If this parameter is true, all the DN values from all of the bands in the input image, subject to the input cube attribute, will be propagated to the output file. Calculations for the other bands that require a sensor model (e.g., phase) will be based on the first band, again subject to the cube attribute. This doesn't affect the values calculated for those bands when the input image bands are spatially aligned, but it is very import when the bands of the input image are not spatially aligned (e.g., Level 1, Odyssey, Themis IR). Use the input cube attribute to select the band used to calculate the other phocube values (e.g., ThemisIR.cub+9,1-5). The geometry of the first band or the first band in the input attribute, will be used to calculate the phocube values. NOTE: If the DN parameter is also set then ALLDNS will take precedence, and DN will be ignored.

Note: The slope is measured relative to a sphere and not a more complex datum like the gravity model

Note: These X, Y, and Z bands are in the body fixed reference frame.

Note: These X, Y, and Z bands are in the body fixed reference frame.

This band is computed from the pixel resolution and emission angle using the following formula:

MorphologyRank = PixelResolution / cos(EmissionAngle)

The resulting output band can be used by automos to create a morphology-based mosaic product. This option uses the local emission angle if the input file is initialized (spiceinit) with an elevation model (DEM); otherwise, it uses the default calculation (from the ellipsoid). All computed cosines are tested for zero. If the result is zero, then the value is set to a constant value very close to zero.

Append the following parameters to the automos command line to utilize this backplane band:

priority=band type=keyword keyname=Name keyvalue=morphologyRank criteria=lesser.

This band is computed from the pixel resolution, incidence angle and emission angle using the following formula:

AlbedoRank = PixelResolution * [(1 / cos(EmissionAngle)) + (1 / cos(IncidenceAngle))]

The resulting output band can be used by automos to create an albedo-based mosaic product. This option always uses the local emission angle and local incidence angle if the input file is initialized (spiceinit) with an elevation model (DEM); otherwise, it uses the default calculation (from the ellipsoid). All computed cosines are tested for zero. If the result is zero, then the value is set to a constant value very close to zero.

Append the following parameters to the automos command line to utilize this backplane band:

priority=band type=keyword keyname=Name keyvalue=albedoRank criteria=lesser.

If this parameter is true, the Solar Illumination Mask (or shadow mask), will be determined for every pixel. This option is primarily useful for small irregular bodies (e.g. comets, asteroids), where terrain is occluded from solar illumination at the surface intersection point at a given pixel. This information cannot be provided solely by incidence or local incidence angles as the occlusion occurs due to foreground terrain, such as lobes in comets, at much larger distances than the proximity of the initial surface point of intersection. The output cube label will contain "Sun Illumination Mask" in the BandBin group, in band sequence of the output file.

The output mask pixel is a boolean value computed using ray trace functions. Pixels are either 1 (illuminated) or 0 (shadowed). A look direction from the sun is computed to the spacecraft (camera) pixel intercept location on the surface. If the solar intercept point on the surface is not the same point as seen from the spacecraft/camera perspective, it is deemed occluded (shadowed). For tessellated plate shape models, which are often used to represent the shape of irregular bodies, both camera and solar surface intercept points must occur on the same triangle at approximately the same location.

If the surface point is occluded/shadowed, a 0 (false) value is written as the output pixel mask value indicating it is not illuminated by the sun. All other cases will result in setting the output pixel mask value to 1 (true) indicating illumination by the sun. Note this mask will also include (i.e., identify pixels in) the local incidence backplane where the angles are greater than 90 degrees.

Note: The computation of this backplane is not supported for all ISIS shape models or for the ellipsoid. At this time we know that it functions properly using the Bullet ray trace engine.

If this parameter is true, the Surface Oblique Detector Resolution will be computed for every pixel and placed in a band in the output cube. This value differs from the Oblique Detector Resolution due to use of the local emission angle for that data. It is computed using the emission angle computed from the ellipsoid, which will produce a smoother data plane. The output cube label will contain "Surface Oblique Detector Resolution" in the BandBin group, in band sequence of the output file. SurfaceObliqueDetectorResolution is in millimeters.

Note: The computation of this backplane is not supported for all ISIS shape models or for the ellipsoid. At this time we know that it functions properly using the Bullet ray trace engine.