Cosmic star formation history with tomographic cosmic infrared background-galaxy cross-correlation

Abstract

In this work we present a new method for probing the star formation history of the Universe, namely tomographic cross-correlation between the cosmic infrared background (CIB) and galaxy samples. The galaxy samples are from the Kilo-Degree Survey (KiDS), while the CIB maps are made from Planck sky maps at 353, 545, and 857 GHz. We measure the cross-correlation in harmonic space within 100<<2000 with a significance of 43. We model the cross-correlation with a halo model, which links CIB anisotropies to star formation rates (SFRs) and galaxy abundance. We assume that the SFR has a lognormal dependence on halo mass and that the galaxy abundance follows the halo occupation distribution (HOD) model. The cross-correlations give a best-fit maximum star formation efficiency of ηmax=0.41-0.14+0.09 at a halo mass log10(Mpeak/M) = 12.14±0.36. The derived star formation rate density (SFRD) is well constrained up to zã1.5. The constraining power at high redshift is mainly limited by the KiDS survey depth. We also show that the constraint is robust to uncertainties in the estimated redshift distributions of the galaxy sample. A combination with external SFRD measurements from previous studies gives log10(Mpeak/M)=12.42-0.19+0.35. This tightens the SFRD constraint up to z=4, yielding a peak SFRD of 0.09-0.004+0.003Myr-1 Mpc-3 at z=1.74-0.02+0.06, corresponding to a lookback time of 10.05-0.03+0.12 Gyr. Both constraints are consistent, and the derived SFRD agrees with previous studies and simulations. This validates the use of CIB tomography as an independent probe of the star formation history of the Universe. Additionally, we estimate the galaxy bias, b, of KiDS galaxies from the constrained HOD parameters and obtain an increasing bias from b=1.1-0.31+0.17 at z=0 to b=1.96-0.64+0.18 at z=1.5, which highlights the potential of this method as a probe of galaxy abundance. Finally, we provide a forecast for future galaxy surveys and conclude that, due to their considerable depth, future surveys will yield a much tighter constraint on the evolution of the SFRD.