Linking Characteristics of the Polycyclic Aromatic Hydrocarbon Population with Galaxy Properties: A Quantitative Approach Using the NASA Ames PAH IR Spectroscopic Database

• Published in: The Astrophysical journal 2022-05, Vol.931 (1), p.38
• Main Authors: Maragkoudakis, A., Boersma, C., Temi, P., Bregman, J. D., Allamandola, L. J.
• Format: Article
• Language: English
• Subjects: Aromatic hydrocarbons; Astronomical models; Astrophysics; Atomic properties; Correlation; Galaxies; Galaxy distribution; Infrared sources; Interstellar line emission; Interstellar medium; Interstellar molecules; Ionization; Polycyclic aromatic hydrocarbons; Size distribution; Spectra; Spectral energy distribution; Star & galaxy formation; Star formation; Star formation rate; Stars & galaxies
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ac666f

Utilizing the data and tools provided through the NASA Ames PAH IR Spectroscopic Database (PAHdb), we study the PAH component of over 900 Spitzer-IRS galaxy spectra. Employing a database-fitting approach, the average PAH size, the PAH size distribution, and PAH ionization fraction are deduced. In turn, we examine their connection with the properties of the host galaxy. We found that PAH population within galaxies consists of middle-sized PAHs with an average number of carbon atoms of N C ¯ = 55, and a charge state distribution of ∼40% ionized—60% neutral. We describe a correlation between the 6.2/11.2 μ m PAH ratio with the ionization parameter ( γ ≡ ( G 0 / n e ) ( T gas / 1 K ) 0.5 ), a moderate correlation between the 8.6/11.2 μ m PAH ratio and specific star formation rate, and a weak anticorrelation between γ and M * . From the PAHdb decomposition, we provide estimates for the 3.3 μ m PAH band, not covered by Spitzer observations, and establish a correlation between the 3.3/11.2 μ m PAH ratio with N C . We further deliver a library of mid-IR PAH template spectra parameterized on PAH size and ionization fraction, which can be used in galaxy spectral energy distribution fitting codes for the modeling of the mid-IR PAH emission component in galaxies.