Temporal and spatial variability of lunar hydration as observed by the deep impact spacecraft

Science

Volumn 326, Issue 5952, 2009, Pages 565-568

  Sunshine, Jessica M ^a   Farnham, Tony L ^a   Feaga, Lori M ^a   Groussin, Olivier ^b   Merlin, Frédéric ^a   Milliken, Ralph E ^c   A'Hearn, Michael F ^a  

^a UNIVERSITY OF MARYLAND   (United States)

^b AIX MARSEILLE UNIVERSITÉ   (France)

^c CALIFORNIA INSTITUTE OF TECHNOLOGY   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

HYDROXYL GROUP; ION; WATER;

HYDRATION; MOON; NEAR INFRARED; PLANETARY ATMOSPHERE; SOLAR RADIATION; SOLAR WIND; SPATIOTEMPORAL ANALYSIS;

ARTICLE; BASALT; CHEMICAL COMPOSITION; HYDRATION; INFRARED RADIATION; MOON; PRIORITY JOURNAL; SOLAR RADIATION; SPACE FLIGHT; STEADY STATE; TEMPERATURE; WATER ABSORPTION; WATER SUPPLY;

EXTRATERRESTRIAL ENVIRONMENT; HYDROXYL RADICAL; MOON; SPACECRAFT; SPECTRUM ANALYSIS; SUNLIGHT; TEMPERATURE; TIME FACTORS; WATER;

EID: 70350490017     PISSN: 00368075     EISSN: 10959203     Source Type: Journal    
DOI: 10.1126/science.1179788     Document Type: Article

References (21)

1. D. L Hampton et al., Space Sci. Rev. 117, 43 (2005).
2. C. M. Pieters et al., Science 326, 568 (2009); published online 24 September 2009 (10.1126/science.1178658).
3. R. N. Clark, Science 326, 562 (2009); published online 24 September 2009 (10.1126/science.1178105).
4. O. Groussin et al., icarus 187, 16 (2007).
5. Materials and methods are available as supporting material on Science Online.
6. V. C. Farmer, The Infrared Spectra of Minerals (Mineralogical Society, monograph 4, London, 1974).
7. The position of this band depends in part on the cation attached to the hydroxyl. Although we cannot yet definitively identify the specific cation, the chemical composition of the Moon suggests it is likely Si, Al, Fe, Mg, Ca, or Na.
8. J. L. Bishop, C. M. Pieters, J. O. Edwards, Clays Clay Miner. 42, 702 (1994).
9. R. E. Milliken, thesis, Brawn University (2006).
10. W. M. Sinton, Icarus 6, 222 (1967).
11. D. F. Jouglet et al.J. Ceophys. Res. 112, E08S06 (2007).
12. R. E. Milliken et al., J. Ceophys. Res. 112, E08S07 (2007).
13. A. S. Rivkin et al., Meteorit. Planet. Sci. 38, 1383 (2003).
14. The depth of the 2.8-u.m band is calculated relative to the continuum. Equivalent width is the width in wavelength (jim) of a 100% absorption of the same total intensity as the overall absorption feature. It is calculated as the integrated area of the absorption feature below the continuum.
15. R. N. Clark, J. Ceophys. Res. 88, 10635 (1983).
16. R. N. Clark, P. G. Lucey, J. Ceophys. Res. 89, 6341 (1984).
17. R. E. Milliken, J. F. Mustard, Icarus 189, 550 (2007).
18. B. W. Hapke, Theory of Reflectance and Emittance Spectroscopy (Cambridge Univ. Press, Cambridge, UK, 1983).
19. G. Gloeckler et al., Eos Trans. AGU 89, U12A-03 (2008).
20. D. H. Crider, R. R. Vondrak, Adv. Space Res. 30, 1869 (2002).
21. EPOXI, the Deep Impact extended mission, is supported by the NASA Discovery Program under contract NNM07AA99C to the University of Maryland. The Deep Impact spacecraft and HRI-IR instrument were built by Ball Aerospace. We gratefully acknowledge the efforts and support of the EPOXI project team at the Jet Propulsion Laboratory in acquiring the data presented here and the continuing work of members of the EPOXI science team in improving the instrument calibration. Laboratory spectra of lunar soils were acquired with the NASA/Keck RELAB, a multi-user facility supported by NASA grant NNG06GJ31G. We also thank R. Clark for discussions on the spectral interpretations of the 3-u.m feature and L. McFadden for comments that improved this manuscript.