The search for organic substances and inorganic volatile compounds in the surface of Mars

Biemann, K.; Oró, J.; Toulmin, Priestley; Orgel, Leslie E.; Nier, Alfred O.; Anderson, Duwayne M.; Simmonds, Peter; Flory, D. A.; Diaz, A. V.; Rushneck, D. R.; Biller, J. E.; Lafleur, Arthur L.

doi:10.1029/js082i028p04641

Cited by 542 publications

(409 citation statements)

References 27 publications

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“…When searching for petroleum reserves, the mass distribution provides a metric of thermal maturity and the potential yield of various types of hydrocarbons from a given well. When searching for evidence of life on Mars, the Viking gas chromatograph and mass spectrometer set an upper limit on the concentration of organics in the lander regions -no organic compounds were detected at the parts per billion level (Biemann et al 1977). Interestingly, however, we note that the Viking experiments were insufficient for detecting the expected background flux from meteorite infall (Benner et al 2000).…”

Section: Spectrometric Signaturesmentioning

confidence: 92%

Spectroscopic and spectrometric differentiation between abiotic and biogenic material on icy worlds

2010

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Abstract. The ability to differentiate abiotic organic material from material of a biological origin is a critical task for astrobiology. Mass spectrometry and spectroscopy provide key tools for advancing this task and are two techniques that provide useful and highly complementary compositional information independent of a specific biochemical pathway. Here we address some of the utility and limitations of applying these techniques to both orbital and in situ exploration of icy moons of the outer solar system.

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Section: Spectrometric Signaturesmentioning

confidence: 92%

Spectroscopic and spectrometric differentiation between abiotic and biogenic material on icy worlds

2010

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“…Water, if it exists near the surface, will be present as ice. Viking's finding of a complete lack of organic molecules in the top few centimeters of soil supports the sterility of the surface (Biemann et al 1976(Biemann et al , 1977. A few tens of centimeters of regolith would shield organisms from radiation (Pavlov et al 2002).…”

Section: Martian Atmospheric Methanementioning

confidence: 99%

A Biomass-Based Model to Estimate the Plausibility of Exoplanet Biosignature Gases

Seager

Bains

2013

ApJ

117

144

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Biosignature gas detection is one of the ultimate future goals for exoplanet atmosphere studies. We have created a framework for linking biosignature gas detectability to biomass estimates, including atmospheric photochemistry and biological thermodynamics. The new framework is intended to liberate predictive atmosphere models from requiring fixed, Earth-like biosignature gas source fluxes. New biosignature gases can be considered with a check that the biomass estimate is physically plausible. We have validated the models on terrestrial production of NO, H 2 S, and CH 4 , CH 3 Cl, and DMS. We have applied the models to propose NH 3 as a biosignature gas on a "cold Haber World" a planet with an N 2 -H 2 atmosphere, and to demonstrate why gases such as CH 3 Cl must have too great of a biomass to be a plausible biosignature gas on planets with Earth or early-Earth-like atmospheres orbiting a sun-like star. To construct the biomass models we developed a functional classification of biosignature gases, and found that gases (such as CH 4 , H 2 S, N 2 O) produced from life that extracts energy from chemical potential energy gradients will always have false positives because geochemistry has the same gases to work with as life does, and gases (such as DMS, CH 3 Cl) produced for secondary metabolic reasons are far less likely to have false positives, but because of their highly specialized origin are more likely to be produced in small quantities. The biomass model estimates are valid to one or two orders of magnitude; the goal is an independent approach to testing whether a biosignature gas is plausible rather than on a precise quantification of atmospheric biosignature gases and their corresponding biomasses.

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“…A second inlet routed the sample through a getter pump to adsorb H 2 and enable collection of additional data to discriminate between 3 He and HD. This instrument provided unanticipated results insofar as the Venusian atmosphere was found to contain 96% CO 2 and 4% N 2 , as well as more primordial argon (as indicated by a high ratio of 36 Ar to 40 Ar) than found on Earth.…”

Section: Pioneer Venus Probementioning

confidence: 99%

“…This instrument was intended for both atmospheric and soil monitoring experiments, with the latter for the purpose of detecting organic chemicals which could potentially indicate the presence of other life in the universe. A schematic of the instrument is shown in Figure 5 [36]. It used an EI source and a double-focusing mass analyzer with the EB configuration (Nier-Johnson geometry).…”

Section: Mars Viking Landermentioning

confidence: 99%

Mass spectrometry in the U.S. space program: Past, present, and future

Palmer

Limero

2001

J. Am. Soc. Mass Spectrom.

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Recent years have witnessed significant progress on the miniaturization of mass spectrometers for a variety of field applications. This article describes the development and application of mass spectrometry (MS) instrumentation to support of goals of the U.S. space program. Its main focus is on the two most common space-related applications of MS: studying the composition of planetary atmospheres and monitoring air quality on manned space missions. Both sets of applications present special requirements in terms of analytical performance (sensitivity, selectivity, speed, etc.), logistical considerations (space, weight, and power requirements), and deployment in perhaps the harshest of all possible environments (space). The MS instruments deployed on the Pioneer Venus and Mars Viking Lander missions are reviewed for the purposes of illustrating the unique features of the sample introduction systems, mass analyzers, and vacuum systems, and for presenting their specifications which are impressive even by today's standards. The various approaches for monitoring volatile organic compounds (VOCs) in cabin atmospheres are also reviewed. In the past, ground-based GC/MS instruments have been used to identify and quantify VOCs in archival samples collected during the Mercury, Apollo, Skylab, Space Shuttle, and Mir missions. Some of the data from the more recent missions are provided to illustrate the composition data obtained and to underscore the need for instrumentation to perform such monitoring in situ. Lastly, the development of two emerging technologies, Direct Sampling Ion Trap Mass Spectrometry (DSITMS) and GC/Ion Mobility Spectrometry (GC/IMS), will be discussed to illustrate their potential utility for future missions. (J Am Soc Mass Spectrom 2001, 12, 656 -675)

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The search for organic substances and inorganic volatile compounds in the surface of Mars

Cited by 542 publications

References 27 publications

Spectroscopic and spectrometric differentiation between abiotic and biogenic material on icy worlds

Spectroscopic and spectrometric differentiation between abiotic and biogenic material on icy worlds

A Biomass-Based Model to Estimate the Plausibility of Exoplanet Biosignature Gases

Mass spectrometry in the U.S. space program: Past, present, and future

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