Biosignatures are observable indicators, such as atmospheric gases or molecular patterns, that suggest the presence of life.A biosignature is any detectable phenomenon (gas, mineral, color) that can only be explained by biological activity. The most compelling biosignatures are gases in chemical disequilibrium; for instance, the simultaneous presence of oxygen (O₂) and methane (CH₄). It is crucial to rule out non-biological sources (volcanoes, photochemical reactions) that can produce false signs of life.
The first ideas about possible signs of life on Mars were voiced back in the 19th century (Schiaparelli's canals). A systematic approach emerged in the 1960s, when James Lovelock analyzed Earth's atmosphere as a product of the biosphere. Carl Sagan and others developed the concept of thermodynamic disequilibrium. With the discovery of exoplanets in the 1990s, the search for biosignatures became a central goal of astrobiology.
During a transit of an exoplanet in front of its star, part of the starlight is filtered by its atmosphere, and absorption lines of molecules appear in the spectrum. Each molecule has a unique spectral 'fingerprint'. By measuring the depth of lines at different wavelengths, the gas composition is determined. A biosignature is considered reliable if a combination of gases is detected that cannot be maintained without a biological source, and all known abiotic pathways under the given conditions (temperature, radiation, geology) are ruled out. Principles of spectroscopy and photochemical modeling are used.
The search for biosignatures in exoplanet atmospheres is the main method for finding extraterrestrial life, driving the development of cutting-edge telescopes.
Earth, with its oxygen-methane atmosphere, would have shone like a beacon for hypothetical alien astronomers for two billion years already.



























