Copyright c 1993 Regents, University of California
This tutorial assumes a certain familiarity with the UNIX operating system and its text editing facilities. Ask your system administrator for a basic introduction.
The RADIANCE reference manual will be required to understand the following examples of scene creation and program interaction. <!Text in italics is user input.>
The scene we will be working towards is shown in Figure 1.
<!A HREF="IMG/side-view.gif"> <!A HREF="IMG/top-view.gif"> It is usually helpful to start with a simple drawing showing the coordinate axis and the relative locations of major surfaces.
The minimum input required to get an image is a source of illumination and an object to reflect light to the "camera". (In fact, a RADIANCE renderer can be thought of an invisible camera in a simulated world.) We will begin with two spheres, one emissive and one reflective. First we define the materials, then the spheres themselves. Actually, the order is only important insofar as each modifier definition (i.e. material) must appear before its first reference. (Consult the RADIANCE manual for an explanation of the primitive types and their parameters.) Start your favorite text editor ("vi" in this example) to create the following file called "room.rad":
% vi room.rad # # My first scene. # # # The basic primitive format is: # # modifier TYPE identifier # number_string_arguments [string arguments...] # number_integer_arguments [integer arguments...] # number_real_arguments [real arguments...] # # The special modifier "void" means no modifier. # TYPE is one of a finite number of predefined types, and # the meaning of the arguments following is determined by # this type. (See RADIANCE Reference Manual for details.) # The identifier may be used as a modifier later # in this file or in files following this one. # All values are separated by white space # (spaces, tabs, newlines). # # this is the material for my light source: void light bright 0 0 3 100 100 100 # red_emission green_emission blue_emission # # this is the material for my test ball: void plastic red_plastic 0 0 5 .7 .05 .05 .05 .05 # red green blue specularity roughness # # here is the light source: bright sphere fixture 0 0 4 2 1 1.5 .125 # xcent ycent zcent radius # # here is the ball: red_plastic sphere ball 0 0 4 .7 1.125 .625 .125Now that we have a simple scene description, we may look at it with the interactive viewing program, rvu. First, however, we must create the "octree" file that will be used to accelerate the rendering process. To accomplish this, type the following command:
% oconv room.rad > test.octNote that the suffixes ".rad" and ".oct" are not enforced by the program, but are merely a convenience to aid the user in identifying files later. The command getinfo can be used to get information on the origin of binary (unviewable) files created by RADIANCE utilities. Try entering the command:
% getinfo test.octThe usefulness of such a function will be apparent when you find yourself with a dozen files named "test.pic". To make an image of our scene, we must select a suitable set of view parameters telling RADIANCE where to point its camera. To simplify our example, we will use the same starting position for all our renderings, and change views only once rvu is started:
% rvu -vp 2.25 .375 1 -vd -.25 .125 -.125 -av .5 .5 .5 test.octThe "-vp" option gives the view point, and the "-vd" option gives the view direction vector. The "-av" option specifies the amount of light globally present in the scene, permitting portions of the scene that are not illuminated directly to be visible. Rvu has many more options, and their default values may be discovered using:
% rvu -defaultsYou should start to see an image of a red ball forming on your screen. Take this opportunity to try each of rvu 's commands, as described in the manual. If you make a mistake in a view specification, use the last command to get back to where you were. It is probably a good idea to save your favorite view using the following command from within rvu:
: view default.vpYou can create any number of "viewfiles" with this command, and retrieve them with:
: last viewfileIf you look around enough, you may even be able to see the light source itself. Unlike many rendering programs, the light sources in RADIANCE are visible objects. This illustrates the philosophy behind the program, which is the simulation of physical spaces. Since it is not possible to create an invisible light source in reality, there is no reason to do it in simulation.
Still, there is no guarantee that the user will create physically meaningful descriptions. For example, we have just floated a red ball next to a light source somewhere in intergalactic space. In the interest of making this scene more realistic, let's enclose the light and ball in a room by adding the following text to "room.rad":
% vi room.rad # the wall material: void plastic gray_paint 0 0 5 .5 .5 .5 0 0 # a box shaped room: !genbox gray_paint room 3 2 1.75 -iThe generator program genbox is just a command that produces a RADIANCE description, and it is executed when the file is read. It is more convenient than specifying the coordinates of four vertices for each of six polygons, and can be changed later quite easily. (See the genbox manual page for further details.)
You can now look at the modified scene, but remember first to regenerate the octree:
% oconv room.rad > test.oct % rvu -vf default.vp -av .5 .5 .5 test.octThis is better, but our ball and light source are still floating, which is an unrealistic condition for most rooms. Let's put a box under the table, and a rod to suspend the light from the ceiling:
# a shiny blue box: void plastic blue_plastic 0 0 5 .1 .1 .6 .05 .1 !genbox blue_plastic box .5 .5 .5 | xform -rz 15 -t .5 .75 0 # a chrome rod to suspend the light from the ceiling: void metal chrome 0 0 5 .8 .8 .8 .9 0 chrome cylinder fixture_support 0 0 7 2 1 1.5 2 1 1.75 .05Note that this time the output of genbox was "piped" into another program, xform. Xform is used to move, scale and rotate RADIANCE descriptions. Genbox always creates a box in the positive octant of 3-space with one corner at the origin. This was what we wanted for the room, but we wanted the box moved away from the wall and rotated slightly. First we rotated the box 15 degrees about the z-axis (pivoting on the origin), then translated the corner from the origin to (.5,.75,0). By no small coincidence, this position is directly under our original ball.
After viewing this new arrangement, you can try changing some of the materials -- here are a few examples:
# solid crystal: void dielectric crystal 0 0 5 .5 .5 .5 1.5 0 # dark brown: void plastic brown 0 0 5 .2 .1 .1 0 0 # light gray: void plastic white 0 0 5 .7 .7 .7 0 0To change the ball from red_plastic to the crystal defined above, simply replace red_plastic sphere ball with crystal sphere ball. Note once again that the definition of the new materials must precede any references to them. Changing the materials for the floor and ceiling of the room is a little more difficult. Since genbox creates six rectangles, all using the same material, it is necessary to replace the command with its output before we can make the required changes. To do this, enter the command directly:
% genbox gray_paint room 3 2 1.75 -i >> room.radThe double arrow ">>" causes the output to be "appended" to the end of the file, rather than overwriting its contents. Now edit the file and change the ceiling material to "white", and the floor material to "brown". (Hint: the ceiling is the polygon whose z coordinates are all high. And don't forget to remove the original genbox command from the file!)
Once you have chosen a nice view, you can generate a high-resolution image in batch mode using the rpict command:
% rpict -vf myview -av .5 .5 .5 test.oct > test.pic & [PID]The ampersand "&" causes the program to run in the background, so you can log out and go home while the computer continues to work on your picture. The bracketed number [PID] printed by the C-shell command interpreter is the process id that can be used later to check the progress or kill the program. This number can also be determined by the ps command:
% psThe number preceding the rpict command is the process id. If you want to kill the process, use the command:
% kill PIDIf you only want a progress report without killing the process, use the form:
% kill -CONT PIDThis sends a "continue" signal to rpict, which then prints out the percentage completion. Note that this is a special feature of rpict, and will not work with most programs. Also note that this works only for the current login session. If you log on later on a different terminal (or window), rpict will not send the report to the correct place. It is usually a good idea, therefore, to give rpict an error file argument if it is running a long job:
% rpict -e errfile ...Now sending an alarm signal will result in rpict reporting to the end of the specified error file. Alternatively, you may use the -t option to generate reports automatically at regular intervals. You can check the reports at any time by printing the file:
% cat errfileThis file will also contain a header, and any errors that occurred.
The new polygon for the window wall is shown in Figure 2.
Figure 2. The window wall with a hole cut in it.
To create the window wall, change the appropriate polygon in the scene file <!(modified part in italics)>. If you haven't done so already, follow the instructions in the previous section to change the genbox command in the file to its corresponding polygons so we may edit them.
% vi room.rad gray_paint polygon room.5137 0 0 30 3 2 1.75 3 2 0 3 0 0 3 0 1.75 3 .625 1.75 3 .625 .625 3 1.375 .625 3 1.375 1.375 3 .625 1.375 3 .625 1.75Next, create a separate file for the window. (The use of separate files is desirable for parts of the scene that will be manipulated independently, as we will see in a moment.)
% vi window.rad # an 88% transmittance glass window has a transmission of 96%: void glass window_glass 0 0 3 .96 .96 .96 window_glass polygon window 0 0 12 3 .625 1.375 3 1.375 1.375 3 1.375 .625 3 .625 .625The vertex order is very important, especially for polygons with holes. Normally, vertices are listed in counterclock-wise order as seen from the front (the room interior in this case). However, the hole of a polygon has its vertices listed in the opposite order. This insures that the seam does not cross itself. The front of the window should face into our room, since it will later act as a light source, and light sources only emit from their front side.
The next step is the description of the scene outside the window. A special purpose generator, gensky, will create a description of the sun and sky which will be stored in a separate file. The arguments to gensky are the month, day and hour (local standard time). The following command produces a description for 10:00am on March 20th at latitude of 40 degrees, longitude 98 degrees:
% gensky 3 20 10 -a 40 -o 98 -m 105 > sky.radThe file "sky.rad" contains only a description of the sun and the sky distribution. The actual sky and ground are still undefined, so we will create another short file containing a generic background:
% vi outside.rad # # A standard sky and ground to follow a gensky sun and sky # distribution. # skyfunc glow sky_glow 0 0 4 .9 .9 1.15 0 sky_glow source sky 0 0 4 0 0 1 180 skyfunc glow ground_glow 0 0 4 1.4 .9 .6 0 ground_glow source ground 0 0 4 0 0 -1 180We can now put these elements together in one octree file using oconv:
% oconv outside.rad sky.rad window.rad room.rad > test.octNote that the above command results in the following error message:
oconv: fatal - (outside.rad): undefined modifier "skyfunc"The modifier is undefined because we put "outside.rad", which uses skyfunc before "sky.rad" where skyfunc is defined. It is therefore necessary to change the order of the files so that skyfunc is defined before it is used:
% oconv sky.rad outside.rad window.rad room.rad > test.octNow let's look at our modified scene, using the same command as before:
% rvu -vf default.vp -av .5 .5 .5 test.octAs you look around the scene, you will need to adjust the exposure repeatedly to be able to see detail over the wide dynamic range now present. To do this, wait a few seconds after choosing each new view and enter the command:
: exposure 1or simply:
: e 1All commands in rvu can be abbreviated by one or two letters. Additional control over the exposure is possible by changing the multiplier factor to a value greater than one to lighten or less than one to darken. It is also possible to use absolute settings and spot normalization. See the rvu manual entry for details.
You may notice that other than a patch of sun on the floor, the window does not seem to illuminate the room. In RADIANCE, certain surfaces act as light sources and others do not. Whether or not a surface is a light source is determined by its material type. Surfaces made from the material types light, illum, spotlight and (sometimes) glow will act as light sources, whereas surfaces made from plastic, metal, glass and other material types will not.
In order for the window to directly illuminate the room, it is therefore necessary to change its material type. We will use the type illum because it is specially designed for "secondary" light sources such as windows and other bright objects that are not merely emitters but have other important visual properties. An illum will act as a light source for parts of the calculation, but when viewed directly will appear as if made from a different material (or disappear altogether). Rather than modify the contents of "window.rad" which is a perfectly valid description of a non-source window, let's create a new file, which we can substitute during octree creation, called "srcwindow.rad":
% vi srcwindow.rad # # An emissive window # # visible glass type for illum: void glass window_glass 0 0 3 .96 .96 .96 # window distribution function, including angular # transmittance: skyfunc brightfunc window_dist 2 winxmit winxmit.cal 0 0 # illum for window, using 88% transmittance at normal # incidence: window_dist illum window_illum 1 window_glass 0 3 .88 .88 .88 # the source polygon: window_illum polygon window 0 0 12 3 .625 1.375 3 1.375 1.375 3 1.375 .625 3 .625 .625There are a couple of things you should notice in this file. The first definition is the normal glass type, window_glass, which is used for the alternate material for the illum window_illum. Next is the window distribution function, which is the sky distribution modified by angular transmittance of glass defined in winxmit.cal. Finally comes the illum itself, which is the secondary source material for the window.
To look at the scene, simply substitute "srcwindow.rad" for "window.rad" in the previous oconv command, thus:
% oconv sky.rad outside.rad srcwindow.rad room.rad > test.octYou can look at the room at different times by changing the gensky command used to create "sky.rad" and regenerating the octree. (Although the octree does not strictly need to be recreated for every change to the input files, it is good to get in the habit until the exceptions are well understood.)
Here is a minimal control file, which we'll call "simple.rif":
# My first "rad input file" ########################### # First, we must specify the "ZONE" for this scene, # which gives the # x, y and z dimensions of our space. The 'I' stands # for "interior", # since we are interested in the inside of this space: # xmin xmax ymin ymax zmin zmax ZONE= I 0 3 0 2 0 1.75 ########################### # Next, we need to tell rad what scene input files to # use and in what order. For this, we use the lower # case variable "scene", which allows multiple values. # Literally, all the values are concatenated by rad, # in the order we give them, on the oconv command line: scene= sky.rad outside.rad scene= srcwindow.rad scene= room.rad ########################### # Technically, we could stop here and let rad figure # out the rest, but it is very useful to also give # an exposure value that is appropriate for this scene. # We may discover this value from within rvu using # the "e =" command once we have found the exposure # level we like. For the interior of our space under # these particular lighting conditions, an exposure # value of 0.5 works well: # This could also have been given as "-1" (f-stops) EXPOSURE= 0.5Once we have this simple input file, we can start using rad to run our commands for us, eg:
% rad -o x11 simple.rifThe -o option tells rad to run rvu under X11 instead of creating pictures (the default action) using rpict. If you are using a different window system, then you should substitute the appropriate driver module for x11. To discover what modules are available with your version of rvu, type:
% rvu -devicesOnce started, rad shows us the commands as it executes them, first oconv then rvu .
Since we didn't specify a view in our control file, rad picks one for us, which it calls "X". This is one of the standard views, and it means "from the maximum x position." As another example, the view "yZ" would be from the minimum y and maximum z position. The actual positions are determined from the "ZONE" specification, and are just inside the boundaries for an interior zone, and well outside the boundaries for an exterior zone. (Please take a few moments at this time to consult the rad (1) manual page under "view" to learn more about these standard identifiers.) We could have selected a different standard view on the command line using the -v option, eg:
% rad -o x11 -v Zl simple.rifThis specification gives us a parallel projection from "Z", the maximum z position (ie. a plan view). Rather than executing another rad command, we can get the same view functionality from within rvu using the "L" command. (This is a single-letter command, corresponding roughly to the "last" command for retrieving views from files, explained earlier.) This command actually consults rad using the current control file to compute the desired view. The complementary "V" command appends the current view to the end of the control file for later access and batch rendering. For example, you can put the default viewpoint into your control file using the rvu commands:
: last default.vpfollowed by:
: V def.(Shorter view names are better because they end up being part of the picture file name, which can get quite long.) Move around in rvu to find a few different views you like, and save them (with sensible names) to the control file using the "V" command. If you make a mistake and save a view you later decide you dislike, you must edit the control file and manually remove the corresponding line.
Looking through the rad manual page, you will notice that there are many variables we have left unspecified in our simple control file. To discover what values these variables are given, we can use the -e option (together with -n and -s to avoid actually doing anything):
% rad -e -n -s simple.rifSome of these default values do not make sense for our scene. In particular, the VARIABILITY is not "Low", because there is sunlight entering our space. We should also change the DETAIL variable from "Medium" to "Low" because our space is really quite simple. Once we are satisfied with the geometry in our scene, we will probably want to raise the quality of output from the default value of "Low". It is also a good idea to specify an ambient file name, so renderings requiring an indirect calculation will be more efficient. We may add the following lines to "simple.rif" to correct these problems:
# We may abbreviate VARIABILITY with just 3 letters VAR= High # Anything starting with upper or lower case 'L' is LOW DET= L # Go for a medium quality result QUAL= Med # The file in which to store indirect values AMB= simple.ambIf we want to create picture files for the selected views in batch mode, we can run rad in the background, ie:
% rad simple.rif &This will, of course, echo the commands before they are executed, which may be undesirable for a background job. So, we can use the "silent" mode instead:
% rad -s simple.rif &Better still, we may want rad to record the commands executed, along with any error reports or other messages, to an error file:
% rad simple.rif >& errs &The ">&" notation is recognized by the C-shell to mean, "redirect both the standard output and the standard error to a file." Bourne shell users should use the following form, instead:
% rad simple.rif > errs 2>&1 &
# Terra Firma: void plastic ground_mat 0 0 5 .28 .18 .12 0 0 ground_mat ring groundplane 0 0 8 0 0 -.01 0 0 1 0 30 # A big, ugly, mirrored glass building: void mirror reflect20 0 0 3 .15 .2 .2 !genbox reflect20 building 10 10 2 | xform -t 10 5 0Note that the groundplane was given a slightly negative z value. This is very important so that the ground does not peek through the floor we have defined. The material type mirror, used to define the neighboring structure, is special in RADIANCE. Surfaces of this type as well as the types prism1 and prism2 participate in something called the "virtual light source" calculation. In short, this means that the surfaces of the building we have created will reflect sunlight and any other light source present in our scene. The virtual light source material types should be used with care since they can result in substantial growth in the calculation. It would be a good idea in the example above to remove the bottom surface of the building (which cannot be seen from the outside anyway) and change the roof type to metal or some non-reflecting material. This can be done using the same manual process described earlier for changing the room surface materials.
Now that we have a better description of the outside, what do we do with it? If we simply substitute it in our scene without changing the description of the window illum, the distribution of light from the window will be slightly wrong because the "skybright" function only describes light from the sky and the ground, not from other structures. Using this approximation might be acceptable in some cases, but other times it is necessary to consider outside geometry and/or shading systems to reach a reasonable level of accuracy. There are two ways to an accurate calculation of light from a window. The first is to treat the window as an ordinary window and rely on the default interreflection calculation of RADIANCE, and the second is to use the program mkillum to calculate the window distribution separately so we can still treat it as an illum light source. Let's try them both.
Using the default interreflection calculation is probably easier, but as we shall see it takes a little longer to get a good result in this case. To use the interreflection calculation, we modify the "scene" specification and a few other variables in "simple.rif" to create a new control file, called "inter.rif":
ZONE= I 0 3 0 2 0 1.75 # new exterior description scene= sky.rad outside2.rad # go back to simple window scene= window.rad scene= room.rad EXP= 0.5 VAR= High DET= L QUAL= Med # Be sure to use a unique name here AMB= inter.amb # One bounce now for illumination INDIRECT= 1 view= def -vp 2.25 .375 1 -vd -.25 .125 -.125To look at the scene with rvu, simply run:
% rad -o x11 inter.rifProbably the first thing you notice after starting rvu is that nothing happens. It takes the calculation a while to get going, as it must trace many rays at the outset to determine the contribution at each point from the window area. Once rvu has stored up some values, the progress rate improves, but it never really reaches blistering speed. A more efficient alternative in this case is to use the program mkillum to create a modified window file that uses calculated data values to define its light output distribution. Applying mkillum is relatively straightforward in this case. Simply create a new control file from "inter.rif", and name it "illum.rif", making the following changes:
ZONE= I 0 3 0 2 0 1.75 scene= sky.rad outside2.rad scene= room.rad # window will be made into illum illum= window.rad EXP= 0.5 VAR= High DET= L QUAL= Med # Be sure to use a unique name here AMB= illum.amb # No interreflections necessary with illum INDIRECT= 0 # Options for mkillum mkillum= -av 18 18 18 -ab 0 view= def -vp 2.25 .375 1 -vd -.25 .125 -.125The -av value given to mkillum is appropriate for the outside, which is much brighter, as suggested by the output of the gensky command stored in "sky.rad". The -ab option is set to 0, because outside the building we do not expect interreflections to play as important a role as in the interior (plus we are trying to save some time). To view the scene interactively, we again use rad:
% rad -o x11 illum.rifYou will notice that the calculation proceeds much more quickly, and even produces a smoother looking result. Aside from waiting for mkillum to finish, there is an additional price for this speed advantage, however. The contribution from the sun patch on the floor is no longer being considered, since we are not performing an interreflection calculation inside our space. The light from the window is being taken care of by the mkillum output, but the solar patch is not. In most cases, we endeavor to prevent direct sun from entering the space, and in the morning hours this is true for our model, but otherwise it is necessary to use the diffuse interreflection calculation to correctly account for all contributions. Note that the interreflection calculation is turned on automatically when the "QUALITY" variable in the control file is changed to "High".
Let's start by generating a fisheye picture of our design space:
% echo view= fish -vta -vp 1.5 .8 1 -vd 0 1 0 -vh 240 -vv 180 >> illum.rif % rad -v fish illum.rifThis picture will be used to identify sources of glare from a particular view point (1.5, 1, 1) about a particular direction (0, 1, 0). Since RADIANCE pictures contain true floating point radiance values, they can be used to analyze a visual environment for problems such as discomfort glare. Once rpict has finished (and this may take the several minutes), you may display the image using ximage or whatever display program you have available on your system. A fisheye perspective is a type of distortion that allows a wider field of view than a standard perspective image. This larger field is used by the program findglare to locate any and all bright spots that might affect visual comfort. Findglare can also use direct calculation with rtrace, but this takes a long time without providing the nice visual feedback one gets from an image.
To facilitate the use of findglare and the associated programs glarendx and xglaresrc, a script has been written called glare. This script asks you some questions and to make it a little easier to get a nice result. To start the script, simply type glare on the command line. When it asks you a name for the glare file you want to work with, enter something innocuous like "test.glr". It will tell you that the file does not exist, so we will have to create it. It then prompts you for the name of the picture and the name of the octree, which are "fish.pic" and "test.oct", respectively. When it asks for the view, just hit return because we want to use the default view from the picture file. Glare then asks what parameters it should use for the rtrace calculation. (Findglare will still use rtrace to calculate any points that it needs which are off the picture we have given it.) For this, you should give the -av setting from before (1 1 1). Then glare will ask you if the sources of glare are small, which they are not, and if you would like to set the glare threshold manually, which you would not. Finally, you will be asked what maximum angle you want to calculate away from the view center. Let's use 60 degrees (to the right and left). Glare then proceeds to call the program findglare to locate the actual glare sources. Once findglare has finished, glare will call the program xglaresrc (if you are running X11) to circle the glare sources found on the image.
You then have a choice of a few different glare indices you may have calculated from the computed sources. The Guth visual comfort probability (VCP) is perhaps the easiest to understand for those who are not familiar with glare metrics, because it gives a result in terms of a percentage of people who would be satisfied. Calculating the Guth VCP in this case, looking straight ahead (ie. 0 degrees), we see that less than 15% of the people would find this visual environment comfortable. Although the visual comfort probability increases as we look to the left (positive angles), it never gets over 20% for the range of angles we've given. That is primarily because the window is unshielded and very near the horizontal line of sight. Skylights and ceiling fixtures are a little nicer from a glare standpoint for that reason.