Linear bias forecasts for emission line cosmological surveys

We forecast the linear bias for Hu-emitting galaxies at high redshift. To simulate a Euclid-like and a WEIRST-like survey, we place galaxies into a large-volume dark matter halo lightconc by sampling a library of luminosity-dependent halo occupation distributions (HMO, which is constructed using a physically motivated galaxy formation model. We calibrate the dust attenuation in the lightcones such that they are able to reproduce the 1-101 luminosity function or the HU cumulative number counts. The angle-averaged galaxy correlation function is computed for each survey in redshift slices of width A z = 0.2. In each redshift bin the linear bias can be fitted with a single, scale-independent value that increases with increasing redshift. Fitting for the evolution of linear bias with redshift, we rind that our Euclid-like and WFIRST-like surveys are both consistent within error with the relation b(z) = 0.7z 0.7. Our bias forecasts are consistent with bias measurements from the IliZELS survey. We rind that the Euclid-like and WFIRST-like surveys yield linear biases that are broadly consistent within error, most likely due to the IIOD for the WFIRST-like survey having a steeper power-law slope towards larger halo masses.