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| Naji, M. |
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| Motta, Antonella |
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| Aletan, Dirar |
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| Mohamed, Tarek |
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| Ertürk, Emre |
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| Taccardi, Nicola |
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| Kononenko, Denys |
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| Petrov, R. H. | Madrid |
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| Alshaaer, Mazen | Brussels |
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| Bih, L. |
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| Casati, R. |
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| Muller, Hermance |
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| Kočí, Jan | Prague |
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| Šuljagić, Marija |
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| Kalteremidou, Kalliopi-Artemi | Brussels |
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| Azam, Siraj |
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| Ospanova, Alyiya |
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| Blanpain, Bart |
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| Ali, M. A. |
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| Popa, V. |
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| Rančić, M. |
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| Ollier, Nadège |
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| Azevedo, Nuno Monteiro |
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| Landes, Michael |
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| Rignanese, Gian-Marco |
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Schneider, Raffaella
in Cooperation with on an Cooperation-Score of 37%
Topics
Publications (12/12 displayed)
- 2016The dust content of the most metal-poor star-forming galaxiescitations
- 2016SN Dust Yields: Fallback, Metallicity and Rotation Impact
- 2015The dust mass in z 〉 6 normal star-forming galaxiescitations
- 2015Supernova dust formation and the grain growth in the early universe: the critical metallicity for low-mass star formationcitations
- 2015The metal and dust yields of the first massive starscitations
- 2015The dust mass in z > 6 normal star-forming galaxiescitations
- 2014Dust grain growth and the formation of the extremely primitive star SDSS J102915+172927citations
- 2013Growth of Dust Grains in a Low-Metallicity Gas and its Effect on the Cloud Fragmentation
- 2012The first low-mass stars: critical metallicity or dust-to-gas ratio?citations
- 2011The origin of the dust in high-redshift quasars:The case of SDSS J1148+5251citations
- 2011The origin of the dust in high-redshift quasars: the case of SDSS J1148+5251citations
- 2006Fragmentation of star-forming clouds enriched with the first dustcitations
Places of action
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article
The dust content of the most metal-poor star-forming galaxies
Abstract
Although dust content is usually assumed to depend uniquely on metallicity, recent observations of two extremely metal-poor dwarf galaxies have suggested that this may not always be true. At a similar oxygen abundance of ̃3 per cent Z<SUB>☉</SUB>, the dust-to-gas and dust-to-stellar mass ratios in SBS 0335-052 and I Zw 18 differ by a factor of 40-70 according to including molecular gas or excluding it. Here, we investigate a possible reason for this dramatic difference through models based on a semi-analytical formulation of chemical evolution including dust. Results suggest that the greater dust mass in SBS 0335-052 is due to the more efficient grain growth allowed by the high density in the cold interstellar medium (ISM), observationally inferred to be almost 20 times higher than in I Zw 18. Our models are able to explain the difference in dust masses, suggesting that efficient dust formation and dust content in galaxies, including those with the highest measured redshifts, depend sensitively on the ISM density, rather than only on metallicity....