Alien Mindscapes—A Perspective on the Search for Extraterrestrial Intelligence

1. Introduction

The Kepler mission and ground-based observatories have revealed thousands of exoplanets in small sectors of our galaxy alone, thus providing powerful evidence that our solar system is not an exception but simply one out of countless others in the Universe (e.g., Borucki et al., 2010; Kopparapu et al., 2013; Seager, 2013; Batalha, 2014; Gaidos et al., 2014; Hatzes, 2014; Quintana et al., 2014; Macintosh et al., 2015). What remains unanswered, however, is whether life—simple or complex—exists beyond Earth.

For nearly 20 years, astrobiology has brought a multidisciplinary vision to this quest through three fundamental science questions: (1) How does life begin and evolve? (2) Does life exist elsewhere in the Universe? (3) What is the future of life on Earth and beyond? In the 2008 version of its roadmap (Des Marais et al., 2008), astrobiology proposed a global approach to these questions through a broad research program with the goals to understand the formation and evolution of habitable planets, to explore and characterize the evolution of planetary environments favorable to life's development in the Solar System and beyond, and to find methods to detect the signatures of life on early Earth and other worlds.

Thirty-five years before the creation of astrobiology, a very similar intellectual approach had been articulated by Frank Drake in the “Drake equation” (Section 2) but with a different intent. The Drake equation provided a probabilistic model to estimate the number of actively communicating extraterrestrial civilizations in the Milky Way, and was formulated around a technological imperative (radio astronomy) and a philosophical question: Are we alone?

Decades of perspective on both astrobiology and the Search for Extraterrestrial Intelligence (SETI) show how the former has blossomed into a dynamic and self-regenerating field that continues to create new research areas with time, whereas funding struggles (Garber, 1999) have left the latter starved of young researchers and in search of both a long-term vision and a development program. A more foundational reason may be that, from the outset, SETI is an all-or-nothing venture where finding a signal would be a world-changing discovery, while astrobiology is associated with related fields of inquiry in which incremental progress is always being made.

Yet in the same way astrobiology approaches the understanding of life in the Universe, SETI carries in its quest fundamental and unique questions that are central to the understanding of who, what, and where intelligent life is, and how to find it. While Are we alone? is their philosophical and popular expression (Zuckerman and Tarter, 1979; Tarter and Chyba, 1999), their scientific formulation can be expressed in these questions: How abundant and diverse is intelligent life in the Universe? How does intelligent life communicate? How can we detect it? If understanding life is the thread woven through the astrobiology roadmap, understanding how intelligent life interacts with its environment and communicates information is central to SETI.

In the following sections, we examine how scientific and technological advances are now allowing us to explore these questions in ways that were not previously possible, and to build the foundation of a long-term, multidisciplinary, and integrated vision for SETI. Here, we offer a perspective on how we could scientifically augment the odds of finding extraterrestrial life (ET) and an invitation to change our mind-set in doing so.

2. Historical Pathway to ET

While the scientific foundation for a living universe was established in the 16^th century with the Copernican revolution, the nature of advanced civilizations remained the domain of philosophers and fiction writers for a few more centuries (e.g., Descartes, 1644; de Fontenelle, 1686; Voltaire, 1752/2002; Kant, 1755/2009; Swendenborg, 1758; Flammarion, 1872—reviews by Dick, 1984; Crowe, 2011). The latter populated the Universe and our psyche with beings and worlds that were no more than idyllic or nightmarish versions of ourselves, our society, and our biosphere. By the end of the 19^th century, the advent of new technologies opened a different epistemological chapter for SETI. At that point, the quest for alien civilizations started to transition from a justifiable belief to a technology-based endeavor. Electricity and radio were first proposed as means to communicate with our close neighbor (Seifer, 1996) after Schiaparelli described channels—canali, in Italian—on Mars that later, Lowell (1906) erroneously claimed were artificial canals constructed by Martians. Over a half-century later, Cocconi and Morrison (1959) became the first to point out the possibility of searching for aliens in the microwave spectrum. Their expectation was that extraterrestrial signals could be pulse-modulated (e.g., Shostak, 2011a), and they proposed to examine solar-mass and red dwarf stars within 15–50 light-years of Earth.

The conclusion of their article in Nature contained key comments that still resonate today. These comments include the realization that technology was finally available to test scientific hypotheses consistent with observational and theoretical astronomy, an understanding of the transformative philosophical and practical implications of a potential contact with an alien civilization (e.g., Almár and Tarter, 2011; Eliott, 2011a), and a concern that their work would be consigned to science fiction by many.

Independently from Cocconi and Morrison, astronomer Frank Drake had been formulating similar plans to conduct an actual search, and within a year of the publication, Project Ozma was launched at Green Bank (Schuch, 2011). Modern SETI was born and set out to search for ET's presence through narrowband radio astronomy. Broadband optical astronomy became an additional search tool in 1998 with OSETI (Ansbro, 2001), although the idea was previously suggested by physics Nobel laureate Charles Townes, whose research led to the maser and the laser (e.g., Schwartz and Townes, 1961; Wright et al., 2014).

Since 1961, SETI's intellectual framework has been centered on a probabilistic argument, the now-famous Drake equation: \documentclass{aastex}\usepackage{amsbsy}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{bm}\usepackage{mathrsfs}\usepackage{pifont}\usepackage{stmaryrd}\usepackage{textcomp}\usepackage{portland, xspace}\usepackage{amsmath, amsxtra}\pagestyle{empty}\DeclareMathSizes{10}{9}{7}{6}\begin{document} \begin{align*}N = R_{*} \cdot f_{\rm p} \cdot n_{\rm e} \cdot f_{\rm l} \cdot f_{\rm i} \cdot f_{\rm c} \cdot L\end{align*} \end{document}

where N is the number of civilizations in the Milky Way whose electromagnetic emissions are detectable; R _* is the average rate of star formation in our galaxy; f _p is the fraction of those stars with planetary systems; n _e is the number of planets, per solar system, with an environment suitable for life; f _l is the fraction of these planets that actually develop life; f _i is the fraction of life-bearing planets that develop intelligent life; f _c is the fraction of civilizations that develop a technology that releases detectable signs of their existence into space; and L is the length of time such civilizations release detectable signals into space. For reviews and discussions about the Drake equation, see, for example, the works of Shostak (1998), Vakoch and Harrison (2011), Maccone (2012), Vakoch (2014), Vakoch and Dowd (2015), and Darling and Schulze-Makuch (2016).

Both lauded and criticized from the day it was formulated, the Drake equation clearly represented a watershed moment in science that gave humanity a glyph with which to spell alien life for the first time. Included as a forethought to the 1961 Green Bank Search for Extraterrestrial Intelligence meeting agenda (Drake, 2011), the so-called equation proved to be anything but. Consisting of a combination of quantitative and speculative factors that were solely meant to engage a discussion within the scientific community on the potential number of extraterrestrial civilizations willing and able to communicate in our galaxy, it quickly became SETI's signature. In hindsight, it was much more.

3. A Roadmap

The term equation is misleading in this context. Nor does the label probabilistic argument fully capture what the formulation truly represents, and the succession of some of its variables could be criticized. For instance, between f _i and f _c the notion of intelligence abruptly gives way to that of civilization, when they are, in fact, distinct notions. On our planet, one has not been demonstrated to necessarily lead to the other. Earth has developed a number of intelligent species, some of which use tools, while others are organized in hierarchical societies. Ultimately, the term technological civilization is what differentiates humankind, that is, an advanced stage of social development and organization, where scientific knowledge is applied for practical purposes on an industrial scale. In our case, this technology allows our species to scientifically explore and characterize our planet, the Solar System, and the Universe—and, on Earth, this is unique to the human species.

Nevertheless, the Drake equation was essentially the first roadmap and the first holistic vision of the search for life in the Universe (Tarter, 2007)—an approach that would become the trademark of the nascent field of astrobiology 35 years later (Des Marais et al., 2008). Even at this seminal time, it captured in one expression the notions of extrasolar planetary systems, habitable zones, habitable planets and environments, the transition from chemistry to biology, life on and beyond Earth, and the evolution of intelligence, civilization, and technology.

In the epistemological sense, the Drake equation provided a reductionist approach by scientifically breaking down the question of technologically advanced civilizations into simpler and smaller parts (the variables). Ultimately, it overlooked its own revolutionary vision as SETI focused on the application of one technology to search for Sun-like stars and red dwarfs (e.g., Tarter, 1979, 2004; Billingham et al., 1980; Gulkis et al., 1981; Heath et al., 1998; Turnbull and Tarter, 2003; Tarter et al., 2007). This rationale remains largely unchanged today despite advances in exploration and science that are relevant to the factors of the equation. As it stands, SETI does not search for all life or for all intelligent life. It focuses exclusively on technologically advanced life.

At the time of its formulation, the Drake equation was simply meant to be a tool to gauge how many technologically advanced civilizations might be “out there.” The focus was clearly on the end-number (N) to evaluate whether radio astronomy and astrophysics could provide successful strategies to intercept ET's signal across interstellar distances (Tarter, 2001a). The focus was not on trying to understand or quantify the processes taking place within each of the factors that lead to the next. Drake himself stated that his equation was not aimed at searching for primordial or primitive life-forms (Drake, 2011). Rather, it was aimed at the radio search. This explains SETI's path from the moment the Tatel Telescope at Green Bank was turned toward Tau Ceti and Epsilon Eridani for the first time. This might also explain why the radio receivers have remained silent since (see Sections 4 and 5).

Over the years, and with the exception of a clear connection to exoplanet detection (Tarter, 2001a, 2001b; Harp et al., 2015) and other astronomical fields, SETI around the world has evolved, for most, independently from core disciplines that rightly should be considered central to its understanding of what alien life could be and, therefore, to an understanding of how to optimize a detection strategy. While individual efforts exist, they have yet to be integrated into one vision and effectively support each other and existing projects (e.g., Fig. 1). It could be argued, but with only partial justification, that the reasons for SETI's all-or-nothing venture are grounded in historical circumstances. Very little data were available to quantify the factors of the Drake equation at the time it was formulated, and most knowledge about the Solar System and the Universe was still primarily coming from ground-based astronomy and astrophysics. President Kennedy was a year away from declaring the race to the Moon, and orbiters were sent to Mars and Venus for the first time. It was a time of discoveries to come, in which the young science of radio astronomy was viewed as a unique tool to help humanity make what would be a world-altering discovery.

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FIG. 1.

Example of an integrated path to ET detection showing basic science questions (e.g., who and what are we searching for, and where?), key multidisciplinary science concepts, and relevant exploration methods (how do we investigate?). The combination of questions and approaches results in a directed and scientifically rich vision to ET detection, whose output is a reasoned exploration target. Since 1960, SETI's exploration strategy has prioritized the detection method (radio and optical searches) without addressing the fundamental nature of who and what ET could be, which has fundamental implications for where and how to search for it. The science concepts and methods shown here are discussed in the text.

4. The Evolution of N in the Past Decades

By contrast to this time, large databases are now available in many relevant fields—and not necessarily only in astronomy—but their integration to SETI's approach has been slow in coming. Yet the means are currently in place to substantially increase the odds of finding ET through the development of an expanded search strategy that reflects this new knowledge.

4.2. Evolutionary and systemic approach to N

Progressing to the right of the Drake equation, astronomy and biology are linked through two concepts: habitable zone and environmental habitability (e.g., Cockell et al., 2016). Both notions are mutable in space and time, the latter even more so than the former; and on Earth, climate change, extreme terrestrial environments, and genomics demonstrate how fast environmental changes can happen and how much the evolution of life and environment are intertwined (Golding and Glikson, 2011). While the initial astronomical and physicochemical conditions may drive the type of prebiotic chemistry possible on a planet, life, as demonstrated on Earth, becomes a primary player in shaping its environment as soon as it takes hold (e.g., atmosphere, landscape, mineralogy). This is the fundamental concept of coevolution of life and environment (e.g., Watson, 1999; Kooijman, 2004; Dietrich et al., 2006; Knoll, 2009; Grenfell et al., 2010; Kolb, 2014). This coevolution will dictate the uniqueness of each planetary experiment (Irwin and Schulze-Makuch, 2001; Schulze-Makuch et al., 2013) and will do so not only when (or if) life reaches the stage of technological advancement. It will start from the very first moment, as it did on Earth.

Earth's biosphere, and all events that led to us, and the way we perceive the environment and the Universe are the result of over 4 billion years of reciprocal influences between environmental and biological processes (Fabbro et al., 2015; Houri-Ze'evi et al., 2016). They are the result of evolutionary bottlenecks induced by geological, climatic, and cosmic events (Lynch and Lande, 1993; Bürger and Lynch, 1995; Bijlsma et al., 2013). An asteroid impacting instead of missing Earth would completely alter the course of evolution at any time.

Ultimately, biological evolution on Earth has been partially dictated by somewhat predictable cycles and events (astronomical, climate) but drastically more so by stochastic events, both geological and biological in nature (Fig. 2) (Pigliucci and Müller, 2010), by when and where they occurred and at what stage of evolution they happened (Gould, 1998; Raup, 1999; Schulze-Makuch and Irwin, 2001; Schulze-Makuch et al., 2013; Keller and Kerr, 2014; Lehman and Miikkulainen, 2015). It follows that, even considering panspermia and planetary exchange as primary seeding mechanisms (e.g., Arrhenius, 1907; Arrhenius and Mojzsis, 1996; Melosh, 1996; Burchell et al., 2004; Napier, 2004; Gladman et al., 2005; Owen, 2008; Worth et al., 2013), two planets with absolutely similar environments and receiving absolutely similar seeding material may have two very distinct biological destinies depending on when extinctions and evolutionary bottlenecks take place, and whether these events have transient or long-lasting effects on the environment. Stochastic events will give each planet a unique fingerprint. If life arises through abiogenesis of simple organic compounds (Des Marais, 1999; Popa, 2004; Shapiro, 2006; Pross, 2012; Pross and Pascal, 2013), this fingerprinting will be even more uniquely connected to its planet of origin, and cosmic chances are that both exogenic and endogenic processes are acting together in proportions specific to each planetary system.

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FIG. 2.

Coevolution of life and environment. Environmental perception and neural systems of the species living on Earth are intimately linked to the coevolution of life and environment, a process that has been subjected to random probability events all along its continuum. This process started with accretion and the specific elements that contributed to planetary formation. As prebiotic chemistry transitioned to life, the period of heavy bombardment continued to spatially randomly deliver material to Earth, contributing equally to the destruction of a nascent life and the development of a new one. Since life took hold, stochastic events have continued in the physical world as environmental and cosmic catastrophes, and in the biological world as adaptive evolution and epigenetic changes. While the notions of habitable zone and environmental habitability are critical in trying to predict whether a planet could host life as we know it, the very random nature of the coevolution of life and environment renders each planet and the life it may bear a unique experiment, which questions the anthropocentric principle underlying the Drake equation.

Moreover, if Earth is any indication of universal planetary laws of evolution, nature produces simple systems in overwhelming numbers compared to complex systems (Mandelbrot, 1982). Statistically, microbial life still dominates today, and for 70% of Earth's history was the only form of life on our planet (Margulis, 1996; Nealson and Conrad, 1999; Wolf et al., 2002). Taking inventory, global species richness estimates suggest that up to 10 million species of eukaryotes and up to 100 million to a billion prokaryote species exist today on Earth (Colwell and Coddington, 1994; Gaston, 2000; Colwell, 2009; Mora et al., 2011; McGinley, 2014), while the most recent studies model up to one trillion species (Locey and Lennon, 2016). In this inventory of all terrestrial life, through competition, only humans have reached technology. However, this statistical snapshot alone does not provide an accurate estimate of a realistic ratio, as it does not reflect the (unknown) total number of species produced by our planet over time. Those include evolutionary dead ends and species that went extinct as a result of climatic or catastrophic events but still played their part in shaping the global biosphere from which we, the human species, emerged. It does not account for the shadow biosphere hypothesis, either (Cleland and Copley, 2005; Davies et al., 2009).

A systemic approach to N shows that it took 4 billion years of symbioses, competition, biodiversification, and the development of all species that did—and did not—survive for us to be here. Some key evolutionary leaps have yet to be completely understood. Only very recently, the common ancestral gene that may have enabled the evolution of complex life over a billion years ago was identified. Without this gene, life on Earth might not have evolved beyond the stage of slime (Lai et al., 2016). We also have yet to understand what led one species of apes to separate itself from the others just a few million years ago (Arsuaga, 2010). Understanding these transformative processes may bear considerable weight on N. It is certainly not necessary to wait for all the answers to start searching for ET, but we must acknowledge that these questions exist, and develop search strategies adapted to the complexity they underscore in order to augment the chances of success.

We are, indeed, the product of local astronomical and planetary factors. However, it would be unreasonable to suggest that similar evolutionary convergence never happened with seemingly so many planets already discovered in the small spatiotemporal window of the Kepler telescope. Somewhere out there, based solely on numbers and probabilities, life may have evolved to bear some resemblance to us—if only fortuitously. It might interact with its planetary environment as we do, and evolve to produce biological forms with logical minds presenting similarities to us who may be willing to communicate in ways we can understand. However, the numbers are unlikely to be in the billions or even the millions in our galaxy. There may be just a handful scattered across vast distances and time.

Taking life's evolution on Earth as a guide, there is likely a universal probabilistic law of evolutionary convergence that is inversely proportional to life's complexity; that is, the simpler life is, the greater chances are that similar life-forms will be abundant throughout the Universe. The more complex life is, the more rare convergence is likely to be. Complexity in life-forms is an integration of temporal evolution and probabilistic events. The longer life is around, the greater chance it has to adapt through regular cycles and, at any given time, to mutate through stochastic events. Looking back at ourselves, it took 70% of Earth's time in the habitable zone and an incredible amount of “chance and necessity” (Monod, 1972) for one species in a complex tree of life to reach civilization and technology.

The longer evolution takes, the greater the chances are that species will be wiped out and ecosystems profoundly transformed (e.g., Alvarez and Asaro, 1990), but with the rise of technology, some of the endogenic and exogenic risks to life can also be offset (e.g., asteroid monitoring, Yeomans, 2013). Conversely, human evolution shows that technology brings its own sets of risks: the natural dynamics are upset (Holocene extinction: Barnosky et al., 2011), the environment modified (Anthropocene: Grinspoon, 2012; Waters et al., 2016), and the terms of the coevolution of life and environment that led to the rise of the dominant species deeply altered.

At this point in time, humans have generated an environmental disequilibrium that reverberates across the biosphere globally and endangers the conditions of planetary habitability that were favorable to its emergence. The notion of self-engineered destruction is certainly present in the last factor of the Drake equation. L reflects on how long a technological civilization might be willing and able to communicate. More than duration, this factor focuses on the odds of detecting a signal; that is, the longer an alien civilization broadcasts its presence, the more chances we have to detect it. Assuming the anthropocentric view of a technological civilization presenting similarities with ours, willingness to communicate may depend on a host of reasons (e.g., political, scientific, technological, philosophical, religious, and social). How long such a civilization would continue to communicate is a more complex issue. Duration can relate to a civilization's ability to avoid self-inflicted—or other—destruction, scientific advances, and interest. It could also relate to a cosmologic perspective we have not yet reached, including a sense of place and responsibility as a member of a universal community (e.g., the Fermi paradox).

As expressed, L examines for how long such a civilization would broadcast a signal in ways we can detect, which are primarily focused on radio and optical astronomy. We could assume, however, that a technological civilization may communicate or broadcast in ways so advanced compared to ours that we simply cannot imagine what they are and are thus unable to detect its signals. Or this civilization may have long since disappeared. These scenarios are implicitly present in the current definition of L. However, there is also an evolutionary dimension to this factor that transcends the existing formulation.

5. Expanding the N Horizon

The evolutionary pathways that lead to complex life on Earth strongly suggest that advanced life as we know it may be rare in the Universe and unlikely to be in a state of advancement that is temporally synchronous with us. However, that does not mean that other types of advanced intelligences are as rare. Limiting our search to something we know and can de facto comprehend is, probabilistically, a constraining proposition, one that leaves no room for an epistemological and scientific foundation to explore alternate hypotheses. To find ET, we must expand our minds beyond a deeply rooted Earth-centric perspective and reevaluate concepts that are taken for granted.

6. An Integrated Vision Moving Forward

So far, a number of perspectives have been offered to explain why radio receivers have remained silent for the past 50 years, including the Fermi paradox and the Zoo hypothesis (Ball, 1973). More recently, two new scenarios have been added: ET is dead, based on the argument for a Gaian bottleneck (Chopra and Lineweaver, 2016), and the opposite view, that we are the oldest civilization in the Galaxy (Sasselov, 2012). It may be that the answer is much simpler and humbling. The fact is that we embarked on this journey only a few decades ago and have applied to it very limited tools and detection strategies. Telescopes have become bigger, arrays larger, resolution better, but the technology and exploration strategies behind SETI have remained basically unchanged. In reality, we have yet to articulate core questions to place SETI in its proper, systemic, and evolutionary context.

In its current scientific and technological form, SETI can be likened to sampling the cosmic ocean with a plankton net, where the size of the antennas and their number are analogous to the mesh size. Refining the mesh size by adding antennas or making them bigger will not make the tool more effective compared to the breadth of exploration at hand. Further, this tool is only focused toward testing one very specific, largely anthropocentric, hypothesis about extraterrestrial intelligence (ETI), when data increasingly suggest that there are probably as many distinct life-forms and intelligences as habitable planetary environments in the Universe. While the historical view of ETI is a valid hypothesis that must be tested, it is one among many, and we should proceed with it acknowledging that the chances of a rendezvous somewhere in time, and space, with that particular alien are remote.

When the odds are small and the object of a search unknown, the rule of thumb is to cast as large a net as possible to increase the chances of success rather than the opposite. In this case, a larger net is not solely a larger set of antennas or more abundant resources focused on one technology or one experiment (Billings, 2015). For SETI, it is critical to fully embrace the multidisciplinary approach that was scripted 50 years ago in the Drake equation and create a well-stocked and diverse tool kit to explore a vision that serves as an umbrella under which many disciplines will synergistically contribute advances to expand the search for alien life beyond the anthropocentric principle.

Some bridges are already in place and being investigated, such as the clear connections between the search for ET and exoplanet exploration (e.g., Tarter, 2007). SETI uses the Kepler catalog and ground-based telescope databases to target high-priority candidates. Prioritization criteria are currently limited to parameters for life as we know it (e.g., exoplanets in the habitable zone of their parent stars; unexplained signals from known exoplanetary systems, see Harp et al., 2015; Schuetz et al., 2015; Abeysekara et al., 2016). Those criteria will be refined over time as universal markers are being identified and as we learn more about possible exotic biochemistries (e.g., McKay, 2004; Ward and Benner, 2007; Davila and McKay, 2014), but the connection is established and will only grow stronger.

In addition to this, new research pathways bear significant promises for a more universal SETI reach, such as ET and systemic planetary disequilibria, the coevolution of life and environment, and neural systems and their role in our perception of the Universe, our interaction with it and how we communicate about it—to name but a few. Figure 3 summarizes a path to achieving this integrated and synergistic vision. It shows a notional network between disciplines with bridges and research avenues connecting together space, planetary, life, geosciences, astrobiology, cognitive, and mathematical sciences. Others will be added as knowledge progresses. It is a dynamical vision forward, built on a connectivity network that represents an expanded version of the Drake equation, one that integrates all the historical factors now broken down into measurable terms.

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FIG. 3.

Connectivity network between disciplines showing the bridges and research avenues that link together space, planetary, and life sciences, geosciences, astrobiology, and cognitive and mathematical sciences. This representation is an expanded version of the Drake equation. It integrates all the historical factors now broken down in measurable terms and expanded to include the search for life we do not know using universal markers, and the disciplines, fields, and methods that will allow us to quantify them.

This vision expands the search to life as we do not know it using universal markers and the disciplines, fields, and methods that will allow us to quantify them. Points of intersection are the knowledge that will be contributed to SETI by integrating these various disciplines. This contribution will be provided in five fundamental areas: (1) scientific rationale (theories, hypotheses); (2) experimental design (methods, protocols, and metrics); (3) communication (universal markers, signals, instruments, systems, technologies); (4) target identification; and (5) missions that will allow SETI to implement its own vision. These sciences are already collecting vast data sets that can now be interrogated in ways we could not have imagined only a few years ago. Bioneural computing, communication theory, machine learning, neural coding, neural network and deep learning, data mining, and big data analysis are the building blocks of the connecting bridges that SETI must build as a prerequisite to a universal exploration of ET versus the current anthropocentric search.

7. Conclusion

Now is the time for SETI to develop a roadmap and long-term vision that includes the search for life as we do not know it. New tools are available that can enable this approach and help us decipher the evolutionary and probabilistic nature of advanced alien life. These tools are found in astronomy and astrophysics but also in the biological, geological, cognitive, mathematical, and computer sciences, among others. All of them must be deployed when thinking about who, what, and where ET could be, and how it might communicate.

To find ET, we will have to turn inward (evolution, perception, and communication) and outward (planetary environments) and challenge our anthropocentric assumptions. Through consilience, we can build a systemic and connective vision of intelligent life in the Universe. To be achieved, this vision requires the exploitation of multidisciplinary synergies and an intellectual framework with a clear agenda and milestones. A similar intellectual and logistical structure was successfully established 20 years ago by NASA with the creation of the NASA Astrobiology Institute (NAI) for the understanding of life on Earth and beyond. However, past and present astrobiology roadmaps have not put substantial emphasis on alien intelligence, communication, or technology.

In the coming months, the SETI Institute will be initiating efforts in this direction, and will invite the United States and international research communities to contribute to the drafting of a new scientific roadmap for SETI. We will explore resources for the development of a virtual institute and an intellectual framework for multidisciplinary projects specifically focused on the advancement of knowledge on ETI. Complementary to, and different from, the astrobiology roadmap, this vision will bridge the NAI roadmap, augment it, and go beyond it.

Its primary goal will be to “Understand how intelligent life interacts with its environment and communicates.”

This will be explored through three main questions:

Question 1: How abundant and diverse is intelligent life in the Universe? With this question, SETI will synergistically use data from astrobiology, biological sciences, space and planetary science and exploration, and geoscience to quantitatively and qualitatively characterize the potential abundance and diversity of intelligent life in the Universe. Its spatiotemporal distribution will be approached using cosmological models of the physicochemical evolution of the Universe and inferred viable biochemistries.

Question 2: How does intelligent life communicate? Cognitive sciences, neuroscience, communication theory, mathematical sciences, bioneural computing, data mining, and big data analysis, among other disciplines, will explore communication in intelligent terrestrial species. They will use physicochemical and biochemical models of known exoplanetary environments to generate and map probabilistic neural and homolog systems, and infer the resulting range of viable alien sensing systems and the perception of the Universe they confer. Spatiotemporal distribution models will be inferred from Question 1–related investigations.

Question 3: How can we detect intelligent life? Exploration strategies, instruments, experimental protocols, technologies, and messaging (content and support) will be designed using the results, data, and databases of research conducted under Questions 1 and 2.

Ultimately, SETI's vision should no longer be constrained by whether ET has technology, resembles us, or thinks like us. The approach presented here will make these attributes less relevant, which will vastly expand the potential sampling pool and search methods, ultimately increasing the odds of detection.

Advanced, intelligent life beyond Earth is most likely plentiful, but we have not yet opened ourselves to the full potential of its diversity. With the vision presented here, we offer a unified and universal approach for the search for extraterrestrial life—one that is measurable and searches for ET at the crossroads of scientific and technological innovation, and imagination.