269-3 Lunar South Pole Boulders: A Database to Support Artemis Exploration

Session: Planetary Geologic Mapping Across the Solar System (Posters)

Poster Booth No.: 212

Presenting Author:

Anthony Lamantia

Authors:

Lamantia, Anthony M¹, Hollingsworth, Isaac L², Racek, Gillian M³, Adepoju, Olufunke Mary⁴, Lynam, Bridget R.⁵, Luna, Jeannette Wolak⁶

(1) Department of Earth Sciences, Tennessee Tech University, Cookeville, TN, USA, (2) School of Environmental Studies, Tennessee Tech University, Cookeville, TN, USA, (3) Department of Earth Sciences, Tennessee Tech University, Cookeville, TN, USA, (4) School of Environmental Studies, Tennessee Tech University, Cookeville, TN, USA, (5) Cookeville High School, Cookeville, TN, USA, (6) Department of Earth Sciences, Tennessee Tech University, Cookeville, TN, USA,

Abstract:

The mapping of surface features around the Lunar South Pole (LSP), including boulders, is critical for understanding the geological history and surface evolution of the moon, as well as supporting future Artemis exploration missions (robotic and crewed). Here, we present a comprehensive, regional analysis of more than 90,000 individual boulders and more than 750 boulder fields in the LSP. This study utilized high-resolution imagery derived from Lunar Reconnaissance Orbiter (LRO) Narrow Angle Camera (NAC) mosaics and Lunar Orbiter Laser Altimeter (LOLA) digital elevation models (DEMs).

The mapping effort for this boulder database was completed using ESRI’s ArcGIS Pro software. Our initial mapping was conducted manually by four mappers over a period of 12 weeks, March to May 2025. We used a consistent mapping scale of 1:1500 throughout the process as well as fine and coarse-scaled grid systems to navigate throughout the 9,878.51 square km map area. By manually identifying boulder locations and density, we classified boulders into three feature classes: individual boulders, boulder clusters, and boulder super clusters. Individual boulders were recorded as point features, while clusters and super clusters were delineated as polygons in ArcGIS Pro.

After the initial mapping effort, we conducted a quality control review to ensure data accuracy. We selected 17 random sub-regions that together represent 493.93 square km, comprising 5% of the total mapping area. Here, existing boulder features were evaluated and re-mapped by different mappers to verify accuracy in the database without repeating full coverage. The review focused on identifying three types of errors for boulder features: false negatives (missed boulders or clusters), false positives (misidentified boulders or clusters), and mapped feature offsets in meters. We note that extensive shadowing throughout the study area limits boulder detection; thus, we assume that our results underestimate the total boulder population in the LSP.

Our results broaden the spatial and geological context of boulder studies at the LSP. Our database provides a unique opportunity to conduct further analysis on lunar boulder evolution and how they relate to the surrounding ancient terrain. Additionally, our database can serve as an analog training dataset for future automated mapping efforts. Ultimately, this work is particularly relevant for surface process modeling, hazard analysis, and landing site selection for upcoming lunar missions, including human exploration initiatives.

Geological Society of America Abstracts with Programs. Vol. 57, No. 6, 2025

doi: 10.1130/abs/2025AM-10568

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