Using CO to Measure Molecular Masses

Abstract

With an increased appreciation for the role of gas in galaxy evolution, there is renewed interest in measuring gas masses for galaxies. I review some of the basic concepts in using CO to determine molecular masses, and discuss some of the recent work.

Proceedings for invited presentation to the 6th Zermatt Symposium, "Conditions and Impact of Star Formation: from Lab to Space", Zermatt Switzerland September 7-11, 2015

References in corpus (6)

• The Spitzer Survey of the Small Magellanic Cloud: FIR Emission and Cold Gas in the SMC
• ALMA Reveals the Molecular Medium Fueling the Nearest Nuclear Starburst
• [CII] 158$\mu$m Emission and Metallicity in PDRs
• The Structure of a Low-Metallicity Giant Molecular Cloud Complex
• Dense cloud cores revealed by CO in the low metallicity dwarf galaxy WLM
• The Relationship between CO Emission and Visual Extinction Traced by Dust Emission in the Magellanic Clouds

Cited by in corpus (3)

• Is there enough star formation in simulated protoclusters?
• A new empirical method to estimate the molecular gas mass in galaxies
• The SCUBA-2 Web Survey: I. Observations of CO(3-2) in hyper-luminous QSO fields