The launch of a new journal is appropriately like a space mission. It is the result of a scientific need, the inspiration of a group of committed scientists and technologists, a series of draft proposals, an approved mission protocol, and a launch. Today is the launch day for a journal whose remit has only recently consolidated from diverse disciplines. Cambridge University Press has an international reputation for astronomy. To this we add extreme biology and its associated environmental research to integrate astrobiology as: ‘the study of the origin, evolution, adaptation and distribution of past and present life in the Universe’.

Astrobiology has three main themes: (1) Origin, evolution and limits of life on Earth; (2) Future of life, both on Earth and elsewhere; (3) Search for habitats, biomolecules and life in the Solar System and elsewhere. These fundamental concepts require the integration of various disciplines, including biology (especially microbiology), chemistry, geology, palaeontology, and the physics of atmospheres, planets and stars. We must also keep our minds wide open about the nature and limits of life. We can safely assume a carbon-based system within Solar Systems as we know them, but our concept of habitable zones expands yearly. We were taught that only the spores of certain bacilli could survive temperatures above the boiling point of water, and yet we now know that the deep-sea vent microbe Pyrolobus can survive an hour at 121 °C, which is the temperature used for sterilising medical instruments. We know of cyanobacteria which can not only live inside deep-frozen Antarctic rocks but also survive on roof-tops in Jerusalem at 80 °C. The bacterium Deinococcus radiodurans tolerates lethal doses of nuclear radiation, and cyanobacteria inside Antarctic desert sandstone receive so little moisture that their carbon turnover time (from its fixation by photosynthesis to its release as carbon dioxide during respiration) is 10,000 years. Life is tolerant, adaptable and tenacious.

Two thermodynamic principles offer considerable insight into the climatic and geological settings for life on other planets, namely (1) that natural systems tend to actually achieve the ideal (‘Carnot’) limit of conversion of heat into work and (2) if a fluid system such as an atmosphere has sufficient degrees of freedom, it will choose the degree of heat transport that maximizes the generation of work (equivalently, that which offers maximum entropy production). The first principle agrees well with results on terrestrial cumulus convection, and the mechanical energy released by tectonic activity. The second principle agrees with the observed zonal climates of Earth, Mars and Titan, and shows promise for planetary interiors too; I discuss applications in the investigation of paleoclimates and habitability. I compare the work performed by planetary atmospheres and interiors on the terrestrial planets and thereby predict a weakly eroded landscape on Titan. The association of life with the production of entropy is also noted, and the possibility of evaluating planetary entropy production by telescopic observation is discussed.

Crossed-beam experiments on the reactions of cyano CN(X2Σ+) and ethinyl C2H(X2Σ+) radicals with the unsaturated hydrocarbons acetylene, ethylene, methylacetylene allene and benzene have been carried out under single-collision conditions to investigate synthetic routes to form nitriles, polyynes and substituted allenes in hydrocarbon-rich atmospheres of planets and their moons. All reactions were found to proceed without an entrance barrier, to have exit barriers well below the energy of the reactant molecules and to be strongly exothermic. The predominant identification of the radical versus atomic hydrogen exchange channel makes these reactions compelling candidates for the formation of complex organic chemicals – precursors to biologically important amino acids – in Solar system environments and in the interstellar medium.

The chemical structure of the dicyanogen photopolymer (CN)x, also known as paracyanogen, prepared in different solvents from dicyanogen (CN)2 photopolymerization under the action of ultraviolet light, is shown to be very similar to the polymer derived from hydrogen cyanide (HCN) and from certain tholins obtained from a simulated Jovian atmosphere. The implications of dicyanogen and its polymer as a precursor of some organic molecules already detected in cometary comas and tails and in meteorites are discussed. In particular, paracyanogen may be present in the cometary nuclei and in the surface of certain low-albedo objects in the Solar system.

The notion that ultraviolet (UV) fluxes, and thus biologically weighted irradiances, were higher on Archaean Earth than on present-day Earth has been a pervasive influence on thinking concerning the nature of early Earth. It directly influences calculations concerning protection strategies that may or may not have been required by early life. Our knowledge of the Earth's changing UV radiation climate over time depends upon our knowledge of a diversity of factors, the magnitudes of which are uncertain. Here these uncertainties are explored. During the Archaean Era, calculations of the surface photobiological environment span a three order of magnitude difference in DNA-damage weighted irradiances with consequences for our assumptions concerning the environment for exposed surface life and the role of UV radiation as a mutagen. These differences are primarily caused by uncertainties in the concentrations of trace gases and the partial pressures of carbon dioxide and nitrogen that affect scattering in the atmosphere. To a lesser extent, the luminosity of the Sun in the UV region is also a factor. During the Proterozoic and Phanerozoic, when we know that an ozone column existed, these uncertainties drop to two orders of magnitude and are primarily caused by poor knowledge about the frequency and atmospheric effects of potentially ozone-depleting agents such as volcanism, impact events and supernovae explosions as well as the effects of global temperatures on ozone concentrations and thus surface UV irradiance. Changes in other atmospheric constituents during this time have less of an effect on photobiological consequences, which include a Palaeozoic oxygen pulse. Understanding the cause of photobiological uncertainties and their consequences constitutes a current challenge for atmospheric chemists and photobiologists.

Solar radiation is the primary energy source for surface planetary life, so that pigments are fundamental components of any surface-dwelling organism. They may therefore have evolved in some form on Mars as they did on Earth. Photosynthetic microbes are major primary producers on Earth, but are concurrently vulnerable to ultraviolet (UV) damage. Using non-intrusive laser Raman spectroscopy to recognize the component parts of biomolecules, we have shown not only the abundance of microbial photosynthetic and photoprotective pigments in situ, but also their spatial distribution within their microhabitat. This essential aspect of their screening or avoidance survival strategies is lost on extraction with solvents. This precise approach is eminently suited to analysis of epilithic (surface) and endolithic (within rocks) communities in Antarctic desert habitats, which are putative analogues of early Mars. Raman spectra for key biomolecules (e.g. the UV screen parietin and the antioxidant β-carotene in epilithic lichens) enable not only the detection of organics in light-stratified habitats, but also the characterization of unknown pigments. Typical biomarkers of astrobiological relevance in our Raman spectral database include scytonemin (a UV screen), chlorophyll (primary photosynthetic pigment), phycocyanin (accessory pigment for shade adaptation) and a hopanoid extracted from 2·5 Gya microbial stromatolite from Australia. This compound dates from the same time period when a wetter Mars could have had a potentially flourishing surface microbial community of its own. Analyses with a laboratory Raman instrument have been extended to a novel miniature Raman spectrometer, operating at the same optimal excitation wavelength (1064 nm) via an In-Ga-As detector. After evaluation in Antarctica, this instrument will be space-qualified for a proposed Mars rover mission to detect biomolecules in the near-surface sediment profile of palaeolakes, using experience with Antarctic biomarkers to interpret alien spectra of fundamental components, without the need for prior knowledge of the identity of the target compounds.

Cryptoendolithic microbial communities living within Antarctic rocks are an example of survival in an extremely cold and dry environment. The extinction of these micro-organisms formerly colonizing sandstone in the Mount Fleming area (Ross Desert), was probably provoked by the hostile environment. This is considered to be a good terrestrial analogue of the first stage of the disappearance of possible life on early Mars. To date, only macroscopically observed indirect biomarkers of the past activity of cryptoendoliths in Antarctic rocks have been described. The present paper confirms, for the first time, the existence of cryptoendolith microbial fossils within these sandstone rocks. The novel in situ application of scanning electron microscopy with backscattered electron imaging and simultaneous use of X-ray energy dispersive spectroscopy allowed the clear detection of microfossils left behind by Antarctic endoliths. Careful interpretation of the morphological features of cells, such as preserved cell walls in algae, fungi and bacteria, cytoplasm elements such as chloroplast membranes in algae and organic matter traces, mineral associations, and the spatial context of these structures all point to their identification as cryptoendolith microfossils. This type of investigation will prompt the development of research strategies aimed at locating and identifying the signs that Martian microbiota, probably only bacteria if they existed, may have been left for us to see.

Many of the recently discovered extrasolar giant planets move around their stars on highly eccentric orbits, and some with e [ges ] 0·7. Systems with planets within or near the habitable zone (HZ) will possibly harbour life on terrestrial-type moons if the seasonal temperature extremes resulting from the large orbital eccentricities of the planets are not too severe. Here we use a three-dimensional general-circulation climate model and a one-dimensional energy-balance model to examine the climates of either bound or isolated earths on extremely elliptical orbits near the HZ. While such worlds are susceptible to large variations in surface temperature, long-term climate stability depends primarily on the average stellar flux received over an entire orbit, not the length of the time spent within the HZ.

For a quarter of a century we have been engaged in a systematic examination of high-quality photographic (optical) sky surveys in the search for new celestial bodies of various kinds. It took about 5000 hours to cover the whole northern celestial hemisphere and half of the southern one. In total, about 12000 new objects were discovered. From the very beginning of our programme we also searched for objects (or groupings of them) of rather peculiar morphology. The motivation was to detect objects revealing exceptional physical processes, on the one hand, but also to discover constructions possibly created by advanced extraterrestrial civilizations (ETCs), on the other hand. A number of very peculiar objects were indeed found (these were mostly studied in detail later), but none of these appeared likely to be the product of alien masterminds. We may conclude that at least within about 10000–20000 light-years around the Solar system no highly advanced ETCs intend to reveal themselves through such objects.