'Dome Alone': A Lunar Mystery Near Herodotus Crater | NASA LRO
The Herodotus Omega dome rises gradually above the surrounding mare. The large, irregularly shaped depression towards the right is likely a summit pit. Image width is 7.5 kilometers, centered at 20.25°N, 309.93°E. The dark mare surface of Oceanus Procellarum is visible, along with its scars of many bright impact craters. The possible summit pit of the dome stands out as a large S-shaped depression.
This view shows the same area as the previous image, but is overlaid with graduated colors to indicate the elevation of the surface. The outside of the dome's boundaries is colored light blue, which gradually changes to dark red as the elevation increases towards the center of the dome, before sharply falling to dark blue at the bottom of the possible summit pit. This color-shaded digital terrain model DTM helps reveal the relief of the Herodotus Omega dome. The elevation ranges from -1,916 m (blue) to -1,523 (red). Image width is 7.5 kilometers, centered at 20.25°N, 309.93°E.
Although active volcanism on the Moon largely ceased over a billion years ago, remnants of ancient volcanic activity persist in many landforms we still see today. These include the lunar maria, as well as rilles, cones, and domes. The focus of this featured image post is the dome, Herodotus Omega, located in central Oceanus Procellarum ("Ocean of Storms") on the western lunar nearside (20.25°N, 309.93°E). Unlike most lunar domes, typically found in clusters, Herodotus Omega stands alone. While the full extent of this dome is difficult to discern in the above image due to its relatively gentle slope and low relief, its diameter measures about 12 kilometers, and it rises to a maximum height of about 220 meters above the surrounding mare surface. As is typical for lunar domes, Herodotus Omega is named by appending a Greek letter to the name of a nearby major crater—Herodotus crater, located about 70 kilometers north of the dome.
Scientists estimate that lunar domes formed over a roughly one-billion year period beginning around 3.7 billion years ago. Although the specific origin of Herodotus Omega remains unknown, it exhibits characteristics similar to other domes found throughout the lunar maria. Mare domes are much more common than non-mare domes, and can be divided into seven distinct classes. Although Herodotus Omega has not been officially classified, characteristics of its (likely) summit pit, cross-sectional shape, diameter, and slope suggest that it belongs to Class 1 or 2 (Head and Gifford, 1980). Like most mare domes, Herodotus Omega also exhibits relatively low albedo (the fraction of sunlight that is diffusely reflected by a body) when compared to non-mare domes, such as those found in the Gruithuisen region.
The western mare features widespread evidence of past volcanic activity. The domes of these lunar seas have long been of interest to the scientific community. NASA once even considered the Hortensius Domes, a group of mare domes in nearby Mare Insularum ("Sea of Islands"), as a possible target for crewed exploration under the Constellation program. However, the program's unfortunate cancellation in 2010 halted those plans. While we hope that Herodotus Omega and the other domes of the western mare eventually welcome their first robotic or human explorer, they currently stand silently awaiting their arrival.
Image Credit: NASA's Lunar Reconnaissance Orbiter/GSFC/Arizona State University
Article Credit: Steven Nystrom
Release Date: July 16, 2025
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