Polycyclic Aromatic Hydrocarbon and CO(2–1) Emission at 50–150 pc Scales in 70 Nearby Galaxies
Ryan Chown, Adam K. Leroy, Karin Sandström, Jérémy Chastenet, Jessica Sutter, Eric W. Koch, Hannah Koziol, Lukas Neumann, Jiayi Sun, Thomas G. Williams, Dalya Baron, Gagandeep S. Anand, Ashley T. Barnes, Zein Bazzi, Francesco Belfiore, Frank Bigiel, Alberto D. Bolatto, M. Boquien, Yixian Cao, Mélanie Chevance, Dario Colombo, Daniel A. Dale, Jakob S. den Brok, Oleg V. Egorov, Cosima Eibensteiner, Éric Emsellem, Hamid Hassani, Jonathan D. Henshaw, Hao He, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, Kirsten L. Larson, Janice Lee, Sharon E. Meidt, E. J. Murphy, Elias K. Oakes, Eve C. Ostriker, Hsi-An Pan, Debosmita Pathak, Erik Rosolowsky, Sumit K. Sarbadhicary, Eva Schinnerer, Yu-Hsuan Teng, David A. Thilker, Tony D. Weinbeck, Elizabeth J. Watkins
Abstract
Abstract Combining Atacama Large Millimeter/submillimeter Array CO(2–1) mapping and JWST near- and mid-infrared imaging, we characterize the relationship between CO(2–1) and polycyclic aromatic hydrocarbon (PAH) emission at ≈100 pc resolution in 70 nearby star-forming galaxies. Leveraging a new Cycle 2 JWST Treasury program targeting nearby galaxies, we expand the sample size by more than an order of magnitude compared to previous ≈100 pc resolution CO–PAH comparisons. In regions of galaxies where most of the gas is likely to be molecular, we find strong correlations between CO(2–1) and 3.3 μ m, 7.7 μ m, and 11.3 μ m PAH emission, estimated from JWST’s F335M, F770W, and F1130W filters. We derive power-law relations between CO(2–1) and PAH emission, with indices in the range 0.8–1.3, implying relatively weak variations in the observed CO-to-PAH ratios across our sample. We find that CO-to-PAH ratios and scaling relationships near H ii regions are similar to those in diffuse sight lines. The main difference between the two types of regions is that sight lines near H ii regions show higher intensities in all tracers. Galaxy centers show higher overall intensities and enhanced CO-to-PAH ratios compared to galaxy disks. Individual galaxies show 0.19 dex scatter in the normalization of CO at fixed I PAH , and this normalization anticorrelates with specific star formation rate and correlates with stellar mass. We provide a prescription that accounts for galaxy-to-galaxy variations, representing our best current empirical predictor to estimate CO(2–1) intensity from PAH emission, allowing one to take advantage of JWST’s excellent sensitivity and resolution to trace cold gas.