<!DOCTYPE html PUBLIC "-//W3C//DTD HTML 4.01 Transitional//EN"> <html> <head> <title>fakeread</title> <meta http-equiv="content-type" content="text/html; charset=ISO-8859-1"> <meta name="author" content="Graeme Gill"> </head> <body> <h2><b>spectro/</b><span style="text-decoration: underline;"></span>spec2cie</h2> <h3>Summary</h3> Convert spectral <a href="File_Formats.html#.ti3">.ti3</a> readings into CIE XYZ or L*a*b* readings. FWA compensation may be applied.<br> <h3>Usage</h3> <small><span style="font-family: monospace;">spec2cie [options] </span><span style="font-style: italic; font-family: monospace;">input.ti3 output.ti3<br> </span></small><small><span style="font-family: monospace;"> -v Verbose mode</span></small><small><span style="font-style: italic; font-family: monospace;"> <br style="font-family: monospace;"> </span><span style="font-family: monospace;"> </span><a style="font-family: monospace;" href="#i">-i <i>illum</i></a><span style="font-family: monospace;"> Choose illuminant for print/transparency spectral data:</span><br style="font-family: monospace;"> <span style="font-family: monospace;"> A, D50 (def.), D65, F5, F8, F10 or file.sp</span><br style="font-family: monospace;"> <span style="font-family: monospace;"> </span><span style="text-decoration: underline; font-family: monospace;"> </span><a style="font-family: monospace;" href="#o">-o <i>observ</i></a><span style="font-family: monospace;"> Choose CIE Observer for spectral data:</span><br style="font-family: monospace;"> <span style="font-family: monospace;"> 1931_2 </span></small><small><span style="font-family: monospace;"> (def.)</span></small><small><span style="font-family: monospace;">, 1964_10, S&B 1955_2, 1964_10c, shaw, J&V 1978_2</span><br style="font-family: monospace;"> <span style="font-family: monospace;"> </span><a style="font-family: monospace;" href="colprof.html#f">-f</a><span style="font-family: monospace;"> Use Fluorescent Whitening Agent compensation</span><br style="font-family: monospace;"> <span style="font-family: monospace;"> </span><a style="font-family: monospace;" href="#I"> -I <i>illum</i></a><span style="font-family: monospace;"> Override instrument illuminant in .ti3 file:</span><br style="font-family: monospace;"> <span style="font-family: monospace;"> A, D50, D65, F5, F8, F10 or file.sp</span><br style="font-family: monospace;"> <span style="font-family: monospace;"> (only used in conjunction with </span><span style="font-weight: bold; font-family: monospace;">-f</span><span style="font-family: monospace;">)<br> <a href="#p">-n</a> Don't output spectral values<br> </span></small><small><span style="font-family: monospace;"> <a href="#p">-p</a> Plot each values spectrum</span></small><br style="font-family: monospace;"> <small><span style="font-family: monospace;"></span><span style="font-family: monospace;"> </span><span style="font-style: italic; font-family: monospace;">input.ti3</span><span style="font-family: monospace;"> Measurement file</span><br style="font-family: monospace;"> <span style="font-family: monospace;"> </span><span style="font-style: italic; font-family: monospace;">output.ti3</span><span style="font-family: monospace;"> Converted measurement file</span></small><br> <h3>Comments</h3> 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.<br> <br> All other columns are copied from the input to the output .ti3 file.<br> <br> If the <span style="font-weight: bold;">-f</span> option is used, the FWA corrected spectral reflectances are written to the output .ti3 file, instead of simply copying the spectral reflectances from the input .ti3 file. In this case, the XYZ_[XYZ] and LAB_[LAB] values are computed from the FWA corrected reflectances as well.<br> <br> <a name="i"></a>The <b>-i</b> flag allows specifying a standard or custom illumination spectrum, applied to spectral .ti3 data to compute PCS (Profile Connection Space) tristimulus values. <b>A</b>, <b>D50</b>, <b>D65</b>, <b>F5</b>, <b>F8</b>, <b>F10</b> are a selection of standard illuminant spectrums, with <b>D50</b> being the default. If a filename is specified instead, it will be assumed to be an Argyll specific <a href="File_Formats.html#.sp">.sp</a> custom spectrum file. This only works if spectral data is available. Illuminant details are:<br> <br> A CIE tungsten filament lamp 2848K<br> D50 CIE daylight 5000K<br> D65 CIE daylight 6500K<br> F5 CIE Fluorescent 6350K, CRI 72<br> F8 CIE Fluorescent 5000K, CRI 95<br> F10 CIE Fluorescent 5000K, CRI 81<br> <br> Custom illuminants are most often used when a fluorescent tube base viewing booth is going to be used to view results. Other illuminant reference files could be created using a suitable measuring instrument such as a spectrocam, or an eyeone, although such instruments do not provide the necessary response down to Ultra Violet that is needed for accurate operation of Fluorescent Whitening Agent compensation.<br> Note that if an illuminant other than D50 is chosen, the resulting ICC profile will not be standard, and cannot be freely interchanged with other profiles that that us the standard D50 illuminant. Profiles should only be linked with other profiles that have the same illuminant and observer.<br> <br> <a name="o"></a> The <b>-o</b> flag allows specifying a tristimulus observer, and is used to compute PCS (Profile Connection Space) tristimulus values. The following choices are available:<br> <b> 1931_2</b> selects the standard CIE 1931 2 degree observer (the default).<br> <b>1964_10</b> selects the standard CIE 1964 10 degree observer.<br> <b>1955_2</b> selects the Stiles and Birch 1955 2 degree observer<br> <b>1964_10c</b> selects a version of the CIE 1964 10 degree observer adjusted for better compatibility with the 1931 2 degree observer.<br> <b>1978_2 </b>selects the Judd and Voss 1978 2 degree observer<br> <b>shaw</b> selects the Shaw and Fairchild 1997 2 degree observer<br> <br> 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.<br> <br> <a name="f"></a> The <b>-f</b> flag enables Fluorescent Whitening Agent compensation. This allows the effects of different levels of Ultra Violet in the viewing illuminant from that used by the instrument, be compensated for.<br> <br> <a name="I"></a>The <b>-I</b> flag allows specifying a an illumination spectrum for the instrument illuminant, overriding that computed from the type of instrument (recorded in the .ti3 file). This flag is can only be used in combination with the <span style="font-weight: bold;">-f</span> flag. If a filename is specified instead, it will be assumed to be an Argyll specific <a href="File_Formats.html#.sp">.sp</a> custom spectrum file. Illuminant details are:<br> <br> A CIE tungsten filament lamp 2848K<br> D50 CIE daylight 5000K<br> D65 CIE daylight 6500K<br> F5 CIE Fluorescent 6350K, CRI 72<br> F8 CIE Fluorescent 5000K, CRI 95<br> F10 CIE Fluorescent 5000K, CRI 81<br> <br> <a name="n"></a>The <span style="font-weight: bold;">-n</span> 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.<br> <br> <a name="p"></a>The <span style="font-weight: bold;">-p</span> flag causes each spectrum to be plotted. If FWA compensation is used, then the before/after compensation spectrums will be shown.<br> <br> <br> <br> <br> <br> <br> </body> </html>
distrib
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Mandriva
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2010.0
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i586
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media
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contrib-release
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by-pkgid
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56e231b080a119bc733fcd74872c9f3d
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files
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