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DC Field | Value | Language |
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dc.citation.endPage | 3869 | - |
dc.citation.number | 3 | - |
dc.citation.startPage | 3845 | - |
dc.citation.title | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | - |
dc.citation.volume | 487 | - |
dc.contributor.author | Caplar, Neven | - |
dc.contributor.author | Tacchella, Sandro | - |
dc.date.accessioned | 2023-12-21T18:47:45Z | - |
dc.date.available | 2023-12-21T18:47:45Z | - |
dc.date.created | 2021-07-27 | - |
dc.date.issued | 2019-08 | - |
dc.description.abstract | We present a framework for modelling the star-formation histories of galaxies as a stochastic process. We define this stochastic process through a power spectrum density with a functional form of a broken power law. Star-formation histories are correlated on short time-scales, the strength of this correlation described by a power-law slope, alpha, and they decorrelate to resemble white noise over a time-scale that is proportional to the time-scale of the break in the power spectrum density, tau(break) We use this framework to explore the properties of the stochastic process that, we assume, gives rise to the log-normal scatter about the relationship between star-formation rate and stellar mass, the so-called galaxy star-forming main sequence. Specifically, we show how the measurements of the normalization and width (sigma(MS)) of the main sequence, measured in several passbands that probe different time-scales, give a constraint on the parameters of the underlying power spectrum density. We first derive these results analytically for a simplified case where we model observations by averaging over the recent star-formation history, We then run numerical simulations to find results for more realistic observational cases. As a proof of concept, we use observational estimates of the main sequence scatter at z similar to 0 and M-star approximate to 10(10) M-circle dot measured in H alpha, UV+IR, and the u-band. The result is degenerate in the tau(break)-alpha space, but if we assume alpha = 2, we measure tau(break) = 170(-85)(+169) Myr. This implies that star-formation histories of galaxies lose 'memory' of their previous activity on a time-scale of similar to 200 Myr. | - |
dc.identifier.bibliographicCitation | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, v.487, no.3, pp.3845 - 3869 | - |
dc.identifier.doi | 10.1093/mnras/stz1449 | - |
dc.identifier.issn | 0035-8711 | - |
dc.identifier.scopusid | 2-s2.0-85072055237 | - |
dc.identifier.uri | https://scholarworks.unist.ac.kr/handle/201301/53336 | - |
dc.identifier.wosid | 000478053200065 | - |
dc.language | 영어 | - |
dc.publisher | OXFORD UNIV PRESS | - |
dc.title | Stochastic modelling of star-formation histories I: the scatter of the star-forming main sequence | - |
dc.type | Article | - |
dc.description.isOpenAccess | FALSE | - |
dc.relation.journalWebOfScienceCategory | Astronomy & Astrophysics | - |
dc.relation.journalResearchArea | Astronomy & Astrophysics | - |
dc.type.docType | Article | - |
dc.description.journalRegisteredClass | scie | - |
dc.description.journalRegisteredClass | scopus | - |
dc.subject.keywordAuthor | galaxies: evolution | - |
dc.subject.keywordAuthor | galaxies: star formation | - |
dc.subject.keywordAuthor | galaxies: statistics | - |
dc.subject.keywordPlus | MASS ASSEMBLY GAMA | - |
dc.subject.keywordPlus | SPECTRAL ENERGY-DISTRIBUTIONS | - |
dc.subject.keywordPlus | GALAXY FORMATION | - |
dc.subject.keywordPlus | UNCERTAINTY PRINCIPLE | - |
dc.subject.keywordPlus | PHYSICAL-PROPERTIES | - |
dc.subject.keywordPlus | FORMATION RATES | - |
dc.subject.keywordPlus | STELLAR | - |
dc.subject.keywordPlus | EVOLUTION | - |
dc.subject.keywordPlus | GAS | - |
dc.subject.keywordPlus | FEEDBACK | - |
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