University of Birmingham > Talks@bham > Astrophysics Seminars > Molecular gas in galaxies at cosmic noon

Molecular gas in galaxies at cosmic noon

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If you have a question about this talk, please contact Nicola Giacobbo.

In the current view of galaxy evolution, galaxies evolve along the so-called main sequence and form their stars inside-out in extended disks. Feedback-driven winds from star formation or active galactic nuclei are then one of the main processes through which galaxies could stop forming their stars and become passive. A central piece for understanding how galaxies grow and quench is the molecular gas, which is the fuel for star formation and stellar mass growth. In my talk I will report on the recent results of an ALMA campaign, systematically targeting several carbon monoxide CO and neutral atomic carbon [CI] transitions (and their underlying continuum) to assess the amount and the excitation properties of the molecular gas in a sample of galaxies on and above the main sequence at z=1-1.7. I will present in this context the serendipitous detection of ID2299 , a massive starburst galaxy above the main sequence at z=1.4 which is ejecting 46±13% of its total molecular gas content at a startling rate of ≳10,000 M⊙yr-1 and might challenge the role of feedback-driven winds in galaxy evolution.

This talk is part of the Astrophysics Seminars series.

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