Time-scales of polycyclic aromatic hydrocarbon and dust continuum emission from gas clouds compared to molecular gas cloud lifetimes in PHANGS-JWST galaxies

TL;DR

This study measures the lifetimes of PAH and dust continuum emissions in gas clouds of nearby galaxies using JWST data, revealing their close correlation with molecular cloud lifetimes and the influence of galaxy environment on mid-IR emission.

Contribution

It provides the first detailed comparison of PAH and dust continuum emission timescales with molecular cloud lifetimes across multiple galaxies using JWST observations.

Findings

Mid-IR emission time-scale ranges from 10 to 30 Myr.

Mid-IR persists for 3-7 Myr after star formation detection.

Mid-IR time-scale closely matches molecular cloud lifetime.

Abstract

Recent JWST mid-infrared (mid-IR) images, tracing polycyclic aromatic hydrocarbons (PAHs) and dust continuum emission, provide detailed views of the interstellar medium (ISM) in nearby galaxies. Leveraging PHANGS-JWST Cycle 1 and PHANGS-MUSE data, we measure the PAH and dust continuum emission lifetimes of gas clouds across 17 nearby star-forming galaxies by analyzing the relative spatial distributions of mid-IR (7.7-11.3$\mu$m) and H$\alpha$ emission at various scales. We find that the mid-IR emitting time-scale of gas clouds in galaxy disks (excluding centers) ranges from 10 to 30Myr. After star formation is detected in H$\alpha$, mid-IR emission persists for 3-7Myr during the stellar feedback phase, covering 70-80% of the H$\alpha$ emission. This significant overlap is due to intense radiation from star-forming regions, illuminating the surrounding PAHs and dust grains. In most galaxies, the mid-IR time-scale closely matches the molecular cloud lifetime measured with CO. Although mid-IR emission is complex as influenced by ISM distribution, radiation, and abundances of dust and PAHs, the similarity between the two time-scales suggests that once gas clouds form with compact mid-IR emission, they quickly provide sufficient shielding for stable CO formation. This is likely due to our focus on molecular gas-rich regions of galaxies with near-solar metallicity. Finally, we find that the mid-IR emitting time-scale is longer in galaxies with well-defined HII regions and less structured backgrounds, allowing photons to more efficiently heat the ambient ISM surrounding the HII regions, rather than contributing to diffuse emission. This suggests that the shape of the ISM also influences mid-IR emission.