162 Planetary Geologic Mapping Across the Solar System
We invite abstracts that showcase planetary geologic maps, discuss mapping strategies, and leverage map-based investigations of planetary surfaces at multiple scales.
Tuesday, 21 October 2025
8:00 AM - 12:00 PM
HBGCC, 214B
A Regional Geologic Map of the Marius Hills Pit
Paper number: 162-7
Program: Technical Sessions
Time: 9:35 AM – 9:50 AM
Authors
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Erin Leonard Presenting AuthorJet Propulsion Laboratory, California Institute of Technology, Pasadena, CA
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Jennifer ScullyJet Propulsion Laboratory, California Institute of Technology, Pasadena, CA
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Catherine ElderJet Propulsion Laboratory, California Institute of Technology, Pasadena, CA
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Abigail FraemanJet Propulsion Laboratory, California Institute of Technology, Pasadena, CA
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Laura KerberJet Propulsion Laboratory, California Institute of Technology, Pasadena, CA
Abstract
The Marius Hills region on the Moon is located near the center of Oceanus Procellarum and primarily west-northwest of Marius Crater. The region consists of a series of isolated and clusters of hills, and a major ridge system running approximately north-south stretching for >1000 km. The Marius Hills pit was the first lunar pit discovered and is hypothesized to be an opening into a lava tube, making it a site of particular interest for future robotic and human exploration. While there have been several studies of the Marius Hills region as a whole, a regional geologic map of the Marius Hills specifically centered on the pit area is needed to provide geologic context for any future exploration. We defined the map region as a 1-degree square, designed to have the Marius Hills pit near the center and extend to contain prominent nearby domes and part of the ridge system. The geologic map is at a scale of 1:100,000 with a digital mapping scale of 1:25,000. Vertex spacing is 20 meters. The minimum size of a unit is ~1 km and the minimum point or linear feature is ~250 m in width. Geologic units are identified using the LROC NAC images and Digital Terrain Model (DTM), LOLA-SELENE DTM, and Clementine UVVIS Hybrid mosaic datasets. The pit is located within a rille, near a sharp ~90-degree bend in the rille. To date, we have identified several geologic units in this region, including dome material, smooth plains material, crater ejecta material, and rille wall material. Additionally, we have identified linear features including rille wall, inferred rille wall, trough, and ridge crest. With the completion of the geologic map, we will construct a geologic history of the region and place the Marius Hills pit in geologic context.
Geological Society of America Abstracts with Programs. Vol. 57, No. 6
doi: 10.1130/abs/2025AM-413803
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