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# Line 2 | Line 2
2   <!-- RCSid $Id$ -->
3   <head>
4   <title>
5 < The RADIANCE 5.1 Synthetic Imaging System
5 > The RADIANCE 6.0 Synthetic Imaging System
6   </title>
7   </head>
8   <body>
# Line 10 | Line 10 | The RADIANCE 5.1 Synthetic Imaging System
10   <p>
11  
12   <h1>
13 < The RADIANCE 5.1 Synthetic Imaging System
13 > The RADIANCE 6.0 Synthetic Imaging System
14   </h1>
15  
16   <p>
# Line 83 | Line 83 | The diagram in Figure 1 shows the flow between program
83   (ovals).  
84   The central program is <i>rpict</i>, which produces a picture from a scene
85   description.
86 < <i>Rview</i> is a  variation  of  rpict  that  computes  and displays images
86 > <i>Rvu</i> is a  variation  of  rpict  that  computes  and displays images
87   interactively, and rtrace computes single ray values.
88   Other programs (not shown) connect many of these elements together,
89   such as the executive programs
# Line 798 | Line 798 | unless the line integrals consider enclosed geometry.
798  
799   <dd>
800          Trans2 is the anisotropic version of <a HREF="#Trans">trans</a>.  
801 <        The string arguments  are  the same as for plastic2, and the real arguments are the same as  for  trans  but  with  an  additional roughness value.
801 >        The string arguments  are  the same as for <a HREF="#Plastic2">plastic2</a>,
802 >        and the real arguments are the same as  for  trans  but  with  an  additional roughness value.
803  
804   <pre>
805          mod trans2 id
# Line 810 | Line 811 | unless the line integrals consider enclosed geometry.
811   <p>
812  
813   <dt>
814 +        <a NAME="Ashik2">
815 +        <b>Ashik2</b>
816 +        </a>
817 +
818 + <dd>
819 +        Ashik2 is the anisotropic reflectance model by Ashikhmin & Shirley.
820 +        The string arguments are the same as for <a HREF="#Plastic2">plastic2</a>, but the real
821 +        arguments have additional flexibility to specify the specular color.
822 +        Also, rather than roughness, specular power is used, which has no
823 +        physical meaning other than larger numbers are equivalent to a smoother
824 +        surface.
825 +        Unlike other material types, total reflectance is the sum of
826 +        diffuse and specular colors, and should be adjusted accordingly.
827 + <pre>
828 +        mod ashik2 id
829 +        4+ ux uy uz funcfile transform
830 +        0
831 +        8 dred dgrn dblu sred sgrn sblu u-power v-power
832 + </pre>
833 +
834 + <p>
835 +
836 + <dt>
837          <a NAME="Dielectric">
838          <b>Dielectric</b>
839          </a>
# Line 1132 | Line 1156 | unless the line integrals consider enclosed geometry.
1156   <p>
1157  
1158   <dt>
1159 +        <a NAME="aBSDF">
1160 +        <b>aBSDF</b>
1161 +        </a>
1162 +
1163 + <dd>
1164 +        The aBSDF material is identical to the BSDF type with two
1165 +        important differences.  First, proxy geometry is not
1166 +        supported, so there is no thickness parameter.  Second, an
1167 +        aBSDF is assumed to have some specular through component
1168 +        (the &rsquo;a&rsquo; stands for &quot;aperture&quot;),
1169 +        which is treated specially during the direct calculation
1170 +        and when viewing the material.  Based on the BSDF data, the
1171 +        coefficient of specular transmission is determined and used
1172 +        for modifying unscattered shadow and view rays.
1173 +
1174 + <pre>
1175 +        mod aBSDF id
1176 +        5+ BSDFfile ux uy uz funcfile transform
1177 +        0
1178 +        0|3|6|9
1179 +             rfdif gfdif bfdif
1180 +             rbdif gbdif bbdif
1181 +             rtdif gtdif btdif
1182 + </pre>
1183 +
1184 + <p>
1185 +        If a material has no specular transmitted component, it is
1186 +        much better to use the BSDF type with a zero thickness
1187 +        than to use aBSDF.
1188 + <p>
1189 +
1190 + <dt>
1191          <a NAME="Antimatter">
1192          <b>Antimatter</b>
1193          </a>
# Line 1405 | Line 1461 | or:
1461          A section of text meant to  depict  a  picture, perhaps using a special purpose font such as hexbit4x1.fnt, calls for uniform  spacing.  
1462          Reasonable  magnitudes  for  proportional  spacing are between 0.1 (for tightly spaced characters) and 0.3 (for wide spacing).
1463  
1464 + <p>
1465 +
1466 + <dt>
1467 +        <a NAME="Spectrum">
1468 +        <b>Spectrum</b>
1469 +        </a>
1470 +
1471 + <dd>
1472 +        The spectrum primitive is the most basic type for introducing spectral
1473 +        color to a material.
1474 +        Since materials only provide RGB parameters, spectral patterns
1475 +        are the only way to superimpose wavelength-dependent behavior.
1476 +
1477 + <pre>
1478 +        mod spectrum id
1479 +        0
1480 +        0
1481 +        5+ nmA nmB s1 s2 .. sN
1482 + </pre>
1483 +
1484 + <p>
1485 +        The first two real arguments indicate the extrema of the
1486 +        spectral range in nanometers.
1487 +        Subsequent real values correspond to multipliers at each wavelength.
1488 +        The nmA wavelength may be greater or less than nmB,
1489 +        but they may not be equal, and their ordering matches
1490 +        the order of the spectral values.
1491 +        A minimum of 3 values must be given, which would act
1492 +        more or less the same as a constant RGB multiplier.
1493 +        As with RGB values, spectral quantities normally range between 0
1494 +        and 1 at each wavelength, or average to 1.0 against a standard
1495 +        sensitivity functions such as V(lambda).
1496 +        The best results obtain when the spectral range and number
1497 +        of samples match rendering options, though resampling will handle
1498 +        any differences, zero-filling wavelenths outside the nmA to nmB
1499 +        range.
1500 +        A warning will be issued if the given wavelength range does not
1501 +        adequately cover the visible spectrum.
1502 +
1503 + <p>
1504 +
1505 + <dt>
1506 +        <a NAME="Specfile">
1507 +        <b>Specfile</b>
1508 +        </a>
1509 +
1510 + <dd>
1511 +        The specfile primitive is equivalent to the spectrum type, but
1512 +        the wavelength range and values are contained in a 1-dimensional
1513 +        data file.
1514 +        This may be a more convenient way to specify a spectral color,
1515 +        especially one corresponding to a standard illuminant such as D65
1516 +        or a library of measured spectra.
1517 +
1518 + <pre>
1519 +        mod specfile id
1520 +        1 datafile
1521 +        0
1522 +        0
1523 + </pre>
1524 +
1525 + <p>
1526 +        As with the spectrum type, rendering wavelengths outside the defined
1527 +        range will be zero-filled.
1528 +        Unlike the spectrum type, the file may contain non-uniform samples.
1529 +
1530 + <p>
1531 +
1532 + <dt>
1533 +        <a NAME="Specfunc">
1534 +        <b>Specfunc</b>
1535 +        </a>
1536 +
1537 + <dd>
1538 +        The specfunc primitive offers dynamic control over a spectral
1539 +        pattern, similar to the colorfunc type.
1540 +
1541 + <pre>
1542 +        mod specfunc id
1543 +        2+ sfunc funcfile transform
1544 +        0
1545 +        2+ nmA nmB A3 ..
1546 + </pre>
1547 +
1548 + <p>
1549 +        Like the spectrum primitive, the wavelength range is specified
1550 +        in the first two real arguments, and additional real values are
1551 +        set in the evaluation context.
1552 +        This function is fed a wavelenth sample
1553 +        between nmA and nmB as its only argument,
1554 +        and it returns the corresponding spectral intensity.
1555 +
1556 + <dt>
1557 +       <a NAME="Specdata">
1558 +       <b>Specdata</b>
1559 +       </a>
1560 +
1561 + <dd>
1562 +        Specdata is like brightdata and colordata, but with more
1563 +        than 3 specular samples.
1564 +
1565 + <pre>
1566 +        mod specdata id
1567 +        3+n+
1568 +                func datafile
1569 +                funcfile x1 x2 .. xn transform
1570 +        0
1571 +        m A1 A2 .. Am
1572 + </pre>
1573 +
1574 + <p>
1575 +        The data file must have one more dimension than the coordinate
1576 +        variable count, as this final dimension corresponds to the covered
1577 +        spectrum.
1578 +        The starting and ending wavelengths are specified in "datafile"
1579 +        as well as the number of spectral samples.
1580 +        The function "func" will be called with two parameters, the
1581 +        interpolated spectral value for the current coordinate and the
1582 +        associated wavelength.
1583 +        If the spectrum is broken into 12 components, then 12 calls
1584 +        will be made to "func" for the relevant ray evaluation.
1585 +
1586 + <dt>
1587 +       <a NAME="Specpict">
1588 +       <b>Specpict</b>
1589 +       </a>
1590 +
1591 + <dd>
1592 +        Specpict is a special case of specdata, where the pattern is
1593 +        a hyperspectral image stored in the common-exponent file format.
1594 +        The dimensions of the image data are determined by the picture
1595 +        just as with the colorpict primitive.
1596 +
1597 + <pre>
1598 +        mod specpict id
1599 +        5+
1600 +                func specfile
1601 +                funcfile u v transform
1602 +        0
1603 +        m A1 A2 .. Am
1604 + </pre>
1605 +
1606 + <p>
1607 +        The function "func" is called with the interpolated pixel value
1608 +        and the wavelength sample in nanometers, the same as specdata,
1609 +        with as many calls made as there are components in "specfile".
1610 +
1611   </dl>
1612  
1613   <p>
# Line 1753 | Line 1956 | The details of this process  are  not  important, but
1956   directs the use of a scene description.
1957   <ul>
1958   <li>
1959 < <a NAME="rvu" HREF="../man_html/rvu.1.html"><b>Rview</b></a>  is  ray-tracing  program  for  viewing  a  scene interactively.  
1959 > <a NAME="rvu" HREF="../man_html/rvu.1.html"><b>Rvu</b></a>  is  ray-tracing  program  for  viewing  a  scene interactively.  
1960   When  the user specifies a new perspective, rvu quickly displays a rough image on the  terminal,  
1961   then progressively increases the resolution as the user looks on.
1962   He can select a particular section of the image to  improve, or  move  to  a different view and start over.  
# Line 1789 | Line 1992 | Pictures may be displayed directly under X11 using the
1992   or converted a standard image format using one of the following
1993   <b>translators</b>:
1994          <ul>
1995 <        <li> <a HREF="../man_html/ra_bmp.1.html"><b>Ra_bmp</b>
1995 >        <li> <a HREF="../man_html/ra_bmp.1.html"><b>Ra_bmp</b></a>
1996                  converts to and from BMP image format.
1997          <li> <a HREF="../man_html/ra_ppm.1.html"><b>Ra_ppm</b></a>
1998                  converts to and from Poskanzer Portable Pixmap formats.
# Line 1818 | Line 2021 | or converted a standard image format using one of the
2021   <pre>
2022   The Radiance Software License, Version 1.0
2023  
2024 < Copyright (c) 1990 - 2014 The Regents of the University of California,
2024 > Copyright (c) 1990 - 2021 The Regents of the University of California,
2025   through Lawrence Berkeley National Laboratory.   All rights reserved.
2026  
2027   Redistribution and use in source and binary forms, with or without
# Line 1891 | Line 2094 | Ecole  Polytechnique  Federale de Lausanne (EPFL Unive
2094   </h2>
2095   <p>
2096   <ul>
2097 +    <li>Ward, Gregory J., Bruno Bueno, David Geisler-Moroder,
2098 +      Lars O. Grobe, Jacob C. Jonsson, Eleanor
2099 +      S. Lee, Taoning Wang, Helen Rose Wilson,
2100 +      &quot;<a href="https://doi.org/10.1016/j.enbuild.2022.111890">Daylight
2101 +      Simulation Workflows Incorporating Measured Bidirectional
2102 +      Scattering Distribution Functions</a>&quot;
2103 +      <em>Energy &amp; Buildings</em>, Vol. 259, No. 11890, 2022.
2104 +    <li>Wang, Taoning, Gregory Ward, Eleanor Lee,
2105 +      &quot;<a href="https://authors.elsevier.com/a/1XQ0a1M7zGwT7v">Efficient
2106 +      modeling of optically-complex, non-coplanar exterior shading:
2107 +      Validation of matrix algebraic methods</a>&quot;
2108 +      <em>Energy & Buildings</em>, vol. 174, pp. 464-83, Sept. 2018.
2109 +    <li>Lee, Eleanor S., David Geisler-Moroder, Gregory Ward,
2110 +      &quot;<a href="https://eta.lbl.gov/sites/default/files/publications/solar_energy.pdf">Modeling
2111 +      the direct sun component in buildings using matrix
2112 +      algebraic approaches: Methods and
2113 +      validation</a>,&quot; <em>Solar Energy</em>,
2114 +      vol. 160, 15 January 2018, pp 380-395.
2115 +    <li>Narain, Rahul, Rachel A. Albert, Abdullah Bulbul,
2116 +       Gregory J. Ward, Marty Banks, James F. O'Brien,
2117 +       &quot;<a href="http://graphics.berkeley.edu/papers/Narain-OPI-2015-08/index.html">Optimal
2118 +       Presentation of Imagery with Focus
2119 +       Cues on Multi-Plane Displays</a>,&quot;
2120 +       <em>SIGGRAPH 2015</em>.
2121 +    <li>Ward, Greg, Murat Kurt, and Nicolas Bonneel,
2122 +        &quot;<a href="papers/WMAM14_Tensor_Tree_Representation.pdf">Reducing
2123 +        Anisotropic BSDF Measurement to Common Practice</a>,&quot;
2124 +        <em>Workshop on Material Appearance Modeling</em>, 2014.
2125 +    <li>Banks, Martin, Abdullah Bulbul, Rachel Albert, Rahul Narain,
2126 +        James F. O'Brien, Gregory Ward,
2127 +        &quot;<a href="http://graphics.berkeley.edu/papers/Banks-TPO-2014-05/index.html">The
2128 +        Perception of Surface Material from Disparity and Focus Cues</a>,&quot;
2129 +        <em>VSS 2014</em>.
2130      <li>McNeil, A., C.J. Jonsson, D. Appelfeld, G. Ward, E.S. Lee,
2131          &quot;<a href="http://gaia.lbl.gov/btech/papers/4414.pdf">
2132          A validation of a ray-tracing tool used to generate

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