CRISM NEXT GENERATION MARS GLOBAL MULTISPECTRAL … · SPECTRAL PARAMETER MAPPING. F. P. Seelos1,...
2
CRISM NEXT GENERATION MARS GLOBAL MULTISPECTRAL MAP – HYDRATED MINERALOGY SPECTRAL PARAMETER MAPPING. F. P. Seelos 1 , S. F. A. Cartwright 1 , G. Romeo 1 , and S. L. Murchie 1 , Johns Hopkins Applied Physics Laboratory, 11100 Johns Hopkins Rd, Laurel, MD 20723, [email protected]. Introduction: The Compact Reconnaissance Im- aging Spectrometer for Mars (CRISM) [1] is a visible through short-wave infrared hyperspectral imaging spectrometer (VNIR S-detector: 364-1055 nm; IR L- detector: 1001-3936 nm; 6.55 nm sampling) that has been in operation on the Mars Reconnaissance Orbiter (MRO) [2] since 2006. Over the course of the MRO mission CRISM has acquired over 320,000 individual mapping observation segments (mapping strips) with a variety of observing modes and data characteristics (VNIR/IR; ~100/200 m/pxl; multi-/hyper-spectral band selection – Table 1) over a wide range of observing conditions (atmospheric state, observation geometry, instrument state). With the retirement of the CRISM cryosystem in early 2018, the acquisition of IR (L- detector) data has been suspended with global IR map- ping coverage at ~87%. In addition, the primary CRISM mapping mosaic product suite that supports hydrated mineral mapping - Multispectral Reduced Data Record (MRDR) map tiles - sources the multi- spectral survey (MSP) and hyperspectral survey (HSP) data sets which are now closed. Map Tile Assembly: The MRDR data processing and tile assembly workflow is tasked with taking as input a set of MSP and HSP observations that intersect a given map tile area (Figure 1A), and producing as output spectral, parameter, and browse mosaic prod- ucts where the spatial/spectral structure is self- consistent across the mosaic and reflective of surface spectral characteristics rather than observation circum- stances (e.g. atmospheric optical depth, observation geometry) or instrument state (e.g. detector operating temperature) (Figure 1B). The two most significant challenges pertain to the marked increase in the promi- nence and complexity of instrument noise present in CRISM IR data acquired at elevated detector tempera- tures (observations acquired since mid-2009), and the limited availably of CRISM-derived atmospheric state information (sourced from CRISM EPF observations through late 2012). The noise remediation challenges unique to the CRISM IR mapping data are accommo- dated by a procedure adapted from the hyperspectral data filtering approach employed in the standard pro- cessing of CRISM targeted observations [3]. The cor- rection of the observed top-of-atmosphere (TOA) spec- tral radiance to atmospherically and photometrically corrected surface spectral reflectance takes one of two paths: a radiative transfer (RT) model based correction is applied to observations where high fidelity atmos- pheric state information is available, and empirical corrections are applied to observations where it is not. These alternate pathways necessitate an empirical mo- saic-wide radiometric optimization that serves to trans- form the empirically corrected TOA data to the RT- established radiometric framework [4]. Hydrated Mineral Spectral Parameter Map- ping: The utility of the expanded CRISM MRDR data processing and tile assembly for hydrated mineral mapping is illustrated in Figure 1 as a series of D2300 spectral parameter maps for CRISM map tile T1250 (which includes the Mars 2020 landing and field sites). The D2300 spectral parameter encodes the spectral drop-off at 2300 nm and highlights pixels where the spectral structure may be consistent with hydroxylated Fe/Mg-silicate and/or Mg-carbonate mineralogy [5]. The full T1250 tile extent is shown in Figure 1A and 1B, and a sub-area that includes Jezero Crater is shown in Figure 1C and 1D. The D2300 parameter map has been calculated from as-acquired apparent I/F data in Figure 1A and 1C, and from the noise-remediated, fully corrected, and radiometrically-reconciled surface spectral reflectance MRDR information in Figure 1B and 1D. The improved inter-observation parameter continuity can be seen in Figure 1A/1B, and the effects of the multispectral noise remediation can be seen in Figure 1C/1D. The MRDR workflow spectral information pro- vides for the calculation of parameter maps of suffi- cient quality and internal consistency to support GIS mapping efforts (Figure 1B, Figure 1D). Further spec- tral data processing and analysis of the assembled map projected spectral and parameter mosaic products are also possible, including supervised and unsupervised classification. This type of high-level processing and analysis of information derived from the constituent mapping observations comprising the tile mosaic would be impractical in the absence of the noise reme- diation and radiometric reconciliation that key the MRDR data processing workflow. In support of Mars In-Situ Resource Utilization (ISRU) considerations, the CRISM MRDR map tile data processing is being taken to scale with the goal of generating near-global maps of spectral parameters that are consistent with and/or indicative of various classes of hydrated mineralogy (Table 2). An overview of the updated MRDR data processing and tile assem- bly procedures as well as the status toward the global parameter mapping effort will be presented. References: [1] Murchie S. L. et al. (2007) JGR, 112, E05, S03. [2] Zurek R. W. and Smrekar S. E. (2007) JGR, E05, S01. [3] Seelos F. P. (2009) AGU Fall Meeting, P23A-1234. [4] Seelos F. P. et al. (2018) LPS XLIX, Abstract #2325. [5] Viviano-Beck C. E. et al. (2014) JGR, 119, 06, 1403–1431. 2635.pdf 50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132)
Transcript of CRISM NEXT GENERATION MARS GLOBAL MULTISPECTRAL … · SPECTRAL PARAMETER MAPPING. F. P. Seelos1,...
CRISM NEXT GENERATION MARS GLOBAL MULTISPECTRAL MAP – HYDRATED MINERALOGY SPECTRAL PARAMETER MAPPING. F. P. Seelos1, S. F. A. Cartwright1, G. Romeo1, and S. L. Murchie1, Johns Hopkins Applied Physics Laboratory, 11100 Johns Hopkins Rd, Laurel, MD 20723, [email protected].
Introduction: The Compact Reconnaissance Im-
aging Spectrometer for Mars (CRISM) [1] is a visible through short-wave infrared hyperspectral imaging spectrometer (VNIR S-detector: 364-1055 nm; IR L-detector: 1001-3936 nm; 6.55 nm sampling) that has been in operation on the Mars Reconnaissance Orbiter (MRO) [2] since 2006. Over the course of the MRO mission CRISM has acquired over 320,000 individual mapping observation segments (mapping strips) with a variety of observing modes and data characteristics (VNIR/IR; ~100/200 m/pxl; multi-/hyper-spectral band selection – Table 1) over a wide range of observing conditions (atmospheric state, observation geometry, instrument state). With the retirement of the CRISM cryosystem in early 2018, the acquisition of IR (L-detector) data has been suspended with global IR map-ping coverage at ~87%. In addition, the primary CRISM mapping mosaic product suite that supports hydrated mineral mapping - Multispectral Reduced Data Record (MRDR) map tiles - sources the multi-spectral survey (MSP) and hyperspectral survey (HSP) data sets which are now closed.
Map Tile Assembly: The MRDR data processing and tile assembly workflow is tasked with taking as input a set of MSP and HSP observations that intersect a given map tile area (Figure 1A), and producing as output spectral, parameter, and browse mosaic prod-ucts where the spatial/spectral structure is self-consistent across the mosaic and reflective of surface spectral characteristics rather than observation circum-stances (e.g. atmospheric optical depth, observation geometry) or instrument state (e.g. detector operating temperature) (Figure 1B). The two most significant challenges pertain to the marked increase in the promi-nence and complexity of instrument noise present in CRISM IR data acquired at elevated detector tempera-tures (observations acquired since mid-2009), and the limited availably of CRISM-derived atmospheric state information (sourced from CRISM EPF observations through late 2012). The noise remediation challenges unique to the CRISM IR mapping data are accommo-dated by a procedure adapted from the hyperspectral data filtering approach employed in the standard pro-cessing of CRISM targeted observations [3]. The cor-rection of the observed top-of-atmosphere (TOA) spec-tral radiance to atmospherically and photometrically corrected surface spectral reflectance takes one of two paths: a radiative transfer (RT) model based correction is applied to observations where high fidelity atmos-pheric state information is available, and empirical corrections are applied to observations where it is not. These alternate pathways necessitate an empirical mo-
saic-wide radiometric optimization that serves to trans-form the empirically corrected TOA data to the RT- established radiometric framework [4].
Hydrated Mineral Spectral Parameter Map-ping: The utility of the expanded CRISM MRDR data processing and tile assembly for hydrated mineral mapping is illustrated in Figure 1 as a series of D2300 spectral parameter maps for CRISM map tile T1250 (which includes the Mars 2020 landing and field sites). The D2300 spectral parameter encodes the spectral drop-off at 2300 nm and highlights pixels where the spectral structure may be consistent with hydroxylated Fe/Mg-silicate and/or Mg-carbonate mineralogy [5]. The full T1250 tile extent is shown in Figure 1A and 1B, and a sub-area that includes Jezero Crater is shown in Figure 1C and 1D. The D2300 parameter map has been calculated from as-acquired apparent I/F data in Figure 1A and 1C, and from the noise-remediated, fully corrected, and radiometrically-reconciled surface spectral reflectance MRDR information in Figure 1B and 1D. The improved inter-observation parameter continuity can be seen in Figure 1A/1B, and the effects of the multispectral noise remediation can be seen in Figure 1C/1D.
The MRDR workflow spectral information pro-vides for the calculation of parameter maps of suffi-cient quality and internal consistency to support GIS mapping efforts (Figure 1B, Figure 1D). Further spec-tral data processing and analysis of the assembled map projected spectral and parameter mosaic products are also possible, including supervised and unsupervised classification. This type of high-level processing and analysis of information derived from the constituent mapping observations comprising the tile mosaic would be impractical in the absence of the noise reme-diation and radiometric reconciliation that key the MRDR data processing workflow.
In support of Mars In-Situ Resource Utilization (ISRU) considerations, the CRISM MRDR map tile data processing is being taken to scale with the goal of generating near-global maps of spectral parameters that are consistent with and/or indicative of various classes of hydrated mineralogy (Table 2). An overview of the updated MRDR data processing and tile assem-bly procedures as well as the status toward the global parameter mapping effort will be presented.
References: [1] Murchie S. L. et al. (2007) JGR, 112, E05, S03. [2] Zurek R. W. and Smrekar S. E. (2007) JGR, E05, S01. [3] Seelos F. P. (2009) AGU Fall Meeting, P23A-1234. [4] Seelos F. P. et al. (2018) LPS XLIX, Abstract #2325. [5] Viviano-Beck C. E. et al. (2014) JGR, 119, 06, 1403–1431.
2635.pdf50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132)
77°E
77°E
19°N
18°N
20 km
77°E
77°E
19°N
18°N
20 km
77°E
77°E
19°N
18°N
20 km
77°E
77°E
19°N
18°N
20 km
80°E
80°E
78°E
78°E
76°E
76°E
22°N
20°N
18°N
50 km50 km
80°E78°E76°E
22°N
20°N
18°N
50 km
80°E78°E76°E
50 kmA B
C D
Applicable ParametersBD2210_2, BD1900_2D2300, BD1900_2BD1900_2, SINDEX_2BD2100, SINDEX_2BD2210_2, BD2250, (BD1900_2)D2300, BD2500_2, MIN2295_2480
PhaseAl-smectiteFe/Mg-smectitePolyhydrated sulfateMonohydrated sulfateHydrated silicaHydrated carbonate
Class
Type
Pixel Size
(m/pxl)
VNIR
Bands
IR
Bands
Observations
[Target IDs]
VNIR
Segments
IR
Segments
MSP ~200 19 55 41786 63011 63091
MSW ~100 19 55 2557 2565 2562
HSP ~200 107 154 16419 20119 20176
HSV ~200 107 N/A 52758 81547 N/A
MSV ~100 90 N/A 50465 69805 N/A
Total: 163985 237047 85829
Table 1. CRISM mapping data acquired through 01/08/2019 (2019-008).
Table 2. Selected hydrated phases and the key CRISM spectral parameters employed to map their spatial distribution.
Figure 1. Comparison of D2300 parameter mapping products for CRISM map tile T1250. (A) Calculated from observed I/F spectral data; (B) Calculated from fully corrected and radiometrically reconciled spectral data. Location of (C,D) indicated by black box in (A,B); Jezero Crater Mars 2020 landing ellipse indicated in white. Parameter data shown at 20% transparency over THEMIS Day IR basemap.
2635.pdf50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132)
