From f6b8e0eae4374f339487a33e3e4fe5462d5816e1 Mon Sep 17 00:00:00 2001 From: =?UTF-8?q?J=C3=B6rg=20Frings-F=C3=BCrst?= Date: Sat, 25 Nov 2017 10:16:00 +0100 Subject: New upstream version 2.0.0 --- doc/spec2cie.html | 149 ++++++++++++++++++++++++++++++++++++++++-------------- 1 file changed, 111 insertions(+), 38 deletions(-) mode change 100644 => 100755 doc/spec2cie.html (limited to 'doc/spec2cie.html') diff --git a/doc/spec2cie.html b/doc/spec2cie.html old mode 100644 new mode 100755 index 2780161..d973289 --- a/doc/spec2cie.html +++ b/doc/spec2cie.html @@ -11,12 +11,17 @@

Summary

Convert spectral .ti3 or .sp readings into CIE XYZ and D50 - L*a*b* readings. Apply FWA, plot spectrums.
+ L*a*b* readings. Apply FWA, plot spectrums. Convert to/from XRGA + standard.
This is assumed to be for a reflective media by default - i.e. that the input .ti3 or .sp file values are spectral reflectances, unless the input is marked as DEVICE_CLASS  + + + + EMISINPUT (See the description of the .ti3 format. This would have to be done manually, as no ArgyllCMS tools generate such @@ -29,52 +34,71 @@ + + + + output.[ti3|sp]
 -v -                +                        + + + + Verbose mode
+  -A NN|AX|AG|XA|XG|GA|GX   XRGA + conversion (default NN)
+  -I illum   + - Verbose mode
-  -I illum   -        Override actual - instrument illuminant in .ti3 or .sp file:
+ + +                + + + + Override actual instrument illuminant in .ti3 or .sp file:
           -          A, C, D50, D50M2, - D65, F5, F8, F10 or file.sp
-                     +               +    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.:
+                    - (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   +                - 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:
+ + + Choose illuminant for computation of CIE XYZ from spectral + data & FWA:
           -          A, C, D50 - (def.), D50M2, D65, F5, F8, F10 or file.sp
+               +   A, C, D50 (def.), D50M2, D65, F5, F8, F10 or file.sp
 -o observ  @@ -82,20 +106,28 @@ -        Choose CIE Observer for - spectral data:
+ + + + +              + + + +   Choose CIE Observer for spectral data:
              -      - +     +          1931_2 + (def.), 1964_10, 2012_2, - 1931_2 (def.), - 1964_10, S&B 1955_2, shaw, J&V 1978_2 or file.cmf
-  -n                + 2012_10, S&B 1955_2, shaw, J&V 1978_2 + or file.cmf
+  -n                        Don't output @@ -104,15 +136,25 @@ output + + + + spectral values
 -p -                +                        + + + + Plot each values spectrum
  input.[ti3|sp] -    Measurement file
+            + Measurement file
 output.[ti3|sp] -   Converted measurement file
+           Converted + measurement file

Comments

This program takes the (usually reflective) spectral data in a .ti3 or .sp file, converts them to XYZ and D50 L*a*b* and fills the @@ -131,12 +173,36 @@ output spectra don't have an illuminant, and will simply be converted to XYZ using the given observer.

+ The -A parameter allows specifying a + conversion between the XRGA measurement + standards:
+
+         The NN argument + disabled any conversion.
+         The AX argument + converts from XRGA to XRDI
+         The AG argument + converts from XRGA to GMDI
+         The XA argument + converts from XRDI to XRGA
+         The XG argument + converts from XRDI to GMDI
+         The GA argument + converts from GMDI to XRGA
+         The GX argument + converts from GMDI to XRDI
+
+ A warning will be issued if the "from" setting doesn't match that + contained in the .ti3 file.
+
+ (XRGA = Modern X-Rite, XRDI = Historical X-Rite, GMD = Historical + GretagMacbeth).

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 + the .ti3 file). This is rarely used. This parameter 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:
@@ -169,6 +235,10 @@ output + + + + colprof -f for a fuller explanation.

The -i parameter allows specifying a @@ -218,14 +288,17 @@ output (the default).
  1964_10 selects the standard CIE 1964 10 degree observer.
+   2012_2 selects the proposed CIE 2012 2 degree observer
+   2012_10 selects the proposed CIE 2012 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
-
- or a .cmf file can be provided as an argument.
+   file.cmf selects an observer specified by the + given .cmf file.

Note that if an observer other than 1931 2 degree is chosen, the resulting ICC profile will not be standard, and cannot be freely -- cgit v1.2.3