McKay, D. S., Gibson, E. K., Thomas-Keprta, K. L., Vali, H., Romanek, C. S., Clemett, S. J., Chillier, X. D. F., Maechling, C. R., Zare, R. N. (1996) Search for Past Life on Mars: Possible Relic Biogenic Activity in Martian Meteorite ALH84001. Science, 273 (5277). 924-930 doi:10.1126/science.273.5277.924

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	Sources of laboratory contamination fall into three categories: sample handling laboratory air and virtual leaks (that is sources of PAHs inside the μL 2 MS vacuum chamber). Possible contamination during sample preparation was minimized by performing nearly all sample preparation at the NASA-JSC meteorite curation facility. In cases where subsequent sample handling was required at Stanford all manipulation was performed in less than 15 minutes using only stainless steel tools previously rinsed and ultrasonicated in methanol and acetone. Dust-free gloves were worn at all times and work was performed on a clean aluminum foil surface. To quantify airborne contamination from exposure to laboratory air two clean quartz discs were exposed to ambient laboratory environments both at NASA-JSC and Stanford. Each disc received an exposure typical of that experienced subsequently by samples of ALH84001 during sample preparation. No PAHs were observed on either quartz disk at or above detection limits. Because contamination can depend on the physical characteristics of the individual sample (for example a porous material will likely give a larger contamination signal than a nonporous one) additional contamination studies have been previously conducted at Stanford [see (29)]. Briefly samples of the meteoritic acid residues of Barwell (L6) and Bishunpur (L3.1) were exposed to laboratory air for 1 and 4 days respectively. Barwell (L6) is known to contain no indigenous PAHs and none were observed on the exposed sample. Bishunpur (L3.1) in contrast contains a rich suite of PAHs but no discernible differences in signal intensities were observed between exposed and unexposed samples. To test for contamination from virtual leaks the μL 2 MS instrument was periodically checked using samples of Murchison (CM2) meteorite matrix whose PAH distribution has been previously well characterized. No variations in either signal intensity or distribution of PAHs were observed for μL 2 MS instrument exposure times in excess of 3 days. No sample of ALH84001 was in the instrument for longer than 6 hours. The μL 2 MS vacuum chamber is pumped by an oil-free system: two turbomolecular pumps and a liquid nitrogen-cooled cyropump.
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	We handpicked small chips in a clean bench from our curatorial allocation of ALH84001. Most chips were from a region near the central part of the meteorite and away from the fusion crust although for comparison we also looked at chips containing some fusion crust. For high-resolution work we used an Au-Pd coating estimated to be ∼2 nm thick in most cases. On some samples we used a thin (<1 nm) coating about 10 s with our sputter coater; these samples usually showed charging effects and could not be used for highest resolution imaging. We more typically used 20 to 30 s. For backscatter and chemical mapping we used a carbon coat of about 5 to 10 nm thick. We monitored the possible artifacts from the coating using other reference samples or by looking at fresh mineral surfaces on ALH84001. We could also estimate relative coating thicknesses by the size of the Au and Pd peaks in the energy dispersive x-ray spectrum. For our heaviest coating a slight crazing texture from the coating is barely visible at a magnification of 50 000× on the cleanest fresh grain surfaces. The complex textures shown in most of the SEM photographs are not artifacts of the coating process but are the real texture of the sample. We used a JEOL 35 CF and a Philips SEM with a field emission gun (FEG) at the JSC. The JEOL and Philips SEMs are equipped respectively with a PGT and Link EDS system. We achieved about 2.0 nm resolution at 30kV. Some images were also taken at lower kV ranging from 1 to 10 kV. In most cases the chips were coated after handpicking with no further treatment. For comparison several chips were ultrasonically cleaned for a few seconds in liquid Freon before coating to remove adhering dust. Several samples were examined uncoated at low kV. We carbon-coated and examined all of the surfaces analyzed for PAHs only after the PAH analyses had been completed.
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	Harzmetz C. P. , Wright I. P. , Pillinger C. T. in Workshop on the Mars Surface and Atmosphere Through Time, R. M. Haberle et al., Eds. (Tech. Rep. 92-02, Lunar and Planetary Institute, Houston, TX, 1992), pp. 67-68], a δ13C of 42 per mil for carbonate in ALH84001 can only be explained by a precipitation temperature around 0°C. This temperature estimate is compatible with an independent range of precipitation temperatures (0° to 80°C) based on the δ18O of the same carbonates (12). If carbon isotopes are distributed heterogeneously on Mars in isolated reservoirs (for example, the crust and atmosphere), precipitation temperature estimates based on stable isotopes are relatively unconstrained. This is probably not the case, though, as other researchers [(3);
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	We thank L. P. Keller V. Yang C. Le R. A. Socki M. F. McKay M. S. Gibson and S. R. Keprta for assistance; and R. Score and M. Lindstrom for their help in sample selection and preparation. The guidance of J. W. Schopf at an early stage of this study is appreciated. We also thank G. Horuchi L. Hulse L. L. Darrow D. Pierson and personnel from Building 37. The work was supported in part by NASA's Planetary Materials Program (D.S.M. and R.N.Z.) and the Exobiology Program (D.S.M.). Additional support from NASA-JSC Center Director's Discretionary Program (E.K.G.) is recognized. C.S.R. and H.V. acknowledge support from the National Research Council. X.D.F.C. acknowledges support from the Swiss National Science Foundation.

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