Over the last century, scientists have used theory and observations to piece together the Big Bang model. This model gives a physical explanation of how our cosmos came to be and allows us to trace its history.
The Universe emerged from a state of extremely high temperature and density about 13.7 billion years ago. Initially, the Universe consisted of a uniform bath of fundamental particles, like quarks, electrons, neutrinos, and photons (the particles of light). Quarks then teamed up in trios, forming protons or neutrons – the constituents of atomic nuclei as we know them today. This all happened within the first second after the beginning: the so-called Big Bang.
About three minutes after, protons and neutrons combined to form the nuclei of hydrogen and helium atoms. At that time, collisions between electrons and photons were so frequent that light could not go far before hitting a particle again and being either absorbed or deviated from its path. Because of these frequent interactions photons could not travel freely, and the Universe was opaque.
As it expanded, the Universe grew cooler and sparser. When the temperature dropped to about 3000°C, electrons and protons combined to form (mainly) hydrogen atoms. This is the first moment in the history of the cosmos when matter was in an electrically neutral state. Particle collisions became so sporadic that photons started to travel freely across space.
This epoch is named ‘recombination’ and marks the time when the Universe became transparent to light. A snapshot of how the Universe looked back then reaches us today in the form of diffuse light in the microwave range: the cosmic microwave background. Its distribution was measured in detail by ESA’s Planck mission.
After a few hundred million years, some gas agglomerates had grown large and dense enough to ignite nuclear fusion and give birth to the first stars. At that point, galaxies also started to form and assemble on large scales.
At that time, however, matter had already been diffused over large distances by the continued expansion of space. The interactions of photons and electrons were much less frequent than before electron-proton recombination. Thus, the Universe remained overall transparent to light, as it is today.
While reionisation was taking place, large clumps of neutral hydrogen were still present in intergalactic space – like clouds scattered in a clear blue sky. Their presence absorbed the far-UV light coming to us from the very early galaxies that were forming during this era.
That's why, when a galaxy is very far away, and very young, there is a prominent bump in the light spectrum of that galaxy. The bump appears in near-infrared and corresponds to the wavelength beyond which the far UV-light is absorbed by the hydrogen clouds. The huge distance travelled by that galaxy’s light through the expanding Universe causes its wavelength to stretch and become longer (cosmological redshift), so the UV bump appears in near-infrared light.
Scientists identify this sharp rise at near-infrared wavelengths and use it to accurately determine a galaxy’s redshift, and from this its distance in light-travel time and the Universe’s age at the time the light left the galaxy.
During this era, the clouds of hydrogen gas were gradually cleared away by powerful UV-light. Astronomers have spent decades trying to identify sources of UV-light strong enough to dissolve this hydrogen ‘fog’ that blanketed the early Universe and to cause the reionisation of the Universe.
Using the unprecedented capabilities of the James Webb Space Telescope, an international team of scientists has obtained the first spectroscopic observations of the faintest, smallest galaxies during the first billion years of the Universe.
The team found that these faint galaxies are vigorous producers of ultraviolet light, at levels that are four times larger than what was previously assumed. Therefore, most of the photons that reionised the Universe likely came from these dwarf galaxies.
After reionisation, the pace with which stars form and galaxies grow entered a higher gear, reaching its peak at around two to three billion years after the Big Bang. Over this relatively short period, galaxies formed about half of their current stellar mass. Scientists refer to this era as cosmic noon.
Despite the great success of the Big Bang model in explaining many aspects of our cosmos, fundamental questions remain unanswered. One of the most profound mysteries is the composition of the Universe.
Based on the way galaxies rotate and orbit one another, and how the Universe is expanding, astronomers believe that two unseen components dominate the content of our cosmos: dark matter and dark energy. Yet, to date, we have not been able to detect either of them directly, only inferring their presence from the effects they have on the Universe at large.
ESA's Euclid mission will chart the large-scale structure of the Universe across space and time by observing billions of galaxies. It will help us shed light on the nature of dark energy and dark matter.
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