services of the National Institute of Standards and Technology are intended to assist the makers and users of precision measuring instruments in achieving the highest possible levels of accuracy, quality, and productivity. NIST offers over 300 different calibrations, special tests, and measurement assurance services. These services allow customers to directly link their measurement systems to measurement systems and standards maintained by NIST. These services are offered to the public and private organizations alike. They are described in NIST Special Publication (SP) 250, NIST Calibration Services Users Guide.

The Users Guide is supplemented by a number of Special Publications (designated as the “SP250 Series”) that provide detailed descriptions of the important features of specific NIST calibration services. These documents provide a description of the: (1) specifications for the services; (2) design philosophy and theory; (3) NIST measurement system; (4) NIST operational procedures; (5) assessment of the measurement uncertainty including random and systematic errors and an error budget; and (6) internal quality control procedures used by NIST. These documents will present more detail than can be given in NIST calibration reports, or than is generally allowed in articles in scientific journals. In the past, NIST has published such information in a variety of ways. This series will make this type of information more readily available to the user.

This document, SP250-37 (1997), NIST Measurement Services: Photometric Calibrations, is a revision of SP250-15 (1987). It covers the calibration of standards of luminous intensity, luminous flux, illuminance, luminance, and color temperature (test numbers 37010C–37100S in SP250, NIST Calibration Services Users Guide). Inquiries concerning the technical content of this document or the specifications for these services should be directed to the author or to one of the technical contacts cited in SP250.

NIST welcomes suggestions on how publications such as this might be made more useful.

Suggestions are also welcome concerning the need for new calibrations services, special tests, and measurement assurance programs.

Stanley D. Rasberry Katharine B. Gebbie Director Director Measurement Services Physics Laboratory iii

ABSTRACT

The National Institute of Standards and Technology supplies calibrated standards of luminous intensity, luminance, and color temperature, and provides calibration services for submitted artifacts for luminous intensity, luminance, color temperature, total luminous flux, and luminance. The procedures, equipment, and techniques used to perform these calibrations are described. Detailed estimates and procedures for determining uncertainties of the reported values are also presented.

Key words : Calibration; Candela; Color temperature; Illuminance; Lumen; Luminance; Luminous flux; Luminous intensity; Lux; Photometry; Standards; Total flux; Unit iv

TABLE OF CONTENTS

Abstract ···························································································································· iv

1. Introduction ·················································································································· 1

1.1 Photometry, physical photometry, and radiometry ······································· 1

1.2 Photometric quantities and units ··································································· 3

1.2.1 Photometric quantities ···································································· 3

1.2.2 Relationship between the SI units and English units ······················ 6

1.3 NIST photometric units ················································································· 7

1.3.1 NIST luminous intensity unit ························································· 7

1.3.2 NIST luminous flux unit ································································· 9

2. Outline of the calibration services ··············································································· 10

3. Luminous intensity (candela) calibrations ···································································11

3.1 NIST illuminance unit and the NIST candela ·············································· 11

3.1.1 Principles of the detector-based candela realization ······················· 11

3.1.2 Design of the NIST standard photometers ····································12

3.1.3 Calibration of the NIST standard photometers ·······························13

3.1.4 Spectral mismatch correction ························································13

3.1.5 Correction for the photometer temperature ·································· 14

3.1.6 Linearity of the NIST standard photometers ································ 15

3.1.7 Uncertainty of the NIST illuminance unit and the candela realization ······················································································ 16

3.1.8 Long-term stability of the NIST standard photometers ··············· 17

3.2 Artifacts for calibration ················································································ 18

3.2.1 Type of test lamps and their characteristics ································· 18

3.2.2 Alignment of test lamps ································································ 20

3.2.3 Operation and handling of test lamps ·········································· 21

3.3 Equipment for calibration ············································································ 22

3.3.1 Photometry bench ········································································· 22

3.3.2 Electrical power supply ································································ 23

3.4 Calibration procedures ················································································· 23

3.5 Uncertainty of calibration ············································································ 24 v

4. Illuminance calibrations ······························································································· 25

4.1 Equipment for calibration ············································································· 25

4.2 Artifacts for calibration ················································································ 25

4.2.1 Types of photometers and illuminance meters ······························ 25

4.2.2 Operation and handling of photometers and illuminance meters ··· 26

4.3 Calibration procedures ················································································· 26

4.3.1 Illuminance responsivity of photometers ······································26

4.3.2 Illuminance meter calibration ························································· 27

4.4 Uncertainty of calibration ·············································································28

5. Total luminous flux calibrations ·················································································· 29

5.1 NIST luminous flux unit ·············································································· 29

5.1.1 Principles of the Absolute Integrating Sphere Method ················· 30

5.1.2 Design of the NIST integrating sphere for the lumen realization ··· 31

5.1.3 Correction for the spatial nonuniformity of the sphere

responsivity ·················································································· 32

5.1.4 Incident angle dependence correction ············································ 33

5.1.5 Spectral mismatch correction ······················································· 34

5.1.6 Calibration of the primary standard lamps ··································· 35

5.2 Artifacts for calibration ················································································ 36

5.2.1 Types of test lamps ······································································ 36

5.2.2 Operation and handling of test lamps ··········································· 37

5.3 Equipment for calibration ············································································· 37

5.3.1 2 m integrating sphere ··································································· 37

5.3.2 Electrical facility for incandescent lamps ······································ 40

5.3.3 Electrical facility for fluorescent lamps ········································· 40

5.4 Calibration procedures ················································································· 41

5.4.1 Correction for the sphere detector temperature ···························· 41

5.4.2 Self-absorption correction ····························································· 42

5.4.3 Spectral mismatch correction ·························································42

5.4.4 Correction for the spatial nonuniformity of the sphere response··· 43

5.4.5 Determination of luminous flux ····················································· 44

5.5 Uncertainty of calibration ············································································ 45

6. Luminance calibrations ································································································ 46

6.1 NIST luminance unit ···················································································· 46

6.2 Artifacts for calibration ·················································································48

6.3 Equipment for calibration ············································································· 49

TABLE OF CONTENTS (continued) vi

6.4 Calibration of luminance sources ·································································· 50

6.5 Calibration of luminance meters ·································································· 51

6.6 Calibration of opal glass luminance coefficient ··········································· 52

6.6.1 Calibration procedures ····································································52

6.6.2 Use of opal glass standards for luminance coefficient ···················· 53

6.6.3 Uncertainty of calibration ·······························································54

7. Color temperature calibrations ···················································································· 55

7.1 General descriptions ····················································································· 55

7.2 NIST color temperature scale ······································································ 56

7.3 Artifacts for calibration ················································································ 57

7.4 Equipment for calibration ············································································· 57

7.5 Calibration procedures ················································································· 59

7.6 Uncertainty of calibration ············································································ 60

8. Future work ··············································································································· 61

8.1 Total spectral radiant flux scale realization ·················································· 61

8.2 Total luminous flux calibration of other discharge lamps ····························· 62

8.3 Issuing calibrated standard lamps ································································· 62

8.4 Flashing light photometric standards ··························································· 62

8.5 High illuminance calibration ········································································· 62

Acknowledgments ··········································································································· 63

References ······················································································································· 64

Appendix A - State of the NIST photometric units in international intercomparisons · A1

Appendix B - SP250, Optical Radiation Measurements, Chapter 7 ···························· A2

Appendix C - Samples of calibration reports ······························································· A5

TABLE OF CONTENTS (continued) vii

LIST OF FIGURES

Figure 1 CIE V(λ) Function ································································································· 2 Figure 2 Realization and maintenance of the NIST photometric units ······························ 7 Figure 3 Construction of the High Accuracy Cryogenic Radiometer ································· 8 Figure 4 Geometry for the detector-based candela realization ·········································· 11 Figure 5 Design of the NIST standard photometer ·························································· 13 Figure 6 Polynomial fit for the spectral mismatch correction factors ······························· 14 Figure 7 The temperature dependence of the photometers’ illuminance responsivity ······ 15 Figure 8 Linearity of one of the NIST standard photometers ··········································· 15 Figure 9 Drift of the illuminance responsivity of the NIST standard photometers over a 5 year period ····································································································· 17 Figure 10 Appearance of the luminous intensity standard lamps and their electrical polarity ················································································································ 18 Figure 11 Aging characteristics of a typical Airway Beacon type lamp at 2856 K ············ 19 Figure 12 Aging characteristics of a selected FEL type lamp at 2856 K ·····························19 Figure 13 Spatial nonuniformity of a typical FEL type lamp ·············································20 Figure 14 Alignment of the bi-post base socket using a jig and a laser beam ······················ 21 Figure 15 Alignment of the distance origin ········································································· 21 Figure 16 NIST Photometry Bench ····················································································22 Figure 17 Basic geometry of the Absolute Integrating Sphere Method ······························· 30 Figure 18 Geometry of the integrating sphere for the luminous flux unit realization ········· 31 Figure 19 SRDF of the NIST 2 m integrating sphere. (θ = 0 is at the detector. φ = 0 is the plane passing through the sphere bottom.) ··················································· 33 Figure 20 NIST 2 m integrating sphere set up for routine calibrations ······························· 38 Figure 21 Spectral characteristics of the NIST integrating sphere ·······································39 Figure 22 Spectral mismatch correction factor of the NIST 2 m integrating sphere as a function of the color temperature of a Planckian source ······························ 39 Figure 23 Measurement circuit for a rapid start fluorescent lamp ······································ 41 Figure 24 Arrangement for NIST luminance unit realization ·············································· 47 Figure 25 Relative spectral responsivity of the reference luminance meter ························ 49 Figure 26 Configuration for opal glass calibration ······························································· 53 Figure 27 Realization of the NIST spectral irradiance scale and the color temperature scale ····················································································································· 56 Figure 28 Configuration for color temperature calibration ·················································· 58 Figure 29 Color temperature correction values for the NIST diode-array spectroradiometer ································································································ 59 viii

LIST OF TABLES

Table 1 Quantities and units used in photometry and radiometry ···································· 4 Table 2 English units and definition ·················································································· 6 Table 3 Conversion between English units and SI units ···················································· 6 Table 4 NIST Photometric Calibration Services ·······························································10 Table 5 Uncertainty budget for the NIST illuminance unit realization ···························· 16 Table 6 Uncertainty budget for the NIST candela realization ·········································· 16 Table 7 Uncertainty budget for luminous intensity calibrations (typical) ······················· 24 Table 8 Uncertainty budget for illuminance responsivity calibrations (typical) ·············28 Table 9 Uncertainty budget for the calibration of an illuminance meter (an example) ····· 29 Table 10 Uncertainty budget for the NIST 1995 luminous flux unit ································· 36 Table 11 Uncertainty budget for total luminous flux calibrations of standard incandescent lamps (typical) ··············································································· 45 Table 12 Uncertainty budget for total luminous flux calibrations of 4 ft linear fluorescent lamps (typical) ················································································· 46 Table 13 Uncertainty budget for the NIST luminance unit realization ······························· 48 Table 14 Uncertainty budget for luminance source calibrations (typical) ··························50 Table 15 Uncertainty budget for luminance meter calibrations (typical) ··························· 52 Table 16 Uncertainty budget for opal glass calibrations ····················································· 54 Table 17 The uncertainty of the spectral irradiance calibration with respect to the

NIST spectral radiance scale ·············································································· 60 Table 18 The uncertainty budget for the NIST color temperature calibration ·················· 60 ix

1. Introduction

This document supersedes the NBS Special Publication 250-15 (1987). In 1992, a new candela was realized based on an absolute cryogenic radiometer, and the old NIST gold-point blackbody-based unit [1] was replaced by the new detector-based unit [2]. A group of eight standard photometers with calibrations based on the cryogenic radiometer holds the NIST candela, and replaces the lamp scheme formerly used. Further, the photometric calibration procedures have been revised to utilize the detector-based methods [3].

This document describes the new photometric calibration procedures for luminous intensity (candela; cd), illuminance (lux; lx), total luminous flux (lumen; lm), luminance (cd/m2) and color temperature (kelvin; K). Throughout this document, uncertainty statements follow the NIST policy given by Taylor and Kuyatt [4], which prescribes the use of an expanded uncertainty with a coverage factor k = 2 for uncertainties of all NIST calibrations.

Descriptions for the individual standards and calibrations available from NIST, as of April 1996, are listed and explained in Section 2. Updated information about calibration services and prices are published periodically in the NIST Calibration Services Users Guide (SP250) [5] and Fee Schedule (SP250 Appendix).

The material presented in this document describes photometric calibration facilities and procedures as they existed at the time of publication. Further improvement of photometric calibration facilities and procedures are underway. Some of these on-going projects are described in Section 8.

1.1 Photometry, physical photometry, and radiometry

The primary aim of photometry is to measure visible optical radiation, light, in such a way that the results correlate with what the visual sensation is to a normal human observer exposed to that radiation. Until about 1940, visual comparison techniques of measurements were predominant in photometry, whereby an observer was required to match the brightness of two visual fields viewed either simultaneously or sequentially. This method of photometry is so-called visual photometry, and is seldom used today.

In modern photometric practice, measurements are made with photodetectors. This is referred to as physical photometry. In order to achieve the aim of photometry, one must take into account the characteristics of human vision. The relative spectral responsivity of the human eye was first defined by CIE (Commission Internationale de l’Éclairage) in 1924 [6], and redefined as part of colorimetric standard observers in 1931 [7]. It is called the spectral luminous efficiency function for photopic vision, or the V(λ) function, defined in the domain 360 nm to 830 nm, and is normalized to one at its peak, 555 nm (Fig. 1). This model gained wide acceptance, republished by CIE in 1983 [8] and published by CIPM (Comité International des Poids et Mesures) in 1982 [9] to supplement the 1979 definition of candela. The tabulated values of the function at 1 nm increments are available in references [8-10]. In most cases, the

– 1 – region 380 nm to 780 nm is used for calculation with negligible errors because the V(λ) function falls below 10-4 outside this region. Thus, a photodetector having a spectral responsivity matched to the V(λ) function replaced the role of human eyes in photometry.

0.2

0.4

0.6

0.8

1.2

350 400 450 500 550 600 650 700 750 va lu e

Wavelength (nm)

Figure 1 CIE V(λ) Function.

Radiometry concerns physical measurement of optical radiation as a function of its wavelength. As specified in the definition of the candela by CGPM (Conférence Générale des Poids et Mesures) in 1979 [11] and CIPM in 1982 [9], a photometric quantity Xv is defined in relation to the corresponding radiometric quantity Xe,λ by the equation:

Xv = Km Xe, λ V(λ) dλ

360 nm

830 nm

(1)

The constant, Km, relates the photometric quantities and radiometric quantities, and is called the maximum spectral luminous efficacy (of radiation) for photopic vision. The value of Km is given by the 1979 definition of candela which defines the spectral luminous efficacy of light at the frequency 540 x 1012 Hz (at the wavelength 555.016 nm in standard air) to be 683 lm/W. The value of Km is calculated as 683 x V(555.000 nm)/V(555.016 nm) = 683.002 lm/W [8]. Km is normally rounded to 683 lm/W with negligible errors [9]. Various photometric and radiometric quantities are described in the next section.

It should be noted that the V(λ) function is based on the CIE standard photometric observer for photopic vision, which assumes additivity of sensation and a 2° field of view at relatively high luminance levels (higher than ~1 cd/m2). The human vision in this level is called photopic vision. The spectral responsivity of human vision deviates significantly at very low levels of luminance (less than ~10-2 cd/m2). This type of vision is called scotopic vision. Its

– 2 – spectral responsivity, peaking at 507 nm, is designated by the V’(λ) function, which was defined by CIE in 1951 [12], recognized by CIPM (Comité International des Poids et Mesures) in 1976 [13], and republished by CIPM in 1982 [9]. The human vision in the region between photopic vision and scotopic vision is called mesopic vision. While active research is being conducted [14], there is no internationally accepted spectral luminous efficiency function for the mesopic region yet. In current practice, almost all photometric quantities are given in terms of photopic vision, even at low light levels, except for special measurements for research purposes.

This document, therefore, does not deal with quantities specified in terms of scotopic or mesopic vision. Further details of definitions outlined in this section are given in Reference [8].

To better understand the international metrology system, it is useful to know the relationship between such organizations as CGPM, CIPM, CCPR (Comité Consultatif de Photométrie et Radiométrie), BIPM (Bureau International des Poids et Mesures), and CIE.

These are all abbreviations of their French names as appeared before. In English, their names would be: CGPM, General Conference of Weights and Measures; CIPM, International Committee for Weights and Measures; CCPR, Consultative Committee of Photometry and Radiometry; BIPM, International Bureau of Weights and Measures; and CIE, International Commission on Illumination. All the SI units are officially defined by CGPM which is the decision-making body for the Treaty of the Meter (Convention du Mètre), signed in 1875. The decisions of CGPM legally govern the global metrology system among those countries signatory to the Treaty of the Meter or agreeing to its usage. CIPM is a committee under CGPM, charged with the management of the international system of units and related fundamental units, consisting of many subcommittees for each technical field. CCPR is a subcommittee under CIPM, that discusses and recommends the units in photometry and radiometry. It consists of representatives of interested national standardizing laboratories. CCPR also holds international intercomparisons of photometric units and radiometric scales. BIPM is a metrology laboratory under the supervision of CIPM, with staff and facilities in Paris. CIE, on the other hand, is originally an academic society in the field of lighting science and was organized to promote uniformity and quality in optical measurements. Many definitions developed by CIE, such as the V(λ) function, the color matching functions, and the standard illuminants, have been adopted by CGPM and by ISO (International Organization for Standardization) as international standards. CIE has recently been recognized officially by ISO as a standards-creating body in the field of optical radiation. NIST staff play active roles in CCPR and CIE activities.

1.2 Photometric quantities and units

1.2.1 Photometric quantities

The base unit of all photometric quantities is the candela. The candela was first defined by CGPM in 1948, based on the radiation from platinum at the temperature of its solidification. It

– 3 – became one of the base SI (Système International) units when SI was established in 1960. Most recently, the candela was redefined by CGPM in 1979 [9] as

“The candela is the luminous intensity, in a given direction, of a source that emits monochromatic radiation of frequency 540 x 1012 hertz and that has a radiant intensity in that direction of (1/683) watt per steradian.”

Table 1 lists photometric quantities and their corresponding radiometric quantities side by side, with units and symbols. The precise definition of each quantity is given by CCPR [10] and

CIE [15].

Table 1. Quantities and units used in photometry and radiometry relationship Photometric quantity Unit with lumen Radiometric Quantity Unit Luminous flux lm (lumen) Radiant flux W (watt) Luminous intensity cd (candela) lm sr-1 Radiant intensity W sr-1

Illuminance lx (lux) lm m-2 Irradiance W m-2

Luminance cd m-2 lm sr-1 m-2 Radiance W sr-1 m-2

Luminous exitance lm m-2 Radiant exitance W m-2

Luminous exposure lx s Radiant exposure W m-2 s Luminous energy lm s Radiant energy J (joule) Color temperature K (kelvin) Radiance temperature K

Although the candela is defined as an SI base unit, luminous flux (lumen) is perhaps the most fundamental photometric quantity, as the four other photometric quantities are defined in terms of lumen with appropriate geometric factors.

Luminous flux (Φv) is the time rate of flow of light as weighted by V(λ). It is defined as

ΦV = Km Φe, λ V(λ) dλ λ

, (2) where Φe,λ is the spectral concentration of radiant flux in (W/nm) as a function of wavelength λ in nm.

Luminous intensity (Iv) is the luminous flux (from a point source) emitted per unit solid angle in a given direction. It is defined as

IV =

dΦV dΩ , (3) where dΦv is the luminous flux leaving the source and propagating in an element of solid angle dΩ containing the given direction.

– 4 –

Illuminance (Ev) is the density of the luminous flux incident on a given point of a surface or a plane. It is defined as

EV =

dΦV dA , (4) where dΦv is the luminous flux incident on an element dA of the surface containing the point.

Luminance (Lv) is the luminous flux from an element of a surface surrounding a given point, emitted into a small solid angle containing the given direction, per unit area of the element projected on a plane perpendicular to that given direction. It is defined as

LV =

d2Φ V dΩ d A cos θ , (5) where dΦv is the luminous flux emitted (reflected or transmitted) by an elementary beam passing through the given point and propagating in the solid angle dΩ containing the given direction; dA is the area of a section of that beam containing the given point; θ is the angle between the normal to that section and the direction of the beam.

Luminous exitance (Mv) is the density of luminous flux leaving a surface at a point. The equation is the same as equation (4), with dΦv meaning the luminous flux leaving a surface. This quantity is rarely used in the general practice of photometry.

Luminous exposure (Hv) is the time integral of illuminance Ev(t) over a given duration ∆t, as defined by

Hv = Ev(t)

∆t dt . (6)

Luminous energy (Qv) is the time integral of the luminous flux (Φv) over a given duration ∆t, as defined by

Qv = Φv(t)

∆t dt . (7)

Color temperature (Tc) is the temperature of a Planckian radiator with radiation of the same chromaticity as that of the light source in question. However, the chromaticity coordinates of most lamps do not fall on the Planckian locus, and in actual lamp calibrations, either distribution temperature or correlated color temperature is used. “Color temperature” is often used informally for the correlated color temperature.

Distribution temperature (Td) is the temperature of a blackbody with a spectral power distribution closest to that of the light source in question, and it is a useful concept for quasi- Planckian sources.

Correlated color temperature (Tcp) is a concept used for sources with a spectral power distribution significantly different from that of Planckian radiation, for example, discharge lamps.

– 5 –

Correlated color temperature is the temperature of the Planckian radiator whose perceived color most closely resembles that of the light source in question. The distribution temperature and correlated color temperature are explained further in Section 7.

General information (definitions, symbols, and expressions) on many other physical quantities and units including photometric and radiometric quantities are given in Reference [16].

1.2.2 Relationship between SI units and English units

Under NIST policy [17], results of all NIST measurements are reported in SI units.

However, the English units shown in Table 2 are still rather widely used. For all the photometric measurements and calculations, use of the SI units shown in Table 1 is recommended, and use of non-SI units is discouraged [18]. The definitions of the English units are described below for conversion purposes only.

Table 2. English units and definition

Unit Quantity Definition foot-candle (fc) illuminance lumen per square foot (lm ft-2) foot-Lambert (fL) luminance 1/π candela per square foot (π-1 cd ft-2)

It should be noted that the definition of foot-Lambert is such that the luminance of a perfect diffuser is 1 fL when illuminated at 1 fc. In SI units, the luminance of a perfect diffuser would be 1/π (cd/m2) when illuminated at 1 lx. For convenience of changing from English units to SI units, the conversion factors are listed in Table 3. For example, 1000 lx is the same illuminance as

92.9 fc, and 1000 cd/m2 is the same luminance as 291.9 fL. Conversion factors to and from some other units are given in Reference [19].

Table 3. Conversion between English units and SI units

To obtain the value in multiply the value in by lx from fc fc 10.764 fc from lx lx 0.09290 cd/m2 from fL fL 3.4263 fL from cd/m2 cd/m2 0.29186 m (meter) from feet feet 0.30480 mm (millimeter) from inch inch 25.400

– 6 –

1.3 NIST photometric units

1.3.1 NIST Luminous intensity unit

Until 1991, the NIST luminous intensity unit was derived from the NIST spectral irradiance scale [20], which was based on a gold-point blackbody, and therefore, dependent on the temperature scale. In 1990, the international temperature scale was revised [21], and the gold point temperature changed from 1337.58 K to 1337.33 K. Due to this change, the magnitude of NIST luminous intensity unit increased by 0.35 %.

In 1992 at NIST, a new luminous intensity unit (candela) was realized based on the absolute responsivity of detectors (using a 100 % Q.E. silicon detectors [2] and subsequently a cryogenic electrical substitution radiometer [3]). The old luminous intensity unit was replaced with the new unit in 1992.

The new candela is realized and maintained on a group of standard photometers (referred to as the NIST standard photometers) which are calibrated for illuminance responsivity in A/lx.

These standard photometers also embody the NIST illuminance unit, and allow luminous intensity to be determined from measured illuminance and distance. The realization and maintenance of the photometric units at NIST are shown in Figure 2. The NIST cryogenic

– 7 –

Absolute Spectral Responsivity Scale

(Silicon Photodiodes)

Luminous Intensity Unit (Transfer Lamps)

Illuminance Responsivity Scale

(Standard Photometers)

Absolute Cryogenic

Radiometer (HACR)

Absolute Spectral Response Transfer

Absolute Spectral Response Transfer Aperture Area Measurement Calculation based on Candela Definition

[A/W]

[ A/lx ]

[ cd ]

Distance Measurement

Interpolation

Luminous Flux Unit ( Primary / Working Standard Lamps )

Luminous Flux Transfer Lamps

Measurements with 2 m Integrating Sphere

Integrating Sphere Method

[ lm ]

Luminance Unit (Primary / Working Standard Sources)

Distance Measurement Aperture Area

Transfer Luminance Sources /

Luminance Meters

Measurements with Reference Luminance Meter

[W]

Figure 2 Realization and maintenance of the NIST photometric units.

radiometer [22] acts as the absolute radiometric base at the top of the chain. The radiometer (called HACR; High Accuracy Cryogenic Radiometer) is cooled by liquid helium to 5 K, and works on the principle of electrical substitution. The construction of the HACR is shown in Figure 3. Based on laser-beam power measurements with the HACR at several wavelengths, the NIST detector spectral responsivity scale is maintained on silicon photodiode light-trapping detectors [23]. The measurement uncertainty in the calibration of a light-trapping detector against the HACR is 0.06 % (relative expanded uncertainty, k=2†) in the visible region [23]. The spectral responsivity scale is transferred to other detectors using the Spectral Comparator Facility (SCF) [25], where the absolute spectral responsivity s(λ) (A/W) of each of the NIST standard photometers is determined. The illuminance responsivity [A/lx] of each photometer is

– 8 –

Brewster Angled Window

Liquid Helium Reservoir

Germanium Resistance Thermometer

50K Radiation Shield

77K Radiation Shield

Radiation Trap (4.2K)

Pumping Port

Laser Beam

Liquid Nitrogen Reservoir

5K Reference Block

Thin Film Heater 10K

Absorbing Cavity (specular black paint)

Alignment Photodiodes

0 100 mm

Figure 3 Construction of the NIST High Accuracy Cryogenic Radiometer.

† Throughout this paper, all uncertainty values are given as an expanded uncertainty with coverage factor k=2, thus a two standard deviation estimate. Uncertainties of fundamental units given as a combined standard uncertainty in other documents are restated as an expanded uncertainty (k=2).

then calculated from s(λ), the area of the aperture, and other correction factors. The relative expanded uncertainty of the illuminance responsivity determination is 0.39 % [2]. The standard photometers are recalibrated annually utilizing the detector spectral responsivity scale. The details of the candela realization are described in Section 3.1 and in Reference [2].

As the result of the candela realization in 1992, the magnitude of the NIST luminous intensity unit changed (increased) by approximately 0.3 %. With the effect of the change of the international temperature scale in 1990 included, the magnitude of the NIST candela is larger (measured values are smaller) by approximately 0.6 % than that reported before 1990. At the latest CCPR international intercomparison [26] in 1985, the NIST candela was 0.6 % smaller than the world mean. The changes of the NIST candela occurred in the direction to reduce its difference from the world mean. At the time of the 1985 intercomparison, the candela and the lumen standards disseminated in different countries varied by ± 1 %. The most recent status of the differences in the magnitude of photometric units for different countries in the world was last published by BIPM in 1988 [27], the copy of which is attached in the Appendix A. The next international intercomparison of photometric units by CCPR is planned to be completed by 1998. In the mean time, NIST occasionally conducts bilateral intercomparisons of photometric units with other national laboratories [28].

1.3.2 NIST luminous flux unit

Until 1994, the NIST luminous flux unit was derived from the previous luminous intensity unit which was based on blackbody radiation. The previous luminous flux unit was last realized in 1985 by goniophotometric measurements [1], and was maintained on a group of six incandescent standard lamps. The unit was periodically transferred to groups of working standard lamps used for routine calibrations.

In 1995, a new NIST luminous flux unit was derived, based on the detector-based candela introduced in 1992, with a new method using an integrating sphere and an external source. The basic principle of this method (Absolute Integrating Sphere Method) is to measure the total flux of a lamp inside the sphere compared to a known amount of flux introduced into the sphere from a source outside the sphere.

This method was first studied theoretically using a computer simulation technique [29], then experimentally verified [30] using a 0.5 m integrating sphere. Utilizing this method with a 2 m integrating sphere, the new NIST luminous flux unit was established in 1995 [31, 32].

Primary standard lamps and working standard lamps are calibrated periodically against the NIST illuminance unit in order to maintain the luminous flux unit and to provide routine calibrations.

The details of the luminous flux unit realization are described in Section 5.1.

The realization of the 1995 luminous flux unit has resulted in a change (increase) of the magnitude of NIST luminous flux unit by approximately 1.1 %. The measured lumen values reported by NIST are smaller by that percentage than those previously reported. At the time of the 1985 CCPR international intercomparison [26], the NIST lumen value was 1.0 % smaller than the

– 9 – world mean. The new luminous flux unit has been disseminated in NIST calibrations since January 1, 1996.

2. Outline of the calibration services

This section provides a list of the photometric calibration services currently available at NIST. The complete description of these services is reported in the NIST Calibration Services Users Guide (SP250) [5]. Chapter 7 (Optical Radiation Measurements) of the SP250 is attached as Appendix B. The details of the artifacts and measurement procedures for calibration are

– 10 –

Table 4. NIST Photometric Calibration Services

Relative expanded Test no. Item of test Range uncertainty (k=2) 37010C Luminous Intensity and Color Temperature 0.5 %

Standard Lamps (~1000 cd, 2856 K) 8 K

37020S Special Tests for Luminous Intensity and 10-1 cd – 104 cd 0.6 % Color Temperature of Submitted Lamps 2856 K 8 K

37030C Color Temperature Standard Lamps 2856 K 8 K

37040C Each Additional Color Temperature 2000 K – 3200 K 4 K – 10 K for 37030C

37050S Special Tests for Color Temperature of 2000 K – 3200 K 4 K – 10 K Submitted Lamps

37060S Special Tests for Total Luminous Flux of 10-1 lm – 105 lm 0.8 % – 2.0 % Submitted Lamps (Incandescent lamps and fluorescent lamps)

37070C Opal Glass Luminance Coefficient Standards ~0.15 sr-1 0.5 %

37080S Special Tests for Submitted Luminance (1 – 4000) cd/m2 0.7 % Sources and Transmitting Diffusers

37090S Special Tests for Photometer heads, (0.1 – 3000) lx 0.5 % - 1 % Illuminance meters, and Luminance meters

37100S Special Photometric Tests described in Sections 3 through 7. Table 4 lists the NIST photometric calibration services with typical measurement ranges and typical uncertainties. All the items listed here, including the Special Tests, are provided routinely. Fixed services (Test Numbers ending in the letter C) are those in which NIST issues calibrated artifacts to customers. Special Tests (Test Number ending with the letter S), on the other hand, are those in which NIST calibrates artifacts submitted by customers.

The fees for the fixed services are listed in the Fee Schedule (SP250 Appendix). The fees for Special Tests depend on the type of artifacts, number of artifacts, measurement range requested, etc. A cost estimate will be given for each request for a Special Test.

Calibrations on special test items or under special conditions, other than listed below, may be available after consultation as Special Photometric Tests 37100S.

3. Luminous intensity (candela) calibrations

3.1 NIST illuminance unit and the NIST candela

3.1.1 Principles of the detector-based candela realization

As stated in Section 1.3, the NIST candela is realized and maintained on a group of eight NIST standard photometers. The illuminance responsivity (A/lx) of these photometers are calibrated annually utilizing the NIST spectral responsivity scale. The principles of the calibration of the photometers are described below.

Precision aperture

Photometer head

V(λ)-correction filter

Silicon photodiode

Light source d [m]

Figure 4 Geometry for the detector-based candela realization.

A standard photometer consists basically of a silicon photodiode, a V(λ)-correction filter, and a precision aperture, as shown in Figure 4. When the absolute spectral responsivity s(λ) (A/W) of the photometer is measured, the photometric responsivity Rv,f (A/lm) of the photometer within the aperture is given by

– 11 –

Rv,f =

P(λ) s(λ)dλ λ

Km P(λ) V(λ)dλ λ

(8) where P(λ) is the spectral power distribution of light to be measured, V(λ) is the spectral luminous efficiency function, and Km is the maximum spectral efficacy (683 lm/W). Usually a Planckian radiator at 2856 K (CIE Illuminant A) is used to provide the light flux P(λ). If the area A (m2) of the aperture is known and the responsivity Rv,f is uniform over the aperture, the illuminance responsivity Rv,i (A/lx) of the photometer is given by

Rv,i = A · Rv,f (9)

When a photometer calibrated for Rv,i is used to measure the illuminance from a point source, the luminous intensity Iv (cd) of the source is given by

Iv = d 2 · y / Rv,i , (10) where d is the distance (m) from the light source to the aperture surface of the photometer and y is the output current (A) of the photometer. In practice, d must be larger than the minimum distance where the deviation from the inverse square law of the light source is negligibly small.

3.1.2 Design of the NIST standard photometers

Figure 5 shows the design of the NIST standard photometers. A silicon photodiode, a V(λ)-correction filter, and a precision aperture are mounted in a cylindrical housing. The photodiode is plugged into a socket with a teflon base of low electrical conductivity. The V(λ)–correction filter is made of several layers of glass filters, and affixed to the photodiode. On the front side of the filter, the precision aperture is glued to a holder which is carefully machined so that its front surface (the reference surface of the photometer) is 3.0 mm from the plane of the aperture knife edge.

An electronic assembly containing a current-to-voltage converter circuit having a high sensitivity and a wide dynamic range [33] is mounted directly behind the photodiode to minimize noise. The circuit has a switchable gain setting from 104 V/A to 1010 V/A ( 1011 V/A for two of the photometers). An input equivalent noise of ~1 fA is achieved at the gain setting of 1011 V/A with an integration time of 1.67 s, and a bandwidth of 0.3 Hz. This high sensitivity feature allows precise measurement of s(λ) even in the wings of the V(λ) curve.

Since the characteristics of the filter and photodiode can change with temperature, a temperature sensor is installed in the front piece of the housing to monitor the photometer temperature [34].

– 12 –

Figure 5 Design of the NIST standard photometer.

3.1.3 Calibration of the NIST standard photometers

The spectral responsivity s(λ) of the photometers is measured with the NIST Spectral Comparator Facility (SCF) [25]. The photometer aperture is underfilled with a beam of 1 mm diameter from the monochromator, and the responsivity of the photometer is mapped over the entire area of the precision aperture at several wavelengths. From the mapping data, the ratio of the average responsivity over the aperture to the responsivity at the center of the aperture is calculated and applied in the responsivity calculation. The f 1

′ values of the eight photometers range from 1.4 % to 6 %. The f 1

′ is a term recommended by CIE [35] to indicate the degree of spectral mismatch of a photometer to the V(λ) function. The illuminance responsivity of NIST photometers, Rv,i [A/lx], are calculated for Planckian radiation at 2856 K (CIE Illuminant A) according to eqs (8) and (9).

3.1.4 Spectral mismatch correction

When the photometers measure light sources whose spectral distribution is different from the 2856 K Planckian source, an error occurs due to the spectral mismatch of the photometers.

This error is corrected by a spectral mismatch correction factor, ccf * , as given by ccf *(St(λ) ) =

SA(λ) srel(λ) dλ λ

S t(λ) V(λ) dλ λ

SA(λ) V(λ) dλ λ

S t(λ) srel(λ) dλ λ

, (11)

– 13 – where St(λ) is the spectral power distribution of the test lamp, SA(λ) is the spectral data of the CIE Illuminant A, and srel(λ) is the relative spectral responsivity of the photometer. Using this equation, the correction factor can be obtained for any light source with known spectral power distribution.

For convenience in measuring incandescent lamps, ccf * is expressed as a function of the distribution temperature Td of the lamp to be measured. The ccf *(St(λ) ) is calculated for Planckian radiation of four temperatures, and then the correction factors are fitted into a polynomial function. The ccf *(Td) is then given by, ccf *(Td) = a j Td jΣ j = 0

. (12)

The polynomial constants are obtained for each of the NIST standard photometers. An example is shown in Figure 6. The spectral mismatch correction factors for incandescent lamps of known distribution temperature are automatically calculated using this polynomial. The output signal of the photometer is multiplied by this correction factor.

0.998

1.000

1.002

1.004

1.006

1.008

1.010

2000 2200 2400 2600 2800 3000 3200 ccf*(T d ) = M

+ M

*T d + M

*T d

+ M

*T d

1.0301M

-1.8473e-05M

3.5933e-09M

-2.8471e-13M cc f*

(T d)

Distribution Temperature Td [K]

Figure 6 Polynomial fit for the spectral mismatch correction factors.

3.1.5 Correction for the photometer temperature

The temperature coefficients of the illuminance responsivity of the photometers, measured in a temperature-controlled chamber, are shown in Figure 7. The figure shows the data for three different photometers in the group. The temperature coefficients, cp, for the eight photometers range from -0.049 %/°C to -0.088 %/°C. Whenever the photometers are used, the temperature correction factor, k(Tp), as given below, is calculated, and the output signal is multiplied by this correction factor.

k(Tp) = 1 - (Tp - T0) cp (13)

– 14 – where T0 is the temperature at which each photometer was calibrated.

0.993

0.994

0.995

0.996

0.997

0.998

0.999

1.000

0 2 4 6 8

R el at iv e R es po ns iv ity

Temperature Increase [°C]

Figure 7 The temperature dependence of the photometers’ illuminance responsivity.

3.1.6 Linearity of the NIST standard photometers

The linearity of the photometers was measured using a beam conjoiner instrument [36], which is a ratio-and-additive beam device designed to test the linearity of photodetectors.

Figure 8 shows the result from one of the NIST standard photometers for a 2856 K source.

These data indicate that the photometer is linear over an output current range of 10– 10 A to

10– 4 A. This corresponds to an illuminance range of 10– 2 lx to 104 lx, and means the photometers can be used to measure a luminous intensity as low as 10 mcd at 1 m, and as high as 105 cd at 3 m, without significantly increasing the uncertainty. If the integration time for the signal is longer, the photometer can be used for even lower levels [33]. The linearity data also assures negligible non-linearity error in the spectral responsivity measurements.

– 15 –

0.996

0.998

1.000

1.002

1.004

10-12 10-10 10-8 10-6 10-4

R el at iv e R es po ns iv ity

Photocurrent [A]

AverageDecade

1.00016-10 – -9

1.00001-9 – -8

0.99999-8 – -7

1.00001-7 – -6

0.99993-6 – -5

1.00003-5 – -4

Figure 8 Linearity of one of the NIST standard photometers.

3.1.7 Uncertainty of the NIST illuminance unit and the candela realization

The uncertainty budgets for the NIST illuminance unit realization and the NIST candela realization are shown in Table 5 and Table 6, respectively. Long-term drift of the standard photometers are not included in these tables, but are taken into account in the uncertainty budgets for the calibrations.