Detecting z > 10 Objects through Carbon, Nitrogen, and Oxygen Emission Lines

Open Access
Publisher Website
Google Scholar
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.
All Related Versions

This publication has 27 references indexed in Scilit: