The evolution of the cold interstellar medium in galaxies following a starburst
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We present the evolution of dust and molecular gas properties in a sample of 11 z ˜ 0.03 starburst to post-starburst (PSB) galaxies selected to span an age sequence from ongoing starburst to 1 Gyr after the starburst ended. All PSBs harbour significant molecular gas and dust reservoirs and residual star formation, indicating that complete quenching of the starburst due to exhaustion or expulsion of gas has not occurred during this timespan. As the starburst ages, we observe a clear decrease in the star formation efficiency, molecular gas and star formation rate (SFR) surface density, and effective dust temperature, from levels coincident with starburst galaxies to those of normal star-forming galaxies. These trends are consistent with a natural decrease in the SFR following consumption of molecular gas by the starburst, and corresponding decrease in the interstellar radiation field strength as the starburst ages. The gas and dust contents of the PSBs are coincident with those of star-forming galaxies and molecular gas-rich early-type galaxies, and are not consistent with galaxies on the red sequence. We find no evidence that the global gas reservoir is expelled by stellar winds or active galactic nuclei feedback. Our results show that although a strong starburst in a low-redshift galaxy may cause the galaxy to ultimately have a lower specific SFR and be of an earlier morphological type, the galaxy will remain in the `green valley' for an extended time. Multiple such episodes may be needed to complete migration of the galaxy from the blue- to red sequence.
Rowlands , K , Wild , V , Nesvadba , N , Sibthorpe , B , Mortier , A , Lehnert , M & da Cunha , E 2015 , ' The evolution of the cold interstellar medium in galaxies following a starburst ' Monthly Notices of the Royal Astronomical Society , vol 448 , pp. 258-279 . DOI: 10.1093/mnras/stu2714
Monthly Notices of the Royal Astronomical Society
Copyright 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society
VW and KR acknowledge support from the European Research Council Starting Grant SEDmorph (P.I. VW).
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