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Long gamma-ray bursts (GRBs) are the most luminous known electromagneticradiation sources in the Universe for the 3 to 300 sec of their prompt flashes(isotropic X/ gamma-ray luminosities up to 10^53 ergs/sec). Their afterglowshave first day rest-frame UV/optical absolute magnitudes AB = -30 to -23. Thisluminous continuum nUV-nIR back-light provides the ultimate probe of the SFR(z)back to the first Pop III to II.5 stars, expected to be massive and GRBprogenitors. GRB afterglow spectra in the first 1 to 3 hours will directlymeasure their host galaxy ionization fraction x_i vs. z in the Epoch ofReionization (EOR), tracing the growth of structure. Only 28% of Swift GRBshave measured redshifts due to limited followup at R, J >21. Some ~25% of GRBsare optically dark due to dust absorption in their host galaxies, but thosewith low NH in their X-ray spectra are likely at z >7. Current 8-10m telescopesand coming ELTs cannot pursue optically dark GRBs promptly, nor can JWST orWFIRST slew within 0.5 to 1 days of a GRB. The Time-domain SpectroscopicObservatory (TSO) is a proposed Probe-class 1.3m telescope at L2, with imagingand spectroscopy (R = 200, 1800) in 4 bands (0.3 to 5um) and rapid slewcapability to 90% of sky. TSO would finally utilize z > 6 to 12 GRBs as themost direct probe of the SFR(z), EOR(z), and possibly the first directdetection of the core collapse of the very first (Pop III) stars.

GRBs as Probes of the Early Universe with TSO