Unravelling the Mysteries of Star Creation in the Whirlpool Galaxy

Unravelling the Mysteries of Star Creation: The Max Planck Institute for Astronomy (MPIA) recently spearheaded an international research team that mapped certain dense and cold gas regions, revealing that the birthplace of stars is not limited to just the Milky Way. Utilizing NOEMA observatory, these observations offer insights into a variety of conditions that promote star formation.

The data obtained from this study has made significant strides in measurement types and allowed researchers to observe early star formation in the history of the Milky Way for the first time. This breakthrough discovery has enabled better models of star formation and has helped explain galaxy evolution throughout the history of the universe.

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The process of star formation may seem paradoxical, as it begins in the coldest regions of the universe – dense clouds of gas and dust that traverse entire galaxies. Observing the early stages of star formation, where stars are born, requires identifying these areas first.

In Astronomy & Astrophysics, researchers measure the radiation emitted by unique molecules that are abundant in these extremely cold and dense zones to better understand this process. By studying these clouds, scientists can gain insights into the mechanisms that govern the formation of stars and planets.

Unravelling the Mysteries of Star Creation Details

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Molecules As Chemical Probes

Astronomers often use hydrogen cyanide (HCN) and diazenylium (N2H+) molecules as chemical probes to study star formation in the Milky Way. These molecules collide with hydrogen molecules, which are difficult to detect themselves, causing other molecules to rotate. As these rotating molecules slow down, they emit radiation at specific wavelengths, typically around 3mm for HCN and N2H+. By analyzing this radiation, astronomers can gather information about the conditions and processes involved in star formation. This technique has proven to be a valuable tool in understanding the origins of stars and galaxies in the universe.

Star Creation in the Whirlpool Galaxy

The measurements are part of the SWAN (Surveying the Whirlpool at Arcsecond with NOEMA) observational program, co-led by Schinnerer and Frank Bigiel from the University of Bonn. The group aims to use the Northern Extended Millimetre Array (NOEMA) to examine the distribution of various molecules within the internal 20,000 light-years of the Whirlpool Galaxy (Messier 51), including hydrogen cyanide and diazenylium. Additionally, the dataset is supplemented by around 70 hours from other observation campaigns using a 30-meter single-dish telescope in southern Spain, in addition to the 214 hours from this program.

Jerome Pety from the Institute de Radioastronomie Millimétrique (IRAM), the group operating the telescopes, mentioned that processing and refining the data from radio interferometers is significantly more complex than telescope images, and it took about another year to complete. Interferometric telescopes such as NOEMA comprise multiple individual antennas, collectively achieving detail resolution comparable to a telescope with a primary reflector diameter equal to the spacing between the individual telescopes.

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Gas properties depend on the environment

The study authors were able to identify unique patterns of individual gas clouds in various regions, including the center and the spiral arms.

• The radiation depth of hydrogen cyanide and diazenylium fluctuates as it moves through the spiral arms, providing consistent effects in measuring gas densities, but astronomers have observed a significant difference in the galactic center of M51.
• In this location, the brightness of HCN emission will increase significantly more than diazenylium.
•  It appears that there is a mechanism present that induces hydrogen cyanide to produce additional light, a phenomenon not yet found in diazenylium.
• “We believe that the active core of the Whirlpool Galaxy is responsible for this,” Schinnerer explains. This is where the gas rotates around the black hole in the form of a spinning disk, surrounding the central massive black hole.
• The fuel accelerates to high speeds as it descends, experiencing frictional heating that causes it to emit intense radiation and contribute to the release of HCN molecules.
• Therefore, in the nearby region of the Whirlpool Galaxy, diazenylium appears to be a more dependable density indicator than hydrogen cyanide. This is significant because hydrogen cyanide is commonly utilized for determining gas mass, which will influence the formation of massive stars in the early universe.
• The findings suggest that there may be more gas available for star formation than previously thought, considering the brightness of hydrogen cyanide.

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A Worthwhile Challenge

Therefore, in the important region of the Whirlpool Galaxy, diazenylium appears to be a more dependable density probe than hydrogen cyanide. However, it emits an average of five times less light for the same fuel density, which significantly increases the observation time required to achieve the necessary additional sensitivity. Scientists are eager to explore the early stages in galaxies beyond the Milky Way, even though it is more difficult to determine the exact structure and location of spiral arms and clouds compared to the molecular clouds and star-forming regions that are closer in the Milky Way.

Stuber points out that while we can learn a lot from the distinctive statement software with the Whirlpool Galaxy, it is essentially a pilot project. The Whirlpool Galaxy emits intense light in response to these chemical probes. Telescopes and devices for other galaxies must be much more advanced. The rest of the extensive collection is currently in the process of planning with high expectations. If everything progresses as expected, it will only be accessible in approximately ten years. In the meantime, the Whirlpool Galaxy provides a valuable opportunity to study star formation on a large scale.

List of MPIA researchers involved

The team of researchers in this study includes Jérôme Pety from IRAM and Observatoire de Paris/PSL, Frank Bigiel from the University of Bonn, Antonio Usero from Observatorio Astronómica Nacional/IGN, Madrid, Spain, Ivana Bešlić from PSL, Miguel Querejeta from OAN, J. María Jiménez-Donaire from OAN and Observatorio de Yebes/IGN, Guadalajara, Spain), Adam Leroy from Ohio State University, Columbus, Jakob den Brok from the Center for Astrophysics at Harvard & Smithsonian in Cambridge, Lukas Neumann and Cosima Eibensteiner from UB.

Yu-Hsuan Teng from the University of California San Diego in La Jolla, Ashley Barnes from European Southern Observatory in Garching Germany (ESO), Mélanie Chevance from Centre for Astronomy at Heidelberg University in Germany (ZAH) and Cosmic Origins of Life Research DAO), Dario Colombo from UB, Daniel A. Dale from the University of Wyoming in Laramie USA), Simon C.O. Glover from ZAH), Daizhong Liu from Max Planck Institute for Extraterrestrial Physics in Garching Germany and Hsi-An Pan from Tamkang University in Taiwan.

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