Detecting z > 10 objects through carbon, nitrogen, and oxygen emission lines

By redshift z = 10, star formation in the first objects should have produce d considerable amounts of carbon, nitrogen, and oxygen. The submillimeter l ines 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 observat ions could potentially detect inhomogeneities in C, N, and O emission, and see the first objects forming at high redshift. We calculate expected inten sity fluctuations and discuss frequency and angular resolution required to detect them. For C II emission, we estimate the intensity using two indepen dent methods: the line-emission coefficient argument and the luminosity-den sity argument. We find they are in good agreement. At 1 + z similar to 10, the typical protogalaxy has a velocity dispersion of 30 km s(-1) and an ang ular size of 1 ". If C II is the dominant coolant, then we estimate a chara cteristic line strength of similar to 0.1 K km s(-1) We also discuss other atomic lines and estimate their signal. Observations with a frequency resol ution of 10(-3) can detect moderately nonlinear fluctuations of amplitude 2 x 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.