Added I/F calibration step to hyb2onccal (#3132)

Pvl hyb2onc2isis(QString fitsFileName, QString outputCubeFileName, CubeAttributeOutput att, QString target) {

  Pvl finalPvl;

  ProcessImportFits importFits;

  importFits.setFitsFile(FileName(fitsFileName));

  importFits.setProcessFileStructure(0);

  // Translate the Instrument group

  FileName transFile(transDir + "hyb2oncInstrument1.trn");

  FileName transFile(transDir + "hyb2oncInstrument.trn");

  if (updatedKeywords) {

    transFile = transDir+"hyb2oncInstrumentUpdated.trn";

  // Convert the image data

  importFits.Progress()->SetText("Importing Hayabusa2 image");

   Pvl finalLabel = *(outputCube->label() );

  importFits.StartProcess();

  importFits.Finalize();

  return finalLabel;

  return outputLabel;

  }

  }

static QString g_iofCorrection("IOF");  //!< Is I/F correction to be applied?

//  I/F variables

static double g_solarDist(1.0);  /**< Distance from the Sun to the target body

(used to calculate g_iof) */

static double g_iof(1.0);        //!< I/F conversion value

static double g_iofScale(1.0);

static double g_solarFlux(1.0);  //!< The solar flux (used to calculate g_iof).

// TODO: we do not have this conversion factor for Hayabusa 2 ONC.

static double g_v_standard(1.0);

// static double g_v_standard(3.42E-3);//!< Base conversion for all filters (Tbl. 9)

static double g_sensitivity(1.0);

static double g_effectiveBandwidth(1.0);

namespace Isis {

/**

* @brief Apply radiometric correction to each line of an AMICA image.

 * @brief linearFun:  The linear correction function (used by the newton_rapheson method)

 * @author 2019-02-12  Tyler Wilson

 * @param Iobs:  The observed intensity

 * @param x:  The ideal intensity.

 * @param g:  The vector of empirically derived coefficients for the third-order polynomial

 * modelling the linear correction (for DN values < 3400 DN)

 * @return The value of the function at the point x.

 */

double linearFun(double Iobs,double x, double g[3]) {

  return Iobs - g[0]*x -g[1]*pow(x,2.0) -g[2]*pow(x,3.0);

}

/**

 * @brief dFun:  The first-order derivative of linearFun

 * @author 2019-02-12  Tyler Wilson

 * @param x:  The ideal intensity.

 * @param g:  The vector of empirically derived coefficients for the third-order polynomial

 * modelling the linear correction (for DN values < 3400 DN)

 * @return

 */

double dFun(double x, double g[3]) {

  return -g[0] - 2*g[1]*x -3*g[2]*pow(x,2.0);

}

/**

 * @brief newton_rapheson

 * @author 2019-02-12 Tyler Wilson

 * @param Iobs:  The observed DN intensity

 * @param x0:  The starting value for the Newton-Rapheson method

 * @param g:  A vector of the coefficients for the linearity function.  It is a third-order

 * polynomial.

 * @param result:  The final approximation of the root of the equation.

 * @param epsilon:  The tolerance on the final solution.

 * @return A root of the linearity correction function, centered near the origin.

 */

bool newton_rapheson(double Iobs,double x0, double g[3],double &result, double epsilon=1e-6 )  {

   double x[2];

   double dx = 1.0;

   int iter = 0;

   int maxIterations=500;

   x[0] = x0;

   while (dx > epsilon)  {

     x[1]=x[0] - linearFun(Iobs,x[0],g)/dFun(x[0],g);

     dx = fabs(x[1]-x[0]) ;

     x[0]=x[1];

     iter++;

     if (iter > maxIterations) {

       return false;

     }

   }

   result = x[1];

   return true;

}

/**

* @brief Apply radiometric correction to each line of a Hayabusa2 image.

* @author 2016-03-30 Kris Becker

* @param in   Raw image and flat field

* @param out  Radometrically corrected image

* @internal

*   @history 2017-07-2017 Ian Humphrey & Kaj Williams - Adapted from amicacal.

*   @history 2019-02-12 Tyler Wilson - Modified to support new calibration settings/formulas.

*/

void Calibrate(vector<Buffer *>& in, vector<Buffer *>& out) {

  for (int i = 0; i < imageIn.size(); i++) {

    imageOut[i] = imageIn[i]*pow(2.0,12-g_bitDepth);

    // Check for special pixel in input image and pass through

    if ( IsSpecial(imageOut[i]) ) {

      imageOut[i] = imageIn[i];

    }

    // Apply compression factor here to raise LOSSY dns to proper response

    imageOut[i] *= g_compfactor;

    // 1) BIAS Removal - Only needed if not on-board corrected

    if ( !g_onBoardSmearCorrection ) {

        continue;

      }

      else {

        imageOut[i] = imageOut[i] - g_bias;

      }

    }

    double dn = imageOut[i];    

    double linearCorrection;

    double result = 1.0;

    double x0 = 1.0;

    newton_rapheson(imageOut[i],x0, g_L,result );    

    newton_rapheson(dn,x0, g_L,result );   

    imageOut[i] = result;

    //qDebug() << dn << ","<< result;

    // DARK Current

    imageOut[i] = imageOut[i] - g_darkCurrent;    

    // READOUT Smear Removal - Not needed if on-board corrected.  Binning is

    //    accounted for in computation of c1 before loop.

    // if (nsubImages <= 1) {

    //  imageOut[i] = c1*(imageOut[i] - smear);

    // }

    //Smear correction

    if (!g_onBoardSmearCorrection) {

      double smear = 0;

      }

    //Linearity Correction

    //In the SIS this adjustment is made just after the bias, but

    //in the Calibration paper it happens just before the flat field correction.

    // FLATFIELD correction

    //  Check for any special pixels in the flat field (unlikely)

      }

      else {

        if (flatField[i] != 0) {

          imageOut[i] /= flatField[i];

          imageOut[i] /= (flatField[i]*g_sensitivity*g_texp);

        }

      }

    }

    // TODO: once the radiance values are known for each band, we can correctly compute I/F.

    // For now, g_iof is 1, so output will be in DNs.

    // 7) I/F or Radiance Conversion (or g_iof might = 1, in which case the output will be in DNs)

    imageOut[i] *= g_iof;

  }

/**

 * @brief Load required NAIF kernels required for timing needs.

 *

 * This method maintains the loading of kernels for HAYABUSA timing and

 * planetary body ephemerides to support time and relative positions of planet

 * bodies.

 */

/* Helper function for sunDistanceAu, don't need this until we have radiance calibration

   parameters for Hayabusa2 ONC-T filters to calculate radiance and I/F

static void loadNaifTiming() {

  static bool naifLoaded = false;

  if (!naifLoaded) {

//  Load the NAIF kernels to determine timing data

    Isis::FileName leapseconds("$base/kernels/lsk/naif????.tls");

    leapseconds = leapseconds.highestVersion();

    Isis::FileName sclk("$hayabusa2/kernels/sclk/hyb2_20141203-20161231_v01.tsc");    

    Isis::FileName pck1("$hayabusa2/kernels/tspk/de430.bsp");

    Isis::FileName pck2("$hayabusa2/kernels/tspk/jup329.bsp");

    Isis::FileName pck3("$hayabusa2/kernels/tspk/sat375.bsp");

    Isis::FileName pck4("$hayabusa2/kernels/spk/hyb2_20141203-20141214_0001m_final_ver1.oem.bsp");

    Isis::FileName pck5("$hayabusa2/kernels/spk/hyb2_20141203-20151231_0001h_final_ver1.oem.bsp");

    Isis::FileName pck6("$hayabusa2/kernels/spk/hyb2_20151123-20151213_0001m_final_ver1.oem.bsp");

//  Load the kernels

    QString leapsecondsName(leapseconds.expanded());

    QString sclkName(sclk.expanded());

    QString pckName1(pck1.expanded());

    QString pckName2(pck2.expanded());

    QString pckName3(pck3.expanded());

    QString pckName4(pck4.expanded());

    QString pckName5(pck5.expanded());

    QString pckName6(pck6.expanded());

    furnsh_c(leapsecondsName.toLatin1().data());

    furnsh_c(sclkName.toLatin1().data());

    furnsh_c(pckName1.toLatin1().data());

    furnsh_c(pckName2.toLatin1().data());

    furnsh_c(pckName3.toLatin1().data());

    furnsh_c(pckName4.toLatin1().data());

    furnsh_c(pckName5.toLatin1().data());

    furnsh_c(pckName6.toLatin1().data());

//  Ensure it is loaded only once

    naifLoaded = true;

  }

  return;

}

*/

/**

 * @brief Computes the distance from the Sun to the observed body.

 *

 * This method requires the appropriate NAIK kernels to be loaded that

 * provides instrument time support, leap seconds and planet body ephemeris.

 *  

 * @return @b double Distance in AU between Sun and observed body.

 */

/* commented out until we have radiance values (RAD/IOF group in calibration trn) for Hayabusa2.

 static bool sunDistanceAU(const QString &scStartTime,

                          const QString &target,

                          double &sunDist) {

  //  Ensure NAIF kernels are loaded

  loadNaifTiming();

  sunDist = 1.0;

  //  Determine if the target is a valid NAIF target

  SpiceInt tcode;

  SpiceBoolean found;

  bodn2c_c(target.toLatin1().data(), &tcode, &found);

  if (!found) return (false);

  //  Convert starttime to et

  double obsStartTime;

  scs2e_c(-37, scStartTime.toLatin1().data(), &obsStartTime);

  //  Get the vector from target to sun and determine its length

  double sunv[3];

  double lt;

  spkpos_c(target.toLatin1().data(), obsStartTime, "J2000", "LT+S", "sun",

                  sunv, &lt);

  NaifStatus::CheckErrors();

  double sunkm = vnorm_c(sunv);

  //  Return in AU units

  sunDist = sunkm / 1.49597870691E8;

  //cout << "sunDist = " << sunDist << endl;

  return (true);

}

*/

/**

 * @brief Translates a 1-banded Isis::Cube to an OpenMat object

 *

* @return FileName Path and name of flat file file

* @internal

*   @history 2017-07-27 Ian Humphrey & Kaj Williams - Adapted from amicacal.

*   @history 2019-02-12 Tyler Wilson - Modified to support new calibration settings/formulas.

*/

FileName DetermineFlatFieldFile(const QString &filter) {

  QString fileName = "$hayabusa2/calibration/flatfield/";

  // FileName consists of binned/notbinned, camera, and filter

  fileName += "flat_" + filter.toLower() + ".cub";

  fileName += "flat_" + filter.toLower() + "_norm.cub";

  FileName final(fileName);

  return final;

}

  PvlGroup &DarkCurrent = g_configFile.findGroup("DarkCurrent");

  PvlGroup &Smear = g_configFile.findGroup("SmearRemoval");

  PvlGroup &solar = g_configFile.findGroup("SOLARFLUX");

  PvlGroup &sensitivity = g_configFile.findGroup("SENSITIVITYFACTOR");

  PvlGroup & effectiveBW = g_configFile.findGroup("EFFECTIVEBW");

  PvlGroup &linearity = g_configFile.findGroup("Linearity");

  // PvlGroup &iof = g_configFile.findGroup("RAD");

  // Compute BIAS correction factor (it's a constant so do it once!)

  g_bias = g_b0+g_b1*g_CCD_T_temperature+g_b2*g_ECT_T_temperature;

  g_bias *= (g_bae0 + g_bae1*g_AEtemperature); //correction factor

  qDebug() << "Bias: " << g_bias;

  //double correction_factor = (g_bae0 + g_bae1*g_AEtemperature);

  g_bias *= (g_bae0 + g_bae1*g_AEtemperature); //bias correction factor

  // Load the Solar Flux for the specific filter

  g_solarFlux = solar[g_filter.toLower()];

  g_sensitivity = sensitivity[g_filter.toLower()];

  g_effectiveBandwidth = effectiveBW[g_filter.toLower()];

  //Load the linearity variables

  g_L[0] = linearity["L"][0].toDouble();

  g_L[2] = linearity["L"][2].toDouble();

  // radiance = g_v_standard * g_iofScale

  // iof      = radiance * pi *dist_au^2

  // g_iofScale   = iof[g_filter];

  return ( calibFile.original() );

}

}

#endif

using namespace std;

//void Calibrate(vector<Buffer *>& in, vector<Buffer *>& out);

//QString loadCalibrationVariables(const QString &config);

  catch (IException &e) {

    QString msg = "Unable to read [BitDepth] keyword in the Instrument group "

    "from input file [" + icube->fileName() + "]";

    //qDebug() << msg;

    g_bitDepth = 12;

  }

  try {

    g_AEtemperature = inst["ONCAETemperature"][0].toDouble();

    qDebug() << "g_AEtemperature:  " << g_AEtemperature;

  }

  catch(IException &e) {

    QString msg = "Unable to read [ONCAETemperature] keyword in the Instrument group "

  try {

    g_CCD_T_temperature = inst["ONCTCCDTemperature"][0].toDouble();

    qDebug() << "g_CCD_T_Temperature:  " << g_CCD_T_temperature;

  }

  catch(IException &e) {

    QString msg = "Unable to read [ONCTCCDTemperature] keyword in the Instrument group "

  try {

    g_ECT_T_temperature = inst["ONCTElectricCircuitTemperature"][0].toDouble();

    qDebug() << "g_ECT_T_temperature: " << g_ECT_T_temperature;

  }

  catch(IException &e) {

    QString msg = "Unable to read [ONCTElectricCircuitTemperature] keyword in the Instrument group "

  if (smearCorrection=="ONBOARD") {

    g_onBoardSmearCorrection=true;

  }

  else {

      qDebug() << icube->fileName();

  }

  QString compmode = inst["Compression"];

  // TODO: verify that the compression factor/scale is actually 16 for compressed Hayabusa2 images.

  g_compfactor = ( "lossy" == compmode.toLower() ) ? 16.0 : 1.0;

  QString target = inst["TargetName"];

  g_target = target;

      Cube *flatOriginal = new Cube(flatfile.expanded() );

      //int transform[5] = {binning,startSample,startLine,lastSample,lastLine};

      double alphaStartSample = alphaCube["AlphaStartingSample"][0].toDouble();

      double alphaStartLine = alphaCube["AlphaStartingLine"][0].toDouble();

      double alphaEndSample = alphaCube["AlphaEndingSample"][0].toDouble();

      double alphaEndLine = alphaCube["AlphaEndingLine"][0].toDouble();

      //int transform[5] = {binning,startSample,startLine,lastSample,lastLine};

      double transform[5] = {(double)binning,alphaStartSample,alphaStartLine,alphaEndSample,alphaEndLine};

      // Translates and scales the flatfield image.  Scaling

  Cube *ocube  = p.SetOutputCube("TO");

  //QString fname = ocube->fileName();

  QString calfile = loadCalibrationVariables(ui.GetAsString("CONFIG"));

  g_timeRatio = g_Tvct/(g_texp + g_Tvct);

  g_iof = 1.0;  // Units of DN

  QString g_units = "DN";

  // if ( "radiance" == g_iofCorrection.toLower() ) {

  calibrationLog.addKeyword(PvlKeyword("CalibrationFile", calfile));

  calibrationLog.addKeyword(PvlKeyword("FlatFieldFile", flatfile.originalPath()

  + "/" + flatfile.name()));

  calibrationLog.addKeyword(PvlKeyword("CompressionFactor", toString(g_compfactor, 2)));

  PvlKeyword sensitivityFactor("SensitivityFactor");

  sensitivityFactor.addValue(toString(g_sensitivity,16));

  calibrationLog.addKeyword(sensitivityFactor);

  // Parameters

  PvlKeyword bn("Bias_Bn");

  bnae.addValue(toString(g_bae0, 8));

  bnae.addValue(toString(g_bae1, 8));

  calibrationLog.addKeyword(bnae);  

#if 0

  PvlKeyword linearityCoefs("Linearity");

  linearityCoefs.addValue(toString(g_L0,8));

  linearityCoefs.addValue(toString(g_L1,8));

  linearityCoefs.addValue(toString(g_L2,8));

  calibrationLog.addKeyword(linearityCoefs);

#endif

  calibrationLog.addKeyword(PvlKeyword("Bias_AETemp", toString(g_AEtemperature, 16)));

  calibrationLog.addKeyword(PvlKeyword("Smear_texp", toString(g_texp, 16)));

  calibrationLog.addKeyword(PvlKeyword("CalibrationUnits", g_iofCorrection));

  calibrationLog.addKeyword(PvlKeyword("RadianceStandard", toString(g_v_standard, 16)));

  calibrationLog.addKeyword(PvlKeyword("RadianceScaleFactor", toString(g_iofScale, 16)));

  calibrationLog.addKeyword(PvlKeyword("SolarDistance", toString(g_solarDist, 16), "AU"));

  calibrationLog.addKeyword(PvlKeyword("SolarFlux", toString(g_solarFlux, 16)));  

  calibrationLog.addKeyword(PvlKeyword("IOFFactor", toString(g_iof, 16)));

  calibrationLog.addKeyword(PvlKeyword("Units", g_units));

  PvlKeyword linearityCoefs("LinearityCoefficients");

  linearityCoefs.addValue(toString(g_L[0],16));

  linearityCoefs.addValue(toString(g_L[1],16));

  linearityCoefs.addValue(toString(g_L[2],16));

  calibrationLog.addKeyword(linearityCoefs);

  PvlKeyword darkCurrentCoefs("DarkCurrentCoefficients");

  darkCurrentCoefs.addValue(toString(g_d0,16));

  darkCurrentCoefs.addValue(toString(g_d1,16));

  calibrationLog.addKeyword(darkCurrentCoefs);

  PvlKeyword darkCurrent("DarkCurrent");

  darkCurrent.addValue(toString(g_darkCurrent,16));

  calibrationLog.addKeyword(darkCurrent);

  // Write Calibration group to output file

  ocube->putGroup(calibrationLog);

  Application::Log(calibrationLog);

<?xml version="1.0" encoding="UTF-8"?>

<!-- $Id$ -->

<application name="hyb2oncal" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance"

<application name="hyb2onccal" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance"

xsi:noNamespaceSchemaLocation="http://isis.astrogeology.usgs.gov/Schemas/Application/application.xsd">

  <brief>

    Calibrates Hayabusa 2 ONC-T images. Calibration includes bias and dark current correction as

    </div>

  </p>

<!--

  <p>

    <h1><a id="Smear">Step 2: Read-out smear:</a ></h1>

    The ONC-T instrument is shuttered electronically.  Images are exposed for a certain

    exposure time in addition to the vertical charge-transfer period. <strong>We could not determine

    of locate this value. Additionally, note that on-board smear correction can be performed.

    </strong>

    It is during the charge-transfer period that a read-out smear in the vertical direction

    is produced. The read-out smear brightness <strong>I<sub>smear</sub></strong>

    for unbinned images is modeled from the observed images as follows:

    <div style="font-size:90%; font-family:monospace; margin:5px; margin-left:30px;">

    <br/><br/>

    <center><strong>I<sub>smear</sub>(H) = SUM(H=0...N<sub>v</sub> -1) { [K*[(I<sub>raw</sub>(H,V) -

    I<sub>sky</sub>(H,V)]/N<sub>v</sub>] } </strong></center>

    <br/><br/>

           <center>Where:  <strong>K = t<sub>VCT</sub>/(t<sub>VCT</sub>+t<sub>exp</sub>)

           </strong></center>

    <br/><br/>

    For binned images a different formula is applied:

     <center><strong>I<sub>smear</sub>(H) = SUM(H=0...N<sub>v</sub> - 1)

     { [ K1*I<sub>raw</sub>(H,V) ] }</strong>

     </center>

    <br/><br/>

           <center>Where:  <strong>K1 = (1/N<sub>v</sub>)*[t<sub>VCT</sub>/

           (t<sub>VCT</sub>+t<sub>exp</sub>)]

           </strong></center>

    <br/><br/>

    A correction factor is then applied after the smear component is subtracted

    from the input image (I<sub>raw</sub>):

    <center> <strong> I<sub>out</sub> = C*(I<sub>raw></sub> - I<sub>smear</sub>)</strong></center>

    <br/><br/>

    <center>Where:  <strong>C = 1/( 1 + K1 * ( (B - 1)/2*B ) ) </strong></center>

    <br/><br/>

    <center><table border = "1" cellpadding="5">

    <tr>

      <td>Variable</td><td>Description</td>

    </tr>

    <tr>

      <td>I<sub>smear</sub></td><td>The read-out smear.</td>

    </tr>

    <tr>

      <td>I<sub>raw</sub></td><td>The intensity of the raw data taken with exposure time

      t<sub>exp</sub>.</td>

    </tr>

    <tr>

      <td>I<sub>sky</sub></td><td>The sum of the bias and the dark current (~300 DN).</td>

    </tr>

    <tr>

      <td>t<sub>VCT</sub></td><td>The vertical charge-transfer period (0.012288 microseconds).</td>

    </tr>

    <tr>

      <td>t<sub>exp</sub></td><td>The exposure time (in microseconds).</td>

    </tr>

    <tr>

      <td>N<sub>v</sub></td><td>The number of pixels along the V-direction (1024).</td>

    </tr>

    <tr>

      <td>H</td><td>The line number of the pixel.</td>

    </tr>

    <tr>

      <td>L</td><td>The sample number of the pixel.</td>

    </tr>

    <tr>

      <td>B</td><td>The binning number.</td>

    </tr>

    </table></center>

    </div>

  </p>

-->

  <p>

    <h1><a id="Flatfield">Step 2: Flat-field correction:</a ></h1>

    Performs a correction for pixel-to-pixel variation in CCD response and vignetting

    pixel in the flat-field image.

  </p>

<!-- We cannot correctly determine I/F or radiance output because we do not have the radiance

values for each band for Hayabusa2 ONC.

  <p>

    <h1><a id="ConvertIOF">Step 3 (Optional): Convert output units to Radiance or I over F:</a ></h1>

    This step is optional, and the formula used depends on the value of the UNITS user parameter.

    <em>Note: we do not currently have the radiance values for the filters, so we cannot correctly

    convert the output units to Radiance.

    If UNITS=RADIANCE, the following formula will be used to convert the raw DN values to radiance

    (W/m2/sr/µm):

    <br/><br/>

     <div style="font-size:90%; font-family:monospace; margin:5px; margin-left:30px;">

      <center><strong>R = Raw*RadianceStandard*RadianceScaleFactor</strong></center>

      <br/><br/>

      <center><table border="1" cellpadding="5">

      <tr>

          <td>Variable</td><td>Description</td>

     </tr>

     <tr>

          <td>R</td><td>The calibrated radiance (w/m2/sr/µm). </td>

     </tr>

     <tr>

          <td>Raw</td><td>The raw DN value. </td>

     </tr>

     <tr>

          <td>RadianceStandard</td><td>The standard conversion factor from DNs to radiance. </td>

     </tr>

     <tr>

          <td>RadianceScaleFactor</td><td>An adjustment factor for each filter.</td>

     </tr>

     </table></center>

     </div>

    If UNITS = IOF, first the above formula will be used to convert from raw DNs to calibrated Radiance, and then

    the following formula will be used to convert the raw DN values to I/F (radiance) units:

    <br/><br/>

     <div style="font-size:90%; font-family:monospace; margin:5px; margin-left:30px;">

      <center><strong>IoF = R*[pi*(R<sub>s</sub>)<sup>2</sup>]/F</strong></center>

      <br/><br/>

      <center><table border="1" cellpadding="5">

      <tr>

          <td>Variable</td><td>Description</td>

     </tr>

     <tr>

          <td>IoF</td><td>The calibrated radiance in units of I over F.</td>

     </tr>

     <tr>

          <td>R</td><td>The calibrated radiance (w/m2/sr/µm). </td>

     </tr>

     <tr>

         <td>R<sub>s</sub></td><td>The distance in Astronomical Units (AU) between the Sun

         and the target body.

         </td>

     </tr>

     <tr>

          <td>F</td><td>The solar flux (w/m2/µm) at 1 AU. </td>

     </tr>

     </table></center>

     </div>

    If UNITS=DN, no output conversion will be performed and the output units will be in raw DNs.

  </p>

-->

  <p>

  <h1><a id="Notes">Notes</a></h1>

  <ol>

    <li>

      Smear correction is not currently provided, as we do not have the readout time

      (charge-transfer period) for the instrument.

    </li>

    <li>

      Similarly, since no radiance values could be found for the instrument filters, the output

      cannot be correctly converted to radiance or I/F.

    </li>

    <li>

    </li>

  </ol>

  </p>

  <p>

    <h1><a id="References">References:</a></h1>

    <ol>

      <li>S. Kameda et al.  <i>"Preflight Calibration Test Results for Optical Navigation

      Camera Telescope (ONC-T) Onboard the Hayabusa2 Spacecraft"</i>.

      Space Sci Rev (2017) 208:17-31.</li>

      Space Sci Rev (2017) 208:17-31.

      </li>

      <li>E. Tatsumi et al.  <i>"Updated Inflight Calibration of Hayabusa2’s Optical Navigation Camera (ONC) for

      Scientific Observations during the Cruise Phase"</i>.

      https://arxiv.org/abs/1810.11065 [astro-ph.IM] 25 Oct, 2018.

      </li>

      <li>H. Suzuki et al. <i>"Initial inflight calibration for Hayabusa2 optical navigation camera

      (ONC) for science observations of asteroid Ryugu"</i>.

      Icarus. 300. 10.1016/j.icarus.2017.09.011

      </li>

    </ol>

  </p>

    <change name="Ian Humphrey and Kaj Williams" date="2017-07-27">

      Original version. Adapted from amicacal.

    </change>

    <change name="Tyler Wilson" date="2019-02-12">

      Modified version to handle the updated calibration values/formulas.

    </change>

  </history>

  <groups>

           the parameters as needed.

        </description>