期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 489, 期 3, 页码 4072-4089出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stz1948
关键词
methods: analytical; dust, extinction; galaxies: evolution; galaxies: formation; galaxies: ISM
资金
- UK STFC DISCnet
- STFC
- Science and Technology Facilities Council [ST/P000525/1]
- European Research Council [246797]
- Zwicky Prize fellowship
- European Union under the Seventh Framework Programme (2007-2013) [606847]
- STFC [2022980, ST/P000525/1] Funding Source: UKRI
We implement a detailed dustmodel into the L-Galaxies semi-analytical model which includes: injection of dust by type II and type Ia supernovae (SNe) and AGB stars; grain growth in molecular clouds; and destruction due to supernova-induced shocks, star formation, and reheating. Our grain growth model follows the dust content in molecular clouds and the inter-cloud medium separately, and allows growth only on pre-existing dust grains. At early times, this can make a significant difference to the dust growth rate. Above z similar to 8, type II SNe are the primary source of dust, whereas below z similar to 8, grain growth in molecular clouds dominates, with the total dust content being dominated by the latter below z similar to 6. However, the detailed history of galaxy formation is important for determining the dust content of any individual galaxy. We introduce a fit to the dust-to-metal (DTM) ratio as a function of metallicity and age, which can be used to deduce the DTM ratio of galaxies at any redshift. At z less than or similar to 3, we find a fairly flat mean relation between metallicity and the DTM, and a positive correlation between metallicity and the dust-to-gas (DTG) ratio, in good agreement with the shape and normalization of the observed relations. We also match the normalization of the observed stellar mass-dust mass relation over the redshift range of 0-4, and to the dust mass function at z = 0. Our results are important in interpreting observations on the dust content of galaxies across cosmic time, particularly so at high redshift.
作者
我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。
推荐
暂无数据