This program calibrates images from the Messenger mission's MDIS instrument. The input image is corrected for the following, in order, during calibration:

• Step 1: Dark current correction
• Step 2: Linearity correction
• Step 3: Readout smear correction
• Step 4: Uniformity (flat field) correction
• Step 5: Absolute coefficient correction
• Step 6: Conversion to I over F
• Step 7: Empirical correction

Step 1: Dark current correction:

Option	Description
None	No dark current correction is performed.
Standard	Messenger images have a strip of dark current data on the left-hand side. This will take a median of the first three sample columns (for unbinned data) and use it for the dark current on a line by line basis.
Linear	This will fit a line across the first column of data, which is dark current data, and use the line to determine the dark current correction.
Model	There are independent dark models, developed on-ground. This will use the most recent of these models to correct the dark current.

There are times when the user selections for dark current correction will be rejected and altered by the program. In these cases a warning message will be printed to alert the user to the change. Below is an explanation of what happens in some special cases:

DARKCURRENT parameter value	Valid dark pixels exist**	Exposure duration exceeds 1 second	Outcome
STANDARD	No	No	Dark current correction method is changed to MODEL. The program prints a warning message.
STANDARD	No	Yes	Dark current correction is turned off, but the rest of the calibration is performed. The program prints a warning message.
STANDARD	Yes	Yes or No	Dark current correction is performed with the original user input MODEL option. No warning message is needed.
LINEAR	No	No	Dark current correction method is changed to MODEL. The program prints a warning message.
LINEAR	No	Yes	Dark current correction is turned off, but the rest of the calibration is performed. The program prints a warning message.
LINEAR	Yes	Yes or No	Dark current correction is performed with the original user input MODEL option. No warning message is needed.
MODEL	Yes or No	No	Dark current correction is performed with the original user input MODEL option. No warning message is needed.
MODEL	No	Yes	Dark current correction is turned off, but the rest of the calibration is performed. The program prints a warning message.
MODEL	Yes	Yes	Dark current correction method is changed to STANDARD. The program prints a warning message.

** Note, there are two binning mode codes in the Instrument group of the input cube's labels, the FpuBinningMode and the PixelBinningMode. The number of valid dark pixels referred to in the table above is determined by using these values. If the sum of these two binning modes is greater than one, then there are no valid dark pixels.

Step 2: Linearity correction:

Linearity measures the variability of a camera's DN level per unit exposure time and radiance, as a function of variation in exposure time or radiance. Using dark-corrected, desmeared DN values (DCDSI) taken from the center quarter of the images, response linearity was measured with both the NAC and WAC binned and not-binned.

Step 3: Smear correction:

Frame transfer smear corrections for MDIS follow the technique described for NEAR MSI image by Murchie et al. (1999). In brief, an image is exposed for a nominal integration time and is then transferred in 3.84 ms to a memory zone on the CCD, from which the analog signal is digitized line-by-line. Accumulation of signal continues during the finite duration of frame transfer, inducing a streak or frame-transfer smear in the wake of an illuminated object in the field of view, parallel to the direction of frame transfer. Note that the frame transfer occurs in the calibration pixels as well as on the imaging pixels. mdiscal accounts for the frame transfer smear contributed from the 16 calibration lines (removed from the PDS-archived images).

Step 4: Uniformity (flat field) correction:

Response uniformity, or flat field, is a measure of pixel-to-pixel variations in responsivity. Measurements of response uniformity of the WAC and NAC were conducted in the OCF, at room temperature and while cold, by imaging the integrating sphere with the two 45W bulbs illuminating the interior.

Step 5: Absolute coefficient correction:

This converts the DN values from responsivity to radiance values.

Step 6: Convert units to I over F:

This converts the DN values radiance values to I over F.

Step 7: Empirical correction:

Performs an empirical correction on the DN values by scaling them using the EmpiricalCorrectionFactor. Note this correction is only applied to WAC images.

Output units

The output units of the DNs will depend on which calibration flags are turned on.

• If IOF=TRUE, output units are measured in I/F
• Otherwise if RADIOMETRIC=TRUE, output units are measured in W/(m**2 micrometer sr)
• If RADIOMETRIC=FALSE, output units are DNs

General calibration limitations

This program will throw an error and exit in the following circumstances:

• The input cube is multiband.
• The input cube has less than 2 samples per line.
• The input cube is not unlutted.
• PixelBinningMode > 0 and unable to reduce.

MESSENGER MDIS calibration document excerpt

The following is an excerpt from the MESSENGER MDIS calibration document on this process

        USAGE
        =====

        Raw units are of DN converted to the physical units
        of radiance or I/F, following the calibration equation:

        L(x,y,f,T,t,b) = Lin[DN(x,y,f,T,t,b,MET) - Dk(x,y,T,t,b,MET) - 
        Sm(x,y,t,b)] / {Flat(x,y,f,b) * t * [Resp(f,b,T)/Correct(f,MET)]}

        where:

        L(x,y,f,T,t,b) is radiance in units of W / (m**-2 microns**-1 sr**-1),
        measured by the pixel in column x, row y, through filter f, at CCD
        temperature T and exposure time t, for binning mode b,

        DN(x,y,f,T,t,b,MET) is the raw DN measured by the pixel in column x, row
        y, through filter f, at CCD temperature T and exposure time t, for binning
        mode b, and Mission Elapsed Time (MET),

        Dk(x,y,T,t,b,MET) is the dark level in a given pixel, derived from
        a model based on exposure time and CCD temperature,

        Sm(x,y,t,b) is the scene-dependent frame transfer smear for the pixel,

        Lin is a function that corrects small nonlinearity of detector response,

        Flat(x,y,f,b) is the non-uniformity or 'flat-field' correction,

        Resp(f,b,T) is the responsivity, relating dark-, flat-, and
        smear-corrected DN per unit exposure time to radiance,

        Correct(f,MET) is a time-variable correction to responsivity
        describing a sudden decrease in transmission of the WAC optics
        on 24 May 2011 and subsequent recovery to normal values, 
        interpreted as due to contamination associated with MESSENGER's
        first periapse season over Mercury's hot pole and the subsequent
        bake-off of the contaminant, 

        and

        t is the exposure time.

        The above equation assumes that data are in the native 12-bit format in
        which they were read off the CCD, and that onboard application of 12-to-8
        bit lookup tables (LUTs) has been inverted.

        This correction is done step-wise using the calibration tables and
        images in this directory as follows.


        (1) Inversion of 12 to 8 bit Compression
        ========================================

        8-to-12 bit inversion of DN values is required when the value of
        MESS:COMP12_8 is 1 (when the data are 8-bit). There are 8 inverse lookup
        tables (LUTs). The table to use is indicated by the value of MESS:COMP_ALG
        from 0 through 7. An 8-bit value (in a row of the table) is inverted by
        replacing it with the 12-bit value in the column corresponding to a
        particular LUT.

        The inversion tables are given in the product MDISLUTINV_0.


        (2) Subtraction of modeled dark level
        =====================================

        Two methods are used for subtraction of the dark level, one for 
        exposure times greater than 1 sec and one for exposure times less than 1 sec.

        In the method for exposure times less than 1 sec, the DN values are valid
        columns in the masked 'dark strip' at the edge of the CCD are fitted
        linearly as a function of line in the image. Then the fits are subtracted
        from the pixels in each line of the CCD.

        In the method for exposure times greater than 1 sec, a model is used which accounts
        for variations in column (sample) in the image, which the previous 
        method cannot do. However if the model were applied to longer exposures,
        it would yield larger residuals than the previous method.

        There are four separate models of dark level (dark current plus
        electronics bias), for the MDIS-WAC and MDIS-NAC (as indicated by the
        keyword INSTRUMENT_ID), and for each camera, without pixel binning turned
        on (MESS:FPU_BIN = 0) or with pixel binning turned on (MESS:FPU_BIN = 1).
        The models estimates the dark level Dk(x,y,t,T) as a function of column
        position x, row position y, exposure time t in milliseconds (as indicated 
        by the keyword MESS:EXPOSURE or EXPOSURE_DURATION), and CCD temperature T 
        (as indicated by the keyword MESS:CCD_TEMP):

        Dk(x,y,t,T) = C(T) + D(T) + [E(T) + F(T) * t] * y + {O(T) + P(T) * t +
         [Q(T) + S(T) * t] * y} * x

        Variables C(T), D(T), E(T), F(T), O(T), P(T), Q(T), and S(T) are all
        third-order functions of CCD temperature, for example:

        C(T) = H0 + H1 * T + H2 * T**2 + H3 * T**3

        In all cases x or y is in the range 0-1023 for a not-binned image (as
        indicated by the keyword MESS:FPU_BIN = 0) or 0-511 for a binned image (as
        indicated by the keyword MESS:FPU_BIN = 1). t is in units of milliseconds,
        and T is in UNCALIBRATED raw counts of CCD temperature.

        For each pixel in column x and row y of an image, application of the
        correction is:

        DN_dark(x,y,t,T) = DN(x,y,t,T) - Dk(x,y,t,T)

        where

        DN(x,y,t,T) is DN in 12-bit format,

        Dk(x,y,t,T) is the predicted DN level from the dark modeldark model, and

        DN_dark(x,y,t,T) is dark-corrected DN.

        The eight sets of coefficients for the WAC not-binned, WAC binned, NAC
        not-binned, and NAC binned dark models are given in the products
        MDISWAC_NOTBIN_DARKMODEL_0, MDISWAC_BINNED_DARKMODEL_0,
        MDISNAC_NOTBIN_DARKMODEL_0, and MDISNAC_BINNED_DARKMODEL_0 respectively.

        (3) Frame Transfer Smear Correction
        ===================================

        Accumulation of signal continues during the finite duration
        of frame transfer induces a streak or frame-transfer smear in the wake
        of an illuminated object in the field of view, parallel to the direction
        of frame transfer. This smear is approximated as:

        Sm(x,y,t,b,f) = SUMM(1,y-1) { t2/t * [DN_dark(x,y,t,b) -
        Sm(x,y,t,b,f)] / Flat(x,y,b,f)}

        where

        Sm(x,y,t,b,f) is the smear in column x and row y at exposure time t
        in binning mode b and filter f,

        Dk_dark (x,y,t,b) is dark-corrected DN in column x and row y at
        exposure time t and temperature T in binning mode b,

        Flat(x,y,b,f) is the flat-field correction in column x and row y in
        binning mode b and filter f,

        t is exposure time in milliseconds, and

        t2 is the time for frame transfer (about 3.4 ms) divided by the number of
        lines in the image in the direction of frame transfer, 1024 for
        full-frame images (when MESS:FPU_BIN = 0) or 512 for binned images (when
        MESS:FPU_BIN = 1).

        For each pixel in column x and row y of an image, application of the
        correction is :

        DN_dark_smear(x,y,t,b,f) = DN_dark(x,y,t,b,f) - Sm(x,y,t,b,f)

        where

        DN_dark_smear(x,y,t,b,f) is dark- and smear- corrected DN,

        DN_dark(x,y,t,b,f) is dark-corrected DN, and

        Sm(x,y,t,b,f) is the smear calculated as shown above.


        (4) Correction for CCD non-linearity
        ====================================

        To remove effects of nonlinearity in WAC image data, the following
        corrections should be applied after correction of dark current, bias,
        and smear.

        For DN_dark_smear > 1
        DN_lin = DN_dark_smear/[0.008760 * Ln(DN_dark_smear) + 0.936321]

        For DN_dark_smear less than or equal to 1
        DN_lin = DN_dark_smear/0.936321

        To remove effects of nonlinearity in NAC image data, the following
        procedure should be applied after correction of dark current, bias,
        and smear.

        For DN_dark_smear > 1
        DN_lin = DN_dark_smear/[0.011844 * Ln(DN_dark_smear) + 0.912031]

        For DN_dark_smear less than or equal to 1
        DN_lin = DN_dark_smear/0.912031

        where

        DN_dark_smear is the input dark- and smear-corrected DN, and

        DN_lin is linearized dark- and smear-corrected DN.


        (5) Flat-field correction
        =========================

        The flat field correction removes pixel to pixel differences in detector
        responsivity, so that the responsivity coefficients can be expressed as
        scalars for each filter. There is a separate flat-field image for MDIS-WAC
        and MDIS-NAC (as indicated by the keyword INSTRUMENT_ID), without pixel
        binning turned on (MESS:FPU_BIN = 0) or with pixel binning turned on
        (MESS:FPU_BIN = 1), for each separate filter (as indicated by the keyword
        FILTER_NUMBER). All of the files are in the 'FLAT' directory.

        For each pixel in column x and row y of an image, application of the
        correction is

        DN_flat(x,y,f,b) = DN_lin(x,y,f,b) / Flat(x,y,f,b)

        where

        DN_flat(x,y,f,b) is flat-fielded, linearized, dark- and smear-corrected
        DN,

        DN_lin(x,y,f,b) is linearized dark- and smear-corrected DN, and

        Flat(x,y,f,b) is the value in the appropriate flat-field image.


        (6) Conversion from DNs to radiance
        ===================================

        The value that relates corrected DN's measured per unit time to radiance
        is the responsivity. Responsivity is modeled as a function of which camera
        is being used (MDIS-WAC or MDIS-NAC as indicated by the keyword
        INSTRUMENT_ID), its binning state (as indicated by the keyword
        MESS:FPU_BIN), and in the case of the WAC the filter number (as indicated
        by the keyword FILTER_NUMBER). The coefficients used to calculate the
        responsivity are in the 'RESPONSIVITY' directory. For a camera, binning
        state, and filter, the responsivity is calculated from uncalibrated CCD
        temperature (as indicated by the keyword MESS:CCD_TEMP) as follows:

        Resp(f,T,b) = R(f,t=-30.3C,b) * [correction_offset(f,b) + T(CCD) * 
        correction_coef1(f,b) + T(CCD)^2 * correction_coef2(f,b)]

        where 

        Resp(f,T,b) is responsivity in filter f at CCD temperature T in binning 
        state b, 

        T(CCD) is raw CCD temperature in units of DNs, 

        R(f,t=-30.3C,b) is responsivity in filter f in binning state b at CCD 
        temperature of 1060 DN (-30.3C), 

        correction_offset(f,b) is camera- and filter-dependent temperature 
        correction offset for filter f and binning state b, 

        correction_coef1(f,b) is the camera- and filter-dependent temperature 
        correction first-order coefficient for filter f and binning state b.

        correction_coef2(f,b) is the camera- and filter-dependent temperature 
        correction second-order coefficient for filter f and binning state b.

        To apply responsivity to obtain radiance L, the expression is

        L(f) = DN_flat(f) / (t * Resp(f,T,b) * Correct(f, MET))

        where

        L is radiance in units of W / (m**2 microns**1 sr**1),

        DN_flat is dark-, smear-, linearity-, and flat field-corrected DN,

        t is the exposure time in seconds, 

        Resp(f,T,b) is the responsivity in filter f at CCD temperature T and
        binning state b, and 

        Correct(f, MET) is the temporal correction to responsivity for 
        filter f at time MET.


        (7) Conversion from radiance to I/F
        ===================================

        To convert from radiance to I/F (also known as radiance factor, the ratio
        of measured radiance to that which would be measured from a white
        perfectly Lambertian surface), the following expression should be applied:

        I_over_F(f) = L(f) * pi * (SOLAR_DISTANCE/149597870.691)**2 / F(f)

        where

        L(f) is calibrated radiance calculated as described above for some filter
        f,

        SOLAR_DISTANCE is that value for distance of the target object from the
        center of the sun in kilometers (as indicated by the keyword
        SOLAR_DISTANCE)

        149597870.691 is the number of kilometers in 1 AU

        F(f) is effective average solar irradiance sampled under the filter
        bandpass.

        The effective average solar radiance for each camera and bandpass is given
        in the SOLAR directory.
    

If run on a non-spiceinited cube, this program requires access to local mission-specific SPICE kernels, in order to find the distance between the sun and the target body. When run on a spiceinited cube, this can be determined using the camera model. Using a spiceinited cube as input has the advantage of not requiring that local mission-specific kernels be available. (See spiceinit web=true.)

Description

This is the ISIS cube from the Messenger mission to be calibrated.

Type	cube
File Mode	input
Filter	*.cub

Description

This is the output file. The output cube will be a radiometrically calibrated version of the input cube.

Type	cube
File Mode	output
Filter	*.cub

Description

Type	string
Default	MODEL
Option List:	Option Brief Description NONE No correction No dark current correction will be applied STANDARD Do a median dark current correction This will use the median of the three leftmost pixels as the dark current, on a line by line basis. LINEAR Use a linear fit This will fit a line to the leftmost pixel values, which should be dark current data, through the lines. The equation derived from these pixels will be used to calculate the dark current correction, on a line by line basis. MODEL Use pre-developed model Messenger has independent dark models, developed on-ground. This will use the most recent of these models to correct the dark current. Note: this method cannot be used if the exposure duration of the image exceeds one second.

Description

If this is selected, the dark current data are set to null in the output image.

Binning affects the number of columns that are determined to be set to null. Thus, KEEPDARK is overloaded in terms of any columns that contain artifacts that are generated by binning (or wavelet compression). These columns are set to null as well.

If no binning is applied, then four columns are set to null. If any combination of DPU or MP (essentially on-board processing) binning is applied, three columns will be set to null. When DPU and MP 2x2 binning occurs (essentially a 4x4 summing) three columns will be set to null. All other combinations of binning will have one column set to the null pixel value.

If KEEPDARK = TRUE, then no columns are set to null on output.

Type	boolean
Default	false

Description

This parameter allows the user to selectively apply the flatfield correction. This parameter can be used in conjunction with DARKCURRENT and RADIOMETRIC to produce additional output products such as DNs (all parameters DARKCURRENT=MODEL and RADIOMETRIC=FALSE).

Type	boolean
Default	True

Description

This parameter allows the user to selectively apply the radiometric correction. This parameter can be used in conjunction with DARKCURRENT and FLATFIELD to produce additional output products such as DNs (all parameters DARKCURRENT=MODEL and FLATFIELD=FALSE). However, if RADIOMETRIC=FALSE, then the program will turn IOF=FALSE.

Type	boolean
Default	True

Description

This option, when set, will convert the output to I/F from radiance values. To convert from radiance to I/F (also known as radiance factor, the ratio of measured radiance to that which would be measured from a white perfectly Lambertian surface), the following expression is applied:

I_over_F(f) = L(f) * PI * (SOLAR_DISTANCE/149597870.691)**2 / F(f)                
            

where L(f) is calibrated radiance calculated for some filter f, SOLAR_DISTANCE is that value for distance of the target object from the center of the sun in kilometers (as indicated by the keyword SOLAR_DISTANCE), 149597870.691 is the number of kilometers in 1 AU and F(f) is effective average solar irradiance sampled under the filter bandpass.

If the observed target is not of a valid body as recognized by NAIF, the output is left in radiance.

Type	boolean
Default	True

Description

This parameter is provided to allow the user to selectively apply the empirical correction.

Type	boolean
Default	True

This example shows the calibration process of a MDIS image

mdiscal FROM=EW0089565626A.cub TO=EW0089565626A.calib.cub DARKCURRENT=MODEL

Calibrating EW0089565626A.cub

Calibrate an MDIS image This is the GUI for mdiscal when converting the uncalibrated cube EW0089565626A.cub to the calibrated cube EW0089565626A.calib.cub.

Input Image

Input Cube This is EW0089565626A.jpg before calibration.

Output Image With Dark Model

Output With Dark Model This is the output generated by the default options.