When the first galaxies started to form a few hundred million years after the Big Bang, the Universe was full of a fog of hydrogen gas. But as more and more brilliant sources — both stars and quasars powered by huge black holes — started to shine they cleared away the mist and made the Universe transparent to ultraviolet light. Astronomers call this the epoch of reionisation, but little is known about these first galaxies, and up to now they have just been seen as very faint blobs. But now new observations using the Atacama Large Millimetre/submillimetre Array (ALMA) are starting to change this.

A team of astronomers led by Roberto Maiolino from the University’s Cavendish Laboratory and Kavli Institute for Cosmology trained ALMA on galaxies that were known to be seen only about 800 million years after the Big Bang. The astronomers were not looking for the light from stars, but instead for the faint glow of ionised carbon coming from the clouds of gas from which the stars were forming. They wanted to study the interaction between a young generation of stars and the cold clumps that were assembling into these first galaxies.

They were also not looking for the extremely brilliant rare objects — such as quasars and galaxies with very high rates of star formation — that had been seen up to now. Instead they concentrated on rather less dramatic, but much more common, galaxies that reionised the Universe and went on to turn into the bulk of the galaxies that we see around us now.

From one of the galaxies — given the label BDF 3299 — ALMA could pick up a faint but clear signal from the glowing carbon. However, this glow wasn’t coming from the centre of the galaxy, but rather from one side.

“These observations enable an unprecedented understanding of the assembly process of the first galaxies formed in the Universe – for the first time we can observe and disentangle the different components contributing to the earliest phases of galaxy formation,” said Maiolino. “These observations have enabled us to test with unprecedented detail theories of galaxy formation in the early Universe.”

The astronomers think that the off-centre location of the glow is because the central clouds are being disrupted by the harsh environment created by the newly formed stars — both their intense radiation and the effects of supernova explosions — while the carbon glow is tracing fresh cold gas that is being accreted from the intergalactic medium.

By combining the new ALMA observations with computer simulations, it has been possible to understand in detail key processes occurring within the first galaxies. The effects of the radiation from stars, the survival of molecular clouds, the escape of ionising radiation and the complex structure of the interstellar medium can now be calculated and compared with observation. BDF 3299 is likely to be a typical example of the galaxies responsible for reionisation.

“We have been trying to understand the interstellar medium and the formation of the reionisation sources for many years. Finally to be able to test predictions and hypotheses on real data from ALMA is an exciting moment and opens up a new set of questions. This type of observation will clarify many of the thorny problems we have with the formation of the first stars and galaxies in the Universe,” said co-author Andrea Ferrara, from the Scuola Normale Superiore in Pisa, Italy.

“This study would have simply been impossible without ALMA, as no other instrument could reach the sensitivity and spatial resolution required,” said Maiolino. “Although this is one of the deepest ALMA observations so far it is still far from achieving its ultimate capabilities. In future ALMA will image the fine structure of primordial galaxies and trace in detail the build-up of the very first galaxies.”

The results are reported in the journal Monthly Notices of the Royal Astronomical Society.

Reference:

R. Maiolino et al., “The assembly of “normal” galaxies at z∼7 probed by ALMA,” Monthly Notices of the Royal Astronomical Society (2015).

Adapted from an ESO press release.