f Integrating Diverse Datasets to Assess Approaches for Characterizing Mare Basalts S. R. Deitrick 1,2,3 , S. J. Lawrence 3 1 Lunar and Planetary Institute, Houston, TX, USA 2 Jacobs, Houston, TX, USA 3 Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX, USA REFERENCES [1] Lawrence S. J. et al. (2013) JGR, 118, 615-634. [2] Heather D. J. et al. (2003) JGR, 108, E3, 5017. [3] Eliason et al. (1999) LPSC XXX. [4] Sato H. et al. (2014) JGR, 119, 1775-1805. Figure 1. a) Regional view of MHVC morphology. b) Global WAC lunar nearside mosaic. Red box indicates location of MHVC. b a 50 km Figure 2. a) Manually mapped color unit boundaries (yellow lines) overlain onto Clementine 5-band color ratio base map. b) WAC color unit boundaries (red lines) overlain onto WAC 7-band multispectral base map. Figure 4. a) Elevation profile of trough at base of SE flank of dome A. b) Profile of trough at the base of the southwestern flank of dome B. c) Profile of trough on southeastern flank of dome B. d) and e) Profiles of basalt flow contact expressions in the mare plains of MHVC. Elevation profiles were extracted from NAC DTMs. All units are in meters. a a b b 50 km 5 km A B C Figure 5. Clementine TiO 2 (a) and FeO (b) unit boundaries (green and blue lines, respectively) for the LOC featured mosaic. Figure 3. a) WAC color unit boundaries (red lines) overlain onto WAC synthetic hillshade data to highlight boundary/topography correlation. b) WAC color unit boundaries (red) and correlated LOC NAC featured mosaic morphology lines (green) overlain onto LOC featured mosaic with volcanic domes of interest labeled with arrows. a a b b 10 km 10 km 10 km 10 km Distance (m) E l e v a t i o n ( m ) The morphologies seen in the NAC frames that parallel the boundaries indicate that WAC color has great potential for identifying mare basalt units. When confirmed with elevation profiles from NAC DTMs, morphologies show embayment of the observed domes, indicating that the mare basalts erupted after dome formation. This implies that the domes are older than the flows and the volcanic activity on the plateau was a complex process [1]. This indicates that not only are the techniques used in this study useful for mapping distinct mare basalt units with WAC data, but will also be helpful in determining relative stratigraphy and ages of the domes and surrounding mare basalts in the MHVC. DISCUSSION The Marius Hills Volcanic Complex (MHVC) (Fig. 1), the largest single concentration of volcanic features on the Moon (~35,000 km 2 ) [1], represents a significant period of lunar magmatism thought to have taken place during the Imbrian (~3.3 Ga) through Eratosthenian (~2.5 Ga) periods [1,2]. Previous studies of the MHVC utilizing Clementine Ultraviolet/Visible (UVVIS) camera, Kaguya Multiband Imager (MI), and Moon Mineralogy Mapper (M 3 ) data have found that the volcanic domes and surrounding mare basalts are compositionally indistinguishable, indicating similar eruption times [1,2], although the domes are embayed by younger mare basalts [1]. This research utilizes new Lunar Reconnaissance Orbiter Camera (LROC) data to re-evaluate the composition of the volcanic domes and surrounding mare basalts in the MHVC. Through this, the compositions and relative ages of the domes and the surrounding flows can be determined. INTRODUCTION AND OBJECTIVES 1. Many domes outlined/crosscut by WAC boundaries (Fig. 3a) 2. A large majority of the boundaries mapped from the WAC base map correlate with morphologies that are evident in the NAC frames (Fig. 3b) 3. Evidence of morphology changes were found to correlate with the boundaries near the flanks of the domes that were observed and show possible embayment of the mare basalt flows on the flanks (Fig. 4a-e) 4. Color units derived from WAC base map correlate strongly with units evident in the Clementine TiO 2 and FeO maps (Fig. 5a,b) 5. The boundaries mapped from the WAC also correlated very well with the mare basalt units mapped by [2], but in general are more detailed and complex RESULTS 1. Color unit boundaries manually mapped using Clementine 5-band color ratio [3] and LROC Wide Angle Camera (WAC) 7- band multispectral [4] base maps (Fig. 2a,b) 2. Boundaries iteratively compared to each other to assess differences between them and were then compared to WAC hillshade and morphology data to assess the quality of correlations between color unit boundaries and topographic features (Fig. 3a) 3. Five LROC Narrow Angle Camera (NAC) featured mosaics along with 30 NAC image pairs were analyzed in order to associate WAC boundaries with morphologies evident in the high-resolution NAC frames (Fig. 3b) 4. Correlated morphologies were mapped and confirmed by taking elevation profiles of NAC Digital Terrain Models (DTMs) (Fig. 4a-e) 5. WAC boundaries compared with Clementine TiO 2 , FeO, (Fig. 5a,b), OMAT data, and the mare basalt units mapped by [2] METHODS 50 km b b 50 km 50 km a d d D D’ d 120 e e E’ E e 500 A A’ a a 400 B B’ b b 600 C C’ c c 700
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fIntegrating Diverse Datasets to Assess Approaches for Characterizing
Mare Basalts S. R. Deitrick1,2,3, S. J. Lawrence3
1Lunar and Planetary Institute, Houston, TX, USA 2Jacobs, Houston, TX, USA 3Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX, USA
REFERENCES[1] Lawrence S. J. et al. (2013) JGR, 118, 615-634. [2] Heather D. J. et al. (2003) JGR, 108, E3, 5017. [3] Eliason et al. (1999) LPSC XXX. [4] Sato H. et al. (2014) JGR, 119, 1775-1805.
Figure 1. a) Regional view of MHVC morphology. b) Global WAC lunar nearside mosaic. Red box indicates location of MHVC.
ba
50 km
Figure 2. a) Manually mapped color unit boundaries (yellow lines) overlain onto Clementine 5-band color ratio base map. b) WAC color unit boundaries (red lines) overlain onto WAC 7-band multispectral base map.
Figure 4. a) Elevation profile of trough at base of SE flank of dome A. b) Profile of trough at the base of the southwestern flank of dome B. c) Profile of trough on southeastern flank of dome B. d) and e) Profiles of basalt flow contact expressions in the mare plains of MHVC. Elevation profiles were extracted from NAC DTMs. All units are in meters.
aabb
50 km
5 km
AA
BBCC
Figure 5. Clementine TiO2 (a) and FeO (b) unit boundaries (green
and blue lines, respectively) for the LOC featured mosaic.
Figure 3. a) WAC color unit boundaries (red lines) overlain onto WAC synthetic hillshade data to highlight boundary/topography correlation. b) WAC color unit boundaries (red) and correlated LOC NAC featured mosaic morphology lines (green) overlain onto LOC featured mosaic with volcanic domes of interest labeled with arrows.
aa bb
10 km10 km 10 km10 km
Distance (m)
Ele
vatio
n (m
)
The morphologies seen in the NAC frames that parallel the boundaries indicate that WAC color has great potential for identifying mare basalt units. When confirmed with elevation profiles from NAC DTMs, morphologies show embayment of the observed domes, indicating that the mare basalts erupted after dome formation. This implies that the domes are older than the flows and the volcanic activity on the plateau was a complex process [1]. This indicates that not only are the techniques used in this study useful for mapping distinct mare basalt units with WAC data, but will also be helpful in determining relative stratigraphy and ages of the domes and surrounding mare basalts in the MHVC.
DISCUSSION
The Marius Hills Volcanic Complex (MHVC) (Fig. 1), the largest single concentration of volcanic features on the Moon (~35,000 km2) [1], represents a significant period of lunar magmatism thought to have taken place during the Imbrian (~3.3 Ga) through Eratosthenian (~2.5 Ga) periods [1,2]. Previous studies of the MHVC utilizing Clementine Ultraviolet/Visible (UVVIS) camera, Kaguya Multiband Imager (MI), and Moon Mineralogy Mapper (M3) data have found that the volcanic domes and surrounding mare basalts are compositionally indistinguishable, indicating similar eruption times [1,2], although the domes are embayed by younger mare basalts [1].
This research utilizes new Lunar Reconnaissance Orbiter Camera (LROC) data to re-evaluate the composition of the volcanic domes and surrounding mare basalts in the MHVC. Through this, the compositions and relative ages of the domes and the surrounding flows can be determined.
INTRODUCTION AND OBJECTIVES
1. Many domes outlined/crosscut by WAC boundaries (Fig. 3a)
2. A large majority of the boundaries mapped from the WAC base map correlate with morphologies that are evident in the NAC frames (Fig. 3b)
3. Evidence of morphology changes were found to correlate with the boundaries near the flanks of the domes that were observed and show possible embayment of the mare basalt flows on the flanks (Fig. 4a-e)
4. Color units derived from WAC base map correlate strongly with units evident in the Clementine TiO2 and FeO maps (Fig. 5a,b)
5. The boundaries mapped from the WAC also correlated very well with the mare basalt units mapped by [2], but in general are more detailed and complex
RESULTS
1. Color unit boundaries manually mapped using Clementine 5-band color ratio [3] and LROC Wide Angle Camera (WAC) 7-band multispectral [4] base maps (Fig. 2a,b)
2. Boundaries iteratively compared to each other to assess differences between them and were then compared to WAC hillshade and morphology data to assess the quality of correlations between color unit boundaries and topographic features (Fig. 3a)
3. Five LROC Narrow Angle Camera (NAC) featured mosaics along with 30 NAC image pairs were analyzed in order to associate WAC boundaries with morphologies evident in the high-resolution NAC frames (Fig. 3b)
4. Correlated morphologies were mapped and confirmed by taking elevation profiles of NAC Digital Terrain Models (DTMs) (Fig. 4a-e)
5. WAC boundaries compared with Clementine TiO2, FeO, (Fig. 5a,b), OMAT data, and the mare basalt units mapped by [2]
METHODS
50 km
bb
50 km50 km
a
dd
D D’
d
120
ee
E’E
e
500
A A’
aa
400
B B’
bb
600
C C’
cc
700
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