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• W2060422077 abstract "A direct measurement of the extragalactic background light (EBL) can provide important constraints on the integrated cosmological history of star formation, metal and dust production, and the conversion of starlight into infrared emission by dust. In this paper we examine the cosmological implications of the recent detection of the EBL in the 125 to 5000 ?m wavelength region by the Diffuse Infrared Background Experiment (DIRBE) and Far Infrared Absolute Spectrophotometer (FIRAS) on board the Cosmic Background Explorer (COBE). We first show that the 140 and 240 ?m isotropic residual emission found in the DIRBE data cannot be produced by foreground emission sources in the solar system or the Galaxy. The DIRBE 140 and 240 ?m isotropic residuals, and by inference the FIRAS residuals as well, are therefore extragalactic. Assuming that most of the 140 and 240 ?m emission is from dust yields a 2 ? lower limit of ?I(?) ? 5 nW m-2 sr-1 for the EBL at 100 ?m. The integrated EBL detected by the COBE between 140 and 5000 ?m is ~16 nW m-2 sr-1, roughly 20%-50% of the integrated EBL intensity expected from energy release by nucleosynthesis throughout cosmic history. This also implies that at least ~5%-15% of the baryonic mass density implied by big bang nucleosynthesis has been processed through stars. The COBE observations provide important constraints on the cosmic star formation rate, and we calculate the EBL spectrum for various star formation histories. The results show that the UV and optically determined cosmic star formation rates fall short in producing the observed 140 to 5000 ?m background. The COBE observations require the star formation rate at redshifts of z ? 1.5 to be larger than that inferred from UV-optical observations by at least a factor of 2. This excess stellar energy must be mainly generated by massive stars, since it otherwise would result in a local K-band luminosity density that is larger than observed. The energy sources could either be yet undetected dust-enshrouded galaxies, or extremely dusty star-forming regions in observed galaxies, and they may be responsible for the observed iron enrichment in the intracluster medium. The exact star formation history or scenarios required to produce the EBL at far-IR wavelengths cannot be unambiguously resolved by the COBE observations and must await future observations." @default.
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• W2060422077 date "1998-11-20" @default.
• W2060422077 modified "2023-10-13" @default.
• W2060422077 title "The<i>COBE</i>Diffuse Infrared Background Experiment Search for the Cosmic Infrared Background. IV. Cosmological Implications" @default.
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• W2060422077 cites W1509641920 @default.
• W2060422077 cites W1546172686 @default.
• W2060422077 cites W1550402681 @default.
• W2060422077 cites W1573037074 @default.
• W2060422077 cites W1588757845 @default.
• W2060422077 cites W1607434071 @default.
• W2060422077 cites W1629829263 @default.
• W2060422077 cites W1835404664 @default.
• W2060422077 cites W1966743452 @default.
• W2060422077 cites W1969070606 @default.
• W2060422077 cites W1970723834 @default.
• W2060422077 cites W1980842862 @default.
• W2060422077 cites W1980917671 @default.
• W2060422077 cites W1985318134 @default.
• W2060422077 cites W1986251797 @default.
• W2060422077 cites W1990307162 @default.
• W2060422077 cites W1993035192 @default.
• W2060422077 cites W2004363840 @default.
• W2060422077 cites W2006869439 @default.
• W2060422077 cites W2009352072 @default.
• W2060422077 cites W2014059545 @default.
• W2060422077 cites W2016530741 @default.
• W2060422077 cites W2017556023 @default.
• W2060422077 cites W2018886162 @default.
• W2060422077 cites W2019252893 @default.
• W2060422077 cites W2020527268 @default.
• W2060422077 cites W2023449041 @default.
• W2060422077 cites W2023869431 @default.
• W2060422077 cites W2027135516 @default.
• W2060422077 cites W2046952294 @default.
• W2060422077 cites W2049136484 @default.
• W2060422077 cites W2051951449 @default.
• W2060422077 cites W2053591448 @default.
• W2060422077 cites W2054246448 @default.
• W2060422077 cites W2059975997 @default.
• W2060422077 cites W2061562981 @default.
• W2060422077 cites W2062612172 @default.
• W2060422077 cites W2063477380 @default.
• W2060422077 cites W2063995567 @default.
• W2060422077 cites W2064826995 @default.
• W2060422077 cites W2066780428 @default.
• W2060422077 cites W2075988470 @default.
• W2060422077 cites W2084674774 @default.
• W2060422077 cites W2090728184 @default.
• W2060422077 cites W2102806080 @default.
• W2060422077 cites W2111817932 @default.
• W2060422077 cites W2117629212 @default.
• W2060422077 cites W2128386009 @default.
• W2060422077 cites W2132802601 @default.
• W2060422077 cites W2140887005 @default.
• W2060422077 cites W2142255666 @default.
• W2060422077 cites W2142286455 @default.
• W2060422077 cites W2168495929 @default.
• W2060422077 cites W2568916682 @default.
• W2060422077 cites W2588946112 @default.
• W2060422077 cites W2976664144 @default.
• W2060422077 cites W3097994407 @default.
• W2060422077 cites W3099112362 @default.
• W2060422077 cites W3099630186 @default.
• W2060422077 cites W3100294349 @default.
• W2060422077 cites W3101606976 @default.
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• W2060422077 cites W3104023965 @default.
• W2060422077 cites W3106135993 @default.
• W2060422077 cites W3106285595 @default.
• W2060422077 cites W3110709559 @default.
• W2060422077 cites W3124069432 @default.
• W2060422077 cites W4241677870 @default.
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• W2060422077 doi "https://doi.org/10.1086/306382" @default.
• W2060422077 hasPublicationYear "1998" @default.
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