et al.

δD (‰ V-SMOW)
400
300
200
100
0
-100
-200
0 -200
0
0 100 200 300 400 500 600 700 800 900 1000 0 200 400 600 800 1000 1200
Temperature (°C)
Temperature (°C)
Fig. 8. Plots of dD versus temperature, showing data for the NWA 7034 bulk sample during stepped heating. The horizontal solid lines represent the
temperature intervals; circles are mid-interval temperatures. The two plots represent two aliquots of the NWA 7034 sample.
in origin. Its major, minor, trace, and isotopic
chemistry is inconsistent with originating from
Earth, the Moon, Venus, or Mercury, and it is
most similar to rocks from Mars. Nonetheless,
NWA 7034 is uniquely different from any other
known martian meteorite, as it is the most geochemically
enriched rock from Mars found to
date. Moreover, the bulk chemistry of NWA 7034
is strikingly similar to recently collected orbital
and lander data collected at the martian surface,
allowing for a direct link between a martian meteorite
and orbital and lander spacecraft data from
Mars. NWA 7034 is also distinct from the SNC
meteorites because it has higher bulk d 18 Oand
D 17 O, suggesting the existence of multiple oxygen
isotopic reservoirs within the lithologic portion
of Mars.
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Acknowledgments: We thank J. Piatek for acquiring the
NWA 7034 specimen and for his generous donation to the
UNM Meteorite Museum, which has enabled this research
and sample allocations for future research on NWA 7034.
We also thank M. Spilde, V. Atudorei, and J. Connolly at the
University of New Mexico for assistance with data collection.
Supported by NASA Cosmochemistry Program grants
NNX11AH16G (C.B.A.) and NNX11AG76G (F.M.M.). S.M.E.
acknowledges support from the New Mexico Space Grant
Consortium, NASA Earth and Space Science Fellowship
NNX12AO15H, and NASA Cosmochemistry grant NNX10AI77G
to Charles K. Shearer. M.H.T. and R.S. acknowledge NSF
award ATM0960594, which allowed the development of an
analytical technique to measure oxygen triple isotopic
composition of small (