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• W1552414458 abstract "By redshift z=10, star formation in the first objects should have produced considerable amounts of carbon, nitrogen, and oxygen. The submillimeter lines of C, N, and O redshift into the millimeter and centimeter bands (0.5 mm-1.2 cm), where they may be detectable. High spectral resolution observations could potentially detect inhomogeneities in C, N, and O emission, and see the first objects forming at high redshift. We calculate expected intensity fluctuations and discuss frequency and angular resolution required to detect them. For C II emission, we estimate the intensity using two independent methods: the line-emission coefficient argument and the luminosity-density argument. We find they are in good agreement. At 1+z~10, the typical protogalaxy has a velocity dispersion of 30 km s-1 and an angular size of 1''. If C II is the dominant coolant, then we estimate a characteristic line strength of ~0.1 K km s-1. We also discuss other atomic lines and estimate their signal. Observations with a frequency resolution of 10-3 can detect moderately nonlinear fluctuations of amplitude 2×10-5 times the microwave background. If the intensity fluctuations are detected, they will probe matter density inhomogeneity, chemical evolution, and ionization history at high redshifts." @default.
• W1552414458 created "2016-06-24" @default.
• W1552414458 creator A5052952027 @default.
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• W1552414458 date "1999-02-20" @default.
• W1552414458 modified "2023-10-03" @default.
• W1552414458 title "Detecting z > 10 Objects through Carbon, Nitrogen, and Oxygen Emission Lines" @default.
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