eprintid: 1398691 rev_number: 39 eprint_status: archive userid: 608 dir: disk0/01/39/86/91 datestamp: 2013-07-05 18:33:49 lastmod: 2021-10-18 00:24:06 status_changed: 2013-07-05 18:33:49 type: article metadata_visibility: show item_issues_count: 0 creators_name: Matsuura, M creators_name: Woods, PM creators_name: Owen, PJ title: The global gas and dust budget of the Small Magellanic Cloud ispublished: pub divisions: UCL divisions: B04 divisions: C06 keywords: stars, AGB and post-AGB, mass-loss, supernovae, dust, extinction, galaxies evolution, galaxies, the Magellanic Clouds note: This article has been published in Monthly Notices of the Royal Astronomical Society © 2012 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. abstract: In order to understand the evolution of the interstellar medium (ISM) of a galaxy, we have analysed the gas and dust budget of the Small Magellanic Cloud (SMC). Using the Spitzer Space Telescope, we measured the integrated gas mass-loss rate across asymptotic giant branch (AGB) stars and red supergiants (RSGs) in the SMC, and obtained a rate of 1.4 × 10−3 M⊙ yr−1. This is much smaller than the estimated gas ejection rate from Type II supernovae (SNe) (2–4 × 10−2 M⊙ yr−1). The SMC underwent an increase in star formation rate in the last 12 Myr, and consequently the galaxy has a relatively high SN rate at present. Thus, SNe are more important gas sources than AGB stars in the SMC. The total gas input from stellar sources into the ISM is 2–4 × 10−2 M⊙ yr−1. This is slightly smaller than the ISM gas consumed by star formation (∼8 × 10−2 M⊙ yr−1). Star formation in the SMC relies on a gas reservoir in the ISM, but eventually the star formation rate will decline in this galaxy, unless gas infalls into the ISM from an external source. The dust injection rate from AGB and RSG candidates is 1 × 10−5 M⊙ yr−1. Dust injection from SNe is in the range 0.2–11 × 10−4 M⊙ yr−1, although the SN contribution is rather uncertain. Stellar sources could be important for ISM dust (3 × 105 M⊙) in the SMC, if the dust lifetime is about 1.4 Gyr. We found that the presence of poly-aromatic hydrocarbons (PAHs) in the ISM cannot be explained entirely by carbon-rich AGB stars. Carbon-rich AGB stars could inject only 7 × 10−9 M⊙ yr−1 of PAHs at most, which could contribute up to 100 M⊙ of PAHs in the lifetime of a PAH. The estimated PAH mass of 1800 M⊙ in the SMC cannot be explained. Additional PAH sources, or ISM reprocessing should be needed. date: 2012-12 official_url: http://dx.doi.org/10.1093/mnras/sts521 vfaculties: VMPS oa_status: green full_text_type: pub language: eng primo: open primo_central: open_green verified: verified_manual elements_source: WoS-Lite elements_id: 837685 doi: 10.1093/mnras/sts521 lyricists_name: Matsuura, Mikako lyricists_name: Woods, Paul lyricists_id: MMATS97 lyricists_id: PWOOD80 full_text_status: public publication: Monthly Notices of the Royal Astronomical Society volume: 429 number: 3 pagerange: 2527 - 2536 issn: 0035-8711 citation: Matsuura, M; Woods, PM; Owen, PJ; (2012) The global gas and dust budget of the Small Magellanic Cloud. Monthly Notices of the Royal Astronomical Society , 429 (3) 2527 - 2536. 10.1093/mnras/sts521 <https://doi.org/10.1093/mnras%2Fsts521>. Green open access document_url: https://discovery.ucl.ac.uk/id/eprint/1398691/1/MNRAS-2013-Matsuura-2527-36.pdf