It is often acknowledged that the search for life on Mars might produce false positive results, particularly via the detection of objects, patterns or substances that resemble the products of life in some way but are not biogenic. The success of major current and forthcoming rover missions now calls for significant efforts to mitigate this risk. Here, we review known processes that could have generated false biosignatures on early Mars. These examples are known largely from serendipitous discoveries rather than systematic research and remain poorly understood; they probably represent only a small subset of relevant phenomena. These phenomena tend to be driven by kinetic processes far from thermodynamic equilibrium, often in the presence of liquid water and organic matter, conditions similar to those that can actually give rise to, and support, life. We propose that strategies for assessing candidate biosignatures on Mars could be improved by new knowledge on the physics and chemistry of abiotic self-organization in geological systems. We conclude by calling for new interdisciplinary research to determine how false biosignatures may arise, focusing on geological materials, conditions and spatiotemporal scales relevant to the detection of life on Mars, as well as the early Earth and other planetary bodies.

Thematic collection: This article is part of the Astrobiology: Perspectives from the Geology of Earth and the Solar System collection available at: https://www.lyellcollection.org/cc/astrobiology-perspectives-from-geology-of-earth-and-solar-system

These are exciting times for astrobiology. The search for evidence of past life on Mars is the central scientific objective of two contemporary rover missions: NASA's Mars 2020 Mission (Perseverance rover, touchdown February 2021) and the ESA-RosCosmos ExoMars Mission (Rosalind Franklin rover, scheduled for launch in 2022). Both rovers will seek geological biosignatures in clay-rich, subaqueously deposited sedimentary rocks of Noachian age (c. 4 Ga), probably representing habitable palaeoenvironments (Horgan et al. 2020; Quantin-Nataf et al. 2021). Both rovers are equipped with sophisticated multispectral cameras and instruments for the analysis of these rocks and any organic matter they may contain.

The two missions differ slightly in their technical abilities. For example, the Rosalind Franklin rover carries a drill capable of extracting samples from 2 m below the surface, where the overlying rock may have protected organic molecules from oxidation or radiation damage. The Perseverance rover can detect organic matter, but not extract it from such depths nor characterize it in as much detail. However, Perseverance is equipped with a sample-caching system that will enable it to extract astrobiologically promising geological samples and seal them for subsequent collection and return to Earth, probably in a joint ESA–NASA operation (Muirhead et al. 2020). These will be the first samples brought back from Mars and will serve as a rich source of data for the investigation of martian geology and astrobiology. In theory, it will become possible to analyse rocks from Mars using almost the full range of techniques used to detect ancient biosignatures on Earth.

Studies of the Earth's biosphere and geological record have illuminated an enormous variety of biosignatures that astrobiologists might detect either in situ on Mars or in returned samples. For instance, samples may contain: morphological fossils as small as individual microbial cells, colonies or biofilms, or as large as stromatolites; organic materials with a compositional profile, complexity, modular molecular construction and/or stereoisomerism that suggest biosynthetic origins; or isotopic, geochemical or mineralogical anomalies that would normally be interpreted as evidence of life (Westall et al. 2015; Hays et al. 2017; Vago et al. 2017, 2019; McMahon et al. 2018).

Astrobiologists have amassed innumerable examples of these and other kinds of microbial biosignatures from ancient and modern Mars-analogue environments, providing an immensely rich set of reference data or ‘search images’. We might reasonably argue, therefore, that the risk of false negative results in the search for life is low, or at least lower for the forthcoming rover missions than it was for the Viking landers of the 1970s: if evidence of life is really present in the materials that either the Rosalind Franklin or Perseverance rover brings to light, there is now a good chance that we will find and recognize it. What concerns us here is the risk of false positive errors in the detection of life, specifically those arising from the misinterpretation of abiotic geological and chemical features that are misleadingly life-like (rather than analytical false positives or spacecraft contamination).

One reason for concern is that such errors have been frequent in the history of palaeobiology and astrobiology down to the present day. In the nineteenth century, intricate layered and tubular structures found in serpentine-rich metacarbonate rocks from the Canadian shield were interpreted as the fossilized tests of ancient forams, designated Eozoon canadense, the ‘dawn animal of Canada’; it took much heated debate, and some decades of careful work, to show that these were abiotic textures (Adelman 2007). Palaeontologists in the twentieth century repeatedly made similar misdiagnoses; examples listed by Cloud (1973) include spurious ‘worm tracks’ (drag marks), ‘medusae’ (pyrite rosettes), ‘arthropods’ (mud curls around desiccation cracks) and numerous Proterozoic ‘microfossils’ (crystallites, contaminating spores and preparation artefacts).

The difficulty of correctly determining the biogenicity of life-like geological substances and structures has continued to plague palaeontology, and the new field of astrobiology, often despite laudable efforts to practice the ‘care, patience, and critical attitude’ recommended by Cloud. For example, McKay et al. (1996) reported multiple lines of evidence in the martian meteorite ALH84001 that were suggestive of past life on Mars, making news bulletins around the world. These included carbonate globules and magnetite crystals resembling bacteriogenic precipitates, polyaromatic hydrocarbon compounds and worm-like microstructures interpreted as morphological fossils. The origins of these features are still unclear today, but abiotic explanations have been offered for all of them, and the overall case for life in ALH84001 no longer seems compelling (Martel et al. 2012). This example warns us that it is not enough to have ‘multiple lines of evidence’ for biogenicity (an oft-repeated mantra) if each line of evidence is ambiguous.

Other ongoing debates concern the oldest fossil and geochemical evidence of life on Earth. Schopf (1993) presented fossil ‘cyanobacteria’ from the 3.5-Gyr-old Apex Chert of Western Australia, which were later reinterpreted as abiotic carbon organized around spherulitic quartz growth and/or worm-like delaminated clay booklets (Brasier et al. 2002, 2005; Wacey et al. 2016a). Recent work highlights the possibility that organic matter in such cherts might be biogenic even if it has been abiotically redistributed (Duda et al. 2018), while Schopf et al. (2018) have claimed that morphology-specific carbon isotope values confirm the biogenicity of the Apex microstructures and reveal them to include methane-cycling archaea; this controversy continues (e.g. Alleon and Summons 2019). Nutman et al. (2016) described triangular features exposed on 3.7-Gyr-old metasedimentary rocks from the Isua supracrustal belt in Greenland and interpreted them as fossil stromatolites; these have been reinterpreted by some researchers as abiotic deformation features on the basis of 3D imaging and geochemical analysis (Allwood et al. 2018; Zawaski et al. 2020), although Nutman and co-workers stand by their original view (Nutman et al. 2021). Dodd et al. (2017) described hematite tubules in a c. 4-Gyr-old hydrothermal chert from the Nuvvuagittuq Greenstone Belt in Canada as the mineralized sheaths of ancient Fe-oxidizing bacteria; these have been queried as possible chemical gardens (McMahon 2019), but further analyses are needed.

These examples show that the return of samples from Mars will not necessarily solve once and for all the problem of the existence of (ancient) life on that planet. Although we must hope for definitive results, candidate biosignatures are likely to be at least somewhat ambiguous (García-Ruiz et al. 2002) and may spark debates that cannot be quickly resolved. To give an extreme example from Earth, the biogenicity of the filamentous mineral networks found in ‘moss agates’ has been unclear for more than 200 years (e.g. Daubenton 1782; MacCulloch 1814; Bowerbank 1842; Göppert 1848; Liesegang 1914; Brown 1957; Hopkinson et al. 1998; Hofmann and Farmer 2000; McMahon 2019; Götze et al. 2020). As in all the debates cited here, the key evidence will come from the investigation of abiotic physicochemical systems and their capacity to mimic the forms and properties of life. Yet this area of enquiry has received rather scant and unsystematic attention from astrobiologists, who have tended to focus their published work on expanding our knowledge of life's signatures rather than its abiotic mimics. This problem was lamented by Cady et al. (2003), who predicted that:

… images and spectroscopic data indicative of life will continue to accumulate in the peer-reviewed literature. At the same time, millions of images and spectra from dubiofossils (of unknown origin) and pseudofossils (abiotic mimics) will also continue to accumulate, yet they will rarely appear in publication.

With this motivation, we here attempt to summarize the physicochemical processes so far known to generate life-like morphologies, minerals, molecules and other phenomena, and consider how and where they may have taken place on early Mars, with a particular focus on the materials that the Rosalind Franklin and Perseverance rovers may encounter and sample at Oxia Planum and Jezero Crater, respectively. We note that, by definition, a biosignature is more than simply a phenomenon produced by life: it is a phenomenon that specifically requires a biological agent – that is, it could not have been produced naturally by non-living systems (e.g. Des Marais et al. 2008). The reliability of any detected biosignatures on Mars therefore depends crucially on our understanding of the abiotic processes that might mimic them (Brasier and Wacey 2012; Chan et al. 2019).

This paper is not intended to criticize or undermine the search for geological evidence of life on Mars (or the early Earth), but to facilitate the formulation and testing of abiotic ‘null hypotheses’ for the evaluation of candidate biosignatures if and when they are discovered. It is intended to complement the many existing reviews on the possible biosignatures that may be found on Mars (e.g. Westall et al. 2015; Hays et al. 2017; Vago et al. 2017; McMahon et al. 2018). For the most part, however, we do not attempt to provide ‘biogenicity criteria’ for evaluating the credibility of candidate biosignatures. Rather, we emphasize that such criteria will become more reliable as the formation of false biosignatures becomes better understood. Significant progress in this field will require the numerical, experimental and analytical skills and specialist knowledge of chemists, physicists, geologists, mineralogists and materials scientists, among others.

The search for ancient organic matter is a central element of the life-detection strategy for ExoMars, Mars 2020 and the anticipated joint ESA–NASA sample return mission. Indigenous martian organic matter with a chemical fingerprint sufficiently similar to (degraded) biomass would be an exciting potential biosignature in its own right and could significantly strengthen the credibility of any associated morphological, isotopic or mineralogical potential biosignatures (Summons et al. 2011). Despite the pervasively oxidizing and ionizing conditions at the martian surface, the Sample Analysis at Mars (SAM) instrument aboard the Curiosity rover has confirmed that ancient organic matter has survived where shielded and protected by minerals, particularly clays. This instrument measured trace amounts of aliphatic and aromatic molecular fragments in drill powder extracted from a Noachian–Hesperian mudstone, which had been exposed relatively recently by scarp retreat (Glavin et al. 2013; Farley et al. 2014; Ming et al. 2014; Freissinet et al. 2015; Eigenbrode et al. 2018). This organic matter has been altered diagenetically (e.g. sulfurized) and may have originally derived partly from carbonaceous meteorites and partly from indigenous sources on Mars (Eigenbrode et al. 2018; Franz et al. 2020). Interaction with perchlorates during sample pyrolysis chlorinated some hydrocarbons, further obscuring their original composition (Szopa et al. 2020). Ancient, probably indigenous, organic matter is also found in some basaltic martian meteorites, probably from abiotic sources (e.g. Steele et al. 2012).

Jezero Crater and Oxia Planum both host clay-rich Noachian sedimentary rocks with good potential to contain preserved organic matter, which both the Perseverance and Rosalind Franklin rovers would be capable of detecting and, to some extent, characterizing. Rosalind Franklin's Mars Organic Molecular Analyzer (MOMA) instrument can fingerprint organic molecules in drill powders with very high sensitivity and specificity, even allowing enantiomeric excesses to be measured in some compounds (Goesmann et al. 2017) (Table 1). Unfortunately, determining the biogenicity of any organic matter detected may not be straightforward. Noachian Mars, like the early Earth, was presumably supplied with a rich complement of organic matter derived from meteorites and from a variety of endogenous abiotic processes (Chyba and Sagan 1992). Among the latter, the most frequently discussed involve either the reduction of inorganic carbon catalysed on mineral surfaces under hydrothermal conditions (e.g. Fischer–Tropsch type synthesis, organosulfur pathways and electrochemical pathways), high-temperature carbonate decomposition or (mineral-catalysed) photochemical carbon fixation and cycling (e.g. McCollom 2013; Milesi et al. 2015; Dalai et al. 2016; Steele et al. 2018; Franz et al. 2020). Taken together, these various sources would have provided, inter alia, polyaromatic hydrocarbons, alkanes, amines, fatty acids/lipids, carboxylic acids, amino acids, nucleobases, aldehydes, ketones and carbohydrates, all of which are present – along with marked enantiomeric excesses – in carbonaceous chondrites (Botta and Bada 2002; Simoneit 2004; Myrgorodska et al. 2015; Dalai et al. 2016; Furukawa et al. 2019; Lai et al. 2019).

Table 1.

Descriptions of analytical and imaging instruments aboard the Perseverance and Rosalind Franklin rovers, with their respective spatial resolutions

Instrument nameDescriptionRelevant spatial resolution
Perseverance rover
 Mastcam-ZLong-range (2–100 m) multispectral, stereoscopic imager; wavelength selection using narrowband filters provides some mineralogical information150 μm per pixel to 7.4 mm per pixel depending on distance
 WATSONCamera for fine-scale imaging of textures and structures on the martian surface15.9 μm per pixel
 SHERLOCDeep UV Raman and fluorescence spectrometer for the detection and mapping of organic molecules and minerals; combined with a high-resolution camera (context imager)c. 50 μm per pixel (spectroscopy)
10.1 μm per pixel (context imager)
 SuperCamLaser-induced breakdown spectroscopy, Raman and time-resolved luminescence spectroscopy, and visible and infrared reflectance spectroscopy for remote (up to c. 12 m) mineralogy and elemental and molecular chemical characterization (including organic molecules); combined with a remote micro-imager0.5–5 mm per spot depending on technique and distance (spectroscopy)
c. 30 μm per pixel at 1.5 m (imager)
 PIXLX-ray fluorescence spectrometer to map the distribution and abundance variations of chemical elements at the sub-millimetre scale58 μm per pixel
Rosalind Franklin rover
 Panoramic camera (PanCAM)Two wide-angle stereo cameras, one high-resolution camerac. 170 μm per pixel at 2 m distance
 CLose UP Imager (CLUPI)Close-range (50 cm) ‘hand lens' imager for imaging rocks and drill powders7.8 μm per pixel
 Infrared Spectrometer for ExoMars (ISEM)Infrared spectrometer for remote mineralogical characterization and identification of rock targets3–10 cm per spot depending on distance
 Mars Multispectral Imager for Subsurface Studies (Ma_MISS)Visible and near-infrared spectroscopy to characterize the mineralogy of the walls of drilled boreholes120 μm spatial resolution
 MicrOmegaNear-infrared and visible light spectromicroscopy for spatially resolved characterization of minerals and organic molecules in drill powders20 μm per pixel
 Raman laser spectrometer (RLS)Raman spectrometry to identify mineralogy and organic matter in drill powdersSpot size c. 50 μm
 Mars Organic Molecule Analyzer (MOMA)UV laser desorption and pyrolysis (with or without derivatization agent), gas chromatography–mass spectrometry to identify and characterize organic molecules (alkanes, lipids, carboxylic acids, fatty acids, amino acids, nucleobases, amines, alcohols; chirality)N/A
Instrument nameDescriptionRelevant spatial resolution
Perseverance rover
 Mastcam-ZLong-range (2–100 m) multispectral, stereoscopic imager; wavelength selection using narrowband filters provides some mineralogical information150 μm per pixel to 7.4 mm per pixel depending on distance
 WATSONCamera for fine-scale imaging of textures and structures on the martian surface15.9 μm per pixel
 SHERLOCDeep UV Raman and fluorescence spectrometer for the detection and mapping of organic molecules and minerals; combined with a high-resolution camera (context imager)c. 50 μm per pixel (spectroscopy)
10.1 μm per pixel (context imager)
 SuperCamLaser-induced breakdown spectroscopy, Raman and time-resolved luminescence spectroscopy, and visible and infrared reflectance spectroscopy for remote (up to c. 12 m) mineralogy and elemental and molecular chemical characterization (including organic molecules); combined with a remote micro-imager0.5–5 mm per spot depending on technique and distance (spectroscopy)
c. 30 μm per pixel at 1.5 m (imager)
 PIXLX-ray fluorescence spectrometer to map the distribution and abundance variations of chemical elements at the sub-millimetre scale58 μm per pixel
Rosalind Franklin rover
 Panoramic camera (PanCAM)Two wide-angle stereo cameras, one high-resolution camerac. 170 μm per pixel at 2 m distance
 CLose UP Imager (CLUPI)Close-range (50 cm) ‘hand lens' imager for imaging rocks and drill powders7.8 μm per pixel
 Infrared Spectrometer for ExoMars (ISEM)Infrared spectrometer for remote mineralogical characterization and identification of rock targets3–10 cm per spot depending on distance
 Mars Multispectral Imager for Subsurface Studies (Ma_MISS)Visible and near-infrared spectroscopy to characterize the mineralogy of the walls of drilled boreholes120 μm spatial resolution
 MicrOmegaNear-infrared and visible light spectromicroscopy for spatially resolved characterization of minerals and organic molecules in drill powders20 μm per pixel
 Raman laser spectrometer (RLS)Raman spectrometry to identify mineralogy and organic matter in drill powdersSpot size c. 50 μm
 Mars Organic Molecule Analyzer (MOMA)UV laser desorption and pyrolysis (with or without derivatization agent), gas chromatography–mass spectrometry to identify and characterize organic molecules (alkanes, lipids, carboxylic acids, fatty acids, amino acids, nucleobases, amines, alcohols; chirality)N/A

On Earth, hydrothermal cherts as old as 3.5 Ga contain abundant kerogen-like carbonaceous matter suggested (although not conclusively demonstrated) to derive from Fischer–Tropsch type synthesis (Lindsay et al. 2005; Alleon et al. 2019) and it has been argued that ‘the abiotic organic output from [such] hydrothermal systems may overwhelm any early biospheric geochemical signal’ (Lindsay et al. 2005). On Mars, the structurally simple products of abiotic carbon fixation may be easier to interpret given the lack of metamorphic overprint compared with the Earth (assuming minimal degradation by diagenesis, oxidation and ionizing radiation).

Difficulty arises, however, from the fact that the relatively simple building blocks produced by abiotic carbon fixation can give rise to much more complex products, especially where thermodynamic disequilibrium is available to drive chemical self-organization; this much is evident from the existence of life on Earth. In other words, abiotic organic matter on Mars may have undergone transformations that are on the road to life (e.g. enantiomeric selection, metabolism-like reaction networks and autocatalytic cycles, the formation of complex polymers with repeating subunits, unexpected molecular weight distributions), but without reaching this destination. We lack a good understanding of these processes or of the diversity of molecular (or multimolecular) pseudofossils they might produce, although computational studies of prebiotic systems chemistry potentially offer some important clues (e.g. Wołos et al. 2020). If current models for the origin of life on Earth are any guide, then homochirality, polypeptides/proteins, RNA and DNA may all have emerged in prebiotic chemical reaction systems prior to the onset of Darwinian life (e.g. Orgel 2004; Brack 2007; Dalai et al. 2016; Erastova et al. 2017; Teichert et al. 2019; Xu et al. 2020), so even these are not necessarily unambiguous biosignatures by themselves.

None of this is to deny that anomalies or patterns in the overall molecular profile of martian organic matter could still be strongly suggestive of biosynthesis (despite pitfalls; even meteoritic carbon can apparently show a preference for odd-over-even carbon numbers; Westall et al. 2018). Some molecules – which, once life is established, it produces continuously – are too complex to assemble in large numbers without biologically evolved machinery (see Marshall et al. 2017 for a discussion of where the abiotic/biotic ‘threshold’ might be). If we are lucky, it may be possible to recognize such anomalies even if martian life is built from a significantly different core chemistry from life on Earth (Goesmann et al. 2017; Marshall et al. 2017). But timing is everything: sedimentary rocks at Jezero Crater and Oxia Planum were probably deposited within only a few hundred million years of the origin of life on Earth; even if they post-date an origin of life on Mars, it may be impossible to detect any biotic signal amid the complex products of a still largely ‘prebiotic’ carbon cycle (Lindsay et al. 2005).

Assessment of the biogenicity of organic matter (or any other candidate biosignature) will require close study of the geological context by the Rosalind Franklin or Perseverance rovers. An association between complex organic matter and evidence for local serpentinization, hydrothermal conditions favourable for Fischer–Tropsch type synthesis, or perhaps ferrocyanide salts (Sasselov et al. 2020), could be especially suggestive of abiotic/prebiotic chemistry rather than biotic chemistry. From this point of view, the lack of clear mineralogical evidence (so far) for local hydrothermal activity at the Oxia Planum landing site is reassuring. However, the large fluvial catchment area in this region may have concentrated organic matter of remote and diverse provenance and carbonate minerals in Jezero Crater could be related to serpentinization (Quantin-Nataf et al. 2021; Zastrow and Glotch 2021).

Conversely, any association between organic matter and other potential biosignatures (e.g. morphologies) could strengthen the case that life has been found. However, caution is needed again here. We lack a good understanding of how abiotic organic matter would have interacted with minerals and fluids on Noachian Mars and several forms of inorganic ‘pseudobiosignature’ might have adsorbed or passively entrained abiotic organic matter in some settings. In addition, organic matter itself can self-organize into life-like morphologies under some conditions (see following section on organic biomorphs).

Microbialites are microbially influenced organo-sedimentary structures that result from the trapping and binding of sediment and the authigenic precipitation of calcium carbonate and other minerals in benthic microbial communities (Burne and Moore 1987). The interplay between these biotically driven processes and extrinsic hydrodynamic, sedimentary and physicochemical conditions generates a wide variety of microbialite morphologies and textures, many of which have a fossil record on Earth reaching back to the Archean (Noffke et al. 2006; Baumgartner et al. 2019). The most abundant fossil microbialites are stromatolites and microbially induced sedimentary structures (MISS). Stromatolites are laminated growth structures that project upwards as cones, domes, ridges and columns, whereas MISS are less vertically extended and can be restricted to single bedding planes (Noffke et al. 2001). MISS include fossil microbial mats, under-mat textures and wrinkle structures formed in microbially biostabilized clastic sediments; these macroscopic forms are commonly accompanied by microtextural features such as oriented grains and crinkly organic-rich laminae (Noffke et al. 2001).

Microbialites have excellent preservation potential in carbonate, chert and siliciclastic facies and might easily be large enough to image at good spatial resolution using the Mars rover cameras and close-up imagers. Structures that resemble microbialites have been highlighted as attractive targets for sampling and return (Westall et al. 2015; Hays et al. 2017; Vago et al. 2017; McMahon et al. 2018). However, it is generally accepted that gross morphology alone is an unreliable indicator of the biogenicity of sedimentary structures and that (micro)textural and geochemical data will be necessary to confirm any tentative identification of microbialites on Mars (Noffke 2018). Relevant observations would include filamentous microfossils, crinkly carbon-rich laminae, fenestrae (fossilized gas bubbles, which can contain mineral grains indicative of local photosynthetic oxidation), oriented grains and grains ‘floating’ in an organic matrix (Noffke et al. 2001; Noffke 2018; Wilmeth et al. 2019). All of these features might (just) be large and distinct enough to resolve in situ using rover cameras (Table 1) if they are found in fresh drillcore (Noffke et al. 2001; Noffke 2018). Abiotic processes are also unlikely to mimic the conical form and regular spacing of some ancient stromatolites, features that are now understood to result from phototactic growth and competition for nutrients and light (e.g. Batchelor et al. 2004; Petroff et al. 2010). Microbialites that lack any of these features (or in which they cannot be detected by rover instruments) may be difficult to distinguish from pseudofossils. Indeed, there are several indications that pseudomicrobialites could have formed both on Earth and on early Mars.

The biogenicity of some stromatolite-like structures in very ancient (meta)sediments on Earth has often been contested (e.g. Grotzinger and Rothman 1996; Allwood et al. 2018; Zawaski et al. 2020). The presence of (pseudo)laminations can result from abiotic factors, including a variable energy/sediment supply during deposition and self-organization during crystallization, diagenesis, metamorphism and chemical weathering (Ortoleva 1994; Brasier et al. 2017, 2019; Allwood et al. 2018; Zawaski et al. 2020) (Fig. 1a). Domes and ridges can form via soft sediment or tectonic deformation (Antcliffe and McLoughlin 2008; Allwood et al. 2018). Grotzinger and Rothman (1996) showed that the laminations seen in some purported Precambrian stromatolites conform to the Kardar–Parisi–Zhang equation, which describes the growth of self-affine interfaces in terms of particle supply, surface-normal growth, random accretion and relaxation/diffusion. Because the Kardar–Parisi–Zhang equation captures the growth of a variety of interfaces, both biotic and abiotic, this result implies that organisms were not necessarily involved in shaping these laminations.

Fig. 1.

Pseudomicrobialites. (a) Laminated red siltstones draping the surface of gneiss boulders (Brasier et al. 2017). (b, c) Stromatolite-like laminated domes and branching columns formed by aerosolized colloidal paint sprayed onto flat surfaces (McLoughlin et al. 2008). Images reproduced with permissions.

Fig. 1.

Pseudomicrobialites. (a) Laminated red siltstones draping the surface of gneiss boulders (Brasier et al. 2017). (b, c) Stromatolite-like laminated domes and branching columns formed by aerosolized colloidal paint sprayed onto flat surfaces (McLoughlin et al. 2008). Images reproduced with permissions.

McLoughlin et al. (2008) showed experimentally that aerosolized colloidal paint sprayed onto a flat surface generates laminated deposits with remarkably stromatolite-like domes and columns, albeit on a small scale (column width <1 cm) (Fig. 1b, c). Many similar examples have been collected from factory floors where spray paint is applied to cars. The ballistic deposition of colloids (which can also be modelled using the Kardar–Parisi–Zhang equation) thus seems to be a plausible abiotic mechanism for the origin of stromatolite-like morphologies in the calcareous and siliceous deposits found in hot spring ‘splash zones’ on Earth. Such deposits commonly contain fossil bacteria, but this does not necessarily mean that bacteria were instrumental in producing the macroscopic stromatolite-like growth pattern (McLoughlin et al. 2008). Small-scale, dendritic stromatolite- (and thrombolite-) like forms can also result from diffusion-limited aggregation at high surface tension (Duarte-Neto et al. 2014).

Less is known about how pseudo-MISS might form, but Davies et al. (2016) emphasized that particle-sticking, loading, fluid escape, impression, shear and shrinkage can generate complex, ‘MISS-like’ sedimentary surface textures in sufficiently cohesive and plastic sediments. They provide examples from modern and ancient settings where abiotic factors have imbued sediments with high viscosity and cohesivity, mimicking some of the patterns and textures associated with biostabilization (Davies et al. 2016).

We speculate that two general attributes of depositional environments on early Mars may have been especially conducive to the formation of pseudomicrobialites. First, fine-grained clay-rich sediments that were presumably not bioturbated by animals would have been naturally cohesive and thus able to form and retain a variety of sedimentary structures that might be mistaken for fossil MISS (Davies et al. 2016). Direct evidence for a high degree of sediment cohesion on early Mars has been discovered at Gale Crater in the form of fossil subaqueous shrinkage cracks, a sedimentary structure sometimes associated with microbial biostabilization on Earth (Siebach et al. 2014; McMahon et al. 2017).

Second, aqueous fluids interacting with early martian sediments may commonly have been rich in silica, salts and other dissolved minerals liable to precipitate as cements and crusts near the sediment–water(–atmosphere) interface, further enhancing sediment cohesion and potentially generating intrastratal cracks, polygons, tepee structures and related macroscopic effects that may superficially mimic MISS (McLennan et al. 2005). Pseudomicrobialites might also have adsorbed and absorbed a certain amount of abiotic organic matter from the environment as carbon-rich laminae (e.g. from ‘primordial oil slicks’; Nilson 2002).

The effects of post-depositional processes may also confound the detection of true microbialites on Mars. Many martian outcrops are sculpted by wind abrasion and are unlikely to display well-preserved textures on bedding planes unless they have been very recently exposed. Irregular textures and forms that seem to resemble microbialites can result merely from the vagaries of erosion. Thus the MISS-like features identified by Noffke (2015) in Curiosity rover imagery from Gale Crater appear not to be primary sedimentary structures (Davies et al. 2016; McMahon et al. 2018).

Sinter-like hot spring silica deposits are unlikely to be encountered by the Perseverance or Rosalind Franklin rovers, but were previously observed by the Spirit rover in Gusev Crater (Ruff and Farmer 2016). This opaline deposit consists of porous, nodular material with millimetre- to centimetre-scale finger-like extensions, resembling fossil-microbe-bearing silica structures from hot springs on Earth described as ‘microbially mediated microstromatolites’ (Ruff and Farmer 2016; Ruff et al. 2020). A potential abiotic explanation for this morphology is that the silica precipitated evaporatively from sprayed or splashed droplets or accumulated from the ballistic deposition of suspended particles (McLoughlin et al. 2008). Experimental work to refine and test this hypothesis would be worthwhile.

Mars rovers are not designed or equipped to detect microfossils of bacterial cell size in situ (Table 1). On Earth, some Archean cellular fossils are >100 μm across, but these are carbonaceous compressions and cannot be visualized clearly until they have been macerated out of the host rock with hydrofluoric acid (Javaux et al. 2010). Many Proterozoic and younger cherts on Earth contain morphologically diverse filamentous and spheroidal microorganisms preserved by carbonaceous material, which can also be hundreds of micrometres in maximum dimension (e.g. Barghoorn and Tyler 1965; Schopf 1968; Garwood et al. 2020). However, these cannot be visualized clearly except in finely polished rock slabs or petrographic thin sections, which will not be produced by the rovers in situ. Nevertheless, pseudofossils on the scale of micrometres to centimetres may confound the search for life on Mars for two reasons. First, objects at the upper end of this size range will be visible to rover cameras and may be associated with other apparent lines of evidence for biogenicity (e.g. organic matter). Second, objects at the lower end may be detected by microscopy in samples cached by the Perseverance rover if and when they are eventually returned to Earth, or in future studies of martian meteorites.

The term ‘biomorph’ is particularly associated with carbonate–silica precipitates, but is used here in a wider sense to describe all small abiotic structures that bear a morphological resemblance to living or fossil microbes (including, for example, mineralized extracellular sheaths). Biomorphs have been discovered in numerous reaction–diffusion–precipitation systems, both in nature and in the laboratory, some of which are more familiar to palaeontologists than others. Chemical gardens were discovered in the seventeenth century and their potential to misleadingly resemble fossils has long been recognized (Liesegang 1914; Hawley 1926), but bears repeating (McMahon 2019). For reasons not altogether clear, candidate fossils are often compared with carbonate–silicate biomorphs, even when other known classes of biomorph are more similar (e.g. Dodd et al. 2017; Gan et al. 2021).

Classical chemical gardens

First described at the dawn of modern chemistry (Glauber 1646), chemical gardens are plant-like structures formed by reactions between transition metal salts and aqueous anionic solutions of, for example, silicate (Barge et al. 2015) (Fig. 2a–d). In the classic chemical garden experiment, a salt seed crystal begins to dissolve in a sodium silicate solution (c. pH 12), releasing acid that reacts spontaneously with the alkaline medium to produce a semipermeable membrane of gelatinous silica around the crystal (within seconds to minutes). Osmotic inflow increases the pressure inside the membrane until it ruptures, expelling a jet of acidic fluid that tends to rise buoyantly. New silica membrane ensheaths the expelled fluid, forming a thin tube that connects to the rupture point and is contiguous with the original membrane envelope. The tube may remain open at the tip and continue to grow for some time; it may also produce branches of equal or lesser thickness. Multiple tubes may develop from a single seed crystal (Fig. 2a). Growth of the chemical garden continues until the seed crystal has fully dissolved.

Fig. 2.

(a–d) Chemical gardens and (e–k) carbonate–silica biomorphs. (a) Rosettes of tubes emerging from seed crystals. (b) Serially branching, irregularly curved tubes. (c) Snail-like coiled tube. (d) Siliceous tube with rough Fe (oxyhydr)oxide-coated interior and hollow central cavity. (e, f) Worm-like braid, (g) helicoidal and (h) mushroom-like biomorphs. (i) Composite of globular, sheet-like and helicoidal morphologies. (j) Close-up of the area depicted by the white rectangle in part (i) showing dendrites produced by fractal growth. (k) Close-up of thin sinuous filaments and globular amorphous silica. Chemical garden images SM (parts a–c) or reproduced from McMahon (2019) under creative commons license (creativecommons.org/licenses/by/4.0/) (part d). Images of carbonate–silica biomorphs courtesy of J. Rouillard and S. Borenstazjn (Institut de Physique du Globe de Paris) (parts e–h) and P. Knoll and O. Steinbock (Florida State University) (parts i–k).

Fig. 2.

(a–d) Chemical gardens and (e–k) carbonate–silica biomorphs. (a) Rosettes of tubes emerging from seed crystals. (b) Serially branching, irregularly curved tubes. (c) Snail-like coiled tube. (d) Siliceous tube with rough Fe (oxyhydr)oxide-coated interior and hollow central cavity. (e, f) Worm-like braid, (g) helicoidal and (h) mushroom-like biomorphs. (i) Composite of globular, sheet-like and helicoidal morphologies. (j) Close-up of the area depicted by the white rectangle in part (i) showing dendrites produced by fractal growth. (k) Close-up of thin sinuous filaments and globular amorphous silica. Chemical garden images SM (parts a–c) or reproduced from McMahon (2019) under creative commons license (creativecommons.org/licenses/by/4.0/) (part d). Images of carbonate–silica biomorphs courtesy of J. Rouillard and S. Borenstazjn (Institut de Physique du Globe de Paris) (parts e–h) and P. Knoll and O. Steinbock (Florida State University) (parts i–k).

Although initially soft and flexible, chemical garden tubes harden and become brittle as metal (oxyhydr)oxides precipitate on their interior walls (McMahon 2019; Kotopoulou et al. 2021) (Fig. 2d). The tubes are typically highly circular in cross-section and can show a variety of interesting biomimetic morphologies formed during growth, including helical twisting, coiling (Fig. 2c), pinching, swelling, tapering, sinuously curving growth trajectories, serial bifurcation (branching) (Fig. 2b) and occasional anastomosis – that is, the reconnection of independent branches (Leduc 1911; McMahon 2019). Tube diameters range from micrometres to several millimetres depending on the experimental conditions, with a wall thickness controlled by the extent of metal oxyhydroxide and silica precipitation, which can largely occlude the internal space (resulting in a porous, but ‘filled’, filament rather than an open tube; McMahon 2019).

Many variations on this theme have been explored, including chemical gardens formed on the injection of acidic solutions rather than the dissolution of salts, ‘inverse' chemical gardens formed on the injection of the alkaline solution into the acid and quasi-2D chemical gardens confined in a narrow space between two flat plates (see Barge et al. 2015 for review). It is clear that chemical gardens can produce tubules from naturally occurring alkaline solutions and minerals, so they should not be dismissed as ‘exotic’ to natural environments (García-Ruiz 2000; García-Ruiz et al. 2017; McMahon 2019; McMahon et al. 2021).

As their name implies, chemical gardens are misleadingly life-like. Once solidified, they resemble fossil microorganisms, particularly Fe-mineralized fossil bacteria and fungi, in size, shape and composition. They may be relevant to the remarkable profusion of filaments composed of metal oxides, oxyhydroxides and (alumino)silicates found in siliceous and calcareous mineral deposits of all ages on Earth, including cavity fills in many volcanic and metavolcanic rocks (McMahon 2019; McMahon and Ivarsson 2019; McMahon et al. 2021). Many of these are probably fossils – indeed, fossils from a deep biosphere hosted in igneous rocks, with special relevance to some scenarios for life on Mars – but some are probably not and may result from chemical-garden-like processes and/or other types of self-organization that lead to filamentous crystals and aggregates (e.g. Hopkinson et al. 1998; Oaki and Imai 2003; Toramaru et al. 2003; Bonev et al. 2005).

The biotic interpretation receives support from the observed mineralizing behaviour of some modern organisms. Filamentous Fe-oxidizing bacteria, such as those in the SphaerotilusLeptothrix group, produce Fe-oxyhydroxide sheaths that conform to the filament surface, producing tubes that can bifurcate where cells divide, and are commonly vacated by cells leaving little or no organic residue (Emerson and Moyer 2002; Chan et al. 2016). The sheath exteriors can accumulate a flocculent Fe-oxyhydroxide coating up to several tens of micrometres thick (Schmidt et al. 2014). These microstructures are easily preserved in a silica matrix (chert) or in calcium carbonate and have a putative fossil record reaching back over million- to billion-year timescales (Dodd et al. 2017; Georgieva et al. 2021), although some of these purported fossils may be abiotic (Hopkinson et al. 1998; McMahon 2019; Johannessen et al. 2020; McMahon et al. 2021). Other Fe-oxidizing bacteria (e.g. Gallionella, Mariprofundus) secrete twisted, ribbon-like ‘stalks’ composed largely of Fe-oxhydroxides, which likewise can bifurcate during cell division (Chan et al. 2016). Again, however, there is a distinct potential for chemical gardens and other processes of crystallization and polycrystalline aggregate formation to generate twisted ribbons and other helical forms (Leduc 1911; García-Ruiz 2000; Oaki and Imai 2003; Jordan 2008).

Natural chemical gardens could plausibly have formed as a consequence of chemical weathering on Mars (García-Ruiz 2000; García-Ruiz et al. 2020; Sainz-Díaz et al. 2021). Soluble Fe and Mg sulfate salts have been identified at various martian localities (Johnson et al. 2007; Bishop et al. 2009; Ojha et al. 2015). Many of these likely formed in part through the dissolution and leaching of basaltic silicate minerals by sulfur-rich, acidic, oxidizing fumarolic fluids and vapours, which can be efficient even at very low temperatures (Tosca et al. 2004; Niles et al. 2017; Ruff et al. 2020); others probably formed by the aqueous oxidation of sulfide minerals (e.g. Dehouck et al. 2012). These sulfates would produce chemical gardens if introduced (as solids or in solution) to sufficiently silica-rich, alkaline fluids (e.g. in the subsurface).

Such fluids would have been supplied in some localities by serpentinization (i.e. the reaction of water with mafic and ultramafic minerals) and by the alteration of serpentinites, which, on Earth, can generate natural waters in which chemical gardens grow readily (García-Ruiz et al. 2017). Mineral assemblages suggestive of local serpentinization and serpentine alteration occur at several localities on Mars, including Jezero Crater (Ehlmann et al. 2010; Michalski et al. 2018; Brown et al. 2020; Zastrow and Glotch 2021). More generally, the copious production of silica-rich fluids on early Mars is attested by the widespread occurrence of hydrated silica deposits in fluviolacustrine and groundwater-influenced settings (Pan et al. 2021). It has been shown experimentally that chemical gardens can form even at temperatures and pressures characteristic of Amazonian and present-day Mars, close to the H2O triple point (Sainz-Díaz et al. 2021).

Carbonate–silica biomorphs

Carbonate–silica biomorphs are strikingly biomorphic inorganic objects composed of amorphous silica and crystalline carbonates of the alkaline earth metals (Ba, Sr or, more rarely, Ca) (Fig. 2e–k). First described by Juan Manuel García-Ruiz in the early 1980s (García-Ruiz and Amorós 1981a, b), they are formed in the laboratory through the slow crystallization of a carbonate phase under moderately alkaline conditions (c. pH 8.5–11) in the presence of silica, originally present as a silica gel or, in more recent work, in solution. They display dimensions ranging from a few micrometres to a few hundred micrometres and can adopt a wide diversity of life-like morphologies, most of which can be classified into three categories: (1) helicoidal filaments (Fig. 2g, i); (2) worm-like braids (Fig. 2e, f); and (3) leaf-like flat sheets (Fig. 2i) (Kellermeier et al. 2012c). Under some conditions, more atypical morphologies – such as flower-like forms, ‘trumpets’, ‘corals’, ‘moths’, ‘snails’ or ‘mushrooms’ (Fig. 2h) – can also be found (Opel et al. 2018; Rouillard et al. 2018).

In addition to their curved or sinuous overall shapes, in appearance more akin to the living than to the mineral world, carbonate–silica biomorphs also display complex internal structures and textures that are reminiscent of biological objects. They frequently possess a core–shell structure, with an enveloping ‘skin’ of amorphous silica and an internal core composed of aggregated carbonate nanocrystals. The following section on mineralogical signatures shows that the polycrystalline core of the carbonate–silica biomorphs can be described as a quasi-mesocrystal, a characteristic of minerals formed by living organisms.

The complex morphologies of the carbonate–silica biomorphs emerge from purely inorganic mineral growth mechanisms. In an initial fractal growth stage, dendrites (Fig. 2j), dumbbells, framboids and spheroids are formed. Fractal growth here is due to silica poisoning of the surface of the carbonate crystallites, causing them to repeatedly split at non-crystallographic angles. In a second stage called ‘curvilinear growth’, polycrystalline mineral sheets grow radially in two dimensions, forming flat structures such as discs and leaves. Curling at the margins of these sheets introduces curvature and leads to the development of twisted shapes, such as helicoidal filaments and braids (García-Ruiz et al. 2009; Kellermeier et al. 2012a; Rouillard et al. 2018). The growth of these curling sheets is fed by an autocatalytic process in which carbonate precipitation locally decreases the pH, triggering the polymerization of amorphous silica, coating and cementing the carbonate crystallites and preventing further growth. In turn, silica polymerization locally increases the pH, allowing the precipitation of new carbonate building blocks (Kellermeier et al. 2012b).

Although purely inorganic, the curved and sinuous shapes of the biomorphs evoke biological objects, such as helical and segmented filamentous microbes, protists and even plants and animals. Interestingly, the hydrophobic surfaces of carbonate–silica biomorphs readily incorporate or adsorb organic molecules (García-Ruiz et al. 2002; Opel et al. 2016), which, as already discussed here, may have an abiotic origin on Mars. Although they have (so far) not been observed to form spontaneously in the environment, carbonate–silica biomorphs were obtained experimentally from natural alkaline silica-rich spring waters derived from serpentinization environments (García-Ruiz et al. 2017) and they may have formed in some hydrothermal environments of the early Earth (García-Ruiz 1994; García-Ruiz et al. 2020). Similar geochemical conditions, also conducive to the formation of chemical gardens, may have prevailed in alkaline, silica-rich fluids associated with serpentinization on early Mars.

Fibrous crystals, trichites and other crystallites

Strong or irregular curvature induced during the growth or deformation of fibrous or acicular crystals can generate shapes reminiscent of filamentous microorganisms. Muscente et al. (2018) described curving Mn oxide (MnO) crystals of probable metasomatic origin preserved in Neoarchean chert from the Pilbara Craton of Australia and noted that their simple morphology could be compared with some purported filamentous microfossils. In addition to Mn oxides, many clay and serpentine group minerals known or predicted to exist on Mars also show a fibrous habit, including sepiolite–palygorskite, celadonite and serpentine (Bishop et al. 2008; Ehlmann et al. 2010; Bristow and Milliken 2011). In addition, spectacularly complex and varied thread-like crystallites (‘trichites’) of pyroxene and other igneous minerals are found in volcanic and impact-related glasses, formed by the quenching of molten rock. Glass fragments are expected to be widespread in wind-blown sediments on Mars, albeit in a chemically weathered condition (Horgan and Bell 2012).

On Earth, trichites in natural glass are readily visible in thin section, where their resemblance to fossil microorganisms was first noted by Cloud (1976). They can be tightly coiled, looped, branched and irregularly curving (worm-like); they are sometimes found in spider-like starburst arrangements (Ross 1962; Engelhardt et al. 1995) (see Fig. 4a). They are commonly subdivided into smaller aligned crystallites, giving them a segmented appearance. Trichites commonly nucleate on the walls of vesicles formed by trapped volatiles. Glass vesicles themselves can also resemble microfossils, as noted with respect to some scoria fragments found in the 3.4-Gyr-old Strelley Pool Formation of Western Australia, where vesicles are coated with kerogen-like carbonaceous material (Wacey et al. 2018).

It is unlikely that fibrous crystals, trichites and other crystallites would be large and distinct enough to resolve with Mars rover cameras (Table 1) and yet at the same time small enough to resemble microorganisms. They may be discovered in returned samples, but if they are well preserved, then it would then be straightforward to exclude them from consideration as microbial fossils because they can be recognized by their composition, crystallographic parameters and angular, faceted cross-sections. Diagnosis may be more difficult, however, where mineral particles have decomposed or altered to produce substances and morphologies more similar to mineralized microfossils, with softened/rounded cross-sections and hollow interiors. Thus, we tentatively suggest that solid and hollow filaments observed in impact glass by Sapers et al. (2014) could be modified trichites of some kind (cf. Pickersgill et al. 2021).

McMahon et al. (2021) described inorganic (Mg silicate + Fe oxide) filamentous dubiofossils occurring in calcite veins from the pervasively oxidized serpentinites of NW Italy and speculated that they might represent coated and recrystallized mineral fibres, among other possible explanations. A misleading association with organic matter can also complicate the interpretation of mineral grains. Horodyski (1981) noted that apatite grains in a Mesoproterozoic shale had acquired a coating of organic matter that created a superficial resemblance to fossil microorganisms. Similarly, Wacey et al. (2016b) showed that carbonaceous microstructures in the 3.5-Gyr-old Apex Chert, previously interpreted as fossil filamentous bacteria, are, in fact, altered particles of potassium mica, which were expanded into worm-like structures (the mineral vermiculite) by hydrous alteration and then coated at a late stage by carbon ‘moving around the system'. Hematite aggregates in the same chert unit are also filament-like and have been described as ‘pseudomicrofossils’ (Marshall et al. 2011). Even genuine microfossils can be secondarily enriched in carbon from such external sources (Rasmussen et al. 2021).

According to biogenicity determination protocols, life-like morphologies with organic composition score more highly than inorganic life-like morphologies (e.g. McLoughlin and Grosch 2015; Neveu et al. 2018). Nevertheless, organic materials are no less capable than mineral particles of forming a wide variety of biomorphs; indeed, structural self-organization in the organic milieu necessarily preceded the origin of life on Earth (and perhaps Mars). Known organic biomorphs can be divided into the recently discovered carbon–sulfur biomorphs and the morphologically simpler spheroids that result from hydrophobic interactions with water. We are aware that chemical gardens can also be produced from organic salts and solutions, but (so far) the known examples are of limited geological relevance (e.g. Bernini et al. 2021).

Carbon–sulfur biomorphs

Carbon–sulfur biomorphs are microscopic spherical and tubular objects composed of elemental sulfur encapsulated within an organic envelope (Fig. 3). Their sizes range from a few tens of nanometres to a few micrometres in diameter. Carbon–sulfur biomorphs form spontaneously in aqueous solutions in which hydrogen sulfide is oxidized in the presence of dissolved organic molecules (including simple prebiotic organic molecules such as glycine) (Cosmidis and Templeton 2016; Cosmidis et al. 2019). The elemental sulfur core of the biomorphs is the product of chemical sulfide oxidation, while their organic envelope is thought to form through the self-assembly of amphiphiles produced by the reaction of organic molecules with sulfides and polysulfides in solution (Cosmidis et al. 2019). Observations of the early stages of carbon–sulfur biomorph formation reveal numerous empty vesicles, suggesting that the organic envelope may form prior to the sulfur core (Fig. 3c).

Fig. 3.

Carbon–sulfur biomorphs. (a) Complex network formed by filaments and spheres. (b) Rosette. (c) Empty organic vesicles during early stages of carbon–sulfur biomorph formation. Small organic vesicles later coalesce into c. 1 μm spheres. (d) Aggregate of spheres and filaments. (e) Spheres with visible organic envelopes. (f) Straight and helical filaments. Images adapted from Nims et al. (2021) (parts a and b) or JC (parts c and f) and courtesy of C. Nims (University of Michigan) (parts d and e).

Fig. 3.

Carbon–sulfur biomorphs. (a) Complex network formed by filaments and spheres. (b) Rosette. (c) Empty organic vesicles during early stages of carbon–sulfur biomorph formation. Small organic vesicles later coalesce into c. 1 μm spheres. (d) Aggregate of spheres and filaments. (e) Spheres with visible organic envelopes. (f) Straight and helical filaments. Images adapted from Nims et al. (2021) (parts a and b) or JC (parts c and f) and courtesy of C. Nims (University of Michigan) (parts d and e).

Fig. 4.

Other types of organic and inorganic biomorphs. (a) Asteroidal trichites radiating from central magnetite grains in a natural volcanic glass (Cougar Mountain, Oregon). (b) Organic microspheres obtained from RNA and quartz mixtures under diagenetic conditions (Criouet et al. 2021). (c) Amphiphilic spherical and tube-like vesicles formed by mixed fatty acids and 1-alkanols (C10–C15) in 10 mM CaCl2. Courtesy of S.F. Jordan. (d) Coacervate microdroplets prepared in water by mixing PDDA with ATP (M. Li et al. 2014). (e, f) Chain-forming and twinning proteinoid microspheres obtained by heating mixtures of amino acids (Fox and Yuyama 1963). (g, h) Apatite particles formed by double diffusion in gelatin mimicking dividing cells and raised polygonal features in embryos (Crosby and Bailey 2017). (i) Rod-shaped silica particles formed on the walls of basalt fractures injected with supercritical CO2 (Schaef et al. 2011). (j) Cryogenic opal filaments and sheets formed in rapidly freezing silica-rich fluids (Channing and Butler 2007). (k) Cryogenic carbonate segmented filaments obtained by freezing of silica-rich alkaline brines (Fox-Powell and Cousins 2021). (l) Rod-shaped apatite particles forming within organic films in sediments (Mänd et al. 2018). (m) Fluoroapatite particle precipitated in the presence of citrate, mimicking dividing coccoid cells (Wu et al. 2010). Images reproduced with permissions (parts a, d–h, j–m) or under creative commons licenses (part b, creativecommons.org/licenses/by-nc-nd/4.0/; part i, creativecommons.org/licenses/by-nc-nd/3.0/).

Fig. 4.

Other types of organic and inorganic biomorphs. (a) Asteroidal trichites radiating from central magnetite grains in a natural volcanic glass (Cougar Mountain, Oregon). (b) Organic microspheres obtained from RNA and quartz mixtures under diagenetic conditions (Criouet et al. 2021). (c) Amphiphilic spherical and tube-like vesicles formed by mixed fatty acids and 1-alkanols (C10–C15) in 10 mM CaCl2. Courtesy of S.F. Jordan. (d) Coacervate microdroplets prepared in water by mixing PDDA with ATP (M. Li et al. 2014). (e, f) Chain-forming and twinning proteinoid microspheres obtained by heating mixtures of amino acids (Fox and Yuyama 1963). (g, h) Apatite particles formed by double diffusion in gelatin mimicking dividing cells and raised polygonal features in embryos (Crosby and Bailey 2017). (i) Rod-shaped silica particles formed on the walls of basalt fractures injected with supercritical CO2 (Schaef et al. 2011). (j) Cryogenic opal filaments and sheets formed in rapidly freezing silica-rich fluids (Channing and Butler 2007). (k) Cryogenic carbonate segmented filaments obtained by freezing of silica-rich alkaline brines (Fox-Powell and Cousins 2021). (l) Rod-shaped apatite particles forming within organic films in sediments (Mänd et al. 2018). (m) Fluoroapatite particle precipitated in the presence of citrate, mimicking dividing coccoid cells (Wu et al. 2010). Images reproduced with permissions (parts a, d–h, j–m) or under creative commons licenses (part b, creativecommons.org/licenses/by-nc-nd/4.0/; part i, creativecommons.org/licenses/by-nc-nd/3.0/).

As a result of their spherical and tubular morphologies, carbon–sulfur biomorphs are reminiscent of microbial spherical and filamentous cells. These structures display more complex morphologies than the spheroids and aggregates produced by other known biomorph systems (see previous section). The tubular biomorphs may branch at 90° and 45° angles (Cosmidis and Templeton 2016), similar to some filamentous bacteria (e.g. Streptomyces), and they can be helicoidal (Fig. 3f), similar to helical bacteria (e.g. cyanobacteria of the genus Oscillatoria, spirochaetes). Tubular carbon–sulfur biomorphs can also form rosettes (Fig. 3b), mimicking those formed by filamentous microbes such as Thiothrix.

Although carbon–sulfur biomorphs are originally composed of organic carbon and elemental sulfur, experiments have shown that their sulfur core rapidly diffuses away during early diagenesis in silica-rich environments, leaving behind empty organic envelopes (Nims et al. 2021). The morphologies of the biomorphs are finely preserved through this diagenetic process as a result of the rapid precipitation of nanocolloidal silica at the surfaces of the organic spheres and tubes (Nims et al. 2021). The resulting silicified organic microstructures are strikingly similar to coccoidal and filamentous organic microfossils preserved in Precambrian cherts by the rapid precipitation of silica at the seafloor, as found, for instance, in the 1.9-Gyr-old Gunflint Formation in Canada (Wacey et al. 2013) or the c. 2.4-Gyr-old Turee Creek Group in Western Australia (Schopf et al. 2015; Barlow and Kranendonk 2018).

Mars has long been considered a ‘sulfur-rich planet’ (King and McLennan 2010), but, as a result of the oxidizing conditions at the surface, the vast majority of this sulfur is currently present as sulfate minerals (Franz et al. 2019). However, in situ sulfur isotope analyses acquired by NASA's Curiosity rover in Gale Crater suggest the existence of an active and fully developed sulfur redox cycle on early Mars (Franz et al. 2017). Evolved gas analyses performed by Curiosity's SAM instrument showed that reduced sulfur phases are present within ancient fluviolacustrine sediments at Gale Crater (McAdam et al. 2014; Wong et al. 2020). SAM also detected evidence for sulfurized organic matter in the 3.5-billion-year-old Murray Formation, indicating interactions between organic molecules and reduced sulfur (Eigenbrode et al. 2018; Heinz and Schulze-Makuch 2020).

Although the full space of physicochemical parameters permitting the formation of carbon–sulfur biomorphs remains to be explored, they have been synthetized in the laboratory at temperatures ranging from 4°C to room temperature, pH values ranging from acidic (c. pH 4) to slightly basic (c. pH 8) and salinities ranging from c. 0% (deionized water) to 3.5% (seawater), encompassing plausible conditions for wet environments on early Mars (Fukushi et al. 2019). As stated earlier, carbon–sulfur biomorphs can be finely preserved through silicification in silica-rich depositional settings, mimicking fossilization in cherts, a major preserving medium for many Archean and Proterozoic putative microfossils on Earth (Schopf 2006; Javaux and Lepot 2018). On Mars, rapidly forming silica deposits may have formed in different types of ancient sedimentary environments (reviewed by McMahon et al. 2018), allowing the preservation of carbon–sulfur biomorphs if they were ever present on that planet.

Other organic biomorphs

Most organic compounds are hydrophobic and tend to aggregate into spheres in the presence of water, commonly with dimensions similar to microorganisms. Thus, spherical organic particles were probably fairly abundant in any prebiotic milieu on early Mars (and Earth). Some of them would have had non-negligible potential to be preserved in the rock record. For example, research in applied chemistry has found that complex organic matter subjected to ‘hydrothermal carbonization’ (devolatilization in water at c. 200°C) assembles into stable, solid spheres similar in size to bacteria, with hydrophobic aromatic cores and hydrophilic shells (‘hydrochar’; Sevilla and Fuertes 2009).

Criouet et al. (2021) found that similar spheres were formed when a mixture of RNA, quartz and water was held at 200°C under Ar for 20 days. These objects were c. 0.5–5 μm in diameter, variously textured and commonly connected together like dividing cells (Fig. 4b). Their composition, as probed, for example, by carbon X-ray absorption near-edge structure (C-XANES), resembles fossil bacteria more closely than it resembles the original RNA. Criouet et al. (2021) infer from previous experimental work on hydrochar that further diagenetic alteration of these structures could render them hollow and thus even more similar to fossil bacteria. The viability of an RNA world on early Mars has been explored – and broadly supported – in light of geochemical considerations (Mojarro et al. 2021), but, in any case, similar spheroids can very probably result from many other organic precursors. Indeed, similarly robust hollow hydrocarbon spheroids <1–50 μm in diameter were recovered from deep groundwater in the Witwatersrand Basin of South Africa, where they appear to have formed through the abiotic reorganization of thermally altered (ultimately biogenic) organic matter (Wanger et al. 2012). Sub-micron hollow organic ‘globules’ have also been identified in carbonaceous meteorites (Nakamura-Messenger et al. 2006).

Fatty acids produced by abiotic Fischer–Tropsch type reactions under hydrothermal conditions, like other amphiphilic compounds, readily self-assemble in water to form membranous vesicles from nanometres to hundreds of micrometres in size. Such vesicles may have played a part in the origin of life by encapsulating protocells (e.g. Deamer 2017). The stability of these vesicles under different conditions depends on the mixture of amphiphiles present. Experiments have shown that relatively long-chain (C10–C15) fatty acids and 1-alkanols generate vesicles in the warm, saline, alkaline waters characteristic of serpentinization-driven marine hydrothermal systems on the early Earth and Mars (Fig. 4c) (Jordan et al. 2019). Vesicle formation by fatty acids is also favoured over a wide pH range in non-marine hot spring settings (Deamer 2021). Lipid vesicles are typically spheroidal, but can extend into tubules and thread-like filaments (e.g. Zhu and Szostak 2009; Deamer 2021). The potential for any of these rather delicate structures to be preserved as morphological fossils is unclear, but has sometimes been mooted (e.g. Javaux et al. 2013).

Other structures discussed in prebiotic chemistry also have relevance as potential pseudofossils. Coacervates – microdroplets of viscous fluid that separate out from a colloidal solution (Fig. 4d) – can incorporate a variety of inclusion structures and were first suggested as possible protocells nearly a century ago (Oparin 1924). Coacervates have been produced from mononucleotides and peptides of surprisingly low molecular weight (Koga et al. 2011). Other coacervates based on similarly small molecules have been silicified in the laboratory to form solid spheroids with multiple sub-compartments, albeit through a rather non-naturalistic chemical process (Fothergill et al. 2014).

‘Proteinoid microspheres’ represent another spheroidal biomorph system once thought to be a plausible model for prebiotic protocells. These were discovered by Sidney Fox and co-workers, who showed that spheroids 1–2 μm in diameter self-assemble from thermally polymerized mixtures of dry amino acids (e.g. at >130°C for 3 h) after the addition of water (e.g. Fox and Yuyama 1963; Brooke and Fox 1977). These objects show a range of biomimetic features, including internal spheroids, sharply defined single or concentric double boundaries, ‘twinned’ growth strongly reminiscent of cells dividing, and aggregation into chains and networks (Fig. 4e, f). These pseudo-cells could presumably have arisen spontaneously on the early Earth or Mars if amino acids (e.g. from meteorites, atmospheric chemistry and hydrothermal reactions) became highly concentrated and subject to dry heat. It has been shown that some of these proteinoid microspheres are readily silicified to form pseudofossils with good preservation potential that can resemble eukaryotes as well as prokaryotes (Francis et al. 1978). Thus, as noted earlier, the availability of silica in both groundwaters and surface waters on early Mars could have assisted the preservation of both pseudofossils and fossils.

Very few natural or experimental systems have yet been studied in relation to their capacity to produce biomorphs in geochemically plausible settings, yet there are some tantalizing hints scattered across the scientific literature. For example, Oaki and Imai (2003) demonstrated the formation of smoothly curving filamentous dendritic aggregates from the precipitation of potassium dichromate in gelatin cooled from 100°C, a finding that may be relevant to the origin of similar structures found in some agates (which precipitate from silica gel). More generally, minerals grown in gels can sometimes adopt rounded and complex shapes (e.g. Dominguez Bella and García-Ruiz 1987; Crosby and Bailey 2017) (Fig. 4g, h).

Silica deposits formed on the walls of basalt fractures injected with wet, supercritical CO2 at sterilizing temperatures resemble rod-shaped and filamentous bacteria (Schaef et al. 2011) (Fig. 4i). Biomorphic particles of opal (Channing and Butler 2007) and carbonates (Fox-Powell and Cousins 2021) resembling microbial filaments precipitate from rapidly freezing mineral-laden waters (Fig. 4j, k), a process which may be particularly relevant for ancient hydrothermal systems on Mars. Abiotic silica spheroids found in hot spring ponds of the Dallol geothermal field, Ethiopia form botryoidal clusters that resemble coccoidal bacterial colonies (Belilla et al. 2019). All these systems require further investigation to elucidate new classes of geologically relevant biomorphs on Mars.

In addition to these processes, mineral structures can often adopt rounded, curved or complex life-like shapes when formed in the presence of organic molecules (which can be abiotic in origin), as already illustrated for carbon–sulfur biomorphs. More generally, ‘organominerals’ (i.e. minerals in which formation is mediated by organic molecules) (Défarge 2011) can present unusual, non-crystallographic morphologies as a result of the templating effect of the organic matrices on which they nucleate, or under the influence of organic molecules in solution during mineral growth. Soluble organic molecules can influence mineral shapes by poisoning some crystal faces after preferential adsorption, preventing further growth, or by stabilizing amorphous precursors and favouring their assembly into complex structures (Gower 2008). Organic molecules can promote the fractal growth of crystals, leading to the formation of rod-shaped particles (Fig. 4l), dumbbells, spherules, divided spheroids mimicking cell division (Fig. 4g, h, m) and ‘cauliflower-like’ structures (Busch et al. 1999; Wu et al. 2010; Sand et al. 2012; Crosby and Bailey 2017; Mänd et al. 2018).

A particularly relevant example for astrobiology is the observation of calcium carbonate particles precipitated in the presence of organic matter extracted from the Murchison CM2 meteorite. The minerals present rounded morphologies reminiscent of coccoid and rod-shaped bacteria (Reitner 2004) and similar to the calcareous structures previously interpreted as fossil microorganisms in the martian meteorite ALH84001 (McKay et al. 1996). More exotic mineral shapes – such as trumpets, helices, twisted ribbons and stars – can also be obtained through precipitation in the presence of large organic molecules, particularly polymers (Mukkamala and Powell 2004; Yu and Cölfen 2004).

Microorganisms can dissolve, etch and bore into solid substrates (Cockell and Herrera 2008). Bioalteration textures apparently resulting from these processes have been reported in various geological materials, most commonly basaltic glass, which is probably fairly widespread on Mars. Experiments have confirmed that bacteria etch cell-sized pits in volcanic glass in the laboratory (Thorseth et al. 1995). Alteration features in natural samples divide into two types: granular textures and tubular textures (extensively illustrated by Staudigel et al. 2006; Fisk and McLoughlin 2013). The granular type consists of closely packed, micrometre-scale spheroidal cavities, giving a spongy overall appearance. The tubular type consists of elongated cavities c. 1–6 μm wide, which extend up to hundreds of micrometres from altered glass surfaces and fractures (McLoughlin et al. 2019). Complex, biogenic organic material has been found in close association with both types (e.g. Fisk et al. 1998; Preston et al. 2011; Wacey et al. 2014), although some examples are less convincing on close inspection than they first appeared (McLoughlin and Grosch 2015; Wacey et al. 2017).

Experimental work has partially succeeded in mimicking the granular form abiotically by reacting basaltic glass with seawater at 150°C (a sterilizing temperature) for 48 days (McCollom and Donaldson 2019). Tubular textures, however, have never been reproduced in experiments, either with or without microbes. Some examples are more compellingly life-like than others, showing a variety of curving, twisting, branching, coiling and other elaborate morphologies suggestive of microbial growth. High-resolution microanalysis has shown that some of the simpler tubules are probably abiotic pseudofossils of uncertain origin (e.g. Pedersen et al. 2015). Titanite-filled ‘microborings’ in Archean basalts from South Africa and Western Australia have also now been convincingly reinterpreted as abiotic mineral growths, probably resulting from thermal metamorphism and seafloor hydrothermal recrystallization, respectively (Grosch and McLoughlin 2014, 2015; McLoughlin et al. 2020). These same processes could probably have generated analogous pseudofossils in basalts on Mars.

Relatedly, White et al. (2014) found linear microtextures and organic carbon associated with fracture-filling alteration minerals in the basaltic martian meteorite Yamato 000593 and interpreted them as possible evidence of microbial bioalteration. This view was rejected by McLoughlin et al. (2019), who showed that the textures were not tubular, but fracture-like, and that the carbon was most likely of hydrothermal origin. McLoughlin and Grosch (2015) present biogenicity criteria for alteration textures in (meta)volcanic rocks. Significantly, they argue that ‘no terrestrial example yet described’ achieves the maximum score of ‘Category 5’ necessary to demonstrate a biogenic origin.

Some features resembling ‘microborings’ are, in fact, ambient inclusion trails (AITs): snaking, tunnel-like cavities (which may be mineral-filled) formed by the propulsion of mineral grains through solid substrates, including quartz/chalcedony (Fig. 5a), phosphate minerals, chlorite and (rarely) altered volcanic glass (Wacey et al. 2008; Lepot et al. 2009, 2011; McLoughlin and Grosch 2015). AITs have also been found in clastic sedimentary rocks of Precambrian age (Fig. 5b). The cross-sectional shape and diameter of AITs are determined by the formative grain, most commonly a euhedral pyrite or magnetite crystal c. 0.5–10 μm across. Longitudinal marks seen in the trail walls are striations made by the grain vertices. The grain is sometimes still present at the end of the AIT. AITs are sometimes found in starburst patterns, indicating that the grains moved outward from a common centre (e.g. Knoll and Barghoorn 1974; Lepot et al. 2009). Examples in Paleoproterozoic chert were misdiagnosed as fossil algae by Gruner (1924) and re-classified as pseudofossils by Barghoorn and Tyler (1963).

Fig. 5.

Ambient inclusion trails (AITs). (a) AITS resembling microborings in agate (basalt-hosted chalcedony) from the Pentland Hills Volcanic Formation, Edinburgh, Lower Devonian. Note opaque terminal grains. Image: SM. (b) Titanite-filled AITs occurring in fine-grained sedimentary rock from the Late Ediacaran Gibbet Hill Formation of Newfoundland. Some trails terminate in pyrite crystals (not visible in this field of view). Image courtesy of J.J. Matthews (Oxford University Museum of Natural History).

Fig. 5.

Ambient inclusion trails (AITs). (a) AITS resembling microborings in agate (basalt-hosted chalcedony) from the Pentland Hills Volcanic Formation, Edinburgh, Lower Devonian. Note opaque terminal grains. Image: SM. (b) Titanite-filled AITs occurring in fine-grained sedimentary rock from the Late Ediacaran Gibbet Hill Formation of Newfoundland. Some trails terminate in pyrite crystals (not visible in this field of view). Image courtesy of J.J. Matthews (Oxford University Museum of Natural History).

AITs typically contain some organic matter and Wacey et al. (2016a) suggested that grain propulsion can be driven by microbially mediated decomposition of this material, which would make some AITs indirect biosignatures after all (Wacey et al. 2016b). However, there is evidence to suggest that the thermal decomposition of organic matter (which can be abiogenic) and metamorphic reactions involving chlorite might have formed some AITs abiotically – for example, in volcanic rocks free of biological influence (Lepot et al. 2009, 2011; Wacey et al. 2016a; Fig. 5a). Thus, these structures cannot be regarded as unambiguous biosignatures despite their life-like morphology and partly organic composition.

Several previous reviews have focused on the use of minerals as biosignatures (Benzerara and Menguy 2009; Benzerara et al. 2019), including in the context of the search for life on Mars (Banfield et al. 2001). Biominerals – that is, minerals whose formation is controlled by living organisms or, at a minimum, induced or influenced by them (see Lowenstam 1981; Dupraz et al. 2009 for definitions of these terms) – can possess specific morphological, structural, textural or chemical characteristics that may allow their discrimination from abiotically produced minerals.

The most obvious feature common to many biominerals is their unusual morphology. Unlike inorganically precipitated minerals, which typically adopt crystal-like prismatic shapes, with sharp angles and straight faces, biominerals often have rounded or curved surfaces and overall morphologies that can be extremely complex. Although this is especially true of eukaryotic biominerals (e.g. the delicate architecture of the silica frustule of a diatom), bacterial biominerals can also display elaborate, non-crystallographic shapes, such as, for instance, the twisted iron-rich stalks and tubular sheaths produced by some microaerophilic Fe-oxidizing bacteria (Chan et al. 2009, 2011) or the sinuous elemental sulfur filaments produced by the sulfur-oxidizing bacterium Candidatus Arcobacter sulfidicus (Taylor and Wirsen 1997; Sievert et al. 2007). Experimental diagenesis (Picard et al. 2015), as well as studies of the geological record (Slack et al. 2007; Hofmann et al. 2008), show that these morphological characteristics can be preserved in rocks. However, as demonstrated in the section on biomorphs, a wide range of abiotic processes can produce mineral, organic and organic–mineral structures with similar life-like shapes, making morphology an ambiguous indicator of biogenicity (García-Ruiz et al. 2002).

Organic–mineral associations

Biominerals are commonly intimately associated with organic molecules and biominerals can often be described as inorganic–organic composite materials. This is especially true of Metazoan biominerals, which tend to be formed within matrices or vesicles composed of organic macromolecules controlling mineral nucleation, crystallization and growth (Weiner 2008; Addadi and Weiner 2014). In microbial systems, biominerals may be enclosed within intracellular organelles, which can be lipidic – as in the case of the magnetosome, an invagination of the cytoplasmic membrane encapsulating magnetic Fe minerals in magnetotactic bacteria (Uebe and Schüler 2016) – or proteinic – as in the case of the envelope surrounding elemental sulfur minerals in some sulfur-oxidizing bacteria (Dahl 2020). Microbial biominerals may also form within the microbial cell wall (Benzerara et al. 2004; Cosmidis et al. 2015), on the cell surface (e.g. on S-layers; Schultze-Lam et al. 1992; Phoenix et al. 2005), on extracellular polymeric substances (Dupraz et al. 2009; Couasnon et al. 2020) and polysaccharidic stalks and sheaths (Chan et al. 2009) or within extracellular organic vesicles (Cron et al. 2019; Marnocha et al. 2019).

Diagenesis experiments have shown that some of the resulting biomineral–organic assemblages may withstand burial at high temperatures and pressures (J. Li et al. 2013, 2014) and observations from the geological record confirm that minerals precipitating on or within microbial cells can lead to well-preserved organic–mineral associations in rocks (e.g. Cosmidis et al. 2013).

The instruments onboard the most recent and future martian rovers have the capability to detect and characterize intimate mineral–organic associations at high spatial resolution, such as SHERLOC on the Perseverance rover and MicrOmega on the Rosalind Franklin rover (using deep UV Raman and near-infrared/visible light spectromicroscopy, respectively; Table 1) (Beegle et al. 2015; Bibring et al. 2017). However, such close associations are expected to be found in non-biological contexts whenever minerals form in the presence of organic molecules (which again may be abiotic in origin).

Organic molecules can be passively adsorbed onto minerals through different types of binding interactions (e.g. Lagaly et al. 2013). Under certain conditions, mineral surfaces can even participate in the polymerization of these adsorbed molecules into larger, life-like macromolecules (as, for instance, in the surface-aided polymerization of amino acids on silicates, oxides and sulfides; Lambert 2008). As shown with the example of carbon–sulfur biomorphs, mineral precipitation in the presence of organic molecules may lead to self-assembled organic–mineral structures mimicking biomineral encapsulation within organic vesicles (e.g. Cron et al. 2019; Marnocha et al. 2019). Different processes on Mars may have led to the preservation of organic molecules at the surface of, or within, mineral particles (reviewed in Fornaro et al. (2018), but for the reasons cited here it is unlikely that the resulting mineral–organic assemblages, even if combined with biological morphologies, may serve as convincing biosignatures.

Mineral structures

Biominerals may present crystal structures that differ from those of their abiotically precipitated counterparts and whose formation is thermodynamically unfavourable under normal temperature and pressure conditions. For example, unstable phases of elemental sulfur, the monoclinic allotropes β-S8 and ɣ-S8, can be formed as biominerals by sulfur-oxidizing bacteria (Cron et al. 2019) and have been proposed as potential biosignatures in astrobiological investigations (Gleeson et al. 2012).

The presence of metastable crystal phases in biominerals likely results from mineral formation on or within organic matrices acting like templates for nucleation (Falini et al. 1996), the stabilization of unstable mineral intermediates by organic molecules (e.g. amorphous calcium carbonate; Addadi et al. 2003) or modifications of the local chemical environment (for instance, increased supersaturation) within internal vesicles (Sviben et al. 2016; Uebe and Schüler 2016) or in the extracellular medium as a result of metabolic activity (Rodriguez-Navarro et al. 2007). Some aspects of the crystal structures of minerals present in martian rock and soil samples can be determined using different techniques such as Raman spectroscopy (SHERLOC and the Raman laser spectrometer onboard the Perseverance and Rosalind Franklin rovers, respectively; Table 1) (Beegle et al. 2015; Rull et al. 2017), although full crystallographic characterization will require sample return.

However, mineral precipitation in the presence of (non-biological) organic molecules can also induce the formation of metastable polymorphs, as demonstrated many times in laboratory experiments. For instance, a range of organic substances, such as alcohols (Sand et al. 2012), citrates (Tobler et al. 2015), amino acids (Hood et al. 2014; Tobler et al. 2014) and polymers (Xu et al. 2008; Sonobe et al. 2015) can impact calcium carbonate polymorphism and induce the formation of unstable carbonate phases such as aragonite and vaterite. The high-temperature sulfur allotropes β-S8 and ɣ-S8 can form abiotically at room temperature when sulfide is oxidized in the presence of different organic molecules, including non-biogenic organic molecules such as glycine (Cosmidis et al. 2019).

Precipitation under inorganic conditions can also produce thermodynamically unstable polymorphs. In the calcium carbonate system, a number of geochemical factors – such as rapid CO2 degassing, high supersaturation or the presence of Mg and other divalent cations – can induce the formation of aragonite instead of calcite in natural springs (Jones 2017). Although rare on Earth, vaterite was found in an extremely cold and dry environment that may be a good analogue for carbonate deposits on other planetary bodies, but its formation and persistence was thought to be abiogenic and favoured by the extreme cold and high-pH waters (Grasby 2003).

These examples illustrate the fact that in order to interpret the presence of unstable polymorphs or other information on crystal structure as biosignatures, the geochemical context of mineral formation (including the fluid chemistry and presence and nature of organic molecules) must be fully known. This may be extremely difficult when investigating ancient sediments on early Mars. Other processes that may alter mineral structure after their formation (e.g. recrystallization) must also be taken into account – for instance, ageing, desiccation and exposure to high-temperature conditions (due to impact and volcanism, even in the absence of a strong geothermal influence during burial).

Beyond general crystal structure, some crystallographic features of biominerals have been proposed as potential biosignatures – for instance, crystal purity and the absence of defects in biogenic magnetites (Fischer et al. 2011; Li et al. 2015). The crystallographic properties of bacterial Mn oxides, such as an abundance of lattice vacancies, have been proposed as mineralogical biosignatures that could be detected on Mars using electron paramagnetic resonance spectroscopy (Kim et al. 2011). More work is needed on a wider range of biominerals and abiotic systems to validate these approaches.

Primary mineral textures

The texture of biominerals, defined here as crystallite size and organization, often differs strongly from that of abiotically precipitated minerals. This is partly due to their crystallization mode: although classical crystal growth proceeds by ion-by-ion addition, biomineralization often proceeds through the addition of pre-formed mineral nanoparticles and, as a result, many biominerals are actually polycrystalline materials (De Yoreo et al. 2015). When the nanoscale building blocks share a common crystallographic orientation, the resulting mineral is described as a mesocrystal (Sturm and Cölfen 2016). Examples are found in coral skeletons, the nacre layer of shells, sea urchin spines and bones (Oaki et al. 2006; Olszta et al. 2007; Seto et al. 2012). Mesocrystals have also been described in calcium carbonates forming in microbial mats, stromatolites and laboratory cultures (Benzerara et al. 2010; Peng and Jones 2013; Han et al. 2017).

Intracellular magnetic iron biominerals in magnetotactic bacteria are usually elongated along specific crystallographic directions and aligned into a chain within the microbial cell (Amor et al. 2020) and hence may be described as 1D mesocrystals (Bergström et al. 2015). These specific textural characteristics are encountered in a fraction of the magnetite nanocrystals present in the martian meteorite ALH84001 and they have thus been described as ‘magnetofossils’ (Friedmann et al. 2001; Thomas-Keprta et al. 2002), although others have argued that their crystallographic and textural signatures could be mimicked abiotically (Golden et al. 2001, 2004; Bell 2007; Martel et al. 2012). Studies of ancient eukaryotic biominerals show that nanocrystalline textures can be preserved in the geological record (Gilbert et al. 2019) and the mesocrystal texture of calcite particles has been used as evidence of microbial influence in the formation of Paleogene micrite deposits (Bralower et al. 2020).

However, polycrystalline mineral textures mimicking biominerals, including mesocrystals, can be reproduced in the laboratory, notably through precipitation with organic additives. Organic molecules appear to play an important part in crystal growth by oriented particle attachment, by stabilizing the nano-building blocks, and guiding and orienting their assembly (Cuif and Dauphin 2005; Oaki et al. 2006; Nouet et al. 2012). Hydrophilic organic polymers are particularly effective in this process and induce the formation of mesocrystals of carbonates, phosphates and metal oxides in laboratory precipitation experiments (Mukkamala and Powell 2004; Yu and Cölfen 2004; Yu et al. 2005; Meldrum and Cölfen 2008) (Fig. 6a), but simple inorganic additives such as Mg2+ can also lead to mesocrystal-like polycrystalline structures (Liu et al. 2020) (Fig. 6c). Magnetite mesocrystals were also obtained through the hydrolysis of organically bound ferric iron (Cai et al. 2014).

Fig. 6.

Biomorphic nanocrystalline structures and mesocrystals. (a) Nanocrystalline calcite ‘microtrumpet’ formed in the presence of a carboxylic-rich organic molecule (Mukkamala and Powell 2004). (b) Co-oriented carbonate nanorods at the surface of a carbonate–silica biomorph (Kellermeier et al. 2012a). (c) Nanocrystalline calcite sphere precipitated in the presence of Mg2+ (Liu et al. 2020). (d) Fe oxide mesocrystal formed by droplet evaporation (Agthe et al. 2014). Images reproduced with permission (parts a–c) or under creative commons license (creativecommons.org/licenses/by/3.0/) (part d).

Fig. 6.

Biomorphic nanocrystalline structures and mesocrystals. (a) Nanocrystalline calcite ‘microtrumpet’ formed in the presence of a carboxylic-rich organic molecule (Mukkamala and Powell 2004). (b) Co-oriented carbonate nanorods at the surface of a carbonate–silica biomorph (Kellermeier et al. 2012a). (c) Nanocrystalline calcite sphere precipitated in the presence of Mg2+ (Liu et al. 2020). (d) Fe oxide mesocrystal formed by droplet evaporation (Agthe et al. 2014). Images reproduced with permission (parts a–c) or under creative commons license (creativecommons.org/licenses/by/3.0/) (part d).

Organization of nanocrystallites at the mesoscale can also emerge from inorganic self-assembly. Carbonate–silica biomorphs are, for instance, composed of carbonate nanorods, uniform in shape and size, that are almost parallel to each other and aligned with respect to their c-axis (the slight misalignment between the nanorods occurs at fixed angles and allows for the radial growth of the sheaths composing the biomorphs) (Kellermeier et al. 2012c) (Fig. 6b). Mesocrystals can also be obtained inorganically by crystallization within silica gels (Dominguez Bella and García-Ruiz 1987) or through hydrothermal processes or solvent evaporation (Agthe et al. 2014; Sturm and Cölfen 2016; Sun et al. 2019) (Fig. 6d).

It has also been suggested that the very small sizes of microbial biominerals forming from highly supersaturated solutions as a result of microbial activity could be used as a biosignature (Banfield et al. 2001). Different microbial biomineralization processes can indeed result in the formation of intra- and extracellular iron, sulfur or carbonate mineral nanoparticles (i.e. with at least one dimension <100 nm) (Mansor and Xu 2020). Crystallites in the nanoparticulate range can also form through nucleation and growth within an organic matrix, as observed in carbonate microbialites (Benzerara and Menguy 2009). However, because mineral nanoparticules can precipitate chemically from highly supersaturated fluids, or as a result of multiple nucleation events on organic or inorganic seeding materials, they do not appear to be robust biosignatures.

Similar to the non-equilibrium mineral structures described in the previous section, signatures based on mineral textures will likely be difficult to interpret, especially in deposits where organics are abundant and/or in the absence of information on their original geochemical formation environment. However, Mars is more suitable than Earth for the long-term preservation of nanocrystalline mineral textures (e.g. the survival of opaline silica over multi-billion-year timescales at many localities on Mars) as a result of its low surface temperature and geothermal gradient and less prevalent fluid circulation. The possibility that such textures will be discovered is thus considerable and more effort is needed to better constrain their biogenic and abiogenic formation mechanisms in Mars-like contexts.

Chemical signatures in minerals

Aside from their structure, the chemical composition of biominerals may be different from that expected to form at equilibrium with the surrounding fluid geochemistry. Organisms can preferentially accumulate or exclude certain elements from their intracellular medium or internal compartments. As a result, intracellular biominerals may display enrichments of specific elements compared with the chemistry of the extracellular environment (e.g. Cam et al. 2016) or high levels of chemical purity (Amor et al. 2015). The PIXL instrument onboard the Perseverance rover can map the distribution and abundance variations of major and trace chemical elements at the sub-millimetre scale in rock and soil samples (Allwood et al. 2020). This technique may enable the detection of fine chemical biosignatures on Mars, such as enrichments of certain trace metals associated with organic matter (Hickman-Lewis et al. 2020).

However, a thorough understanding of the geochemical context for mineral formation, as well as diagenetic history, are necessary to interpret mineral chemistry in terms of biosignatures. For instance, the Mg–Ca carbonate dolomite forms in an environment associated with microbial mats (e.g. DiLoreto et al. 2019), although, unlike calcium carbonates, this mineral is very difficult to precipitate in the laboratory at low temperatures. The presence of dolomite in microbial mats is explained by organic templating effects and the interaction of Mg2+ with the carboxylic groups of extracellular polymeric substances (Krause et al. 2012; Roberts et al. 2013; Petrash et al. 2017). Dolomite can also form abiotically at high temperatures by precipitation from hydrothermal fluids or by the replacement of other primary carbonates during diagenesis or metamorphism (Bontognali 2019), or at low temperatures under certain geochemical conditions (e.g. in evaporative saline alkaline lakes; Wanas and Sallam 2016), preventing its use as a robust biosignature. More work is required from experiments under simulated martian conditions or from studies of analogue environments on Earth (e.g. Hays et al. 2017) to identify relevant and unambiguous mineralogical biosignatures that might be detected on Mars.

Neither the Rosalind Franklin nor Perseverance rover is equipped to measure the isotopic compositions of martian samples in situ, but samples returned to Earth will undoubtedly be analysed with isotope mass spectrometry in due course. Unidirectional, enzyme-catalysed metabolic reactions tend to select the lighter isotopes of carbon, sulfur, nitrogen, iron and many other elements because of their lower bond energies. This kinetic effect generates isotopically light products while leaving the substrates depleted in the light isotopes (i.e. relatively enriched in heavier isotopes. In some heavy elements this pattern is actually reversed for reasons to do with nuclear size and shape (e.g. uranium; Brown et al. 2018).

The interpretation of isotopic anomalies as biosignatures in geological materials (including fluids, minerals and organic matter) is a well-established practice on Earth, but relies critically on a thorough understanding of the history and context of the sample as well as the (bio)geochemical cycle of the relevant element – that is, the isotopic composition of the major reservoirs and the fractionations associated with the main fluxes between them (which, in the case of biotic processes, depend on the particular enzymes involved) – and changes in these values across geological time. As others have noted, such an understanding is not available for Mars, which limits (but does not completely eliminate) the potential for discovering definitive isotopic biosignatures on that planet (Summons et al. 2011; Vago et al. 2017).

More generally, false positive isotopic biosignatures can occur where the interpreter does not take sufficient account of the abiotic pathways of isotope fractionation involving either kinetic or equilibrium processes (van Zuilen et al. 2003; Anbar 2004; Thomazo et al. 2009; Brown et al. 2018). This broad caveat applies to both bulk measurements and to more sophisticated analyses of the isotopic structure of molecules (e.g. clumped or site-specific isotope compositions), although the latter hold great promise for astrobiological applications (Eiler et al. 2018). We briefly discuss how false isotopic biosignatures may arise in the carbon, sulfur, nitrogen and iron systems.

Carbon isotopes

Biological uptake of carbon causes a kinetic isotope fractionation such that biologically fixed carbon exhibits a relatively negative δ13C value (the 13C/12C ratio of a sample expressed as a per mil deviation relative to a standard). On Earth, organic matter in the marine sedimentary rock record is characterized by δ13C values 20–30‰ lower than carbonates of the same age. The persistence and ubiquity of this offset over c. 3.5 Gyr of global geological history is considered strong evidence for the antiquity of life (Schidlowski 2001).

However, attributing individual samples of ancient carbonaceous matter to biotic or abiotic carbon fixation on the basis of δ13C values alone can be problematic even on Earth. On the one hand, the biological fractionation effect can be small in some circumstances (e.g. Takai et al. 2008; Reeves and Fiebig 2020). On the other hand, kinetic isotope effects associated with several abiotic pathways yield CH4 and/or other organic compounds with highly negative δ13C values (Horita 2005). For example, hydrocarbons produced by experimental Fischer–Tropsch type synthesis (at 250°C and 325–350 bar using formic acid as a carbon source) are reportedly depleted in 13C by as much as 36‰ (McCollom and Seewald 2006; McCollom et al. 2010).

Some researchers have noted that ‘abiotic photosynthesis’ (CO2 reduction photo-catalysed on mineral surfaces, with water as an electron donor) may also have produced isotopically light organic matter on early Mars (Franz et al. 2020), although experimental work is needed to test this hypothesis and to explore the isotopic effects of abiotic organic synthesis more generally. Van Zuilen (2008) has pointed out two further challenges for the identification of carbon isotopic biosignatures on Mars. First, martian sedimentary rocks may preserve debris from carbonaceous chondrites, which contain reduced carbon phases (some of them macromolecular) with δ13C values of about −15 to −20‰, similar to biomass on Earth. This material may be difficult to discriminate from biological organic matter. Second, the carbon isotopic composition of CO2 in the martian atmosphere probably changed significantly with the decline of volcanic outgassing and the drawdown and loss of CO2 early in martian history. To establish the isotopic fractionation associated with the formation of any endogenous organic carbon in recovered samples, it will therefore be necessary to identify carbonate minerals representative of contemporaneous atmospheric CO2, which may be challenging.

More generally, the isotopic composition of martian carbon is poorly understood. Martian meteorites contain reduced magmatic carbon characterized by δ13C values of about −20‰ (i.e. about 15‰ lighter than magmatic carbon in basalts on Earth, for unclear reasons), as well as carbonates with widely varying positive δ13CPDB values, up to about +60‰ (Grady et al. 2004; Steele et al. 2016). Pyrolysis of aeolian fines by the SAM instrument suite onboard the Curiosity rover yielded CO2 with δ13C values between c. −6 and +20‰ (Leshin et al. 2013). Subsequently, Noachian–Hesperian siliciclastic sedimentary rocks analysed by the same instrument yielded CO2 with δ13C values ranging from −25 ± 20 to +56 ± 11‰ (Franz et al. 2020). Both datasets suggest the presence of multiple carbon-bearing phases, including carbonates and reduced carbon, but little is known about their age and identity.

Sulfur isotopes

Variations in sulfur isotope ratios have been investigated as potential biosignatures in martian meteorites (Farquhar et al. 2000b) and sedimentary rocks (Franz et al. 2017) based on the fact that some microbial metabolisms produce mass-dependent fractionations of the sulfur isotopes (Ono 2008). In particular, microbial sulfate reduction can produce sulfide significantly depleted in the heavier 34S (i.e. relatively enriched in 32S) compared with the substrate (sulfate), resulting in isotopic fractionations of several tens of δ34S units (‰) (Kaplan and Rittenberg 1964; Canfield and Teske 1996). High-temperature abiotic sulfate reduction also fractionates sulfur isotopes (up to 20‰ at 100°C; Thomazo et al. 2009), but can probably be ruled out for many samples obtainable from the martian near-surface, which have not been exposed to high temperatures.

Microbial sulfur disproportionation and sulfide oxidation also fractionate sulfur isotopes and it can be difficult to disentangle the effects of these different metabolisms in sediments (Canfield et al. 1998; Philippot et al. 2007; Sim et al. 2011; Pellerin et al. 2019), particularly after further sulfur-cycling by post-depositional and diagenetic processes (Fike et al. 2015). Isotopically light sulfide has been interpreted as evidence of microbial sulfur-cycling microorganisms in Archean rocks on Earth, often in combination with other biosignatures such as microfossils or stromatolites (e.g, Wacey et al. 2011; Bontognali et al. 2012; Marin-Carbonne et al. 2018). However, this interpretation requires ruling out contributions from abiogenic processes that can also fractionate sulfur isotopes. For instance, isotopic exchange with sulfate in hydrothermal contexts can endow sulfide with δ34S values similar to microbially reduced sulfide (Ohmoto and Lasaga 1982).

Atmospheric processes such as SO2 photolysis can lead to mass-independent fractionation of sulfur isotopes (Farquhar et al. 2001). Signatures of mass-independent fractionation are commonly recorded in Archean rocks (Farquhar et al. 2000a), but are rarely observed today on Earth because the creation and preservation of mass-independent fractionation signals is unlikely in an oxygen-rich atmosphere (Pavlov and Kasting 2002; Halevy 2013).

Sulfur in martian meteorites records clear isotopic evidence of atmospheric photochemical mass-independent fractionation effects (Farquhar et al. 2000b; Franz et al. 2014). The Curiosity rover's SAM instrument suite measured δ34S values ranging from −47 to +28‰ in samples collected in Gale Crater, some of which are ‘broadly consistent with' the effects of microbial sulfur-cycling (Franz et al. 2017). However, these isotopic compositions could also be explained by the effects of equilibrium fractionation in the impact-driven hydrothermal system of the crater, combined with atmospheric chemical and photochemical processes (Franz et al. 2017).

High-precision measurements of the abundances of all four sulfur isotopes (32S, 33S, 34S and 36S) introduce new Δ33S and Δ36S isotopic ratios, which, in combination with geological contextual analysis, may help to discriminate the effects of biological, hydrothermal and photochemical fractionation processes (Philippot et al. 2007; Ono 2008; Kamyshny et al. 2014; Aoyaa and Ueno 2018). Such techniques will no doubt be applied to returned samples. The study of sulfur-rich Mars-analogue environments suggest that combining δ34S, Δ33S and Δ36S measurements with steady-state models of sulfur-cycling may be a possible diagnostic tool for biosignature detection (Moreras-Marti et al. 2021). However, this method requires an in-depth understanding of the martian geological, geochemical and atmospheric context, which, despite significant recent advances (Franz et al. 2019), may still be out of reach in the near future.

Nitrogen isotopes

Nitrogen undergoes a highly complex biogeochemical cycle on Earth, in which several important metabolic pathways impart isotopic fractionations of different amplitudes and directions (reported as δ15N, with Earth's atmospheric N2 providing the usual standard). The δ15N signature of marine biomass (about +5‰ today) can be preserved in fossil organic matter and as mineral-bound NH4+ derived from organic decay, with minimal diagenetic modification (Boyd and Philippot 1998; Thomazo et al. 2009). Organic matter in Archean metasediments records a systematic variation in δ15N over geological time, probably reflecting changes in the preponderance of different microbial metabolisms under increasingly oxidizing conditions (Ader et al. 2016); there are some interpretative difficulties relating to metamorphic overprint, but these will not be an issue on Mars.

The martian atmosphere is c. 3% nitrogen today and nitrogen-bearing organic molecules of uncertain origin have already been found in martian meteorites (Koike et al. 2020); they may soon be encountered in returned samples. It will be challenging to interpret δ15N in this material without a broader understanding of Noachian–Hesperian nitrogen cycling, particularly in relation to the isotopic effects of atmospheric escape and declining volcanism over geological time; NH4+ in clay minerals may provide a contemporaneous standard (van Zuilen 2008).

The risk of isotopic false positives arising in this context is not yet well understood, but large δ15N fractionations are already known to result from several relevant abiotic processes. Nitrate fixed by lightning may be isotopically light (Stüeken 2016). Organic nitrogen produced experimentally from NH3 in Miller–Urey reactions with CH4 and H2 is reportedly enriched in 15N by 10–12‰, while plasma discharge in mixtures of N2, CH4, CO and H2 causes fractionation of up to 25‰ in the opposite direction (Kung et al. 1979; Thomazo et al. 2009; Kuga et al. 2014). Nitrogen isotope fractionation may also occur during Fischer–Tropsch type organic synthesis (Kung et al. 1979; Thomazo et al. 2009). Chondritic meteoritic debris may also be present in returned samples and can contain organic nitrogen with δ15N values ranging from +25 to +150‰ (Sephton et al. 2003).

Iron isotopes

Fe isotopes have been investigated as potential signatures of microbial Fe cycling (Johnson et al. 2008; Poitrasson 2015), including in the context of Mars (Anand et al. 2006; van Zuilen 2008), although candidates for Fe isotopic biosignatures have not yet been detected in martian materials.

It has been reported that magnetite biomineralized by the magnetotactic bacterium Magnetospirillum magneticum AMB-1 is strongly depleted in heavy Fe isotopes (Amor et al. 2016). Moreover, mass-independent fractionation in 57Fe was observed during magnetite biomineralization, but not in the even Fe isotopes (54Fe, 56Fe and 58Fe), implying a magnetic isotope effect. This signature is apparently not produced abiotically or by other Fe-metabolizing bacteria (Amor et al. 2016), but it remains to be seen whether it can be detected in the rock record.

The oxidation of aqueous Fe(II) precipitates solid Fe(III) phases that are typically slightly enriched in the heavy Fe isotopes regardless of whether Fe(II) oxidation was biologically mediated or not (e.g. Bullen et al. 2001; Balci et al. 2006), so it is generally admitted that microbial Fe oxidation does not leave any robust isotopic biosignature (e.g. van Zuilen 2008; Thomazo et al. 2009). However, microbial dissimilatory Fe reduction, which couples the reduction of Fe(III) to the oxidation of organic matter, leads to an enrichment of the Fe(II) product in the light Fe isotopes (e.g. Percak-Dennett et al. 2011). Under certain conditions (in particular, low pH), the Fe isotope fractionation induced by microbial dissimilatory Fe reduction may exceed in amplitude the fractionation associated with the abiotic reductive dissolution of Fe(III) (e.g. Johnson et al. 2008; Thomazo et al. 2009; Chanda et al. 2021).

On Earth, isotopic signals related to microbial dissimilatory Fe reduction are, for instance, thought to be recorded in some banded iron formations (Johnson et al. 2008). However, a number of processes may overprint or even erase biologically driven Fe isotopic signals, such as the preferential binding of heavy Fe isotopes by organic ligands in solution (e.g. Lotfi-Kalahroodi et al. 2021) or isotopic exchange between Fe minerals during diagenesis or metamorphism (Whitehouse and Fedo 2007; Hyslop et al. 2008). Here again, the use of Fe isotopes to search for traces of biological activity necessarily requires an in-depth understanding of the mineralogical and geochemical context during primary sediment deposition and subsequent history, and their interpretation should be conducted in conjunction with other mineralogical, chemical and isotopic indicators (Poitrasson 2015).

In writing this review, we have been struck by the following five points. First, abiotic processes can mimic not only morphological biosignatures, but also chemical/molecular, mineralogical, isotopic and textural biosignatures; a critical attitude is required in all cases and morphological data are not necessarily less reliable than other possible lines of evidence for life (cf. García-Ruiz et al. 2002). Indeed, independent categories of false biosignature may often coincide in the same sample and thus ‘multiple lines of evidence’ suggestive of biology can be found in some non-biological systems.

Second, many abiotic materials that resemble life are produced by the dissipation of energy in systems characterized by strong thermodynamic and/or chemical gradients and the presence of liquid water (e.g. the hydrothermal synthesis of complex organic matter, the hydrothermal fractionation of carbon isotopes; chemical gardens, carbon–sulfur biomorphs and carbonate–silica biomorphs). Although in many ways unsurprising, this has paradoxical implications. Environments conducive to the origin and maintenance of life may also, by their very nature, be conducive to the formation of false biosignatures. Therefore a cell-like, organic, ambiguously biogenic structure found in a tenuously habitable, energy-poor environment (e.g. a cold desert) may be more credible as a biosignature than a similar structure found in the midst of a reducing hydrothermal system because the former is more difficult to explain abiotically than the latter. It follows that the search for evidence of life should not focus only on environments where life is most likely to have arisen (cf. Longo and Damer 2020) because it is here that the evidence will be most ambiguous.

Third, silica precipitation plays a key part in the formation of a wide variety of false biosignatures (e.g. carbonate–silicate biomorphs, chemical gardens, cryogenic opal biomorphs and, potentially, the formation of pseudomicrobialites in splash zones). Siliceous materials might be favoured targets for analysis and sample return because silica can help to preserve organic matter and morphological fossils as a cement and entombing medium (e.g. McMahon et al. 2018). It will be especially important to consider how self-organization might have influenced the textural and morphological features of these samples.

Fourth, interactions between water and basaltic lava, although probably contributing to habitability on early Mars in various important ways, is also associated with a number of pseudobiosignatures (e.g. quench crystallites, alteration textures, the production of chemical garden ‘seed’ minerals and the production of alkaline, silica-rich fluids that can generate biomorphs). Neither the potential occurrence of biosignatures nor the potential occurrence of pseudobiosignatures should be overlooked in the sampling and analysis of aqueously altered volcanic materials (Ivarsson et al. 2020, 2021).

Fifth, the study of false biosignatures requires input from colleagues and methods across several disciplines. Physical chemists, condensed matter physicists and materials scientists have long been interested in symmetry-breaking, self-assembly and the emergence of complex structures and materials under far from equilibrium conditions. There is a vast literature – only a tiny sample of which has been cited in this review – on the numerical and experimental interrogation of these processes and the analytical characterization of their products. This expertise now needs to be translated into a geological and astrobiological context by focusing on the minerals, fluids and pressure–temperature conditions present on Mars today and in the geological past (e.g. Sainz-Díaz et al. 2021). Some important theoretical foundations have been laid (e.g. Ortoleva 1994; García-Ruiz et al. 2020), but there is more work to be done, both to identify relevant sources of false biosignatures and to characterize them in detail. Ideally, multiple high-resolution analytical techniques should be used to facilitate in-depth comparisons with candidate biosignatures. Recent studies of probable Precambrian fossils have presented rich, multi-scale, multi-proxy datasets combining morphological, textural and compositional (chemical, mineralogical and isotopic) information (e.g. Alleon et al. 2018; Lepot et al. 2019; Hickman-Lewis et al. 2020; Marin-Carbonne et al. 2020). Studies of false biosignatures should be similarly comprehensive.

What about biogenicity criteria?

A number of protocols and strategies have been devised to assess the credibility of candidate biosignatures (e.g. Buick 1990; Brasier and Wacey 2012; McLoughlin and Grosch 2015; Vago et al. 2017; Neveu et al. 2018; Rouillard et al. 2021). Most of these schemes use multiple, nested criteria to assess biogenicity: did the object (or population of objects) form in a demonstrably habitable (palaeo)environment, with appropriate evidence of endogeneity and syngenicity? If so, is its morphology consistent with a biotic origin and inconsistent with an abiotic origin? If so, is its chemical composition distinctively life-like? And so on. The more definitely and completely the object (including its geological context) meets the criteria, the higher the biogenicity score.

Biogenicity determination protocols meet an important need, but most real fossils (whether on Earth or Mars) are likely to fall short of ideal standards and achieve only middling scores, along with pseudofossils. Thus a failure to meet some of the relevant biogenicity criteria is expected and can often be explained away by researchers claiming to have discovered biosignatures. A deeper worry is that biogenicity criteria are unable to discriminate sensitively and reliably between biosignatures and pseudobiosignatures unless they are grounded in extensive knowledge and understanding of both classes of phenomena. Even protocols that do not explicitly rely on binary criteria must necessarily appeal to reference data from relevant abiotic systems (e.g. Rouillard et al. 2021). However, most known varieties of pseudobiosignature have not been characterized or understood in sufficient detail for this to be possible. Moreover, given the haphazard and unsystematic way in which varieties of false biosignature have so far been identified, we can only assume that many others remain undiscovered. Here, the expertise and methods of mineralogists, chemists, physicists and materials scientists are as valuable to biosignature science as those of microbiologists and palaeontologists.

Although the discovery of new forms of pseudobiosignature will tend to undermine existing biogenicity protocols (e.g. McMahon 2019; Nims et al. 2021), in the long run this will lead to better protocols (e.g. McLoughlin et al. 2007; Johannessen et al. 2020).

If we are lucky, plain and unequivocal biosignatures will be discovered on Mars in the coming decades. But in light of the many cautionary tales in the history of palaeontology and astrobiology, it seems prudent to anticipate more ambiguous results. In interpreting these, it will be important to understand how misleadingly life-like objects and substances might have formed abiotically on Mars. We have summarized some of the examples that have already been discovered in the laboratory, in terrestrial rocks and in meteorites. We have argued that many other examples probably await discovery because abiotic self-organization processes relevant to the geology of Mars have not been explored systematically. Because life itself is presumed to be the product of self-organization in abiotic geochemical reactions, the complexity of abiotic natural products should not be underestimated. Nevertheless, we are optimistic that the problem of false biosignatures is not intractable. The better these phenomena are understood, the more sensitively we will be able to discriminate between true evidence of life and these impostors.

Relevant false biosignatures should therefore now be sought systematically in Mars-analogue field and experimental systems and characterized in detail with multiple analytical instruments and at multiple scales to provide datasets that are as rich as those available for biosignatures. Further work on the physics and chemistry of far-from-equilibrium systems will ultimately reveal the limits of abiotic self-organization and may even lead to new discoveries on the organizing principles at the origin of life on Earth. Such efforts have an important part to play in the interpretation of Earth's rock record as well as the search for life on Mars and elsewhere in the solar system.

The perspectives in this article were shaped in part by SM's participation in the EU Cost Action CA17120 Chemobrionics. We thank an anonymous reviewer and Mark van Zuilen for helpful comments that improved this paper.

SM: conceptualization (lead), investigation (equal), writing – original draft (lead), writing – review & editing (equal); JC: conceptualization (supporting), investigation (equal), writing – original draft (supporting), writing – review & editing (equal).

This research received no specific grant from any funding agency in the public, commercial, or not-for-profit sectors.

Data sharing is not applicable to this article as no datasets were generated or analysed during the current study.

Scientific editing by Peter Grindrod

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