Detailed dust modelling in the L-GALAXIES semi-analytic model of galaxy formation. Vijayan, A. P., Clay, S. J., Thomas, P. A., Yates, R. M., Wilkins, S. M., & Henriques, B. M. Monthly Notices of the Royal Astronomical Society, 489:4072–4089, November, 2019. ![Detailed dust modelling in the L-GALAXIES semi-analytic model of galaxy formation [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper doi abstract bibtex We implement a detailed dust model 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 ∼ 8, type II SNe are the primary source of dust, whereas below z ∼ 8, grain growth in molecular clouds dominates, with the total dust content being dominated by the latter below z ∼ 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 ≲ 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.
@article{vijayan_detailed_2019,
title = {Detailed dust modelling in the {L}-{GALAXIES} semi-analytic model of galaxy formation},
volume = {489},
issn = {0035-8711},
url = {http://adsabs.harvard.edu/abs/2019MNRAS.489.4072V},
doi = {10.1093/mnras/stz1948},
abstract = {We implement a detailed dust model 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 ∼ 8, type II SNe are the
primary source of dust, whereas below z ∼ 8, grain growth in
molecular clouds dominates, with the total dust content being dominated
by the latter below z ∼ 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 ≲ 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.},
urldate = {2020-03-26},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Vijayan, Aswin P. and Clay, Scott J. and Thomas, Peter A. and Yates, Robert M. and Wilkins, Stephen M. and Henriques, Bruno M.},
month = nov,
year = {2019},
keywords = {Astrophysics - Astrophysics of Galaxies, dust, extinction, galaxies: ISM, galaxies: evolution, galaxies: formation, methods: analytical},
pages = {4072--4089},
}
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At early times, this can make a significant difference to the dust growth rate. Above z ∼ 8, type II SNe are the primary source of dust, whereas below z ∼ 8, grain growth in molecular clouds dominates, with the total dust content being dominated by the latter below z ∼ 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 ≲ 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.","urldate":"2020-03-26","journal":"Monthly Notices of the Royal Astronomical Society","author":[{"propositions":[],"lastnames":["Vijayan"],"firstnames":["Aswin","P."],"suffixes":[]},{"propositions":[],"lastnames":["Clay"],"firstnames":["Scott","J."],"suffixes":[]},{"propositions":[],"lastnames":["Thomas"],"firstnames":["Peter","A."],"suffixes":[]},{"propositions":[],"lastnames":["Yates"],"firstnames":["Robert","M."],"suffixes":[]},{"propositions":[],"lastnames":["Wilkins"],"firstnames":["Stephen","M."],"suffixes":[]},{"propositions":[],"lastnames":["Henriques"],"firstnames":["Bruno","M."],"suffixes":[]}],"month":"November","year":"2019","keywords":"Astrophysics - Astrophysics of Galaxies, dust, extinction, galaxies: ISM, galaxies: evolution, galaxies: formation, methods: analytical","pages":"4072–4089","bibtex":"@article{vijayan_detailed_2019,\n\ttitle = {Detailed dust modelling in the {L}-{GALAXIES} semi-analytic model of galaxy formation},\n\tvolume = {489},\n\tissn = {0035-8711},\n\turl = {http://adsabs.harvard.edu/abs/2019MNRAS.489.4072V},\n\tdoi = {10.1093/mnras/stz1948},\n\tabstract = {We implement a detailed dust model into the L-Galaxies semi-analytical \nmodel which includes: injection of dust by type II and type Ia\nsupernovae (SNe) and AGB stars; grain growth in molecular clouds; and\ndestruction due to supernova-induced shocks, star formation, and\nreheating. Our grain growth model follows the dust content in molecular\nclouds and the inter-cloud medium separately, and allows growth only on\npre-existing dust grains. At early times, this can make a significant\ndifference to the dust growth rate. Above z ∼ 8, type II SNe are the\nprimary source of dust, whereas below z ∼ 8, grain growth in\nmolecular clouds dominates, with the total dust content being dominated\nby the latter below z ∼ 6. However, the detailed history of galaxy\nformation is important for determining the dust content of any\nindividual galaxy. We introduce a fit to the dust-to-metal (DTM) ratio\nas a function of metallicity and age, which can be used to deduce the\nDTM ratio of galaxies at any redshift. At z ≲ 3, we find a fairly\nflat mean relation between metallicity and the DTM, and a positive\ncorrelation between metallicity and the dust-to-gas (DTG) ratio, in good\nagreement with the shape and normalization of the observed relations. We\nalso match the normalization of the observed stellar mass-dust mass\nrelation over the redshift range of 0-4, and to the dust mass function\nat z = 0. Our results are important in interpreting observations on the\ndust content of galaxies across cosmic time, particularly so at high\nredshift.},\n\turldate = {2020-03-26},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Vijayan, Aswin P. and Clay, Scott J. and Thomas, Peter A. and Yates, Robert M. and Wilkins, Stephen M. and Henriques, Bruno M.},\n\tmonth = nov,\n\tyear = {2019},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, dust, extinction, galaxies: ISM, galaxies: evolution, galaxies: formation, methods: analytical},\n\tpages = {4072--4089},\n}\n\n","author_short":["Vijayan, A. P.","Clay, S. J.","Thomas, P. A.","Yates, R. M.","Wilkins, S. M.","Henriques, B. 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