Tiny dust molecules known as polycyclic aromatic hydrocarbons (PAHs) are among the most widespread organic molecules in the universe and important astronomical tools. For instance, they are considered to be fundamental building blocks of prebiotic compounds, which may have played a key role in the origin of life. PAH molecules produce extremely bright emission bands in the infrared region when they are illuminated by stars, enabling astronomers to not only trace star-formation activity, but also to use them as sensitive barometers of the local physical conditions.
This new analysis, led by Dr Ismael García-Bernete from Oxford University’s Department of Physics, used JWST’s cutting-edge instruments to characterise, for the first time, the PAH properties in the nuclear region of three luminous active galaxies. The study was based on spectroscopic data from the James Webb Space Telescope’s MIRI which specifically measures light in the 5-28 micron wavelength range. The researchers then compared the observations with theoretical predictions for these molecules.
Surprisingly, the results overturned those of previous studies that had predicted that PAH molecules would be destroyed in the vicinity of the black hole at the centre of an active galaxy. Instead, the analysis revealed that PAH molecules can actually survive in this region, even where very energetic photons could potentially rip them apart. A potential reason could be that the molecules are protected by large amounts of molecular gas in the nuclear region.
Dr Ismael García-Bernete said: ‘The JWST MIRI provides us with a fantastic opportunity to observe galaxies in a way that just hasn’t been possible up until now. We were excited to find that these organic molecules can actually survive in extremely harsh conditions.’
However, even where PAH molecules survived, the results showed that the supermassive black holes at the heart of galaxies had a significant impact on their properties. In particular, the proportion of larger and neutral molecules became greater, indicating that more fragile small and charged PAH molecules may have been destroyed. This brings severe limitations to using these PAH molecules to probe how rapidly an active galaxy makes new stars.
‘This research is of great interest to the wider astronomy community, particularly those focused on the formation of planets and stars in the most distant and faint galaxies’ said Dr García-Bernete. ‘It is incredible to think that we can observe PAH molecules in the nuclear region of a galaxy and the next step is to analyse a larger sample of active galaxies with different properties. This will enable us to better understand how PAH molecules survive and which are their specific properties in the nuclear region. Such knowledge is key to using PAHs as an accurate tool for characterising the amount of star formation in galaxies, and thus, how galaxies evolve over time.'
The study is published in Astronomy and Astrophysics: https://www.aanda.org/articles/aa/full_html/2022/10/aa44806-22/aa44806-22.html
The PAH models were developed by Professor Dimitra Rigopoulou’s research group, in a joint effort with the Physical Chemistry group at the University of Oxford. The work was funded by the University of Oxford's Fell Fund.
For media inquiries and interviews, contact: Elizabeth Indaco, Head of Communications, Department of Physics, University of Oxford: email@example.com
Astronomy and Astrophysics
Method of Research
Subject of Research
A high angular resolution view of the PAH emission in Seyfert galaxies using JWST/MRS data