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Galaxies As “Cosmic Cauldrons”

23.05.2019

Young stars heat molecular clouds and drive hot interstellar gas bubbles throughout galaxies

Star formation within interstellar clouds of gas and dust, so-called molecular clouds, proceeds very rapidly yet highly “inefficiently”. Most of the gas is dispersed by stellar radiation, revealing galaxies to be highly dynamic systems, like “cosmic cauldrons”, consisting of components that constantly change their appearance.


The video demonstrates that molecular clouds (top right) and young stars (top left) are anti-correlated in the nearby NGC 300 galaxy. As the video plays, the spatial resolution increases and the ratio between molecular clouds and young stars (bottom left) changes from white (strong correlation) on large scales to bright red and blue (strong anti-correlation) on small scales. The graph in the bottom-right panel quantifies this behaviour. Source: Diederik Kruijssen & Nature

Based on new observations of the NGC 300 spiral galaxy, a team of scientists led by astrophysicist Dr Diederik Kruijssen from Heidelberg University has now managed for the first time to reconstruct the time-evolution of molecular clouds and the star formation process within them.

Their analysis shows that these clouds are short-lived structures undergoing rapid lifecycles, driven by the intense radiation from the new-born stars. The findings were published in “Nature”.

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).

Video caption:
The video demonstrates that molecular clouds (top right) and young stars (top left) are anti-correlated in the nearby NGC 300 galaxy. As the video plays, the spatial resolution increases and the ratio between molecular clouds and young stars (bottom left) changes from white (strong correlation) on large scales to bright red and blue (strong anti-correlation) on small scales. The graph in the bottom-right panel quantifies this behaviour. Source: Diederik Kruijssen & Nature

Contact:
Dr Guido Thimm
Centre for Astronomy of Heidelberg University (ZAH)
Phone +49 6221 54-1805
thimm@ari.uni-heidelberg.de

Heidelberg University
Communications and Marketing
Press Office, phone +49 6221 54-2311
presse@rektorat.uni-heidelberg.de

Wissenschaftliche Ansprechpartner:

Dr Diederik Kruijssen
Zentrum für Astronomie der Universität Heidelberg (ZAH)
Phone +49 6221 54-1877
kruijssen@uni-heidelberg.de

Originalpublikation:

Original publication:
J.M.D. Kruijssen, A. Schruba, M. Chevance, S.N. Longmore, A.P.S. Hygate, D.T. Haydon, A.F. McLeod, J.J. Dalcanton, L.J. Tacconi & E.F. van Dishoeck: Fast and inefficient star formation due to short-lived molecular clouds and rapid feedback. Nature, doi: 10.1038/s41586-019-1194-3

Weitere Informationen:

http://wwwstaff.ari.uni-heidelberg.de/kruijssen/News/News.html
http://wwwstaff.ari.uni-heidelberg.de/MUSTANG/Home.html
https://youtu.be/ZbNCXDLrFRo

Marietta Fuhrmann-Koch | idw - Informationsdienst Wissenschaft

Further reports about: ALMA Cosmic ESO Galaxies massive stars molecular clouds spiral galaxy star formation young stars

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