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Linking Stellar Populations to H II Regions across Nearby Galaxies. II. Infrared Reprocessed and UV Direct Radiation Pressure in H II Regions

  • Authors: Debosmita Pathak, Adam K. Leroy, Todd A. Thompson, Laura A. Lopez, Ashley. T. Barnes, Daniel A. Dale, Ian Blackstone, Simon C. O. Glover, Shyam H. Menon, Jessica Sutter, Thomas G. Williams, Dalya Baron, Francesco Belfiore, Frank Bigiel, Alberto D. Bolatto, Médéric Boquien, Rupali Chandar, Mélanie Chevance, Ryan Chown, Kathryn Grasha, Brent Groves, Ralf S. Klessen, Kathryn Kreckel, Jing Li, J. Eduardo Méndez-Delgado, Erik Rosolowsky, Karin Sandstrom, Sumit K. Sarbadhicary, Jiayi Sun, Leonardo Úbeda

Debosmita Pathak et al 2025 The Astrophysical Journal 982 .

  • Provider: AAS Journals

Caption: Figure 10.

Here we compare the median﹩{P}_{{\rm{Reprocessed}}}^{{\rm{Rad}}}﹩ (maroon hexagons), ﹩{P}_{{\rm{Direct}}}^{{\rm{Rad}}}﹩ (blue diamonds), and ﹩{P}_{{\rm{Ion}}}^{{\rm{Rad}}}﹩ (green squares; top row), and ﹩{f}_{{\rm{trap}}}={P}_{{\rm{Reprocessed}}}^{{\rm{Rad}}}/{P}_{{\rm{Direct}}}^{{\rm{Rad}}}﹩ (maroon hexagons) and ﹩{P}_{{\rm{Ion}}}^{{\rm{Rad}}}/{P}_{{\rm{Direct}}}^{{\rm{Rad}}}﹩ (green squares; bottom row) with the average star formation rate (SFR), total stellar mass (M*), and specific star formation rate (sSFR) for all 19 galaxies. Each marker shows the median for each galaxy, and the error bars denote the 16th–84th percentile range in values. The Spearman rank coefficient ρ for the correlation between each median and galaxy property is noted in the top left of each panel.

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