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Grant Agreement

776276

Acronym

PLANMAP

Project full title

Planetary mapping

 

 

Deliverable

D 4.1

Deliverable Name

Spectral index and RGB maps – v.1

Nature of deliverable

R

Dissemination level

PU

Scheduled delivery date`

31st August 2018

Status

Final

 

 

Prepared by:

Francesca Zambon, Cristian Carli, Francesca Altieri

Verified by:

Sabrina Ferrari, David Rothery

Approved by:

Matteo Massironi

 

 

  

Disclaimer

This document is the property of the PLANMAP Consortium.

This document may not be copied, reproduced, or modified in the whole or in the part for any purpose without written permission from the PLANMAP Coordinator with acceptance of the Project Consortium.


Executive summary

List of Acronysm

1. Introduction

2. Map production

3. Spectral indices and RGB map

References

Annex

Executive summary

 

The purpose of this deliverable is to describe the parameters defined as diagnostics of the spectral variability of the Hokusai Quadrangle. We introduced the meaning of the spectral parameters to summarize the spectral information, and the dataset used for the 8-color mosaic of Mercury surface. We report the procedure used to produce the mosaic, and the projection. We have defined spectral parameters and RGB, which are important to develop in the future the spectral units of the Hermean surface. In particular, because of the spectral properties of Mercury (featureless) and the multispectral dataset (between 400 and 1000 nm), we could not define spectral parameters related to absorption bands. Therefore, we defined two parameters related to the reflectance (value of reflectance at 750 nm, and the PC1) and two parameters related to the slopes (spectral slope between 966 and 433 nm, and the PC2). Moreover, we have produced three different RGBs, describing the color variability influenced by reflectance and slope variations, that are in turn indicative of differences in spectral properties associated with terrain composition and maturity.

List of Acronysm

 

Acronym

Explanation

MDIS

Mercury Dual Imaging System

WAC

Wide Angle Camera

NAC

Narrow Angle Camera

EDR

Experiment Data Record

DEM

Digital Elevation Model

ISIS

Integrated Software for Imagers and Spectrometers

PCA

Principal Component Analysis

RGB

Red - Green - Blue

USGS

U.S. Geological Survey

MESSENGER

MErcury Surface, Space ENvironment, GEochmistry, and Ranging

INAF

Istituto Nazionale di AstroFisica

IAPS

Istituto di Astrofisica e Planetologia Spaziali

 

 

1.   Introduction

 

The deliverable 4.1, the first of the WP4 lead by INAF-IAPS Rome, regards the release of spectral indices and RGB-color composite maps of one of the primary PLANMAP targets, the Hokusai quadrangle (H-5) on Mercury, located in the northern hemisphere of the planet (22.5°N-65°N, 0°-90°E) (Figure 1).

We retrieved the spectral parameter maps from the data provided by the MESSENGER MDIS-WAC (Hawkins et al., 2007; and Denevi et al., 2018).

The first step was to produce the 8-color (filter) mosaic of the Hokusai quadrangle, necessary to derive the spectral indices and the RGB maps required. Among the 11 WAC filters devoted to the scientific analysis, we considered the 8 filters with the higher number of images that cover the whole quadrangle at a spectral range between 400 and 1000 nm (see Table 1). MDIS-WAC was equipped with a multi-filter rotating wheel, and the images were acquired one by one for each filter, therefore images captured in different moments do not exactly overlap each other. Furthermore, an upstream filter selection has been done during the acquisition. Among the 10,373 images available for the Hokusai quadrangle only 5,024 are useful for our purpose. These images cover a large spatial resolution interval (103-171920 m/px) then a further selection on spatial resolution is needed. We selected images with a spatial resolution lower than 1000 m/pixel, choosing for the final mosaic an average spatial resolution of 450 m/pixel.


 

Fig.1: Mercury quadrangle scheme. Red square indicates the H-5 Hokusai quadrangle.


2.   Map production


The steps applied to produce the 8-color mosaic of Hokusai quadrangle are the following:

 

  1. selection of the 8-filters group of overlapping images;
  2. calibration of the EDR images;
  3. application of the Kaasalainen-Shkuratov photometric correction model (Domingue et al., 2016), considering the DEM by USGS 2016, with a spatial resolution of 665 m/pixel (see https://astrogeology.usgs.gov/search/map/Mercury/Topography/MESSENGER/Mercury_Messenger_USGS_DEM_Global_665m). The images were normalized to standard photometric geometry of 30° incidence angle, 0° emission angle and 30° phase angle.
  4. coregistration of the 8-filters overlapping group of images with respect to the F filter (430nm);
  5. creation of the 8-filter cubes ordered for increasing wavelengths;
  6. 8-filter cube projection with a spatial resolution of 450m/pixel, centered at     43.75°N and 45°E in equirectangular projection;
  7. creation of the Hokusai quadrangle 8-color mosaic in equirectangular projection averaging the overlapping pixels.
  8. conversion on the 8-color mosaic into Lambert-Conformal projection with the same spatial resolution (see Annex).

 

The data processing and map production has been performed by using the Integrated Software for Imagers and Spectrometers (ISIS3) (https: //isis.astrogeology.usgs.gov/Application/index.html).

 

TABLE 1 - 5,024 images were used of the following 8-filters: wavelengths and bands width measured at -26°C are reported (Hawkins et al., 2007).


 

Filter

Wavelength (nm)

Bandwidth (nm)

F

430.0

18.0

C

480.4

8.9

D

559.2

4.6

E

628.8

4.4

G

749.0

4.5

L

828.6

4.1

J

898.1

4.3

I

996.8

12.0


3.   Spectral indices and RGB map


The spectral indices and RGB color combination choice is helpful to enhance compositional variations and to understand the geology of a surface. Each surface is characterized by specific spectral features, therefore a proper spectral parameters selection is needed for each body. Mercury surface spectra are characterized by the lack of evident absorption bands in the visible and near-infrared. Only a shallow band centered at 600 nm has been identified in very localized regions, in correspondence of sublimation depressions called hollows (Vilas et al., 2016; Lucchetti et al., 2018, in press), or associated to low reflectance materials (Klima et al., 2018). At the global scale, the Hermean surface is characterized by reflectance and spectral slope variations. The main goal of this delivery is to identify spectral indices and RGB color combinations that may emphasize spectral variations across the Hokusai quadrangle. Below we report the spectral indices and RGB maps selected to better point out the Hokusai quadrangle spectral diversity (see Table 2 and following figures).


Table 2 - summary of calculated parameters/RGB images.


parameter/RGB combination

Description

R750

Reflectance at 750 nm (Fig.2)

PC1

PCA first channel, reflectance variation (Fig.3)

PC2

PCA second channel, color variation (Fig.4)

S996−430

(R996- R430)/((996-430)*R433 (Fig.5)

RGB "Enhanced Color Mosaic"

R: PC2, G: PC1, B: 430/996nm (Fig.6)

RGB "False Color Mosaic"

R: 996 nm, G: 750nm, B: 430 nm (Fig.7)

RGB "Clementine Color Mosaic"

R: R(748 nm)/R(430 nm), G: R(748 nm)/R(828 nm), B: R(430 nm)/R(748 nm) (Fig.8)

 


Figure 2. R750: Reflectance at 750 nm is a standard wavelength useful to emphasize reflectance variation where often no absorption bands occur. The linear stretch applied is 0.060-0.215. This parameter permits to differentiate bright material to darker one, and it has been used to threshold different color units (see Murchie et al., 2015).

 

The PCA allows for converting a set of possibly correlated variables into a set of linearly uncorrelated variables called principal components by applying an orthogonal transformation. Almost all the information is contained in the first bands. We performed it using the PCA ISIS3 command.

 

 


Figure 3. PC1: Here, we show the PC1, with a linear stretch between 0.10 and 0.45. This parameter is principally able to enhance reflectance variations.

 

 

Figure 4. PC2: Here, we show the PC2, where the applied linear stretching is: 0.03-0.10. This parameter permits to discriminate color variations, which in the case Mercury is strongly correlated with slope variability.

 

 

Figure 5. S996-430: The spectral slope between 996 and 430 nm (S996−430 = (R996- R430)/((996-430)*R430), see Cuzzi et al., 2009, Filacchione et al., 2012) is indicative of the global MDIS-WAC spectral slope. Low spectral slope regions (bluer slopes) are representative of fresh terrains (dark pixels), conversely higher spectral slope values (redder slopes) are indicative of older terrains (bright pixels). The linear stretch applied is 0.0010-0.0025.


Figure 6: RGB color composite combination, called ”Enhanced Color Mosaic“, R: PC2, G: PC1, B: 430/996nm. This RGB color composite combination is useful for identifying the main terrain units and feature present on Mercury surface, such as smooth plains in yellow, pyroclastic deposits (faculae) in orange, intercrater plains in blue, and crater rays in light cyan. For this reason this map represents one of the principal RGB color combination considered by the MESSENGER team (e.g. Denevi et al., 2009, Murchie et al., 2015). The linear stretches applied are PC2: 0.03 - 0.10, PC1: 0.10 - 0.45, 430/996nm: 1.6 - 2.4.

Figure 7: RGB false color mosaic: Hokusai quadrangle, R: 996 nm, G: 750 nm, B: 430 nm. This RGB combination emphasizes the color variations on Mercury surface, showing regions where the reflectance at longer (red), intermediate (green) and shorter (blue) wavelengths dominates. The linear stretches are 996 nm: 0.040 - 0.130, 747 nm: 0.060-0.215, 430 nm: 0.080 - 0.245.

 

Figure 8 : RGB "Clementine Color Mosaic" color assignments similar to those used for the Clementine maps of the Moon (Pieters, C.M. et al., 1994): RED = R(748 nm)/R(430 nm), GREEN = R(748 nm)/R(828 nm), and BLUE = R(430 nm)/R(748 nm).  This color combination can introduce information related to the maturity, mafic or glassic components, secondary elements locally concentrated. In Hokusai mosaic, this color composite highlights regions with differing spectral characteristics. Yellow areas typically represent high-reflectance material and blue areas indicate low-reflectance material and crater rays. Green areas represent regions with higher intermediate slope, and red areas have steeper visible slopes relative to bluer areas. The orange/red regions are those with the steepest visible slopes. The linear stretch applied are R(748 nm)/R(430 nm): 1.47 - 1.83, R(748 nm)/R(828 nm): 0.83 - 0.94, R(430 nm)/R(748 nm): 0.54 - 0.68.


References

 

J.N. Cuzzi et al. 2009. Ring particle composition and size distribution, in Saturn from Cassini-Huygens, edited by M.K. Dougherty, L.W. Esposito, and S.M. Krimigis, Springer, Berlin, 459-509, Doi:10.1007/978-1-4020-9217-6 15

 

B.W. Denevi et al. 2009. The evolution of Mercury’s crust: A global perspective from MESSENGER. Science 324, 613–618. Doi: 10.1126/science.1172226

 

B.W. Denevi et al. 2018. Calibration, Projection, and Final Image Products of MESSENGER’s Mercury Dual Imaging System. Space Sci. Rev., 214:2. Doi: 10.1007/s11214-017-0440-y

 

G. Filacchione et al. 2012. Saturn’s icy satellites and rings investigated by Cassini–VIMS: III – Radial compositional variability. Icarus, 200, 1064-1096.  Doi: 10.1016/j.icarus.2012.06.040

 

S.E. Hawkins et al. 2007. The Mercury Dual Imaging System on the MESSENGER spacecraft. Space Sci. Rev., 131, 247–338. Doi: 10.1007/s11214-007-9266-3

 

R.L. Klima et al. 2018. Global distribution and spectral properties of low-reflectance material on Mercury. Geoph. Res. Lett. 45, 2945–2953. Doi: 10.1002/2018GL077544

 

A. Lucchetti et al. in press. Mercury Hollows as Remnants of Original Bedrock Materials and Devolatilization Processes: a Spectral Clustering and Geomorphological Analysis. J.G.R. Planets, Doi: 10.1029/2018JE005722

 

S.L. Murchie et al. 2015. Orbital multispectral mapping of Mercury with the MESSENGER Mercury Dual Imaging System: Evidence for the origins of plains units and low-reflectance material. Icarus 254, 287–305. Doi: 10.1016/j.icarus.2015.03.027

 

C.M. Pieters et al., 1994. A sharper view of impact craters from Clementine data, Science, 266, 1844-1848. Doi: 10.1126/science.266.5192.1844

 

F. Vilas et al. 2016. Mineralogical indicators of Mercury's hollows composition in MESSENGER color observations. Geoph. Res. Lett., Doi: 10.1002/2015GL067515


Annex

Map template used to project the images with ISIS3:

 

Group = Mapping

  ProjectionName     = Equirectangular

  CenterLongitude    = 45

  CenterLatitude     = 43.75

  TargetName         = Mercury

  EquatorialRadius   = 2439700.0 <meters>

  PolarRadius        = 2439700.0 <meters>

  LatitudeType       = Planetocentric

  LongitudeDirection = PositiveEast

  LongitudeDomain    = 360

  PixelResolution    = 450.0 <meters/pixel>

End_Group

End

  

N.B.: The map conversion from equirectangular to lambert conformal projection has been done by using QuantumGIS:

+proj=lcc +lat_1=30 +lat_2=58 +lat_0=43.75 +lon_0=45 +x_0=0 +y_0=0 +a=2439700 +b=2439700 +units=m +no_defs


The data are available at the following link:

https://cloud.planmap.eu/index.php/apps/files/?dir=/Planmap/WP4&fileid=184


 

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