Sunyaev-Zeldovich Fluctuations from the First Stars?

Abstract

WMAP's detection of high electron-scattering optical depth suggests substantial star formation at high redshift z~17 +/- 5. On the other hand, the recovered sigma_8 ~ 0.84 +/-0.04 disfavors a cluster Sunyaev-Zeldovich (SZ) origin for the observed small-scale-CMB fluctuation excess, which generally requires sigma_8 ~ 1.1. Here we consider the effects of high-redshift star formation on the CMB. We derive a fairly model-independent relation between the electron scattering optical depth and the number of ionizing photons emitted per baryon, and use this to calibrate the amount of high-redshift supernova activity. The resulting supernova remnants Compton cool against the CMB creating a Compton-y distortion y ~ few x 10^-6, within observational bounds. However they also create small-scale SZ fluctuations, which could be comparable with SZ fluctuations from unresolved galaxy clusters. This raises the exciting possibility that we have already detected signatures of the first stars not just once, but twice, in the CMB.

Fixed typo in Fig. 1 caption; few other minor changes

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