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ISIS 3 Application Documentation


photomet

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Perform photometric corrections on a cube

Overview Parameters Example 1 Example 2 Example 3 Example 4 Example 5 Example 6

Description

This program performs photometric correction on image pixels acquired under different illumination and viewing geometries by adjusting the brightness and contrast such that the resulting image appears as if obtained under uniform conditions. The photometric correction is applied to each pixel by computing a photometric model based on local photometric angles and a set of parameters that defines the model. Currently, no default values are assigned for any parameter names in the ISIS3 version of photomet.

Photometric angles can be computed from the following:

This program sets all pixels that have an incidence angle and/or emission angle greater than or equal to 90 degrees to NULL pixel values, regardless of the photometric angles resulting from using a topographic model.

The user must select a photometric model and a normalization model, with the option of adding an atmospheric model. Each of these models has a set of parameters that specifies its operation, which the user must provide. The different models can be mixed and matched to produce variations of the photometric correction.

  • You may enter the desired parameters by using the program GUI, which is recommended
  • A PVL file containing the photometric parmeters may be used if you opt to use the "frompvl" parameter
  • Within the GUI you may select a PVL file, and in addition, select the "frompvl" drop-down menu and photomet will load the values from the PVL file into the appropriate parameter names in the GUI for you. Note, if more than one model type for phtname, atmname, or normname parameters are in the PVL file, then the parameter values for the first model type encountered by the program are loaded. Review the parameter values to make sure the correct options are selected and have correct values before executing the program.
  • Values also can be entered manually at the command line
Note: If any parameter names are entered into the GUI after specifying "frompvl", the new values entered into the GUI will take precedence over the values entered in the PVL file.

There are three aspects of a photometric correction that should be considered when running the photomet program:

  1. The surface photometric function model type that describes the planetary surface. Any one of the surface photometric functions can be used in combination with any of the normalization type models and optionally an atmospheric photometric model.
  2. The atmospheric photometric function model type used when atmospheric scattering is present. The models that end with "1" use a first order scattering approximation, and those that end with "2" use a second order approximation; the second order has slower processing time because it uses more iterations and a quadratic equation versus fewer iterations and a linear equation used in the first order approximation.
  3. The type of normalization applied to the image to equalize the albedo or the topographic contrasts, or a combination of the two. One of the available modes must be selected.

The intent of topographic normalization is to correct for the variation in incidence, emission, and phase angles within and between images. Topographic normalization involves both a multiplicative correction that adjusts the contrast for a unit slope to reference conditions, and an additive correction to keep the average brightness uniform.

In practice, the albedo may be nonuniform, so a multistep process is used:

  1. Photomet is run in albedo mode, which decreases the brightness variations across the individual image and removes any additive atmospheric contribution.
  2. The output image in step 1 is divided by a low-pass-filtered version of itself, which removes the albedo variations if they have broader spatial scales than the topographic shading as is often the case.
  3. And finally, photomet is run again in topography mode on the output image from step 2, which reverses the albedo normalization of the first pass and then applies the topographic normalization.
In the absence of an atmosphere, the "albedo mode" is very simple: the image is divided by the photometric model evaluated at the actual angles and then multiplied by the model at a reference geometry. If an atmosphere is present, the additive component of the atmospheric scattering is subtracted at the real conditions before a multiplicative step, and added back as calculated for the standard conditions at the end. The "mixed mode" of normalization is used for images that span very large ranges of incidence angles. In the mixed mode, the albedo correction is applied at small incidence angles where albedo variations dominate topographic shading, and the topographic normalization is performed at large incidence angles where the reverse is true. A user-specified parameter "incmat" controls the incidence angle at which a smooth transition from one type of normalization to the other takes place.

The normalization models that use an atmospheric correction are albedoatm, shadeatm, and topoatm. If using the GUI interface photomet will automatically exclude all atmospheric models for normaliztion types that do not require an atmospheric correction.

Question: What happens if the normalization model I chose does not perform an atmospheric correction although I have an atmospheric model defined in my PVL file?
Answer: If you have chosen a normalization model that does not perform atmospheric correction, then the image is normalized without applying the atmospheric correction.

New Developments

A new parameter name "chngpar" was added to photomet to allow the user to enter a string consisting of parameter names and values outside of the PVL files. This string replaces any parameter already defined. This is useful when one or two parameter values change for each image but all the other parameter values remain the same.

The parameter name "ZEROB0STANDARD" was shortened to "ZEROB0ST," but the longer name will still work for backward compatibility. The default is to get the user setting for "ZEROB0ST" from the PVL file. If no PVL file exists and the user does not specify a "FALSE" or "TRUE" option, the program will automatically default to "TRUE" to follow the default setting in previous photomet versions. PLEASE NOTE: This change was actually not added because the ability to support aliases (or deprecated) values has not been fully implemented in ISIS. As a result, you must use the full ZEROB0STANDARD parameter name.

The parameter name "INCMAT" is no longer required when the "ALBEDO" normalization model is selected. The parameter name will still appear in the GUI for backward compatibility, but does not need to be defined by the user in the GUI or on the command line.

A set of photomet PVL templates for Mars and other planetary bodies developed in ISIS2 are now available in $ISIS3DATA/base/templates/photometry/ directory. There are also additional examples of PVL files for different photometric models under "Example PVL files," later in this document.

Note: The NoNormalization model has been removed because it duplicated the functionality of the shade model. Use shade with incref=0 and albedo=1.0 instead.

The program photemplate can be used to set up the PVL file containing the selected options for photomet.

The tables below show the models and their related parameter requirements along with the ISIS2 default values. The ISIS2 default values are only meant to serve as possible initial values to test backward compatibility since there are no default values defined in ISIS3.





SURFACE PHOTOMETRIC FUNCTION MODELS


Available photometric function models and required parameter names
Name Required parameter names
Hapkehen B0, hg1, hg2, hh, theta, wh
Hapkeleg Theta, wh, bh, ch, hh, b0, zerob0st
Lambert None
LommelSeeliger None
LunarLambert L
LunarLambertEmpirical Phaselist, llist, phasecurvelist
LunarLambertMcEwen None
Minnaert K
MinnaertEmpirical Phaselist, klist, phasecurvelist


Photometric model parameter names and settings
Name Description ISIS2 default Valid range
B0 Hapke opposition surge component 0.0 0 <= value
Bh Hapke Legendre coefficient for single particle phase function 0.0 -1 <= value <= 1
Ch Hapke Legendre coefficient for single particle phase function 0.0 -1 <= value <= 1
Hg1 Hapke Henyey Greenstein coefficient for single particle phase function 0.0 0 <= value <= 1
Hg2 Hapke Henyey Greenstein coefficient for single particle phase function 0.0 0 <= value <= 1
Hh Hapke opposition surge component 0.0 0 <= value
K Minnaert function exponent 1.0 0 <= value
L Lunar-Lambert function weight 1.0 No limit
Theta Hapke macroscopic roughness component 0.0 0 <= value <= 90
Wh Hapke single scattering albedo component 0.5 0 < value <= 1
Zerob0st Flag to set opposition surge B0 to zero True True or False
Phaselist Phase list for empirical functions None String
Llist Exponent list of limb darkening values None String
Klist Exponent list of limb darkening values None String
Phasecurvelist Phase curve list of brightness values None String

The functions are defined as follows, where phase is the phase angle, and u0 and u are the cosines of the incidence and emission angles, respectively:

Lambert
FUNC=u0
LommelSeeliger
FUNC=u0/(u0+u)
Minnaert
FUNC=u0**K * u**(K-1)
LunarLambert (Lunar-Lambert, "lunar" part is Lommel-Seeliger)
FUNC=(1-L)*u0 + 2*L*u0/(u0+u)
MinnaertEmpirical
FUNC=B(phase) * u0**K(phase) * u**(K(phase)-1)
LunarLambertEmpirical
FUNC=B(phase) * ((1-L)*u0 + 2*L*u0/(u0+u))


ATMOSPHERIC PHOTOMETRIC FUNCTION MODELS


Available atmosphereic functions and required parameter names
Function model name Required parameters
Anisotropic1 Bha, hnorm, nulneg, tau, tauref, wha
Anisotropic2 Bha, hnorm, nulneg, tau, tauref, wha
HapkeAtm1 Hga, hnorm, nulneg, tau, tauref, wha
HapkeAtm2 Hga, hnorm, nulneg, tau, tauref, wha
Isotropic1 Hnorm, nulneg, tau, tauref, wha
Isotropic2 Hnorm, nulneg, tau, tauref, wha


Atmospheric models parameter names and settings
Name Description ISIS2 Default Valid Range
Bha Coefficient of the single particle Legendre phase function 0.85 -1 <= value <= 1
Hga Coefficient of single particle Henyey Greenstein phase function 0.68 -1 < value < 1
Hnorm Atmospheric shell thickness normalized to the planet radius 0.003 0 <= value
Nulneg Specifies if negative values after removal of atmospheric effects will be set to NULL NO YES or NO
Tau Normal optical depth of the atmosphere 0.28 0 <= value
Tauref Reference value of tau to which the image will be normalized 0.0 0 <= value
Wha Single scattering albedo of atmospheric particles 0.95 0 < value < 1




PHOTOMETRIC NORMALIZATION MODELS


Available photometric normalization functions and required parameter names
Function name Normalization function type Required parameter names
Albedo Albedo contrasts uniform Albedo, incref, thresh
AlbedoAtm Albedo with atmosphere Incref
Mixed Albedo at low incidence blended to topo at high incidence Albedo, incmat, incref, thresh
MoonAlbedo Special Lunar model Bsh1, d, e, f, g2, h, wl, xb1, xb2, xmul
Shade Shaded relief model Albedo, incref
ShadeAtm Shaded relief with atmosphere Albedo, incref
Topo Topographic shading uniform Albedo, incref, thresh
TopoAtm Topographic shading with atmosphere Albedo, incref


Normalization model parameter names and settings
Name Description ISIS2 default Valid range
Albedo Albedo to which the image will be normalized 1.0 No limit
Bsh1 Albedo dependent phase function normalization parameter 0.08 0 <= value
D Albedo dependent phase function normalization parameter 0.14 No limit
E Albedo dependent phase function normalization parameter -0.4179 No limit
F Albedo dependent phase function normalization parameter 0.55 No limit
G2 Albedo dependent phase function normalization parameter 0.02 No limit
H Albedo dependent phase function normalization parameter 0.048 No limit
Incmat Specifies incidence angle where albedo normalization transitions to incidence normalization 0.0 0 <= value < 90
Incref Reference incidence angle to which the image will be normalized 0.0 0 <= value < 90
Thresh Sets upper limit on amount of amplification in regions of small incidence angle 30.0 No limit
Wl Wavelength in micrometers of the image being normalized 1.0 No limit
Xb1 Albedo dependent phase function normalization parameter -0.0817 No limit
Xb2 Albedo dependent phase function normalization parameter 0.0081 No limit
Xmul Used to convert radiance to reflectance or apply a calibration fudge factor 1.0 No limit


Example PVL files:
    Example 1:

    Object = PhotometricModel
      Group = Algorithm
        PhtName = Lambert
      EndGroup
    EndObject
    Object = NormalizationModel
      Group = Algorithm
        NormName = Shade
	Incref = 0.0
	Albedo = 1.0
      EndGroup
    EndObject

    --------------------------------
    Example 2:

    Object = PhotometricModel
      Group = Algorithm
        PhtName = Minnaert
	K = 0.5
      EndGroup
    EndObject
    Object = NormalizationModel
      Group = Algorithm
        NormName = Albedo
	Incref = 0.0
	Incmat = 0.0
	Albedo = 1.0
	Thresh = 30.0
      EndGroup
    EndObject

    --------------------------------
    Example 3:

    Object = PhotometricModel
      Group  = Algorithm
        PhtName = Hapkehen
	Wh = 0.52
	Hh = 0.0
	B0 = 0.0
	Theta = 30.0
	Hg1 = 0.213
	Hg2 = 1.0
      EndGroup
    EndObject
    Object = AtmosphericModel
      Group = Algorithm
        AtmName = hapkeatm2
	Hnorm = 0.003
	Tau = 0.28
	Tauref = 0.0
	Wha = 0.95
	Hga = 0.68
      EndGroup
    EndObject
    Object = NormalizationModel
      Group = Algorithm
        NormName = albedoatm
	Incref = 0.0
      EndGroup
    EndObject

    --------------------------------
    Example 4 (Used to process Clementine UVVIS filter "a" data):

    Object = PhotometricModel
      Group  = Algorithm
        PhtName = LunarLambertMcEwen
      EndGroup
    EndObject
    Object = NormalizationModel
      Group = Algorithm
        NormName = MoonAlbedo
	D = 0.0
	E = -0.222
	F = 0.5
	G2 = 0.39
	H = 0.062
	Bsh1 = 2.31
        Wl = 1.0
        Xb1 = 1.0
        Xb2 = 1.0
      EndGroup
    EndObject

    --------------------------------
    Example 5 (Used to process Clementine UVVIS filter "b" data):

    Object = PhotometricModel
      Group  = Algorithm
        PhtName = LunarLambertMcEwen
      EndGroup
    EndObject
    Object = NormalizationModel
      Group = Algorithm
        NormName = MoonAlbedo
	D = 0.0
	E = -0.218
	F = 0.5
	G2 = 0.4
	H = 0.054
	Bsh1 = 1.6
        Wl = 1.0
        Xb1 = 1.0
        Xb2 = 1.0
      EndGroup
    EndObject

    --------------------------------
    Example 6 (Used to process Clementine UVVIS filter "cde" data):

    Object = PhotometricModel
      Group  = Algorithm
        PhtName = LunarLambertMcEwen
      EndGroup
    EndObject
    Object = NormalizationModel
      Group = Algorithm
        NormName = MoonAlbedo
	D = 0.0
	E = -0.226
	F = 0.5
	G2 = 0.36
	H = 0.052
	Bsh1 = 1.35
        Wl = 1.0
        Xb1 = 1.0
        Xb2 = 1.0
      EndGroup
    EndObject

    --------------------------------
    Example 7 (Used for Mars red filter data to apply empirical photometric models):

    Object = PhotometricModel
    # For Mars red filter images
    # The phase angles at which the coefficient values for the Lunar Lambert
    # Empirical (LunarLambertEmpirical) L and the Minnaert Empirical K approximation are
    # calculated, along with the brightness (phase curve) values at those
    # points (ALL ON ONE LINE!)

      Group = Algorithm
	PhtName = LunarLambertEmpirical
	PhaseList = "0.,10.,20.,30.,40.,50.,60.,70.,80.,90.,100.,110.,120.,130.,140.,150.,160.,170.,180."
	LList = "0.946,0.748,0.616,0.522,0.435,0.350,0.266,0.187,0.118,0.062,0.018,-0.012,-0.027,
	   -0.035,-0.036,-0.037,-0.031,-0.012,-0.010"
	PhaseCurveList = "0.1578,0.1593,0.1558,0.1484,0.1391,0.1292,0.1194,0.1099,0.1008,0.09176,
	   0.08242,0.07234,0.06165,0.05106,0.04091,0.03137,0.02171,0.01038,0."
      EndGroup

      Group = Algorithm
	PhtName = MinnaertEmpirical
	PhaseList = "0.,10.,20.,30.,40.,50.,60.,70.,80.,90.,100.,110.,120.,130.,140.,150.,160.,170.,180."
	KList = "0.518,0.595,0.660,0.709,0.753,0.796,0.837,0.875,0.904,0.922,0.926,0.935,0.954,0.986,
	   1.019,1.063,1.099,1.095,1.090"
	PhaseCurveList = "0.1574,0.1582,0.1546,0.1470,0.1375,0.1273,0.1174,0.1077,0.09797,0.08750,
	   0.07594,0.06466,0.05471,0.04665,0.03935,0.03339,0.02642,0.01482,0."
      EndGroup
    EndObject


  References:

  Chandrasekhar, S., 1960.  Radiative Transfer. Dover, 393 pp.
  Hapke, B. W., 1981. Bidirectional reflectance spectroscopy 1: Theory. J.
     Geophys. Res., pp. 86,3039-3054.
  Hapke, B., 1984. Bidirectional reflectance spectroscopy3: Corrections for
     macroscopic roughness. Icarus, 59, pp. 41-59.
  Hapke, B., 1986. Bidirectional reflectance spectroscopy 4: The extinction
     coefficient and the opposition effect. Icarus, 67, pp. 264-280.
  Johnson, J. R., et al., 1999, Preliminary Results on Photometric Properties of
     Materials at the Sagan Memorial Station, Mars, J. Geophys. Res., 104, 8809.
  Kirk, R. L., Thompson, K. T., Becker, T. L., and Lee, E. M., 2000.
     Photometric modelling for planetary cartography. Lunar Planet. Sci., XXXI,
     Abstract #2025, Lunar and Planetary Institute, Houston (CD-ROM).
  Kirk, R. L., Thompson, K. T., and Lee, E. M., 2001. Photometry of the martian
     atmosphere:  An improved practical model for cartography and photoclinometry.
     Lunar Planet. Sci., XXXII, Abstract #1874, Lunar and Planetary Institute,
     Houston (CD-ROM).
  McEwen, A. S., 1991. Photometric functions for photoclinometry and other
     applications.  Icarus, 92, pp. 298-311.
  Thorpe, T. E., 1973, Mariner 9 Photometric Observations of Mars from November
     1971 through March 1972, Icarus, 20, 482.
  Tomasko, M. G., et al., 1999, Properties of Dust in the Martian Atmosphere from
     the Imager on Mars Pathfinder, J. Geophys. Res., 104, 8987.
  

Categories


Related Applications to Previous Versions of ISIS

This program replaces the following application existing in previous versions of ISIS:
  • photomet

Related Objects and Documents

Applications


History

Tammy Becker1989-02-15 Original version - based on Tammy Becker's photom/photompr programs which were later converted to Randy Kirk's photomet
Janet Barrett2008-03-07 Added code to acquire the BandBin Center keyword from the input image. This value is needed in case the user chooses the MoonAlbedo normalization method.
Steven Lambright2008-05-13 Removed references to CubeInfo
Jeannie Walldren2009-01-08 Added MAXEMISSION and MAXINCIDENCE parameters. Modified code to set off-target pixels to NULL. Added appTests for new parameters. Added user documentation examples.
Eric Hyer2010-11-10 Added USEDEM parameter.
Janet Barrett2010-11-22 Added error check for situations where there is not an intersection with the DEM and the local photometric angles are requested.
Janet Barrett2010-11-23 Added capability to use both ellipsoid and DEM photometric angles in atmospheric corrections. This provides the ability to do shading using a DEM surface.
Janet Barrett2011-02-22 The USEDEM parameter has been removed and the ANGLESOURCE parameter has been added. The ANGLESOURCE parameter lets you specify the source where the photometric angles will come from: ellipsoid, DEM, or center of image.
Janet Barrett2011-03-29 The CENTER option of the ANGLESOURCE parameter has been removed and the CENTER_FROM_IMAGE, CENTER_FROM_LABEL and CENTER_FROM_USER options have been added. This allows the user to determine where the center photometric angles will come from.
Janet Barrett2011-09-23 The following changes were made to the program for the ISIS3.3.0 release: 1) The PHOPAR parameter name was changed to FROMPVL - this was done to have consistent parameter names throughout the photometry software. 2) All radio button options are now accessed through drop down menus. The only radio button options that existed prior to this release were those for choosing the ANGLESOURCE. In order to use any of the drop down menus, click on the drop down menu and hold the mouse button down while navigating to the choice that you want. 3) Added a USEDEM option which will let you determine how the trim is performed. If you don't check the USEDEM box, then trimming is performed based on the photometric angles of the ellipsoid. If you check the USEDEM box, then the trimming is performed based on the photometric angles of the DEM (if one is specified in the image labels). If there is no DEM associated with your FROM file, then the default is to use the ellipsoid. 4) The program now lets you specify the photometric model, atmospheric model, and normalization model through the PHTNAME, ATMNAME, and NORMNAME drop down menus. Prior to this release, you were forced to provide an input PVL file with all of the model information in it. You can now provide the model information through the PVL, the GUI, or a combination of both. If you provide a FROMPVL file, then you need to use the GUI to specify which model(s) to use from that file. If you change any of the model-specific parameters in the GUI, then they will override the values in the FROMPVL file. 5) The BHAREF, HGAREF, and WHAREF parameters have been removed because they were obsolete. 6) The NONORMALIZATION model was removed because it duplicated the functionality of the SHADE model. 7) More photometric models have been added. The Hapke Legendre, Minnaert Empirical, and Lunar Lambert Empirical models have been added. The Minnaert Empirical model has parameters PHASELIST, PHASECURVELIST, and KLIST associated with it. The information for the new parameters is a list of comma delimited values (phase angle goes in PHASELIST, brightness values go in PHASECURVELIST, and limb darkening values go in KLIST). The Lunar Lambert Empirical model has parameters PHASELIST, PHASECURVELIST, and LLIST where LLIST is similar to the KLIST parameter for Minnaert Empirical. 8) A USEDEM parameter has been added which allows the user to determine which photometric angles to use for trimming. If the USEDEM parameter is set to false, then the photometric angles of the ellipsoid are used. If USEDEM is set to true, then the photometric angles of the DEM shape model are used for trimming. 9) Helper buttons were added to the FROMPVL to allow you to View a PVL or to Load a PVL. PLEASE NOTE: When loading a Minnaert Empirical or Lunar Lambert Empirical model from a PVL, only the first value will be loaded into the GUI. This is a known problem and will be fixed in the next patch or release to ISIS. 10) ***NOTE*** The Minnaert Empirical and Lunar Lambert Empirical models do not load properly from a PVL file when using the Load PVL helper button. This is a known problem and will be fixed in the next patch or release of ISIS.
Janet Barrett2011-11-04 The ZEROB0STANDARD parameter for the Hapke models was not added to the new update of photomet during the last release. This parameter is responsible for determining if the Hapke opposition surge component B0 is set to zero when calculations are based on standard conditions. This parameter has been added to the new interface to photomet.
Janet Barrett2012-01-10 The program was fixed to make it backwards compatible with older PVL files. If you tried running this program with an older PVL, then you most likely got the following error message "A Normalization model must be specified before running this program." This message would have occurred even if you had a Normalization model specified in your FROMPVL file. This problem has been fixed. If your FROMPVL file specifies a Normalization model, then you aren't required to specify one through the program interface as well.
Janet Barrett2012-05-04 A new BACKPLANE option was added to ANGLESOURCE. This BACKPLANE option allows you to input photometric angle information using separate ISIS cube files. Files containing geometric, photometric, etc. information pixel by pixel for the input image file are normally referred to as backplanes. This option was added to support image data that does not have a camera model associated with it. If you have a way to generate the photometric angles for such data, then you will be able to do photometric correction on it. This option is also very useful for speeding up the processing done by photomet. If you have all the photometric information pre-computed, then this information no longer needs to be generated every time the program is run. You can input photometric information using a combination of files and photometric angle constants. For example, if you have a file containing the phase angle for every pixel, a file containing the incidence angle for every pixel, and you know that the emission angle is 0.0 for every pixel, then you can use the PHASE_ANGLE_FILE, INCIDENCE_ANGLE_FILE, and EMISSION_ANGLE fields to input the 2 file names and the emission angle constant.
Ella Mae Lee2012-10-05 Improved the documentation, reference Mantis issue #453, #843
Janet Barrett2012-10-24 The following changes were made to the program: 1) Added a new parameter, CHNGPAR, which allows the user to change any of the model- related parameter settings without having to specify the model name on the command line or in the GUI. Before the CHNGPAR parameter was added, you could only change a model-related parameter on the command line or in the GUI if you also specified the model name using the PHTNAME, ATMNAME, or NORMNAME parameter. Any value you set using the CHNGPAR parameter will override changes that are specified in the GUI. Any value that is changed through the GUI will override values specified in the FROMPVL file. **PLEASE NOTE**: Any parameter that you type into the CHNGPAR string MUST be spelled correctly and using the full name (no partial parameter names). Otherwise, the program will not recognize the parameter and it won't get used. 2) Added new output groups to the print.prt log file so that the user can see exactly which values were used to run photomet. The new groups that get written to the print.prt file include NormalizationModelParametersUsed, AtmosphericModelParametersUsed, and PhotometricModelParametersUsed. 3) Fixed photomet so that the INCMAT parameter is no longer required for the ALBEDO normalization model. The INCMAT parameter is not used by the ALBEDO normalization model, so the user is no longer required to input an INCMAT value for that model. 4) Fixed a problem which was causing the NULNEG and ZEROB0STANDARD parameters to be loaded incorrectly if specified in the FROMPVL file. 5) Added a more meaningful error message when a normalization model is not specified by the user either through the GUI, command line, or FROMPVL file. 6) Changed the ZEROB0STANDARD parameter name to ZEROB0ST. This was to help prevent the user from needing to resize the GUI each time they opened it because the parameter name was too long. We are maintaining backwards compatibility by supporting both ZEROB0STANDARD and ZEROB0ST in the photomet code. This will allow you to run a script with the old parameter name without any problems.
Janet Barrett2012-12-07 PLEASE NOTE (in reference to change made on 2012-10-24): The backwards compatibility for the shorter ZEROB0ST parameter name has not been fully implemented in ISIS. As a result, this change has been removed and the full ZEROB0STANDARD parameter name must be used. Support for aliases (deprecated values) must be fully implemented in ISIS before the shorter parameter name (ZEROB0ST) will be available. Fixes #1288.
Lynn Weller2013-02-25 Removed links to applications imbedded in text and replaced with italicized application name. Added application links to the "Related Objects and Documents" section of the documentation. Fixes mantis ticket #1525.
Kelvin Rodriguez2016-08-24 Added cast to void on 'changePar.simplified()' function call to silience unused return value warnings on OS X
Curtis Rose2016-11-16 Decoupled ANGLESOURCE and USEDEM parameters. They were working incorrectly before and were tangled together a bit. They are separated now and working as expected. Anglesource DEM makes the photometric calculations based on the DEM of the image if it exists. Anglesource ELLIPSOID makes the photometric calculations based on the radius obtained from the DEM shape model. Usedem true trims the image using the photometric calculations on the radius obtained from the DEM shape model. Usedem false trims the image using the from the IAU/NAIF target body file, which is defined within the cube's kernel group as the TargetAttitudeShape. Fixes #4180.
Lauren Adoram-Kershner2019-11-07 Added a warning when the 'DEM' angle source option is used with 'mixed' or 'topo' normalization method. Fixes #3451 and #3452.

Parameter Groups

Files

Name Description
FROM Input cube file
TO Output cube file
FROMPVL Input PVL file

Change Parameters

Name Description
CHNGPAR Change parameter string

Trim Parameters

Name Description
MAXEMISSIONMaximum emisson angle to trim image
MAXINCIDENCEMaximum incidence angle to trim image
USEDEM Specify if DEM photometric angels will be used to trim image

Angle Source Options

Name Description
ANGLESOURCE Source of photometric angles: ELLIPSOID, DEM, CENTER, or FILE
PHASE_ANGLE_FILE Phase angle cube file
INCIDENCE_ANGLE_FILE Incidence angle cube file
EMISSION_ANGLE_FILE Emission angle cube file
PHASE_ANGLE Center phase angle
INCIDENCE_ANGLE Center incidence angle
EMISSION_ANGLE Center emission angle

Photometric Model

Name Description
PHTNAME Photometric model to be used
THETA Macroscopic roughness angle
WH Single scattering albedo
HG1 Hapke Henyey Greenstein coefficient
HG2 Hapke Henyey Greenstein Coefficient
BH Hapke Legendre coefficient
CH Hapke Legendre coefficient
HH Hapke opposition surge
B0 Hapke opposition surge
ZEROB0STANDARD Specifies if opposition surge is set to zero under standard conditions
L Lunar-Lambert function weight
K Minnaert function exponent
PHASELIST Empirical functions phase angle list
KLIST Minnaert Empirical function limb darkening parameter list
LLIST Lunar Lambert Empirical function limb darkening parameter list
PHASECURVELIST Empirical functions phase curve (brightness) value list

Atmospheric Model

Name Description
ATMNAME Atmospheric model to be used
NULNEG Specifies if negative values will be set to NULL
TAU Optical depth of atmosphere
TAUREF Reference value of tau
HGA Henyey Greenstein coefficient
WHA Single scattering albedo
BHA Legendre coefficient
HNORM Atmospheric shell thickness

Normalization Model

Name Description
NORMNAME Normalization model to be used
INCREF Reference incidence angle
INCMAT Photometric transition incidence angle
THRESH Amplification threshold
ALBEDO Albedo
D Albedo normalization parameter
E Albedo normalization parameter
F Albedo normalization parameter
G2 Albedo Normalization Parameter
H Albedo normalization parameter
XMUL Radiance to reflectance or calibration factor
WL Wavelength
BSH1 Albedo normalization parameter
XB1 Albedo normalization parameter
XB2 Albedo normalization parameter
X

Files: FROM


Description

This is the input filename that will be photometrically corrected.

Type cube
File Mode input
Filter *.cub
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Files: TO


Description

This output file will contain the results of the photometric correction.

Type cube
File Mode output
Pixel Type real
Close Window
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Files: FROMPVL


Description

This text file contains the parameter names and values to be used to perform the photometric correction.

Type filename
File Mode input
Default Path $base/templates/photometry
Internal Default None Specified
Filter *.pvl
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Change Parameters: CHNGPAR


Description

Chngpar is used to enter a string of parameter names and values enclosed in quotes that will be added to or replaces the pre-defined parameter values. PLEASE NOTE: Any parameter names used in the CHNGPAR string input MUST be spelled out completely and without any errors. Otherwise, they will be ignored by the program.

Example:
photomet from=f1.cub to=pho.cub frompvl=my.pvl chngpar="tau=0.5 tauref=30"

Type string
Default None
Internal Default None
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Trim Parameters: MAXEMISSION


Description

The maximum number of degrees allowed for the emission angle in order to retain the data. This number must be between 0.0 and 90.0.

Type double
Default 90.0
Minimum 0.0 (inclusive)
Maximum 90.0 (inclusive)
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Trim Parameters: MAXINCIDENCE


Description

The maximum number of degrees allowed for the incidence angle in order to retain the data. This number must be between 0.0 and 90.0.

Type double
Default 90.0
Minimum 0.0 (inclusive)
Maximum 90.0 (inclusive)
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Trim Parameters: USEDEM


Description

This specifies if the image will be trimmed based on the photometric angles obtained from the ellipsoid (default) or the DEM surface.

The ellipsoid is retrieved from the IAU/NAIF target body file, which is defined within the cube's kernel group as the TargetAttitudeShape. If this parameter is set to false, then the photometric angles will be obtained from the ellipsoidal surface.

The photometric angles obtained from the DEM surface (shape model) for each pixel are obtained using an ellipsoid defined by the radius obtained from the DEM shape model. Note that photomet does not trim using local slopes.

Type boolean
Default FALSE
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Angle Source Options: ANGLESOURCE


Description

The incidence, emission, and phase angles are determined based on the source defined by the user. The available options are listed below:

ELLIPSOID (default)
The photometric angles for each pixel are obtained using an ellipsoid defined by the radius obtained from the DEM shape model.
DEM
The photometric angles for each pixel are obtained using the DEM shape model (if one is defined in the image labels). The surface roughness is taken into account to calculate a surface normal, which is used to calculate the photometric angles. i.e. slope, local emission, local incidence.
CENTER_FROM_IMAGE
The photometric angles are obtained from the center of the input image using the ellipsoid shape model. These angles are applied to every pixel in the input file. This option is best for images where the photometric angles do not vary much and when faster processing is desired.
CENTER_FROM_LABEL
The photometric angle keywords are obtained from the label of the input image, and applied to every pixel in the file. The keywords "IncidenceAngle," "EmissionAngle," and "PhaseAngle" must be in the image labels. This option is best for images where the photometric angles do not vary much and when faster processing is desired.
CENTER_FROM_USER
The photometric angles are obtained from the values defined for IncidenceAngle, EmissionAngle, and PhaseAngle parameter names. These angles are applied to every pixel in the file. This option is best for images where the photometric angles do not vary much and when faster processing is desired.
BACKPLANE
The photometric angles are obtained from separate cube files, which contain the information for each pixel in the input file. These angles are applied to every pixel in the file. This option is best for images that will be processed through the same steps many times with different photometric settings because the photometric angles are not recomputed each time for every pixel. This option is also used for images that do not have a camera model associated with them. If no camera model is available, then create files that contain the photometric angle information for each pixel in the input file with fx or another program. It is very important that the new files have the same number of samples and lines as the input file.

Type combo
Default ELLIPSOID
Internal Default ELLIPSOID
Option List:
Option Brief Description
ELLIPSOIDGet angles from ELLIPSOID The photometric angles for each pixel are obtained using an ellipsoid defined by the radius obtained from the DEM surface (shape model).

Exclusions

  • PHASE_ANGLE_FILE
  • INCIDENCE_ANGLE_FILE
  • EMISSION_ANGLE_FILE
  • PHASE_ANGLE
  • INCIDENCE_ANGLE
  • EMISSION_ANGLE
DEMGet angles from DEM The photometric angles for each pixel are obtained using the DEM surface (shape model).

Exclusions

  • PHASE_ANGLE_FILE
  • INCIDENCE_ANGLE_FILE
  • EMISSION_ANGLE_FILE
  • PHASE_ANGLE
  • INCIDENCE_ANGLE
  • EMISSION_ANGLE
CENTER_FROM_IMAGEGet angles from center of image The photometric angles are obtained from the center of the input image using the ellipsoid shape model.

Exclusions

  • PHASE_ANGLE_FILE
  • INCIDENCE_ANGLE_FILE
  • EMISSION_ANGLE_FILE
  • PHASE_ANGLE
  • INCIDENCE_ANGLE
  • EMISSION_ANGLE
CENTER_FROM_LABELGet angles from image label The keyword values for "IncidenceAngle," "EmissionAngle," and "PhaseAngle" are extracted from the image labels and used for the photometric angles to apply to every pixel.

Exclusions

  • PHASE_ANGLE_FILE
  • INCIDENCE_ANGLE_FILE
  • EMISSION_ANGLE_FILE
  • PHASE_ANGLE
  • INCIDENCE_ANGLE
  • EMISSION_ANGLE
CENTER_FROM_USERGet the angles from user The photometric angles are obtained from the user and applied to every pixel in the file.

Exclusions

  • PHASE_ANGLE_FILE
  • INCIDENCE_ANGLE_FILE
  • EMISSION_ANGLE_FILE

Inclusions

  • PHASE_ANGLE
  • INCIDENCE_ANGLE
  • EMISSION_ANGLE
BACKPLANEGet the angles from separate file(s) The photometric angles are obtained from separate backplane band(s) or file(s) which contain the angle information for each pixel in the input image file.

Exclusions

  • PHASE_ANGLE
  • INCIDENCE_ANGLE
  • EMISSION_ANGLE
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Angle Source Options: PHASE_ANGLE_FILE


Description

This file must contain the phase angle information for the input cube.

Type cube
File Mode input
Pixel Type real
Internal Default No file
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Angle Source Options: INCIDENCE_ANGLE_FILE


Description

This file must contain the incidence angle information for the input cube.

Type cube
File Mode input
Pixel Type real
Internal Default No file
Close Window
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Angle Source Options: EMISSION_ANGLE_FILE


Description

This file must contain the emission angle information for the input cube.

Type cube
File Mode input
Pixel Type real
Internal Default No file
Close Window
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Angle Source Options: PHASE_ANGLE


Description

The center phase angle to use if the CENTER_FROM_USER option is chosen.

Type double
Default 0.0
Minimum 0.0 (inclusive)
Maximum 180.0 (inclusive)
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Angle Source Options: INCIDENCE_ANGLE


Description

The center incidence angle to use if the CENTER_FROM_USER option is chosen.

Type double
Default 0.0
Minimum 0.0 (inclusive)
Maximum 90.0 (inclusive)
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Angle Source Options: EMISSION_ANGLE


Description

The center emission angle to use if the CENTER_FROM_USER option is chosen.

Type double
Default 0.0
Minimum 0.0 (inclusive)
Maximum 90.0 (inclusive)
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Photometric Model: PHTNAME


Description

Specify the name of the surface photometric function model to apply to the input image. The available options are the following:

FROMPVL
Gets the photometric model from the PVL file. If the required parameter names and values are missing from the PVL file, either add them to the PVL file, or enter the values at the command line or use the GUI to enter the values.
LAMBERT
A simple photometric model which predicts that light incident on a surface is scattered uniformly in all directions; the total amount of reflected light depends on the incidence angle of the illumination. This function does not depend upon the outgoing light direction.
HAPKEHEN
Derive model albedo using the complete Hapke model with Henyey-Greenstein single-particle phase function whose coefficients are hg1 and hg2, plus single scattering albedo wh, opposition surge parameters hh and b0, and macroscopic roughness theta. For a smooth model with opposition effect use theta=0.

The table below shows the Hapke parameters for Mars from Johnson et al. (1999) for IMP data of Photometry Flats (soil) and may be reasonably representative of Mars as a whole. Note that (hg1, hg2=1.0) is equivalent to (-hg1, hg2=0.0).

Parameter settings for Mars
Band Wh B0 Hh Hg1 Hg2
Red 0.52 0.025 0.17 0.213 1.0
Green 0.29 0.29 0.17 0.19 1.0
Blue 0.16 0.995 0.17 0.145 1.0
HAPKELEG
Derive model albedo using complete Hapke model with Henyey Legendre two-term Legendre polynomial phase function whose coefficients are bh and ch, plus single scattering albedo wh, opposition surge parameters hh and b0, and macroscopic roughness theta.
LOMMELSEELIGER
This model takes into account the radiance that results from single scattering (scattering of collimated incident light) and does not take into account the radiance that results from multiple scattering (scattering of diffuse light which has made its way indirectly to the same position by being scattered one or more times). This model depends on the incidence and emission angles.
LUNARLAMBERTMCEWEN
This model was developed specifically for use with the Moon, and designed to be used in conjunction with the MoonAlbedo normalization model.
LUNARLAMBERTEMPIRICAL, LUNARLAMBERT, MINNAERTEMPIRICAL, and MINNAERT
These models combine a weighted sum of the LommelSeeliger and Lambert models. Given a suitable value for the LunarLambert function weight, L, these models fit the true reflectance behavior of many planetary surfaces equally well as the Hapke model. These models also depend on the incidence and emission angles.

Type combo
Default FROMPVL
Internal Default FROMPVL
Option List:
Option Brief Description
FROMPVLGet from photomet PVL Get photometric model from the PVL file. Add missing parameters to the PVL file, or enter the values at the command line or use the GUI to enter the values.

Exclusions

  • THETA
  • WH
  • HG1
  • HG2
  • HH
  • B0
  • ZEROB0STANDARD
  • BH
  • CH
  • L
  • K
  • PHASELIST
  • KLIST
  • LLIST
  • PHASECURVELIST
LAMBERT Lambert Photometric Model Simple photometric model which predicts that light incident on a surface is scattered uniformly in all directions.

Exclusions

  • THETA
  • WH
  • HG1
  • HG2
  • HH
  • B0
  • ZEROB0STANDARD
  • BH
  • CH
  • L
  • K
  • PHASELIST
  • KLIST
  • LLIST
  • PHASECURVELIST
HAPKEHEN Hapke-Henyey-Greenstein Photometric Model Derive model albedo using complete Hapke model with Henyey-Greenstein single-particle phase function.

Exclusions

  • BH
  • CH
  • L
  • K
  • PHASELIST
  • KLIST
  • LLIST
  • PHASECURVELIST

Inclusions

  • THETA
  • WH
  • HG1
  • HG2
  • HH
  • B0
  • ZEROB0STANDARD
HAPKELEG Hapke Legendre Polynomial Photometric Model Derive model albedo using complete Hapke model with Henyey Legendre two-term Legendre polynomial phase function.

Exclusions

  • HG1
  • HG2
  • L
  • K
  • PHASELIST
  • KLIST
  • LLIST
  • PHASECURVELIST

Inclusions

  • THETA
  • WH
  • BH
  • CH
  • HH
  • B0
  • ZEROB0STANDARD
LOMMELSEELIGER Lommel-Seeliger Photometric Model This model takes into account the radiance that results from single scattering (scattering of collimated incident light).

Exclusions

  • THETA
  • WH
  • HG1
  • HG2
  • BH
  • CH
  • HH
  • B0
  • ZEROB0STANDARD
  • L
  • K
  • PHASELIST
  • KLIST
  • LLIST
  • PHASECURVELIST
LUNARLAMBERTEMPIRICAL Lunar Lambert Empirical Photometric Model This model combines a weighted sum of the LommelSeeliger and Lambert models.

Exclusions

  • THETA
  • WH
  • HG1
  • HG2
  • BH
  • CH
  • HH
  • B0
  • ZEROB0STANDARD
  • K
  • L
  • KLIST

Inclusions

  • PHASELIST
  • LLIST
  • PHASECURVELIST
LUNARLAMBERTMCEWEN Lunar Lambert-McEwen Photometric Model This model was designed for the Moon to be used in conjunction with the MoonAlbedo normalization model.

Exclusions

  • THETA
  • WH
  • HG1
  • HG2
  • BH
  • CH
  • HH
  • B0
  • ZEROB0STANDARD
  • L
  • K
  • PHASELIST
  • KLIST
  • LLIST
  • PHASECURVELIST
LUNARLAMBERT Lunar Lambert Photometric Model This model combines a weighted sum of the LommelSeeliger and Lambert models.

Exclusions

  • THETA
  • WH
  • HG1
  • HG2
  • BH
  • CH
  • HH
  • B0
  • ZEROB0STANDARD
  • K
  • PHASELIST
  • KLIST
  • LLIST
  • PHASECURVELIST

Inclusions

  • L
MINNAERTEMPIRICAL Minnaert Empirical Photometric Model This model combines a weighted sum of the LommelSeeliger and Lambert models.

Exclusions

  • THETA
  • WH
  • HG1
  • HG2
  • BH
  • CH
  • HH
  • B0
  • ZEROB0STANDARD
  • K
  • L
  • LLIST

Inclusions

  • PHASELIST
  • KLIST
  • PHASECURVELIST
MINNAERT Minnaert Photometric Model This model combines a weighted sum of the LommelSeeliger and Lambert models.

Exclusions

  • THETA
  • WH
  • HG1
  • HG2
  • BH
  • CH
  • HH
  • B0
  • ZEROB0STANDARD
  • L
  • PHASELIST
  • KLIST
  • LLIST
  • PHASECURVELIST

Inclusions

  • K
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Photometric Model: THETA


Description

The "macroscopic roughness" of the surface as it affects the photometric behavior, used for Hapkehen or Hapkeleg. This is the RMS slope at scales larger than the distance photons penetrate the surface but smaller than a pixel. See Hapke (1986). The roughness correction, which is evaluated if theta is given any value other than 0.0, but is extremely slow. See Hapke (1986).

Type string
Default None Specified
Internal Default None Specified
Minimum 0.0 (inclusive)
Maximum 90.0 (inclusive)
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Photometric Model: WH


Description

The Hapke single scattering albedo of surface particles, see Hapke (1981).

Type string
Default None Specified
Internal Default None Specified
Minimum 0.0 (exclusive)
Maximum 1.0 (inclusive)
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Photometric Model: HG1


Description

Asymmetry parameter used in Hapke Henyey Greenstein model for the scattering phase function of single particles in the surface. See Hapke (1981). The two parameter Henyey Greenstein function is:

P(phase)=(1-hg2) * (1-hg1**2)/(1+hg1**2+2*hg1*cos(phase))**1.5 + hg2 * (1-hg1**2)/(1+hg1**2-2*hg1*cos(phase))**1.5

Type string
Default None Specified
Internal Default None Specified
Minimum -1.0 (exclusive)
Maximum 1.0 (exclusive)
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Photometric Model: HG2


Description

The Hapke Henyey Greenstein coefficient for single particle phase function. The second parameter of the two-parameter Henyey-Greenstein model for the scattering phase function of single particles in the surface. This parameter controls the proportions in a linear mixture of ordinary Heneyey Greenstein phase functions with asymmetry parameters equal to +hg1 and -hg1. See HG1 for the full formula.

Type string
Default None Specified
Internal Default None Specified
Minimum 0.0 (inclusive)
Maximum 1.0 (inclusive)
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Photometric Model: BH


Description

The Hapke Legendre coefficient for single particle phase function. A two-term Legendre polynomial is used for the scattering phase function of single particles in the surface:

P(phase) = 1 + bh * p1(cos(phase)) + ch * p2(cos(phase))
Bh is not to be confused with the Legendre coefficient bha of the phase function for atmospheric particles, used when atmname=anisotropic1 or anisotropic2.

Type string
Default None Specified
Internal Default None Specified
Minimum -1.0 (exclusive)
Maximum 1.0 (exclusive)
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Photometric Model: CH


Description

The Hapke Legendre coefficient for single particle phase function. A two-term Legendre polynomial is used for the scattering phase function of single particles in the surface:

P(phase) = 1 + bh * p1(cos(phase)) + ch * p2(cos(phase))

Type string
Default None Specified
Internal Default None Specified
Minimum -1.0 (exclusive)
Maximum 1.0 (exclusive)
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Photometric Model: HH


Description

The Hapke opposition surge component. The width parameter for the opposition effect for the surface if Hapkehen or Hapkeleg is used. See Hapke (1984).

Type string
Default None Specified
Internal Default None Specified
Minimum 0.0 (inclusive)
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Photometric Model: B0


Description

The Hapke opposition surge component. The magnitude of the opposition effect for the surface if Hapkehen or Hapkeleg is used. See Hapke (1984).

Type string
Default None Specified
Internal Default None Specified
Minimum 0.0 (inclusive)
Close Window
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Photometric Model: ZEROB0STANDARD


Description

This specifies if the opposition surge component B0 is set to zero during the standard conditions phase. The program will automatically default to "true" if "ZEROB0STANDARD" is not defined in the PVL FILE when the "READFROMPVL" option is selected, and the user did not choose either "FALSE" or "TRUE" option.

Type string
Default READFROMPVL
Option List:
Option Brief Description
READFROMPVL Get ZEROB0STANDARD value from the FROMPVL file Retrieve and set the ZEROB0STANDARD parameter from the FROMPVL file. If a FROMPVL file is not provided, then an error will occur.
FALSE B0 will not be set to zero for standard conditions phase This option specifies that the opposition surge B0 will not be set to zero during the standard conditions phase.
TRUE B0 will be set to zero for standard conditions phase This option specifies that the opposition surge B0 will be set to zero during the standard conditions phase.
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Photometric Model: L


Description

The Lunar Lambert function weight that governs limb-darkening in the lunar lambert photometric function:

Func=(1-L)*u0 + 2*L*u0/(u0+u)
The values generally fall in the range from 0 (Lambert function) to 1 (Lommel-Seeliger or "lunar" function).

Type string
Default None Specified
Internal Default None Specified
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Photometric Model: K


Description

The Minnaert function exponent that governs limb-darkening in the Minnaert photometric function:

Func=u0**K * u**(K-1)
The values generally fall in the range from 0.5 ("lunar-like", almost no limb darkening) to 1.0 (Lambert function).

Type string
Default None Specified
Internal Default None Specified
Minimum 0.0 (inclusive)
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Photometric Model: PHASELIST


Description

The Minnaert Empirical and Lunar Lambert Empirical function phase angle list entered as a comma delimited string describing how the parameters of the empirical function vary with phase angle. See "$ISIS3DATA/base/templates/photometry/marsred.pvl" for an example.

Type string
Default No List
Internal Default No List
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Photometric Model: KLIST


Description

The Minnaert Empirical function exponent list of limb darkening values entered as a comma delimited string that describes how the parameters of the empirical function vary with phase angle. See "$ISIS3DATA/base/templates/photometry/marsred.pvl" for an example.

Type string
Default No List
Internal Default No List
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Photometric Model: LLIST


Description

The Lunar Lambert Empirical function parameter list of limb darkening values entered as a comma delimited string that describes how the parameters of the empirical function vary with phase angle. See "$ISIS3DATA/base/templates/photometry/marsred.pvl" for an example.

Type string
Default No List
Internal Default No List
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Photometric Model: PHASECURVELIST


Description

The Minnaert Empirical or Lunar Lambert Empirical function phase curve list of brightness values corresponding to a set of phase angles defined in the PHASELIST parameter. See "$ISIS3DATA/base/templates/photometry/marsred.pvl" for an example.

Type string
Default No List
Internal Default No List
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Atmospheric Model: ATMNAME


Description

This is the name of the atmospheric photometric function model to be applied. The models ending with "1" use a first order scattering approximation. Those ending with "2" use a second order scattering approximation, and are slower but more accurate than the first order scattering approximation. The atmospheric correction can be used with only three atmospheric normalization models: albedoatm, shadeatm, and topoatm. See Kirk et al. (2001).

The table below are photometric parameter values for Mars, adopted from Tomasko et al. (1999):

Band Wha Hga
Red 0.95 0.68
Blue 0.76 0.78

Type combo
Default NONE
Internal Default NONE
Option List:
Option Brief Description
NONENo Atmospheric Model No atmospheric correction will be applied.

Exclusions

  • HNORM
  • BHA
  • TAU
  • TAUREF
  • WHA
  • HGA
  • NULNEG
ANISOTROPIC1 Anisotropic 1 atmospheric model Uses Chandrasekhar's solution for anisotropic scattering described by a one-term Legendre polynomial.

Exclusions

  • HGA

Inclusions

  • HNORM
  • BHA
  • TAU
  • TAUREF
  • WHA
ANISOTROPIC2 Anisotropic 2 atmospheric model Uses Chandrasekhar's solution for anisotropic scattering described by a one-term Legendre polynomial.

Exclusions

  • HGA

Inclusions

  • HNORM
  • BHA
  • TAU
  • TAUREF
  • WHA
HAPKEATM1 Hapke 1 Atmospheric Model Provides an approximation for strongly anisotropic scattering that is similar to Hapke's model for a planetary surface. The Chandrasekhar solution for isotropic scattering is used for the multiple scattering terms, and a correction is made to the singly scattered light for anisotropic particle phase function. A one-term Henyey Greenstein function is used.

Exclusions

  • BHA

Inclusions

  • HNORM
  • HGA
  • TAU
  • TAUREF
  • WHA
HAPKEATM2 Hapke 2 atmospheric model Provides an approximation for strongly anisotropic scattering that is similar to Hapke's model for a planetary surface. The Chandrasekhar solution for isotropic scattering is used for the multiple scattering terms, and a correction is made to the singly scattered light for anisotropic particle phase function. A one-term Henyey Greenstein function is used.

Exclusions

  • BHA

Inclusions

  • HNORM
  • HGA
  • TAU
  • TAUREF
  • WHA
ISOTROPIC1 Isotropic 1 atmospheric model Uses Chandrasekhar's solution for isotropic scattering.

Exclusions

  • HGA
  • BHA

Inclusions

  • HNORM
  • TAU
  • TAUREF
  • WHA
ISOTROPIC2 Isotropic 2 atmospheric model Uses Chandrasekhar's solution for isotropic scattering.

Exclusions

  • HGA
  • BHA

Inclusions

  • HNORM
  • TAU
  • TAUREF
  • WHA
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Atmospheric Model: NULNEG


Description

This specifies if negative values after removal of atmospheric effects will be set to NULL. Negative values are only generated in modes that include atmospheric correction and occur when the optical depth "tau" is overestimated, so that the atmospheric radiance subtracted from the image is brighter than the darkest observed pixels. In this case "tau" should be decreased until no negative values are present in the output file.

Type string
Default READFROMPVL
Option List:
Option Brief Description
READFROMPVL Get NULNEG value from the FROMPVL file Retrieve and set the NULNEG parameter from the FROMPVL file. An error is reported if a PVL file is not provided.
NO Do not set negative values to NULL This option specifies not to set negative values to NULL after the removal of atmospheric effects.
YES Negative values will be set to NULL This option specifies to set negative values to NULL after the removal of atmospheric effects.
Close Window
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Atmospheric Model: TAU


Description

The normal optical depth of the atmosphere.

Type string
Default None Specified
Internal Default None Specified
Minimum 0.0 (inclusive)
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Atmospheric Model: TAUREF


Description

The reference value of tau to which the image will be normalized. This would normally be 0.0 unless one is interested in simulating a hazy atmosphere scene.

Type string
Default None Specified
Internal Default None Specified
Minimum 0.0 (inclusive)
Close Window
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Atmospheric Model: HGA


Description

The coefficient of single particle Henyey Greenstein phase function. Henyey-Greenestein asymmetry parameter for atmospheric particle phase function, used in hapkeatm1 and hapkeatm2 atmospheric models. Not to be confused with corresponding parameter hg1 for the surface particles.

Type string
Default None Specified
Internal Default None Specified
Minimum -1.0 (exclusive)
Maximum 1.0 (exclusive)
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Atmospheric Model: WHA


Description

The single scattering albedo of atmospheric particles.

Type string
Default None Specified
Internal Default None Specified
Minimum 0.0 (exclusive)
Maximum 1.0 (inclusive)
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Atmospheric Model: BHA


Description

The coefficient of the single particle Legendre phase function. Coefficient of p1 (cosine) term of atmospheric particle phase function, used in anisotropic1 and anisotropic2 atmospheric models. Not to be confused with corresponding coefficient bh for the surface particles.

Type string
Default None Specified
Internal Default None Specified
Minimum -1.0 (inclusive)
Maximum 1.0 (inclusive)
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Atmospheric Model: HNORM


Description

The atmospheric shell thickness normalized to the planet radius, used to modify angles to get more accurate path lengths near the terminator (Ratio of scale height to the planetary radius). For Mars MDIM2.1 mosaic "0.003" was defined, which is the only planet for which the atmospheric modes are currently used.

Type string
Default None Specified
Internal Default None Specified
Minimum 0.0 (inclusive)
Close Window
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Normalization Model: NORMNAME


Description

This is the name of the normalization model to be performed

FROMPVL
Get normalization model from the PVL file. If the parameter names and values are missing in the PVL file, then either add them to the PVL file, or enter the values at the command line, or use the GUI to enter the parameter values.
ALBEDOATM
Normalization with atmosphere. For each pixel, a model of atmospheric scattering is subtracted and a surface model is divided out, both evaluated at the actual geometry of the pixel. Then, the resulting value is multiplied by the surface function at the reference conditions and the atmospheric model at reference conditions is added. In normal usage, the reference condition has normal incidence (incref=0) and no atmosphere (tauref=0), but in some cases it may be desirable to normalize images to a different incidence angle or a finite optical depth to obtain a more uniform appearance. As with the albedo model, if topographic shading is present, it will be amplified more at high incidence angles and will not appear uniform.
ALBEDO
Normalization without atmosphere. Each pixel is divided by the model photometric function evaluated at the geometry of that pixel, then multiplied by the function at reference geometry with incidence and phase angles equal to incref and emission angle at 0 degree. This has the effect of removing brightness variations due to incidence angle and showing relative albedo variations with the same contrast everywhere. If topographic shading is present, it will be amplified more in regions of low incidence angle and will not appear uniform.
MIXED
Normalization without atmosphere. This option is used to perform albedo normalization over most of the planet, but near the terminator it will normalize the topographic contrast to avoid the seams that can occur with the usual albedo normalization. The two effects will be joined seamlessly at the incidence angle set for incmat. Incmat must be adjusted to give the best equalization of contrast at all incidence angles. The albedo parameter must also be adjusted so the topographically normalized regions at high incidence angle are set to an albedo compatible with the albedo-normalized data at lower incidence.
MOONALBEDO
Normalization without atmosphere specifically designed to work with lunar data using the LunarLambertMcEwen photometric function model. A photometric correction plus an albedo-dependent phase angle correction which varies with the value of each input DN will be applied. The final output value is the reflectance at incidence and phase angles of 30 degrees, and emission angle of 0 degrees.

The following are ISIS2 default values used in the past, but may be obsolete:
  • D = 0.14
  • E = -0.3575 * wavelength(WL) - 0.0607 if WL is less than 1.0: otherwise -0.4179
  • F = 0.55
  • G2 = -0.9585 * WL + 0.98 if WL is less than 1.0: otherwise 0.02
  • Xmul = 1.0
  • WL = get WL from labels
  • H = 0.048
  • BSH1 = 19.89 - 59.58 * WL + 59.86 * WL**2 - 20.09 * WL**3
  • XB1 = -0.0817
  • XB2 = 0.0081
SHADEATM
Normalization with atmosphere. The surface photometric function is used to simulate an image by relief shading, just like the shade model, but the effects of atmospheric scattering are also included in the calculation.
SHADE
Normalization without atmosphere. The surface photometric function is evaluated at the geometry of the image in order to calculate a shaded relief image of the ellipsoid or DEM. The radiance of the model surface is set to albedo at incidence angle defined by incref and zero phase. The image data are not used.
TOPOATM
Normalization with atmosphere. As with the topo model, this option is used in the final step of a three-step process: (1) normalize with the albedoatm model, incref=0, and tauref=0 to temporarily remove atmosphere and normalize albedo variations; (2) use divide filter to remove albedo variations and emphasize features; and (3) normalize with the topoatm model to undo the temporary normalization and equalize topographic shading.
TOPO
Normalization without atmosphere. This option is used to normalize the topographic shading to uniform contrast regardless of the incidence angle, and exagerates the albedo variations at large incidence angles. So, this model is used as part of a three-step process in which (1) the image is temporarily normalized for albedo; (2) a divide filter is applied to remove regional albedo variations and emphasize features; and (3) the image is renormalized with the topographic mode to reverse the first normalization and equalize topographic shading. The reference state in the first step must have incref=0 because this is what is reversed in the final step. If there are no significant albedo variations, step (2) can be skipped but step (1) must not be skipped.

Type combo
Default FROMPVL
Internal Default FROMPVL
Option List:
Option Brief Description
FROMPVLGet model from PVL file Get the normalization model from the PVL file. Add missing parameters to the PVL file, or enter the values at the command line, or use the GUI to enter the values.

Exclusions

  • INCREF
  • INCMAT
  • THRESH
  • ALBEDO
  • ATMNAME
  • D
  • E
  • F
  • G2
  • XMUL
  • WL
  • H
  • BSH1
  • XB1
  • XB2
  • HNORM
  • TAU
  • WHA
  • NULNEG
  • TAUREF
  • HGA
  • BHA
ALBEDOATM Albedo normalization model with atmosphere Albedo normalization with atmosphere. In normal usage, the reference condition has normal incidence (incref=0) and no atmosphere (tauref=0), but in some cases it may be desirable to normalize images to a different incidence angle or a finite optical depth to obtain a more uniform appearance.

Exclusions

  • INCMAT
  • THRESH
  • ALBEDO
  • D
  • E
  • F
  • G2
  • XMUL
  • WL
  • H
  • BSH1
  • XB1
  • XB2

Inclusions

  • ATMNAME
  • INCREF
ALBEDO Albedo normalization model Albedo normalization without atmosphere. This has the effect of removing brightness variations due to incidence angle and showing relative albedo variations with the same contrast everywhere.

Exclusions

  • ATMNAME
  • D
  • E
  • F
  • G2
  • XMUL
  • WL
  • H
  • BSH1
  • XB1
  • XB2
  • HNORM
  • TAU
  • WHA
  • NULNEG
  • TAUREF
  • HGA
  • BHA

Inclusions

  • INCREF
  • THRESH
  • ALBEDO
MIXED Mixed normalization model Mixed normalization without atmosphere. Used for albedo normalization over most of the planet, but near the terminator it will normalize topographic contrast so the two effects will be joined seamlessly at incidence angle defined for the incmat parameter.

Exclusions

  • ATMNAME
  • D
  • E
  • F
  • G2
  • XMUL
  • WL
  • H
  • BSH1
  • XB1
  • XB2
  • HNORM
  • TAU
  • WHA
  • NULNEG
  • TAUREF
  • HGA
  • BHA

Inclusions

  • INCREF
  • INCMAT
  • THRESH
  • ALBEDO
MOONALBEDO Moon albedo normalization model This model was designed specifically for use on lunar data without atmosphere. It will compute normalized albedo for the Moon, normalized to 0 degrees emission angle and 30 degrees illumination and phase angles.

Exclusions

  • ATMNAME
  • INCREF
  • INCMAT
  • THRESH
  • ALBEDO
  • HNORM
  • TAU
  • WHA
  • NULNEG
  • TAUREF
  • HGA
  • BHA

Inclusions

  • D
  • E
  • F
  • G2
  • XMUL
  • WL
  • H
  • BSH1
  • XB1
  • XB2
SHADEATM Shade normalization with atmosphere The surface photometric function is used to simulate an image by relief shading, just like the shade model, but the effects of atmospheric scattering are also included in the calculation.

Exclusions

  • INCMAT
  • THRESH
  • D
  • E
  • F
  • G2
  • XMUL
  • WL
  • H
  • BSH1
  • XB1
  • XB2

Inclusions

  • ATMNAME
  • INCREF
  • ALBEDO
SHADE Shade normalization model Normalization without atmosphere. The surface photometric function is evaluated at the geometry of the image in order to calculate a shaded relief image of the ellipsoid or DEM. The radiance of the model surface is set to albedo at incidence angle defined for incref and zero phase. The image data is not used.

Exclusions

  • ATMNAME
  • INCMAT
  • THRESH
  • D
  • E
  • F
  • G2
  • XMUL
  • WL
  • H
  • BSH1
  • XB1
  • XB2
  • HNORM
  • TAU
  • WHA
  • NULNEG
  • TAUREF
  • HGA
  • BHA

Inclusions

  • INCREF
  • ALBEDO
TOPOATM Topographic normalization with atmosphere Normalization with atmosphere. As with the topo atmospheric model, this option is used in the final step of a three-step process.

Exclusions

  • INCMAT
  • THRESH
  • D
  • E
  • F
  • G2
  • XMUL
  • WL
  • H
  • BSH1
  • XB1
  • XB2

Inclusions

  • ATMNAME
  • INCREF
  • ALBEDO
TOPO Topographic normalization model Normalization without atmosphere. Used to normalize topographic shading to uniform contrast regardless of the incidence angle. Such a normalization would exagerate albedo variations at large incidence angles, so this model is used as part of a three-step process.

Exclusions

  • ATMNAME
  • INCMAT
  • D
  • E
  • F
  • G2
  • XMUL
  • WL
  • H
  • BSH1
  • XB1
  • XB2
  • HNORM
  • TAU
  • WHA
  • NULNEG
  • TAUREF
  • HGA
  • BHA

Inclusions

  • INCREF
  • THRESH
  • ALBEDO
Close Window
X

Normalization Model: INCREF


Description

This is the reference incidence angle to which the image will be normalized. Most normalization modes attempt to normalize the appearance of the surface to a set of standard conditions, in particular, a fixed incidence angle given by the incref parameter. In most cases, a value of 0 degrees is used for albedo and albedoatm normalization modes, though 30 degrees is sometimes used. Incref of 0 degrees is also the usual choice for specifying the albedo of shaded relief images calculated with shade and shadeatm normalization modes. Incref of 30 degrees is the standard value for topographic normalization modes topo and topoatm because topographic shading disappears at 0 degree incidence angle and cannot be normalized to this value.

Type string
Default None Specified
Internal Default None Specified
Minimum 0.0 (inclusive)
Maximum 90.0 (exclusive)
Close Window
X

Normalization Model: INCMAT


Description

This specifies the incidence angle where albedo normalization transitions to topographic normalization. When mixed normalization mode is selected, the image will be normalized so that albedo variation is constant for small incidence angles and topographic shading is constant for large incidence angles. This parameter must be set by trial and error to achieve the best appearance, because it depends on the relative amount of albedo variations and shading for any given planet or satellite. The value of the albedo parameter must also be adjusted for this mode to match the mean brightness of the high incidence angle region to that of the data at lower incidence angles.

Type string
Default None Specified
Internal Default None Specified
Minimum 0.0 (inclusive)
Maximum 90.0 (exclusive)
Close Window
X

Normalization Model: THRESH


Description

This sets upper limit on the amount of amplification in regions of small incidence angle. Operating modes that involve topographic normalization topo, topoatm, and mixed options will amplify variations in the input image in regions of small incidence angle where the shading in the input image is weak. Thresh is an upper limit on the amount of amplification that will be attempted. If it is set too low, low-incidence areas of the image may appear bland, but if thresh is set too high these regions may contain amplified noise rather than useful shading information.

Type string
Default None Specified
Internal Default None Specified
Close Window
X

Normalization Model: ALBEDO


Description

The albedo to which the image will be normalized. The value of the desired model albedo, used with shade, topo, mixed, shadeatm, and topoatm. This is the albedo (I/F value at incidence angle defined for incref and zero phase) used to simulate a shaded relief image when shade or shadeatm normalization models are used. For the other modes, it is the albedo that the image will be normalized to have. The program stats can be run to get the average albedo of an input image, but for constructing mosaics the same value of albedo should be used for all images in order to achieve a uniform result.

Type string
Default None Specified
Internal Default None Specified
Close Window
X

Normalization Model: D


Description

This is the empirically derived coefficient for the albedo dependent phase function normalization parameter.

Type string
Default None Specified
Internal Default None Specified
Close Window
X

Normalization Model: E


Description

This is the empirically derived coefficient for the albedo dependent phase function normalization parameter.

Type string
Default None Specified
Internal Default None Specified
Close Window
X

Normalization Model: F


Description

This is the empirically derived coefficient for the albedo dependent phase function normalization parameter.

Type string
Default None Specified
Internal Default None Specified
Close Window
X

Normalization Model: G2


Description

This is the empirically derived coefficient for the albedo dependent phase function normalization parameter.

Type string
Default None Specified
Internal Default None Specified
Close Window
X

Normalization Model: H


Description

This is the empirically derived coefficient for the albedo dependent phase function normalization parameter.

Type string
Default None Specified
Internal Default None Specified
Close Window
X

Normalization Model: XMUL


Description

This is used to convert radiance to reflectance, or apply a calibration fudge factor.

Type string
Default None Specified
Internal Default None Specified
Close Window
X

Normalization Model: WL


Description

The wavelength in micrometers of the image being normalized.

Type string
Default None Specified
Internal Default None Specified
Close Window
X

Normalization Model: BSH1


Description

This is the empirically derived coefficient for the albedo dependent phase function normalization parameter.

Type string
Default None Specified
Internal Default None Specified
Close Window
X

Normalization Model: XB1


Description

This is the empirically derived coefficient for the albedo dependent phase function normalization parameter.

Type string
Default None Specified
Internal Default None Specified
Close Window
X

Normalization Model: XB2


Description

This is the empirically derived coefficient for the albedo dependent phase function normalization parameter.

Type string
Default None Specified
Internal Default None Specified
Close Window

Example 1

Photometric correction with any valid photometric angles

Description

This example shows the photometric correction of a cube file using the hapkehen (Hapkehen) photometric model and the albedo normalization model without trimming the image data based on incidence or emission angle.

Command Line

photomet from=EW0131773041G_cal.cub to=EW0131773041G_cal_hapkehen_albedo.cub frompvl=photomG.pvl phtname=hapkehen theta=9 wh=0.218651 hg1=0.178965 hg2=0.971493 hh=0.085 b0=2.7 normname=albedo incref=0 thresh=1e+31 albedo=1.0
Run photomet with default maximum angles

GUI Screenshot

photomet GUI

Example GUI

Screenshot of GUI version of the application. The default value for the MAXEMISSION and MAXINCIDENCE parameters is 90.0. The parameter values were loaded into the appropriate parameter names using the drop-down menu for the "FROMPVL" parameter name.

Input Image

Input image

Input file

Parameter Name: FROM

Screenshot of the input image before the photometric correction has been performed.

Data File

Links open in a new window.
Example of a PVL file The PVL file contains the photometric parameters to be applied to the input cube file. Load the PVL file parameters using the photomet GUI drop-down menu and add the additional required parameter value for "ALBEDO."

Output Image

Output image

Output file

Parameter Name: TO

Screenshot of the output image after the photometric correction. Notice the features have consistent tones except near the limb where the pixels are brighter because it is over-corrected. A histogram stretch is applied automatically when the image is displayed, so the image appears darker due to the higher DN values at the terminator.


Example 2

Photometric correction with mixed normalization option

Description

This example shows the photometric correction of a cube file by using the hapkehen (Hapkehen) photometric model and mixed normalization model that performs an albedo normalization for most of the planet, and transitions to a topographic normalization at 75 degrees. Adjust the INCMAT parameter value to get the best equalization of contrast at all incidence angles.

Command Line

photomet 0131773041G_cal.cub to=EW0131773041G_cal_hapkehen_mixed.cub frompvl=photomG.pvl phtname=hapkehen theta=9 wh=0.218651 hg1=0.178965 hg2=0.971493 hh=0.085 b0=2.7 normname=mixed incref=0 incmat=75 thresh=30.0 albedo=0.0
Run photomet with hapkehen photometric model and mixed normalization model.

GUI Screenshot

photomet GUI

Example GUI

Screenshot of GUI version of the application. The default value for MAXEMISSION and MAXINCIDENCE parameters is 90.0, but the INCMAT parameter is set to 75 degrees.

Input Image

Input image

Input file

Parameter Name: FROM

Screenshot of the input image before the photometric correction has been performed.

Data File

Links open in a new window.
Example of the PVL file The PVL file containing the photometric parameters to be applied to the input cube. Load the PVL file parameters using the photomet GUI and add additional required parameter values for "INCMAT" and "ALBEDO."

Output Image

Output image

Output file

Parameter Name: TO

Screenshot of the output image after the photometric correction. Notice the limb area was over-corrected in the previous example, but now shows more consistent tones in the output image.


Example 3

Photometric correction with mixed normalization and trim options

Description

This example shows the photometric correction of a cube file using the hapkehen (Hapkehen) photometric model and a mixed normalization model that performs an albedo normalization for most of the planet, but will also trim the image data beyond 75.0 degrees incidence angle. This is to show where the transition between the two types of normalization occurred in the previous example.

Command Line

photomet from=EW0131773041G_cal.cub to=EW0131773041G_cal_hapkehen_mixed_trim_at75.cub frompvl=photomG.pvl maxincidence=75 phtname=hapkehen theta=9 wh=0.218651 hg1=0.178965 hg2=0.971493 hh=0.085 b0=2.7 normname=mixed incref=0 incmat=75 thresh=30.0 albedo=0.0
Run photomet with hapkehen photometric model and mixed normalization model, and trim at 75.0 degree incidence angle.

GUI Screenshot

photomet GUI settings

Example GUI

Screenshot of GUI version of the application. The MAXEMISSION is set to 90.0; the MAXINCIDENCE and INCMAT parameters are set to 75.0 degrees.

Input Image

Input image

Input file

Parameter Name: FROM

Screenshot of the input image before the photometric correction has been performed.

Data File

Links open in a new window.
Example of the PVL file The PVL file containing the photometric parameters to be applied to the input cube file. Load the PVL file parameters using the photomet GUI and add additional required parameter values for "INCMAT" and "ALBEDO."

Output Image

Output image

Output file

Parameter Name: TO

Screenshot of the output image after the photometric correction. Notice the limb area, where it was over-corrected in the first example, has been trimmed.


Example 4

Photometric correction using maximum emission and incidence angle parameters

Description

This example shows the photometric correction of a cube file by setting the maximum emission angle to 75.0 degrees and the maximum incidence angle to 85.0 degrees. The photometric model and normalization model along with the parameter values are defined in the input PVL file. This example uses a PVL file that follows the format for a previous ISIS3 release. The photomet program will recognize some older formats and parameter names, but if an error is returned, then update the settings using the latest parameter names and/or options listed in the tables under "DESCRIPTION."

Command Line

photomet from=input.cub frompvl=input.pvl to=output.cub maxemission=75.0 maxincidence=85.0
Run photomet with maximum emission and incidence angles less than the default value of 90 degrees.

GUI Screenshot

photomet GUI

Example GUI

Screenshot of GUI version of the application. Notice the MAXEMISSION and MAXINCIDENCE parameters are changed from the default value of 90.0.

Input Image

Input image

Input file

Parameter Name: FROM

Screenshot of the input image before the photometric correction has been performed.

Data File

Links open in a new window.
Input PVL file The PVL file contains the input photometric parameters for the input file.

Output Image

Output image

Output file

Parameter Name: TO

Screenshot of the output image after the photometric correction. Notice the output image has been trimmed based on the photometric angles defined by the user.


Example 5

Photometric correction using maximum emission and incidence angle parameters as well as anglesource and usedem parameters.

Description

This example shows the photometric correction of a cube file by setting the maximum emission angle to 75.0 degrees and the maximum incidence angle to 85.0 degrees. The photometric model being used is MINNAERT and the normilization model is ALBEDO. The usedem parameter is describing how to trim the image. In this case the trimming is being done using the radius obtained from the DEM. The anglesource parameter describes how to calculate the photometric angles. In this example the calculation is also being done using the DEM.

Command Line

photomet photomet from=uncropped.cub to=TrimmedTestAngleSourceDemUsedemFalse.cub maxemission=87.0 anglesource=dem phtname=minnaert k=0.5 normname=albedo incref=0 incmat=80 thresh=30 albedo=1.0
Run photomet with maximum incidence at 90 degrees and maximum emission less than 90 degrees. Photometric model is MINNAERT and normilization model is ALBEDO. Usedem is false and anglesource is set to DEM.

GUI Screenshot

photomet GUI

Example GUI

Screenshot of GUI version of the application. Notice the MAXEMISSION has changed from the default value of 90.0, usedem is set to it's default, and anglesource is set to DEM.

Input Image

Input image

Input file

Parameter Name: FROM

Screenshot of the input image before the photometric correction has been performed.

Output Image

Output image

Output file

Parameter Name: TO

Screenshot of the output image after the photometric correction. Notice the output image has been trimmed based on the photometric angles defined by the user.


Example 6

Photometric corrections using a three-step approach for MDIM2.1 of Mars

Description

A multistep process is used to apply photometric correction to Mars images:
  1. Photomet is run in albedo mode, which decreases brightness variations across the individual image and removes the additive atmospheric contribution, if any;
  2. The output image from step 1 is divided by a low-pass-filtered version of itself, which removes albedo variations if they have broader spatial scales than topographic shading as is often the case; and
  3. Photomet is run again on the output image of step 2 in topography mode, which undoes the albedo normalization of the first pass and then applies the topographic normalization.
The final result would need to be equalized and mosaicked together.

Data File

Links open in a new window.
Sample script This script contains the three-step processing sequence of programs that need to be executed for the three test images.

Output Image

Input and output images

Collage of images

The images shown are subareas at 1:1 scale to emphasize the result of the photometric correction at each stage. There are four rows in the image collage containing the following:

  • Row 1 - Calibrated images without photometric correction
  • Row 2 - Applied Hapkehen photometric model, albedoatm normalization model and an hapkeatm2 atmospheric model
  • Row 3 - Applied a divide filter
  • Row 4 - Applied Hapkehen photometric model, topoatm normalization model and an hapkeatm2 atmospheric model