Abstract

A recent breakthrough publication has reported complex organic molecules in the plumes emanating from the subglacial water ocean of Saturn's moon Enceladus (Postberget al.,2018,Nature 558:564–568). Based on detailed chemical scrutiny, the authors invoke primordial or endogenously synthesized carbon-rich monomers (<200 u) and polymers (up to 8000 u). This appears to represent the first reported extraterrestrial organics-rich water body, a conceivable milieu for early steps in life's origin (“prebiotic soup”). One may ask which origin-of-life scenario appears more consistent with the reported molecular configurations on Enceladus. The observed monomeric organics are carbon-rich unsaturated molecules, vastly different from present-day metabolites, amino acids, and nucleotide bases, but quite chemically akin to simple lipids. The organic polymers are proposed to resemble terrestrial insoluble kerogens and humic substances, as well as refractory organic macromolecules found in carbonaceous chondritic meteorites. The authors posit that such polymers, upon long-term hydrous interactions, might break down to micelle-forming amphiphiles. In support of this, published detailed analyses of the Murchison chondrite are dominated by an immense diversity of likely amphiphilic monomers. Our specific quantitative model for compositionally reproducing lipid micelles is amphiphile-based and benefits from a pronounced organic diversity. It thus contrasts with other origin models, which require the presence of very specific building blocks and are expected to be hindered by excess of irrelevant compounds. Thus, the Enceladus finds support the possibility of a pre-RNA Lipid World scenario for life's origin.

1. The Chemistry of Life

A central objective of any astrobiology roadmap is finding out how life began and evolved (Des Maraiset al.,2008; Hornecket al.,2016). While the chemical paths by which life emerged are far from consensual, it is highly likely that life arose in water and that the necessary building blocks were organic compounds. Since a widely accepted definition is “life is that which replicates and evolves” (Nowak and Ohtsuki,2008), life's origin appears to entail a transition from the abiogenic availability of various organic compounds to chemical entities capable of producing their own copies.

Organic compounds are those that contain covalently bound combinations of carbon with one or more of the five other main life elements, hydrogen, nitrogen, oxygen, phosphorus, and sulfur. It appears that molecular size and complexity are necessary but not sufficient conditions for being relevant to life, as some very large carbon-based molecules are abiotic (Fig. 1). Therefore, it appears that what defines life molecules is their capacity to undergo specific mutual interactions, leading to the emergence of complex networks (Toparlak and Mansy,2018). A complementary approach has been offered (Marshallet al.,2017), which aims to evaluate complex objects as possible biosignatures. The complexity measure offered (Pathway Complexity) identifies the shortest pathway to assemble an object from its basic building units.

In the time of Berzelius (1779–1848), big strides were made in studying molecules derived from living organisms, from metabolites to proteins (Kyle and Steensma,2018). While it was clear that life molecules obeyed the rules of standard chemistry, an incapacity prevailed in synthesizing them. For the latter, Berzelius coined the term “organic” and posited that avital force was necessary for their generation. A few decades later, Wöhler discovered that urea may be generated from the inorganic salt ammonium cyanate, a turning point that led to the undermining of Vitalism (Kinne-Saffran and Kinne,1999).

Today's origin-of-life studies curiously reflect an analogous state of affairs. Contemporary laboratories can synthesize practically every molecule of life, but it appears necessary to make a distinction between organic molecules that could form abiogenically and such that could only form within evolving protocellular entities. It thus appears that our current perception of organic chemistry has shifted from a human handicap to an astrochemical one. The central challenge is deciding which organic molecules are too complex for abiogenesis, necessitating further evolution (Mann,2012). Different origin-of-life models differ vastly in this respect.

2. Life's Elusive Origin: Soup or Not

Life's origin indisputably necessitates an ample supply of organic molecules. While the origin of terrestrial organic compounds remains only partly deciphered, there is clear evidence for carbon-containing compounds wherever one probes in the Solar System. There are ample data on carbon-containing molecules up to atomic mass of 200 u in interstellar space (Fig. 2,Table 1). In icy comets, about 25% of the nucleus mass consists of carbon compounds (Greenberg,1998). On the surface of Saturn's moon Titan there is a coexistence of organic lakes and water-ice rocks (Tokano,2009). Based on the reported estimates of carbon infall (from dust, meteorites, and comets) during Earth's first billion years (Chyba and Sagan,1992), one can compute that by the end of such a period the terrestrial oceans would have had an appreciable layer of insoluble organic matter in addition to ample dispersible carbon compounds.

The pioneering work of Oparin (1938) provided a rational scenario, whereby abiogenic reactions and supply mechanisms delivered an abundant supply of chemical components essential for life's emergence. The organic solution that has formed in the ocean was referred to as the “Primordial Soup” or “Prebiotic Broth” (Oparin,1962). In the century that has passed since the original Russian edition of Oparin's book, numerous scenarios have been offered regarding such supply of organic molecules. One possible path is terrestrial endogenous synthesis of organic compounds from very simple carbon-containing molecules, which necessitates a free energy source, such as light, electric discharge, or concentration gradients.

A groundbreaking example was the Miller-Urey experiment (Miller,1953), which demonstrated the generation of soup-worthy organic compounds from simple reducing gases energized by spark discharge. This experiment motivated several decades of scrutiny in which life-related molecules were shown to be abiotically synthesized from different precursors and based on electrical, thermal, chemical, and photochemical energy as reviewed (Ferris and Hagan,1984; Maden,1995; Cleaves,2012; Bada,2013). This mode of soup generation is represented as the abiotic path from simple primordial compounds to dispersible and nondispersible organics (Fig. 3).

While terrestrial endogenous syntheses quite strongly dominate the origin-of-life literature, exogenous infall mechanisms are at least as important (Ehrenfreundet al.,2011), with sources including interplanetary dust particles, meteorites, and comets. A relevant example is the presence of dipeptides in comets, as reviewed (Kaiseret al.,2013). Together, such extraneous supplies might exceed the capacity of local syntheses (Chyba and Sagan,1992) (cf. Section 3). Delivered carbon compounds may also be dispersible or not; the latter referred to as insoluble organic matter (IOM,Fig. 1), which may undergo differentiation to generate smaller (monomeric) compounds with better water solubility that therefore become soup components with higher life-generation potential.

There is a faction within origin-of-life research that discounts the idea of prebiotic soup altogether (Maden,1995). The expressed doubts go back to the Miller-Urey experiment, originally performed with hydrogen-rich reducing gases (CH₄, NH₃, H₂). Subsequently, new data emerged, suggesting that at the relevant time the atmosphere was likely more oxidizing (CO₂, CO, N₂), making spark-induced synthesis less effective. This led to a change of mind about the existence of prebiotic soup but was later reassessed and partly reversed (Cleaveset al.,2008). Notably, the soup opponents disregarded the fact that only one of many sources for soup provisions became less tenable.

Parallel support for the no-soup party came from the longstanding trophism dichotomy (Fig. 3). Two different scenarios have been invoked regarding the early steps in life's emergence. Aheterotrophic setting assumes that emerging protolife feeds upon the organic supply in the primordial soup (Oparin and Gladilin,1980; Bada and Lazcano,2003). The alternativeautotrophic setting proposed that the appearance of protocells could transpire via mineral-catalyzed thermally or photochemically energized syntheses of every organic molecule necessary, without any dependence on ready-made soup components (Hartman,1975; Maden,1995; Martinet al.,2008; Branscomb and Russell,2018; Kitadaiet al.,2018). Such a “no soup” stand has been strongly advocated based on energy and catalysis provided by the iron sulfide minerals (Wächtershäuser,1988).

The significant doubts regarding life's origin via an autotrophic scenario (Ross,2008; Cleaves,2012) help keep the heterotrophic prebiotic soup concept strongly viable. The present authors are convinced that protocells with metabolism and reproduction capacities could not have emerged in water bodies totally devoid of dissolved organic compounds, as previously stated (von Kiedrowski,1996). We posit that the invoked synthetic reactions at mineral surfaces should better be viewed as yet another soup-forming path (Gutekunst,2018) (Fig. 3), allowing protolife to emerge heterotrophically and reach pure autotrophy at a much later evolutionary stage (Quayle and Ferenci,1978; Maden,1995).

The great challenge is thus to identify concrete examples of possible prebiotic soups and probe their composition. This should guide our struggle to decide how far abiogenesis can go, before the inescapable advent of reproduction-based evolution (Oparin and Gladilin,1980). We describe here some inferences derived from the large water body on Enceladus, recently shown by direct experimental approaches to contain a diversity of organic compounds from several likely sources (Postberget al.,2018). Such direct observations, on what has been coined “the best astrobiology target in the solar system” (McKayet al.,2014), constitute an excellent route to obtain hints on a possible soup composition on early Earth, and may help assess models for life's emergence out of such a soup.

3. The Enceladus Message

The early flybys of the Cassini–Huygens mission to the saturnian system revealed the incredible nature of Saturn's moon Enceladus. This is an active, dynamic world, including cryovolcanic plumes ejecting ice grains and vapor from faults near its south pole (Waiteet al.,2006; Thomaset al.,2016), as reviewed (Dougherty and Spilker,2018). Mission modifications led to Cassini flying close to Enceladus 23 times over a decade, in order to obtain more details about the moon. This established the existence on Enceladus of a 26–31 km deep global salty water ocean, which lies under a 21–26 km thick water-ice crust, with a thinner crust (≤13 km) at the south pole. The moon's center constitutes a porous rocky core of ∼200 km radius (Thomaset al.,2016). The energy maintaining water in liquid state and driving the plumes' eruptions is likely derived from tidal dissipation (Nimmoet al.,2014).

Early chemical analyses of the plumes, and of Saturn's E-ring generated from their ejecta, established compositions of organic molecules in an H₂O-dominated context (Waiteet al.,2006; Postberget al.,2008,2011). These observations suggested organic compounds with 2–4 carbon atoms, potentially derived from larger aromatic entities. A recent publication (Postberget al.,2018) has extended these observations, providing a much more detailed picture of the enceladan ocean's organic repertoire (Fig. 4). The new data suggest that some of the ice grains contain concentrated and much more complex organic material. Using their nominal sensitivity range, we found that the mass spectrometry observations extend the organics' size range from <50 u (atomic mass units) to ≤200 u (Fig. 4). This higher range, defined as high-mass organic cations (HMOCs), likely represents molecules with 7–15 carbon atoms.

Extended mass spectra (beyond the nominal range of the Cassini instrument) exhibited indication for yet larger molecules, with atomic masses up to ∼8000 u, with prominent propensity peaks at 200–300, 800–1100, and 1600–1800 u (Fig. 4). Further support for such large molecules is obtained by inference based on the relative intensities of the increasingly heavy HMOC peaks at <200 u, and on their dependence on grain impact speed, suggesting that HMOCs are fragments of higher-mass parent macromolecules, with up to 150 carbon atoms (2000 u).

The very large molecules are inferred, based on interpeak spacing and carbon to hydrogen ratio of ∼1, to be composed of polymerized isolated aromatic rings, along with unsaturated aliphatic links, potentially with functional groups containing oxygen and probably nitrogen. A lower likelihood is ascribed to the possibility that the detected macromolecules constitute fused-rings polycyclic aromatic hydrocarbons (PAHs), which would show higher carbon to hydrogen ratio. The present authors suggest that the macromolecular compounds detected in the enceladan plumes at the heavier end of the spectrum are related to complex molecules with a web of mutual covalent links (Fig. 1).

4. Enceladus' Primordial Soup

The discovery of diverse organic compounds within a substantial water body on a Solar System moon allows one to obtain new information regarding possible conditions on early Earth. The enceladan subglacial ocean appears to be the first observationally discovered concrete example of what may well be a primeval soup. We note that this statement could be hampered if some forms of life exist now or existed earlier in the enceladan ocean. This scenario could be examined, for example, if a more detailed analysis of amphiphiles embodied in the enceladan organic matter showed correspondence to the characteristic lipid pattern expected from a biological process (Georgiou and Deamer,2014). However, in the absence of evidence to the contrary, a biotic origin of Enceladus' organics remains a remote possibility (Postberget al.,2018).

What Cassini has discovered in the plumes must reflect the chemical and physical conditions of the subsurface ocean and its dynamics over time. In particular, one is curious about the organic molecules that are dissolved, dispersed, or suspended in this aqueous body. The power generated in the core from tidal friction creates high temperatures and thermal gradients in the ocean (Chobletet al.,2017). Further, silicon-rich nanoparticles observed in the plumes have suggested the existence of active hydrothermal vents at the water-rock interface, where temperatures are about 90°C and alkaline pH of 8.5–10.5 and pressures of 10–80 MPa prevail (Hsuet al.,2015). Temperatures inside the porous core, where hydrothermal activity is initiated, may be much higher (Travis and Schubert,2015).

Organic layers, whether liquid oils floating on the ocean's surface (Postberget al.,2018) or organic solids sinking to the rocky core, would undergo chemical alteration and differentiation, interacting with core minerals and metal ions to generate new chemical compositions. Molecular hydrogen, detected in the plumes and likely reflecting hydrothermal activity at the core (Waiteet al.,2017), along with other reducing gases such as methane and ammonia could contribute to further chemical modifications.

The plume analytics in all probability should represent such cross-oceanic chemistry based on the reported upward transportation having a timescale of years (Sekineet al.,2015). The cumulative evidence from the enceladan ocean thus suggests a chemically rich and physically dynamic water body, as befits a prebiotic soup (Wollrabet al.,2016). Further, that the enceladan ocean resides under a thick layer of ice and still becomes rich in increasingly complex organic compounds opposes the notion that atmospheric sparking is crucial for the emergence of a prebiotic soup (Maden,1995). We note, however, that alternative free radical reactions could supplement this missing synthetic pathway.

5. Monomers and Polymers

How fully do the instrumental observations from Enceladus reflect the potential chemical diversity of the subglacial ocean? Regrettably, the resolution of Cassini's instrumentation rarely allows one to identify individual organic molecules in the plume ice grains. Judging merely by size, the lower mass range could represent diverse bio-monomers, such as amino acids (75–200 u), nucleosides (100–300 u) and sugars (200–400 u). However, chemical scrutiny indicates that the molecular properties of the enceladan compounds are quite different from those of most biomolecules. First, the abundance of heteroatoms (oxygen and nitrogen) appears low, similar to that of primordially accreted organic matter (O/C ≈ 0.2, N/C ≈ 0.04) (Alexanderet al.,2017). On the other hand, the observations are consistent with a predominance of relatively long unsaturated hydrocarbon chains, aliphatic or aromatic, with a small number of polar heteroatoms. These molecular characteristics are reminiscent of those affiliated with amphiphilic compounds. We note that while most present-day cellular lipids have aliphatic hydrocarbon chains (Georgiou and Deamer,2014), there are reported instances of lipids with aromatic hydrophobic moieties (Bhattacharya and Biswas,2010).

The higher mass spectrometry fraction (1000–8000 u) spans a range akin to oligomeric or polymeric macromolecules. By size, these could represent linear biopolymers, for example 10–70 amino acid long polypeptides, or a 2–16 long oligonucleotide or 3–40 long oligosaccharide. However, there are counter-indications that make this hypothesis untenable, including the CH-rich, aromatic nature and apparent water insolubility of the observed high molecular mass organics, for which the more probable candidates are kerogen-like compounds (Postberget al.,2018).

The Enceladus mass spectrometry measurements have left it open whether the organic compounds in the plumes actually include monomers (<200 u). As mentioned (Section 4), it is possible that the low-mass-range molecules are artifactual fragmentation products of the higher-mass substances. If so, what was detected in the plumes contains majorly insoluble polymeric substances. But this does not mean that the moon's ocean would not contain smaller molecules. It is possible that the saltwater grains contain monomeric organic material, which stays below the sensitivity threshold of the Cassini instruments. Future missions might be able to characterize such organic molecules, by extending the geophysical characterization toward the search for life-worthy organic molecules (McKayet al.,2014). We note that another set of Cassini results was obtained near Saturn's moon Titan, in which the atmosphere was scrutinized by mass spectrometry without the involvement of ice grains (Waiteet al.,2007). This shows a very similar picture to that reported for Enceladus, that is, carbon compounds in the monomer range (80–350 u) as well as polymers sized up to 8000 u, perhaps pointing to bona fide organic monomers in Titan's atmosphere.

6. Toward Life

It is important to assess the capacity of Enceladus' aqueous organic content to jump-start life. This complements other legitimate questions regarding the similarity of the moon's environments to those proposed by some as essential for terrestrial life's origin—hydrothermal vents and volcanic fields (Deamer and Damer,2017). Obviously, kerogen-like water-insoluble organic polymers would be judged by many as far from optimal for life's emergence. Therefore, one should explore the possible chemical paths by which smaller molecules would coexist with, or be generated from, the water-insoluble mass.

In this realm, considerable insight may be obtained from the experiments performed on carbonaceous meteorites (Cronin and Chang,1993; Pizzarello and Shock,2017). This is a group of asteroid fragments containing between 2% and 8% carbon (Kerridge,1985), including kerogen-like macromolecules (Fig. 1) (Kerridgeet al.,1987), as well as numerous simpler compounds (Cronin,1998). They therefore may carry a record of early carbon chemistry, and provide clues to the organic compounds on planetary and subplanetary bodies, including on ocean worlds, pointing to the compositions that might have led to the onset of life (Pizzarello and Shock,2017). Such an approach is vindicated by published statements that the composition of Enceladus' core bears similarity to that of carbonaceous chondrites (Sekineet al.,2015; Postberget al.,2018).

Earlier analyses of the Murchison carbonaceous meteorite showed that its organic material is largely macromolecular. But in focused analysis aimed at lifelike small molecules, extracts were found to contain a complex mixture of hundreds of monomeric compounds, including carboxylic acids, amino acids, hydroxy acids, phosphonic acids, amines, amides, nitrogen heterocycles (including purines and pyrimidines), alcohols, as well as aliphatic, aromatic, and polar hydrocarbons (Cronin and Chang,1993; Cronin,1998). A more recent paper (Schmitt-Kopplinet al.,2010) provided a nontargeted high-resolution molecular analysis of the solvent-accessible compounds. The results portray ∼30,000 different molecular compositions sized 100–1000 u, each being a compound set sharing an empirical formula. Thus, the meteorite appears to contain millions of specific molecular structures yet to be fully resolved. An example analysis indicated that among methanol-soluble compounds with only C, H, and O atoms, the great majority have 12–30 carbons and 1–2 oxygens, attesting to a likely preponderance of amphiphiles (Fig. 5A). Another analysis that includes all compounds with C, H, N, and O atoms (Fig. 5B), shows empirical formulae corresponding to specific fatty acid lipids. Such data lend strong support to the earlier observation that components in a Murchison extract form vesicular boundary structures (Deamer,1985). One could thus hypothesize that future detailed analyses of Enceladus' insoluble organic polymers could reveal similar chemical constituents, stemming either from a possible native heteroatom content of the insoluble matter, as in humic substance and in the Murchison meteorite (Fig. 1), or from hydrolysis (see below).

In parallel, high-temperature hydrous pyrolysis experiments of solid fossil fuels such as kerogen and bitumen, in the presence or absence of mineral catalysts, gave rise to a plethora of low-molecular-weight organics. The products included alkanes, alkenes, and isoprenoids (Huizingaet al.,1987) as well as long-chain fatty acids (Kawamuraet al.,1986; Siskin and Katritzky,1991). In another set of studies, hydrous pyrolytic degradation of petroleum sediments (kerogen) has been examined both in hydrothermal vents and in the laboratory (Leif and Simoneit,1995). A major set of products constituted amphiphilic n-alkanones with chain lengths from C₁₁ to C₃₃. A similar set of results showed how hydrothermal pyrolysis leads to the formation of diverse polar compounds, including alkanoic acids and alcohols, isoprenoid ketones, and alkanoate esters, in the C₉–C₃₃ range (Rushdi and Simoneit,2011). All these results are consistent with the possible generation of monomeric organics from insoluble polymers under conditions similar to those prevailing on Enceladus. Whether this actually happens on Enceladus could only be verified by future missions and analyses.

In the above portrayals, many of the monomeric compounds are of low polarity. Would such molecules become water-dispersed in an Enceladus-like ocean, and in sufficiently high concentrations to afford the formation of a prebiotic soup? One relevant fact is that H₂O at high temperatures becomes a much better solvent for organic molecules (Siskin and Katritzky,1991). In parallel, it is noteworthy that amphiphiles, prominently featured in the above studies, naturally aggregate to form micelles and vesicles, thereby greatly enhancing their dispersal capacity. Thus, while a C₁₆ fatty acid lipid has a ∼1 nM monomeric solubility (Smith and Tanford,1972), it can easily reach a micellar concentration × 10,000 higher before it approaches the point of phase change (Lobryet al.,1999). Along similar lines, the Enceladus report (Postberget al.,2018) suggests the formation of amphiphilic micelles upon water-mediated oxygenation of the reported plume macromolecules.

Further, micelles of amphiphilic compounds help solubilize otherwise water-insoluble hydrophobic compounds, absorbing them into their lipophilic cores (Bissetteet al.,2014). At higher absorption stoichiometry, structures with larger hydrophobic cores emerge, such as nano- and micro-emulsion droplets (Kronberget al.,2014; Kampmannet al.,2016), thus increasing the aqueous concentrations of the water-insoluble compounds 1,000-fold (Uchegbu,2013). In the same vein, it has been proposed that insoluble disordered organic compounds (tars) could be incorporated into ordered lipid bilayer structures (Yeomet al.,1995; Bywater,2012). Importantly, micelles may also catalyze the covalent transformation of such absorbed hydrophobic molecules to generate additional amphiphiles (Postet al.,2018).

In sum, the enceladan apparent soup may well have a significant and diverse organic repertoire. It may be profusely populated with dispersible aggregates containing both amphiphiles and hydrophobic compounds (Fig. 6), bearing significant resemblance to Oparin's originally invoked colloidal coacervates (Oparin,1938; Oparin and Gladilin,1980). The exact constituents and relative amounts are presently unknown, but such information could be gleaned by further analyses of the Cassini results and by carefully crafted future missions, equipped with capacities to identify individual monomeric species.

7. Prioritizing Origin Scenarios

In an insightful review (Chang,1993), the author asks a fundamental question: What organic compounds were required for the origin of life? He points out that historically the answer has been shaped by a scientist's favorable model: “Metabolism First” calls for carbohydrates, “Protein First” assigns a key role to amino acids, “Lipids First” claims a major involvement of compartment-forming amphiphiles, and “RNA First” advocates the primacy of nucleic acids. The author summarizes this essential incongruity by pointing out that practically all answers are molded by predictions on what early life would have looked like, rather than by consideration of the actual environments in which life may have arisen.

Thus, Chang suggests that any discussion of life's origin should reflect a planetary environmental perspective. Accordingly, we focus here on asking which emergence-of-life scenario is most compatible with the best predictions regarding the organic content of actual prebiotic water bodies. In doing so, it seems appropriate to focus on the likely monomeric compounds as a basis for prioritizing origin-of-life hypotheses. This is because it is more difficult to envisage life emerging directly from simple gases or from random polymers: life's common origin must at one point pass through biochemistry-like mutual interactions of medium-sized molecules such as amino acids, nucleotides, and lipids (Patelet al.,2015).

The most prominent characteristic of the astrobiological monomer repertoire as described above is its molecular diversity. Carbonaceous meteorites contain at least 30,000 monomer types with carbon atom counts of 6–37 and with a relatively narrow abundance range (Schmitt-Kopplinet al.,2010) (Fig. 5C). Similar monomer diversity arises in Miller-type synthesis with mixtures of gases (Wollrabet al.,2016). The authors note: “The capacity to spontaneously produce this extremely high degree of molecular variety in a very simple experiment is a remarkable feature of organic chemistry and possibly prerequisite for life to emerge. It remains a future task to uncover how dedicated, organized chemical reaction pathways may have arisen from this degree of complexity” (Wollrabet al.,2016).

The scenarios of Metabolism First, Protein First, and RNA First require very specific monomers, which may well be represented in the soup at <1/1000 fractions. The enormous chemical competition from “nonbiological” monomers would make the probability of biopolymer synthesis from such monomer mixtures vanishingly small (Shapiro,2000). It thus becomes advisable to explore an origin scenario that fulfills the following criteria:

• (a) 

  Unexclusive involvement of present-life-like monomers and polymers

• (b) 

  Consistency with large monomer diversity

• (c) 

  Consistency with and benefitting from high abundance of carbon-rich compounds

• (d) 

  Compatibility with low organic compounds concentrations

• (e) 

  Compatibility with extreme conditions

• (f) 

  Independence of an external energy source

As befits a good scientific model, many of these criteria are related to a single chemical phenomenon, namely hydrophobic interactions, as portrayed by Tanford (1978). But rewardingly, the entire set of criteria results in a chemical gestalt that helps prioritize origin models.

It appears that among the major origin scenarios one stands out as having a higher conformity with the above set of criteria. This is the Lipid World scenario, as described by Segréet al. (2001a,b) and Lancetet al. (2018). In its full-fledged manifestation, it goes beyond proposing that lipids were essential for encapsulating informational molecules and catalysts (Deamer,2017). Rather, it posits that the first replicators were lipid assemblies (most likely micelles), capable of reproducing their compositional information, driven by non-enzymatic catalysis in the realm of mutually catalytic networks (Lancetet al.,2018). It is further suggested that the advent of life-like nucleic acids, proteins, and metabolites was the result of a prolonged evolutionary progression of reproducing amphiphile assemblies, which gradually developed a capacity to absorb or endogenously synthesize the necessary heteroatom-rich monomers.

In more detail, the Lipid World scenario, embodied in the Graded Autocatalysis Replication Domain (GARD) model, fulfills all the above-mentioned needed criteria as follows (Lancetet al.,2018) (seeFig. 7 for additional details and comparison to the RNA World model):

• (a) 

  The GARD model is opportunistic: it does not necessarily require the availability of specific molecular types, not even specific present-life lipids, such as phospholipids, sphingolipids, and cholesterols. Rather, any amphiphile with the right physicochemical properties is legitimate.

• (b) 

  A prerequisite of the GARD model is the availability of a highly diverse repertoire of lipid-like molecules, which generate multitudes of assemblies with different molecular compositions. Kinetic computer simulations demonstrate that some such assemblies will have a capacity to reproduce by homeostatic growth followed by random splits, a dynamic state called composome (Segréet al.,2000).

• (c) 

  Simple amphiphiles are carbon-rich by nature, typically having 10–30 carbon atoms in their hydrophobic tail (or tails), and very few (1–3) heteroatoms.

• (d) 

  Because of spontaneous assembly formation, for example micelles, lipid-like molecules can undergo effective mutual interactions. Critical micelle concentration values for different lipids cover a wide range between 10 mM and 1 nM (Marsh,2013), with lower values for compounds with longer chains and/or 2 acyl chains. Thus, under prebiotic conditions micelles are likely to form for at least some of the amphiphilic soup components, even if present at rather low concentrations, and without a need for drying processes.

• (e) 

  Lipid assemblies are heat resistant, as they form via hydrophobic interactions, which increase in strength with elevated temperatures (van Dijket al.,2015). Such assemblies also withstand extreme pH (Otzen and Andersen,2013).

• (f) 

  While other models require an external energy supply (activated monomers) for covalent polymerization, GARD feeds on endogenous energy—the formation of micelle (noncovalent “polymers”) driven by hydrophobic interactions is naturally downhill in terms of free energy change.

It is still necessary to ask whether the enceladan ocean environment is conducive to a Lipid First scenario. When judging such a scenario in terms of the formation of cell-like containers, it is necessary to take into account parameters such as amphiphile concentration and structure, temperature, mineral involvement, salt concentrations, and pH ranges (Deamer and Georgiou,2015). We, however, note that a scenario such as GARD is less sensitive to many of these parameters, because in its early stages it does not necessitate an aqueous lumenal enclosure within a stable bilayer.

8. Can Lipids Beget Life?

Some seminal questions are often posed regarding the validity of the Lipid World scenario. These are briefly addressed below and in considerably more detail in Lancetet al. (2018). The main questions are as follows.

9. Conclusions

A prebiotic soup is any water body containing organic compounds from a variety of supply sources. Arguments against the existence of a prebiotic soup are not strong enough to negate its likely existence and role in life's origin. The Enceladus observations teach us by direct measurements that an extraterrestrial organic-rich soup exists even in the absence of an atmosphere. Such a soup is likely fed by primordial accretion, infall, and subsequent abiotic chemical modifications and syntheses, the combination of which may increase its diversity.

The Enceladus data are consistent with a soup replete with highly diverse organic compounds, which could serve as chemical supply for the formation of early lifelike entities. Abiogenesis and further evolution would necessarily occur in a heterotrophic path, until the much later advent of cellular autotrophy. The suitability of a model for life's origin would depend on the degree to which it fits the inferred soup composition, including supplementation by widely published paths for the abiotic synthesis of lifelike molecules (Cafferty and Hud,2014). This review addresses a possible parsimonious scene, whereby the advent of very early life may have depended chiefly on the components of the non-supplemented Enceladus-like soup, and that this course fits well with our Lipid First GARD model.

We point to several characteristics of the GARD Lipid World scenario, which are highly compatible with Enceladus-style soup. First, GARD is consistent with, and in fact benefits from, a soup's large molecular diversity. Second, the moon's chemistry is consistent with considerable amphiphilic abundance. Third, GARD is compatible with low concentrations of organic compounds. Fourth, while other models require an external energy supply, GARD feeds on endogenous energy. And fifth, lipid assemblies are much more resistant to extreme conditions. We further note that the GARD model affords a gradual simulatable path from Lipid World to life as we know it, turning such emergence into a problem in evolutionary dynamics.

Our comparison between the RNA First and Lipid First scenarios (Fig. 7) is not intended to negate the crucial role of RNA in life's emergence. Rather, it points to the possibility that Lipid First non-equilibrium, catalysis-based dynamics could serve as a pre-RNA first step on a long road to full-fledged protocells. Such portrayal addresses the widely expressed doubts regarding the probability of molecules as complex as self-copying covalently strung RNA to emerge directly from random chemical mixtures (Shapiro,2006). We suggest that such direct emergence may be more probable for a much simpler system, a self-copying noncovalent assembly of catalytically interacting amphiphiles. This statement is backed by explicit computations of the probability of appearance, on a planetary scale, of self-reproducing lipid micelles (Lancetet al.,2018, Section 13).

A nagging question is which of the two scenarios is more probable, when assessing the transition from an initial replicator to a full-fledged protocell with RNA, proteins, membranes, and metabolism. This transition is considered by some to be on the verge of magic (Ralser,2018). In this context, RNA First proponents use statements such as “The first … [entities] are RNA replicase and a self-replicating vesicle, [which later] combined into a protocell, enabling rapid evolutionary optimization” (Szostaket al.,2001). Similarly, it is stated, “[at] first … RNA was the only component of biological catalysts, the second episode began with the invention of translation-based synthesis of proteins” (Benneret al.,1989). These portrayals do not specify a molecular mechanism for the major transitions involved. The key difficulty is that, in an RNA-centric view, evolution cannot begin before several life component types join forces. An advantage of the GARD Lipid World view is that rudimentary evolution becomes possible at the lipid-only stage, and RNA, proteins, and metabolism may then emerge in the realm of a long, gradual Darwinian evolutionary process, in a set of molecularly describable routes (Lancetet al.,2018, andFig. 7).

The Enceladus analyses do not constitute a factual proof for the Lipid First scenario; they only make it more likely in terms of building block availability. Thus, at present, it is hard to reach a final verdict regarding an overall favorable scenario for life's origin. The idea of compositionally rooted lipid-based origin may therefore offer important though unorthodox goals for planetary missions. A focus on sequence-encoded information calls for seeking linear polyelectrolytes (Benner,2017). In contrast, the lipid composition scenario suggests a quest for early assemblies of more apolar and smaller molecules. A higher mass-spectrometry resolution could reveal the predicted lower-mass building blocks and their diversity. It may also be able to detect narrower chemical repertoires in molecular assemblies as compared to that of their environment, as predicted (McKayet al.,1996; Lancetet al.,2018). These further points of evidence could be of help when seeking evolving entities in the enceladan ocean and elsewhere. In sum, more extensive evidence from astrobiological research, chemical experimentation, and computer analyses would be necessary for the ultimate arbitration between origin-of-life scenarios.

Acknowledgments

We thank Dr. Reut Sorek Abramovich and Dr. Raphael Zidovetzki for critically reading the manuscript, and the Minerva foundation for support through a grant “The emergence & evolution of early life under extreme planetary conditions.”

Abbreviations Used

GARD

Graded Autocatalysis Replication Domain

HMOCs

high-mass organic cations

IOM

insoluble organic matter

u

atomic mass units

References