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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 coaler; 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 50,000X 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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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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