| Issue |
EPJ Web of Conferences
Volume 265, 2022
Multi-line Diagnostics of the Interstellar Medium
|
|
|---|---|---|
| Article Number | 00011 | |
| Number of page(s) | 4 | |
| DOI | https://doi.org/10.1051/epjconf/202226500011 | |
| Published online | 07 September 2022 | |
https://doi.org/10.1051/epjconf/202226500011
CO-dark gas: What fuels the star formation in low metallicity dwarf galaxies?
AIM, CEA Département d’Astrophysique, CNRS, Université Paris-Saclay, Université Paris Diderot, Sorbonne Paris Cité, 91191 Gif-sur-Yvette, France
* e-mail: suzanne.madden@cea.fr
Published online: 7 September 2022
While star-forming dwarf galaxies have little molecular gas traced by CO, their extreme observed [Cii]/CO(1-0) and [Oiii]/[Cii] ratios set them apart from metal-rich star-forming galaxies. The decreased dust abundance, along with their star formation activity, encourages the photodissociation of CO and the presence of relatively prominent C+ envelopes which can harbor a significant self-shielded H2 reservoir, with CO being an inaccurate proxy for the total H2 gas mass. Modeling the Dwarf Galaxy Survey allows us to quantify the mass of the CO-dark H2 gas and derive a [Cii]-to-H2 gas mass conversion factor as well as a new CO-to-H2 conversion factor as a function of metallicity.
© The Authors, Published by EDP Sciences, 2022
This is an Open Access article distributed under the terms of the Creative Commons Attribution License 4.0 (http://creativecommons.org/licenses/by/4.0/).
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.