A biosignature (sometimes called chemical fossil or molecular fossil) is any substance – such as an element, isotope, molecule, or phenomenon – that provides scientific evidence of past or present life. Measurable attributes of life include its complex physical and chemical structures and also its utilization of free energy and the production of biomass and wastes. Due to its unique characteristics, a biosignature can be interpreted as having been produced by living organisms; however, it is important that they not be considered definitive because there is no way of knowing in advance which ones are universal to life and which ones are unique to the peculiar circumstances of life on Earth. Nonetheless, life forms are known to shed unique chemicals, including DNA, into the environment as evidence of their presence in a particular location.
In geomicrobiology[edit | edit source | hide | hide all]
The ancient record on Earth provides an opportunity to see what geochemical signatures are produced by microbial life and how these signatures are preserved over geologic time. Some related disciplines such as geochemistry, geobiology, and geomicrobiology often use biosignatures to determine if living organisms are or were present in a sample. These possible biosignatures include: (a) microfossils and stromatolites; (b) molecular structures (biomarkers) and isotopic compositions of carbon, nitrogen and hydrogen in organic matter; (c) multiple sulfur and oxygen isotope ratios of minerals; and (d) abundance relationships and isotopic compositions of redox sensitive metals (e.g., Fe, Mo, Cr, and rare earth elements).
For example, the particular fatty acids measured in a sample can indicate which types of bacteria and archaea live in that environment. Another example are the long-chain fatty alcohols with more than 23 atoms that are produced by planktonic bacteria. When used in this sense, geochemists often prefer the term biomarker. Another example is the presence of straight-chain lipids in the form of alkanes, alcohols an fatty acids with 20-36 carbon atoms in soils or sediments. Peat deposits are an indication of originating from the epicuticular wax of higher plants.
Life processes may produce a range of biosignatures such as nucleic acids, lipids, proteins, amino acids, kerogen-like material and various morphological features that are detectable in rocks and sediments. Microbes often interact with geochemical processes, leaving features in the rock record indicative of biosignatures. For example, bacterial micrometer-sized pores in carbonate rocks resemble inclusions under transmitted light, but have distinct size, shapes and patterns (swirling or dendritic) and are distributed differently from common fluid inclusions. A potential biosignature is a phenomenon that may have been produced by life, but for which alternate abiotic origins may also be possible.
In astrobiology[edit | edit source | hide]
Astrobiological exploration is founded upon the premise that biosignatures encountered in space will be recognizable as extraterrestrial life. The usefulness of a biosignature is determined, not only by the probability of life creating it, but also by the improbability of nonbiological (abiotic) processes producing it. Concluding that evidence of an extraterrestrial life form (past or present) has been discovered, requires proving that a possible biosignature was produced by the activities or remains of life. As with most scientific discoveries, discovery of a biosignature will require of evidence building up until no other explanation exists.
Possible examples of a biosignature might be complex organic molecules and/or structures whose formation is virtually unachievable in the absence of life. For example, cellular and extracellular morphologies, biomolecules in rocks, bio-organic molecular structures, chirality, biogenic minerals, biogenic stable isotope patterns in minerals and organic compounds, atmospheric gases, and remotely detectable features on planetary surfaces, such as photosynthetic pigments, etc.
In general, biosignatures and habitable environment signatures can be grouped into ten broad categories:
- Stable isotope patterns: Isotopic evidence or patterns that require biological processes.
- Chemistry: Chemical features that require biological activity.
- Organic matter: Organics formed by biological processes.
- Minerals: Minerals or biomineral-phases whose composition and/or morphology indicate biological activity (e.g., biomagnetite).
- Microscopic structures and textures: Biologically formed cements, microtextures, microfossils, and films.
- Macroscopic physical structures and textures: Structures that indicate microbial ecosystems, biofilms (e.g., stromatolites), or fossils of larger organisms.
- Temporal variability: Variations in time of atmospheric gases, reflectivity, or macroscopic appearance that indicate the presence of life.
- Surface reflectance features: Large-scale reflectance features due to biological pigments, which could be detected remotely.
- Atmospheric gases: Gases formed by metabolic and/or aqueous processes, which may be present on a planet-wide scale.
- Technosignatures: Signatures that indicate a technologically advanced civilization.
Chemical[edit | edit source | hide]
No single compound will prove life once existed. Rather, it will be distinctive patterns present in any organic compounds showing a process of selection. For example, membrane lipids left behind by degraded cells will be concentrated, have a limited size range, and comprise an even number of carbons. Similarly, life only uses left-handed amino acids. Biosignatures need not be chemical, however, and can also be suggested by a distinctive magnetic biosignature.
On Mars, surface oxidants and UV radiation will have altered or destroyed organic molecules at or near the surface. One issue that may add ambiguity in such a search is the fact that, throughout Martian history, abiogenic organic-rich chondritic meteorites have undoubtedly rained upon the Martian surface. At the same time, strong oxidants in Martian soil along with exposure to ionizing radiation might alter or destroy molecular signatures from meteorites or organisms. An alternative approach would be to seek concentrations of buried crystalline minerals, such as clays and evaporites, which may protect organic matter from the destructive effects of ionizing radiation and strong oxidants. The search for Martian biosignatures has become more promising due to the discovery that surface and near-surface aqueous environments existed on Mars at the same time when biological organic matter was being preserved in ancient aqueous sediments on Earth.
Morphology[edit | edit source | hide]
Another possible biosignature might be morphology since the shape and size of certain objects may potentially indicate the presence of past or present life. For example, microscopic magnetite crystals in the Martian meteorite ALH84001 were the longest-debated of several potential biosignatures in that specimen because it was believed until recently that only bacteria could create crystals of their specific shape. For example, the possible biomineral studied in the Martian ALH84001 meteorite includes putative microbial fossils, tiny rock-like structures whose shape was a potential biosignature because it resembled known bacteria. Most scientists ultimately concluded that these were far too small to be fossilized cells. A consensus that has emerged from these discussions, and is now seen as a critical requirement, is the demand for further lines of evidence in addition to any morphological data that supports such extraordinary claims. Currently, the scientific consensus is that "morphology alone cannot be used unambiguously as a tool for primitive life detection." Interpretation of morphology is notoriously subjective, and its use alone has led to numerous errors of interpretation.
Atmospheric properties and composition[edit | edit source | hide]
The atmospheric properties of exoplanets are of particular importance, as atmospheres provide the most likely observables for the near future, including habitability indicators and biosignatures. Over billions of years, the processes of life on a planet would result in a mixture of chemicals unlike anything that could form in an ordinary chemical equilibrium. For example, large amounts of oxygen and small amounts of methane are generated by life on Earth.
Also, an exoplanet's color —or reflectance spectrum— might give away the presence of vast colonies of life forms at its surface.
The presence of methane in the atmosphere of Mars indicates that there must be an active source on the planet, as it is an unstable gas. Furthermore, current photochemical models cannot explain the presence of methane in the atmosphere of Mars and its reported rapid variations in space and time. Neither its fast appearance nor disappearance can be explained yet. To rule out a biogenic origin for the methane, a future probe or lander hosting a mass spectrometer will be needed, as the isotopic proportions of carbon-12 to carbon-14 in methane could distinguish between a biogenic and non-biogenic origin, similarly to the use of the δ13C standard for recognizing biogenic methane on Earth. In June, 2012, scientists reported that measuring the ratio of hydrogen and methane levels on Mars may help determine the likelihood of life on Mars. According to the scientists, "...low H2/CH4 ratios (less than approximately 40) indicate that life is likely present and active." The planned ExoMars Trace Gas Orbiter, launched in March 2016 to Mars, will study atmospheric trace gases and will attempt to characterize potential biochemical and geochemical processes at work.
Other scientists have recently reported methods of detecting hydrogen and methane in extraterrestrial atmospheres. Habitability indicators and biosignatures must be interpreted within a planetary and environmental context. For example, the presence of oxygen and methane together could indicate the kind of extreme thermochemical disequilibrium generated by life. Two of the top 14,000 proposed atmospheric biosignatures are dimethyl sulfide and chloromethane (CH
3Cl). An alternative biosignature is the combination of methane and carbon dioxide.
Indirect evidence[edit | edit source | hide]
Scientific observations include the possible identification of biosignatures through indirect observation. For example, electromagnetic information through infrared radiation telescopes, radio-telescopes, space telescopes, etc. From this discipline, the hypothetical electromagnetic radio signatures that SETI scans for would be a biosignature, since a message from intelligent aliens would certainly demonstrate the existence of extraterrestrial life.
Robotic surface missions[edit | edit source | hide]
- The Viking missions to Mars
The Viking missions to Mars in the 1970s conducted the first experiments which were explicitly designed to look for biosignatures on another planet. Each of the two Viking landers carried three life-detection experiments which looked for signs of metabolism; however, the results were declared inconclusive.
- Mars Science Laboratory
The Curiosity rover from the Mars Science Laboratory mission, with its Curiosity rover is currently assessing the potential past and present habitability of the Martian environment and is attempting to detect biosignatures on the surface of Mars. Considering the MSL instrument payload package, the following classes of biosignatures are within the MSL detection window: organism morphologies (cells, body fossils, casts), biofabrics (including microbial mats), diagnostic organic molecules, isotopic signatures, evidence of biomineralization and bioalteration, spatial patterns in chemistry, and biogenic gases. The Curiosity rover targets outcrops to maximize the probability of detecting 'fossilized' organic matter preserved in sedimentary deposits.
- ExoMars rover
The 2016 ExoMars Trace Gas Orbiter (TGO) is a Mars telecommunications orbiter and atmospheric gas analyzer mission. It delivered the Schiaparelli EDM lander and then began to settle into its science orbit to map the sources of methane on Mars and other gases, and in doing so, will help select the landing site for the ExoMars rover to be launched in 2020. The primary objective of the ExoMars rover mission is the search for biosignatures on the surface and subsurface by using a drill able to collect samples down to a depth of 2 metres (6.6 ft), away from the destructive radiation that bathes the surface.
- Mars 2020 Rover
The Mars 2020 rover, planned to launch in 2020, is intended to investigate an astrobiologically relevant ancient environment on Mars, investigate its surface geological processes and history, including the assessment of its past habitability, the possibility of past life on Mars, and potential for preservation of biosignatures within accessible geological materials. In addition, it will cache the most interesting samples for possible future transport to Earth.
- Titan Dragonfly
The planned Dragonfly lander/aircraft to launch in 2025, would seek evidence of biosignatures on the organic-rich surface and atmosphere of Titan, as well as study its possible prebiotic primordial soup.
See also[edit | edit source | hide]
References[edit | edit source | hide]
- ↑ 1.0 1.1 1.2 Steele; Beaty; et al. (September 26, 2006). "Final report of the MEPAG Astrobiology Field Laboratory Science Steering Group (AFL-SSG)" (.doc). The Astrobiology Field Laboratory. U.S.A.: the Mars Exploration Program Analysis Group (MEPAG) - NASA. p. 72.
- ↑ "Biosignature - definition". Science Dictionary. 2011. Archived from the original on 2010-03-16. Retrieved 2011-01-12.
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 Summons, Roger E.; Jan P. Amend; David Bish; Roger Buick; George D. Cody; David J. Des Marais; Dromart, G; Eigenbrode, J. L.; Knoll, A. H.; Sumner, D. Y. (23 February 2011). "Preservation of Martian Organic and Environmental Records: Final Report of the Mars Biosignature Working Group" (PDF). Astrobiology. 11 (2): 157–81. Bibcode:2011AsBio..11..157S. doi:10.1089/ast.2010.0506. PMID 21417945. Retrieved 2013-06-22.
- ↑ Carol Cleland; Gamelyn Dykstra; Ben Pageler (2003). "Philosophical Issues in Astrobiology". NASA Astrobiology Institute. Archived from the original on 2011-07-21. Retrieved 2011-04-15.
- ↑ Zimmer, Carl (January 22, 2015). "Even Elusive Animals Leave DNA, and Clues, Behind". The New York Times. Retrieved January 23, 2015.
- ↑ "SIGNATURES OF LIFE FROM EARTH AND BEYOND". Penn State Astrobiology Research Center (PSARC). Penn State. 2009. Retrieved 2011-01-14.
- ↑ Tenenbaum, David (July 30, 2008). "Reading Archaean Biosignatures". NASA. Archived from the original on November 29, 2014. Retrieved 2014-11-23.
- ↑ Fatty alcohols
- ↑ 9.0 9.1 Beegle, Luther W.; Wilson, Michael G.; Abilleira, Fernando; Jordan, James F.; Wilson, Gregory R.; et al. (August 2007). "A Concept for NASA's Mars 2016 Astrobiology Field Laboratory". Astrobiology. 7 (4): 545–577. Bibcode:2007AsBio...7..545B. doi:10.1089/ast.2007.0153. PMID 17723090. Retrieved 2009-07-20.
- ↑ Bosak, Tanja Bosak; Virginia Souza-Egipsy; Frank A. Corsetti & Dianne K. Newman (May 18, 2004). "Micrometer-scale porosity as a biosignature in carbonate crusts". Geology. 32 (9): 781–784. Bibcode:2004Geo....32..781B. doi:10.1130/G20681.1. Retrieved 2011-01-14.
- ↑ 11.0 11.1 Rothschild, Lynn (September 2003). "Understand the evolutionary mechanisms and environmental limits of life". NASA. Archived from the original on 2011-01-26. Retrieved 2009-07-13.
- ↑ 12.0 12.1 NASA Astrobiology Strategy 2015.(PDF), NASA
- ↑ 13.0 13.1 Rover could discover life on Mars – here's what it would take to prove it. Claire Cousins, PhysOrg. 5 January 2018.
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- ↑ Crenson, Matt (2006-08-06). "After 10 years, few believe life on Mars". Associated Press (on usatoday.com). Retrieved 2009-12-06.
- ↑ McKay, David S.; Gibson Jr, Everett K.; Thomas-Keprta, Kathie L.; Vali, Hojatollah; Romanek, Christopher S.; Clemett, Simon J.; Chillier, Xavier D. F.; Maechling, Claude R.; Zare, Richard N.; et al. (1996). "Search for Past Life on Mars: Possible Relic Biogenic Activity in Martian Meteorite ALH84001". Science. 273 (5277): 924–930. Bibcode:1996Sci...273..924M. doi:10.1126/science.273.5277.924. PMID 8688069.
- ↑ 17.0 17.1 Garcia-Ruiz, Juan-Manuel Garcia-Ruiz (December 30, 1999). "Morphological behavior of inorganic precipitation systems – Instruments, Methods, and Missions for Astrobiology II". SPIE Proceedings. Instruments, Methods, and Missions for Astrobiology II. Proc. SPIE 3755: 74. doi:10.1117/12.375088. Retrieved 2013-01-15.
It is concluded that "morphology cannot be used unambiguously as a tool for primitive life detection."
- ↑ Agresti; House; Jögi; Kudryavstev; McKeegan; Runnegar; Schopf; Wdowiak (3 December 2008). "Detection and geochemical characterization of Earth's earliest life". NASA Astrobiology Institute. NASA. Archived from the original on 23 January 2013. Retrieved 2013-01-15.
- ↑ Schopf, J. William; Kudryavtsev, Anatoliy B.; Czaja, Andrew D.; Tripathi, Abhishek B. (28 April 2007). "Evidence of Archean life: Stromatolites and microfossils" (PDF). Precambrian Research. 158 (3–4): 141–155. Bibcode:2007PreR..158..141S. doi:10.1016/j.precamres.2007.04.009. Retrieved 2013-01-15.
- ↑ "Artificial Life Shares Biosignature With Terrestrial Cousins". The Physics arXiv Blog. MIT. 10 January 2011. Retrieved 2011-01-14.
- ↑ 21.0 21.1 Seager, Sara; Bains, William; Petkowski, Janusz (20 April 2016). "Toward a List of Molecules as Potential Biosignature Gases for the Search for Life on Exoplanets and Applications to Terrestrial Biochemistry". Astrobiology. 16 (6): 465–85. Bibcode:2016AsBio..16..465S. doi:10.1089/ast.2015.1404. PMID 27096351. Retrieved 2016-05-07.
- ↑ Berdyugina, Svetlana V.; Kuhn, Jeff; Harrington, David; Santl-Temkiv, Tina; Messersmith, E. John (January 2016). "Remote sensing of life: polarimetric signatures of photosynthetic pigments as sensitive biomarkers". International Journal of Astrobiology. 15 (1): 45–56. Bibcode:2016IJAsB..15...45B. doi:10.1017/S1473550415000129.
- ↑ Hegde, Siddharth; Paulino-Lima, Ivan G.; Kent, Ryan; Kaltenegger, Lisa; Rothschild, Lynn (31 March 2015). "Surface biosignatures of exo-Earths: Remote detection of extraterrestrial life". PNAS. 112 (13): 3886–3891. Bibcode:2015PNAS..112.3886H. doi:10.1073/pnas.1421237112. PMC 4386386 . PMID 25775594. Retrieved 2015-05-11.
- ↑ Cofield, Calla (30 March 2015). "Catalog of Earth Microbes Could Help Find Alien Life". Space.com. Retrieved 2015-05-11.
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- ↑ Mars Trace Gas Mission Archived 2011-07-21 at the Wayback Machine. (September 10, 2009)
- ↑ Remote Sensing Tutorial, Section 19-13a Archived 2011-10-21 at the Wayback Machine. - Missions to Mars during the Third Millennium, Nicholas M. Short, Sr., et al., NASA
- ↑ 28.0 28.1 Oze, Christopher; Jones, Camille; Goldsmith, Jonas I.; Rosenbauer, Robert J. (June 7, 2012). "Differentiating biotic from abiotic methane genesis in hydrothermally active planetary surfaces". PNAS. 109 (25): 9750–9754. Bibcode:2012PNAS..109.9750O. doi:10.1073/pnas.1205223109. PMC 3382529 . PMID 22679287. Retrieved June 27, 2012.
- ↑ Staff (June 25, 2012). "Mars Life Could Leave Traces in Red Planet's Air: Study". Space.com. Retrieved June 27, 2012.
- ↑ Mark Allen; = Olivier Witasse (June 16, 2011), "2016 ESA/NASA ExoMars Trace Gas Orbiter" (PDF), MEPAG June 2011, Jet Propulsion Laboratory (PDF)
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- ↑ Where are they? (PDF) Mario Livio and Joseph Silk. Physics Today, March 2017.
- ↑ Wall, Mike (24 January 2018). "Alien Life Hunt: Oxygen Isn't the Only Possible Sign of Life". Space.com. Retrieved 24 January 2018.
- ↑ Krissansen-Totton, Joshua; Olson, Stephanie; Catlig, David C. (24 January 2018). "Disequilibrium biosignatures over Earth history and implications for detecting exoplanet life". 4 (1, eaao5747). doi:10.1126/scidv.aao5747. Retrieved 24 January 2018.
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- ↑ 41.0 41.1 ExoMars rover
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- ↑ Chang, Alicia (July 9, 2013). "Panel: Next Mars rover should gather rocks, soil". Associated Press. Retrieved July 12, 2013.
- ↑ Schulte, Mitch (December 20, 2012). "Call for Letters of Application for Membership on the Science Definition Team for the 2020 Mars Science Rover" (PDF). NASA. NNH13ZDA003L.
- ↑ Dragonfly: Exploring Titan's Surface with a New Frontiers Relocatable Lander. American Astronomical Society, DPS meeting #49, id.219.02. October 2017.
- ↑ Dragonfly: Exploring Titan's Prebiotic Organic Chemistry and Habitability (PDF). E. P. Turtle, J. W. Barnes, M. G. Trainer, R. D. Lorenz, S. M. MacKenzie, K. E. Hibbard, D. Adams, P. Bedini, J. W. Langelaan, K. Zacny, and the Dragonfly Team. Lunar and Planetary Science Conference 2017.
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