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- W2017626434 abstract "We consider the formation of molecules in primordial prestellar clumps and evaluate the line luminosities to assess detectability by next-generation observational facilities. If the initial |$mathrm{H}_2$| fraction is sufficiently high, HD becomes an important coolant in the clumps. The luminosity from such HD cooling clumps is lower than that from |$mathrm{H}_2$| cooling ones because of the lower temperature (|$<100 ,mathrm{K}$|). As for Li reactions, we include the three-body LiH formation approximately. The Li molecular fraction remains very low (|$<10^{-3}$|) throughout the evolution, owing to the high dissociative reaction rate of |$mathrm{LiH} + mathrm{H} rightarrow mathrm{Li} + mathrm{H}_2$|. LiH does not become an important coolant in any density range. The luminous emission lines from the prestellar cores include |$mathrm{H}_2$| rovibrational lines [1–0 Q(1), 1–0 O(3), 1–0 O(5)] and pure rotational lines [0–0 S(3), 0–0 S(4), 0–0 S(5)]. The next-generation facilities SPICA and JWST are able to detect |$mathrm{H}_2$| emission in a large pre-galactic cloud that forms metal-free stars at a high rate of |$sim 10^3 ,{{{M}_{odot}}} ,mathrm{yr}^{-1}$| at a redshift of |$z < 10$|. We also derive an analytical expression for the luminosity that reproduces the numerical results." @default.
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- W2017626434 date "2005-12-25" @default.
- W2017626434 modified "2023-09-28" @default.
- W2017626434 title "Primordial Molecular Emission in Population III Galaxies" @default.
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- W2017626434 doi "https://doi.org/10.1093/pasj/57.6.951" @default.
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