Galaxies as 'cosmic cauldrons'

The observed intensity of star formation in the NGC 300 spiral galaxy can be explained in two ways. Molecular clouds may be very long-lived and eventually convert all of their mass into stars. In this case, the positions of young stars should generally match those of the molecular clouds from which they formed. Alternatively, stars may form very rapidly within molecular clouds and disperse the gas with their intense radiation, causing only a small fraction of the gas to be converted into stars. In this case, young stars and molecular clouds should generally reside in different locations.

To decide which of these models of the molecular cloud lifecycle is correct, Dr Kruijssen and his team combined two different sets of observations of the NGC 300 galaxy, which is about six million light years away from the Milky Way. The first observation is a map of light emitted by carbon monoxide which shows where molecular clouds reside. The second is a map of hot, ionised hydrogen which marks the positions of massive, newly formed stars. These maps were obtained using the Atacama Large Millimeter Array (ALMA) of the European Southern Observatory (ESO) and the 2.2-meter telescope of the Max Planck Society and ESO. The ALMA observations were carried out by Dr Andreas Schruba, scientist at the Max Planck Institute for Extraterrestrial Physics in Garching and one of the co-authors of the study. The scientists analysed the data using a new statistical method which determines how molecular gas and star formation in galaxies are related on different spatial scales. For the first time, this method enables the positions of molecular clouds and young stars to be precisely quantified relative to one another.

According to the scientists, the results left no doubt: the positions of molecular clouds and young, massive stars rarely coincide. This effect becomes stronger on smaller scales. The scientists conclude that stars form very rapidly, such that gas and young stars represent distinct, subsequent phases in the lifecycle of molecular clouds. "Our findings demonstrate that star formation proceeds very rapidly and highly inefficiently," explains Dr Kruijssen, research group leader at the Institute for Astronomical Computing. "Molecular clouds in NGC 300 live for about ten million years and take only about 1.5 million years to be destroyed, well before the most massive stars have reached the end of their lives and explode as supernovae." Dr Mélanie Chevance, a researcher in his team and also co-author of the paper, adds: "The intense radiation from young stars disperses their parent molecular cloud by heating it and dispersing it in the form of hot interstellar gas bubbles. This way, only two to three percent of the mass in molecular clouds is actually converted into stars."

The team of researchers now wants to apply their new statistical method to observations of very distant galaxies to infer how star formation in molecular clouds proceeded across the history of the Universe. "We will now proceed to investigate the relation between molecular clouds and young stars in galaxies throughout the cosmos. In the near future, this will allow us to understand galaxies as collections of components that undergo star formation-driven lifecycles and together shape the appearance of their host galaxies," explains Dr Kruijssen.

The research was conducted in collaboration with researchers from the United Kingdom, the United States, and the Netherlands. The work was funded by the German Research Foundation (DFG) and the European Research Council (ERC).