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dc.contributor.authorLoeb, Abraham
dc.contributor.authorHaiman, Zoltan
dc.date.accessioned2019-09-24T12:03:42Z
dc.date.issued1997
dc.identifier.citationLoeb, Abraham, and Zoltan Haiman. 1997. “Signatures of Intergalactic Dust from the First Supernovae.” The Astrophysical Journal 490 (2): 571–76. https://doi.org/10.1086/304919.
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.urihttp://nrs.harvard.edu/urn-3:HUL.InstRepos:41393180*
dc.description.abstractWe quantify the consequences of intergalactic dust produced by the first Type II supernovae in the universe. The fraction of gas converted into stars is calibrated based on the observed C/H ratio in the intergalactic medium at z = 3, assuming a Scale mass function for the stars. The associated dust absorbs starlight energy and emits it at longer wavelengths. For a uniform mix of metals and dust with the intergalactic gas, we find that the dust distorts the microwave background spectrum by a y-parameter in the range (0.06-6) x 10(-5) (M-SN/0.3 M.), where M-SN is the average mass of dust produced per supernova. The opacity of intergalactic dust to infrared sources at redshifts of z greater than or similar to 10 is significant, tau(dust) = (0.1-1) x (M-SN/0.3 M.), and could be detected with the Next Generation Space Telescope. Although dust suppresses the Ly alpha emission from early sources, the redshifts of star clusters at z = 10-35 can be easily inferred from the Lyman limit break in their infrared spectrum between 1 and 3.5 mu m.
dc.language.isoen_US
dc.publisherAmerican Astronomical Society
dash.licenseLAA
dc.titleSignatures of Intergalactic Dust from the First Supernovae
dc.typeJournal Article
dc.description.versionVersion of Record
dc.relation.journalThe Astrophysical Journal
dash.depositing.authorLoeb, Abraham::9975df1f269ab49c1ad5a328a1ec1476::600
dc.date.available2019-09-24T12:03:42Z
dash.workflow.comments1Science Serial ID 95253
dc.identifier.doi10.1086/304919
dash.source.volume490;2
dash.source.page571-576


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