Constraints on the volatile distribution within Shackleton crater at the lunar south pole

Maria T. Zuber (), James W. Head, David E. Smith, Gregory A. Neumann, Erwan Mazarico, Mark H. Torrence, Oded Aharonson, Alexander R. Tye, Caleb I. Fassett, Margaret A. Rosenburg and H. Jay Melosh
Additional contact information
Maria T. Zuber: Atmospheric and Planetary Sciences, Massachusetts Institute of Technology
James W. Head: Brown University
David E. Smith: Atmospheric and Planetary Sciences, Massachusetts Institute of Technology
Gregory A. Neumann: NASA/Goddard Space Flight Center
Erwan Mazarico: Atmospheric and Planetary Sciences, Massachusetts Institute of Technology
Mark H. Torrence: Stinger Ghaffarian Technologies
Oded Aharonson: California Institute of Technology
Alexander R. Tye: Brown University
Caleb I. Fassett: Brown University
Margaret A. Rosenburg: California Institute of Technology
H. Jay Melosh: Purdue University

Nature, 2012, vol. 486, issue 7403, 378-381

Abstract: Observations from the Lunar Orbiter Laser Altimeter reveal the Moon’s Shackleton crater to be an ancient, unusually well-preserved simple crater whose interior walls are younger than its floor and rim; the relative brightness of the floor at 1,064 nanometres is most readily explained by minimal volatile accumulation since crater formation and decreased space weathering due to permanent shadow.

Date: 2012
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DOI: 10.1038/nature11216

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