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Modeling the molecular gas content and CO-to-H2 conversion factors in low-metallicity star-forming dwarf galaxies by Ramambason, L.; Lebouteiller, V.; Madden, S. C.; Galliano, F.; Richardson, C. T.; Saintonge, A.; De Looze, I.; Chevance, M.; Abel, N. P.; Hernandez, S.; Braine, J. is a scholarly article available to read on EtoBox.

What is Modeling the molecular gas content and CO-to-H2 conversion factors in low-metallicity star-forming dwarf galaxies about?

Low-metallicity dwarf galaxies often show no or little CO emission, despite the intense star formation observed in local samples. Both simulations and resolved observations indicate that molecular gas in low-metallicity galaxies may reside in small dense clumps, surrounded by a substantial amount of more diffuse gas, not traced by CO. Constraining the relative importance of CO-bright versus CO-dark H2 star-forming reservoirs is crucial to understand how star formation proceeds at low metallicity. We put to the test classically used single component radiative transfer models and compare their results to those obtained assuming an increasingly complex structure of the interstellar gas, mimicking an inhomogeneous distribution of clouds with various physical properties. We compute representative models of the interstellar medium as combinations of several gas components, each with a specific set of physical parameters. We introduce physically-motivated models assuming power-law distributions for the density, ionization parameter, and the depth of molecular clouds. We confirm the presence of a predominantly CO-dark molecular reservoir in low-metallicity galaxies. The predicted total H2

Author

Ramambason, L.; Lebouteiller, V.; Madden, S. C.; Galliano, F.; Richardson, C. T.; Saintonge, A.; De Looze, I.; Chevance, M.; Abel, N. P.; Hernandez, S.; Braine, J.

Published

2023

Language

EN