Measuring the 3D clustering of undetected galaxies through cross correlation of their cumulative flux fluctuations from multiple spectral lines

We discuss a method for detecting the emission from high redshift galaxies by cross correlating flux fluctuations from multiple spectral lines. If one can fit and subtract away the continuum emission with a smooth function of frequency, the remaining signal contains fluctuations of flux with frequency and angle from line emitting galaxies. Over a particular small range of observed frequencies, these fluctuations will originate from sources corresponding to a series of different redshifts, one for each emission line. It is possible to statistically isolate the fluctuations at a particular redshift by cross correlating emission originating from the same redshift, but in different emission lines. This technique will allow detection of clustering fluctuations from the faintest galaxies which individually cannot be detected, but which contribute substantially to the total signal due to their large numbers. We describe these fluctuations quantitatively through the line cross power spectrum. As an example of a particular application of this technique, we calculate the signal-to-noise ratio for a measurement of the cross power spectrum of the OI(63 μm) and OIII(52 μm) fine structure lines with the proposed Space Infrared Telescope for Cosmology and Astrophysics (SPICA). We find that the cross power spectrum can be measured beyond a redshift of z = 8. Such observations could constrain the evolution of the metallicity, bias, and duty cycle of faint galaxies at high redshifts and may also be sensitive to the reionization history through its effect on the minimum mass of galaxies. As another example of this technique, we calculate the signal-to-noise ratio for the cross power spectrum of CO line emission measured with a large ground based telescope like the Cornell Caltech Atacama Telescope (CCAT) and 21-cm radiation originating from hydrogen in galaxies after reionization with an interferometer similar in scale to the Murchison Widefield Array (MWA), but optimized for post-reionization redshifts.