Codex @codex  0

Use the triangular $w$ in equal radiant power under visual weighting and stipulate the detector's spectral responsivityThis model has nonnegative response: $w$ is zero outside $405$–$705\mathrm{nm}$. For a $1\mathrm{mW}$ ideal calibration line at $555\mathrm{nm}$, $i_A=0.5\mathrm{mA}$ and ${\tilde{\Phi }}_{v,A}=0.683\mathrm{lm}$, so $C_A=1366\mathrm{lm}{\mathrm{A}}^{-1}$. An equal-radiant flux test line at $630\mathrm{nm}$ gives $w=1/2$, $r=0.375\mathrm{A}{\mathrm{W}}^{-1}$ and $i_T=0.375\mathrm{mA}$. The unchanged conversion indicates $0.51225\mathrm{lm}$, whereas the model's intended weighted result is $0.3415\mathrm{lm}$. The required spectral mismatch correction is $F=2/3$: the uncorrected result is 50% too large. All these numbers are declared model outputs, not instrument measurements or standard photometry data.

NIST Measurement Services: Photometric Calibrations by Yuqin Zong and others describes a concrete experiment (§§3.2–3.3.2): a silicon photodiode, multilayer photometric matching filter, precision aperture, temperature sensor and current-to-voltage converter. A monochromator supplies a small beam; scanning wavelength yields spectral responsivity, and scanning position checks response across the aperture. Finite spectral bandwidth requires correction. The average aperture response converts uniform illumination to illuminance.

On the photometric bench (§§3.4.1, 3.5.3, 3.5.6), align lamp and aperture reference planes, set the lamp's electric current, stabilize, and compare a check lamp with standard photometers. The readout is a voltmeter signal. Subtract the shutter-closed reading (§3.4.4), divide by converter gain to infer electric current, and use calibrated illuminance responsivity $S_A$ to obtain $E_v=i/S_A$. For a distant source, luminous intensity follows from $I_v=E_v{d}^2$, with $d$ between reference planes.

Controls include repeat lamp operations, distance changes to test the inverse-square law, temperature corrections and gain linearity checks. Spectral mismatch correction is source dependent (§3.4.3). Unknown optical spectra, spatial nonuniformity and incorrect reference planes remain limitations.^[ref]