fakeread

From 22f703cab05b7cd368f4de9e03991b7664dc5022 Mon Sep 17 00:00:00 2001 From: =?UTF-8?q?J=C3=B6rg=20Frings-F=C3=BCrst?= Date: Mon, 1 Sep 2014 13:56:46 +0200 Subject: Initial import of argyll version 1.5.1-8 --- doc/spec2cie.html | 207 ++++++++++++++++++++++++++++++++++++++++++++++++++++++ 1 file changed, 207 insertions(+) create mode 100644 doc/spec2cie.html (limited to 'doc/spec2cie.html') diff --git a/doc/spec2cie.html b/doc/spec2cie.html new file mode 100644 index 0000000..192ee64 --- /dev/null +++ b/doc/spec2cie.html @@ -0,0 +1,207 @@ + + + + fakeread + + + + +

spectro/spec2cie

Summary

+ Convert spectral .ti3 + readings into CIE XYZ or L*a*b* readings. FWA compensation may be + applied.
+

Usage

+ spec2cie [options] input.ti3 + output.ti3 + -v + + Verbose mode
+ -I illum + Override + actual instrument illuminant + in .ti3 file: + + + A, C, D50, D50M2, D65, F5, + F8, F10 or file.sp + + (only + used in conjunction with -f) + -f [illum] + Use Fluorescent Whitening Agent compensation + [simulated inst. illum.: + + M0, M1, M2, A, C, D50 (def.), D50M2, D65, F5, F8, F10 or + file.sp] + -i illum + Choose illuminant for computation of CIE XYZ + from spectral data & FWA: + + + + A, C, D50 (def.), D50M2, D65, F5, + F8, F10 or file.sp + -o + observ + Choose CIE Observer for spectral + data: + + + + 1931_2 (def.), + 1964_10, S&B + 1955_2, shaw, J&V 1978_2 + -n +Don't +output + spectral values + -p + + Plot + each values spectrum++ input.ti3 +Measurement + file + output.ti3 + Converted + measurement file
+

Comments

+ This program takes the spectral data in a .ti3 file, converts them + to + XYZ and Lab and fills the XYZ_[XYZ] and LAB_[LAB] columns in the + output + .ti3 file with the computed XYZ and Lab values. If the columns + XYZ_[XYZ] and/or LAB_[LAB] are missing in the input file, they are + added to the output file.
+
+ All other columns are copied from the input to the output .ti3 file.
+
+
+ The -I parameter allows specifying a an + illumination + spectrum for the actual instrument illuminant, overriding that + computed from + the type of instrument (recorded in the .ti3 file). This is rarely + used. This parameter is can + only be used in combination with the -f + flag. If a + filename is specified instead, it will be assumed to be an Argyll + specific .sp + custom spectrum file. + Illuminant details are:
+
+         A   CIE + tungsten + filament lamp 2848K
+         D50 CIE daylight 5000K
+         D65 CIE daylight 6500K
+         F5 CIE Fluorescent + 6350K, CRI 72
+         F8 CIE Fluorescent + 5000K, CRI 95
+         F10 CIE Fluorescent + 5000K, + CRI 81
+
+
+ The -f flag enables Fluorescent Whitening + Agent (FWA) compensation. This only works if spectral data is + available and, the instrument is not UV filtered. FWA + compensation adjusts the spectral samples so that they appear to + have been measured using an illuminant that has a different level of + Ultra Violet to the one the instrument actually used in the + measurement. The optional illumination parameter allows specifying a + standard or custom illumination spectrum to be used as the similated + instrument illuminant, overriding the default D50 or CIE + computation illuminant used for FWA (see -i below). See + colprof -f for a fuller explanation.
+
+ The -i parameter allows specifying a + standard or custom illumination spectrum, applied to spectral .ti3 + data to compute PCS (Profile Connection Space) tristimulus values. A, + D50, D65, F5, F8, F10 are a + selection of standard illuminant spectrums, with D50 being + the default. If a filename is specified instead, it will be assumed + to be an Argyll specific .sp + custom spectrum file. This only works if spectral data is available. + Illuminant details are:
+
+         A   CIE + tungsten filament lamp 2848K
+         D50 CIE daylight 5000K
+         D65 CIE daylight 6500K
+         F5 CIE Fluorescent + 6350K, CRI 72
+         F8 CIE Fluorescent + 5000K, CRI 95
+         F10 CIE Fluorescent + 5000K, CRI 81
+
+ Custom illuminants are most often used when a viewing booth or + other known viewing conditions is going to be used to view results. + Other illuminant reference files could be created using a suitable + measuring instrument such as a spectrolino, or an eyeone using spotread, although such instruments do + not themselves provide the necessary response down to Ultra Violet + that is needed for accurate operation of Fluorescent Whitening Agent + compensation. The best way of measuring a custom illuminant is to + use illumread, since it uses a special + method to estimate the illuminant UV in a way that complements FWA + compensation. (See the discussion above for the -f flag).
+
+ Note that if an illuminant other than D50 is chosen, the resulting + ICC profile will not be standard, and may not work perfectly with + other profiles that that use the standard ICC D50 illuminant, + particularly if the absolute rendering intent is used. Profiles + should generally be linked with other profiles that have the same + illuminant and observer.
+
+ The -o flag allows specifying a tristimulus + observer, and is used to compute PCS (Profile Connection Space) + tristimulus values. The following choices are available:
+ 1931_2 selects the standard CIE 1931 2 degree observer + (the default).
+ 1964_10 selects the standard CIE 1964 10 degree + observer.
+ 1955_2 selects the Stiles and Birch 1955 2 degree + observer
+ 1978_2 selects the Judd and Voss 1978 2 degree + observer
+ shaw selects the Shaw and Fairchild 1997 2 degree + observer
+
+ Note that if an observer other than 1931 2 degree is chosen, the + resulting ICC profile will not be standard, and cannot be freely + interchanged with other profiles that that us the standard 1931 2 + degree + observer. Profiles should only be linked with other profiles that + have + the same illuminant and observer.
+
+
+
+ The -n flag + disables the output of the spectral values. If just the XYZ and + L*a*b* + values are needed, this makes for a smaller, easier to read file.
+
+ The -p flag + causes each spectrum to be plotted. If FWA compensation is used, + then + the before/after compensation spectrums will be shown.
+
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+ + -- cgit v1.2.3