Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 461, Issue 3, Pages 2856-2866Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stw1467
Keywords
galaxies: star formation; infrared: ISM
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Funding
- NSERC
- University of Western Ontario
- DustPedia, a collaborative focused research project - European Union [606847]
- Cardiff University, UK
- National Observatory of Athens, Greece
- Ghent University, Belgium
- Universite Paris Sud, France
- National Institute for Astrophysics, Italy
- CEA (Paris), France
- National Aeronautics and Space Administration
- Aladin
- NASA's Astrophysics Data System Bibliographic Services
- Spanish MICINN/MINECO [AyA2008-02156, AyA2011-24052]
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Several dedicated surveys focusing on early-type galaxies (ETGs) reveal that significant fractions of them are detectable in all interstellar medium phases studied to date. We select ETGs from the Herschel Reference Survey that have both far-infrared Herschel and either HI or CO detection (or both). We derive their star formation rates (SFRs), stellar masses and dust masses via modelling their spectral energy distributions. We combine these with literature information on their atomic and molecular gas properties, in order to relate their star formation, total gas mass and dust mass on global scales. The ETGs deviate from the dust mass-SFR relation and the Schmidt-Kennicutt relation that SDSS star-forming galaxies define: compared to SDSS galaxies, ETGs have more dust at the same SFR, or less SFR at the same dust mass. When placing them in the M-star-SFR plane, ETGs show a much lower specific SFR as compared to normal star-forming galaxies. ETGs show a large scatter compared to the Schmidt-Kennicutt relation found locally within our Galaxy, extending to lower SFRs and gas mass surface densities. Using an ETG's SFR and the Schmidt-Kennicutt law to predict its gas mass leads to an underestimate. ETGs have similar observed-gas-to-modelled-dust mass ratios to star-forming galaxies of the same stellar mass, as well as they exhibit a similar scatter.
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