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The formation of the first galaxies is influenced by the radiative feedbackfrom the first generations of stars. This feedback is manisfested by theheating and ionization of the gas which lies within the H II regionssurrounding the first stars, as well as by the photodissociation of hydrogenmolecules within the larger Lyman-Werner (LW) bubbles that surround thesesources. Using a ray-tracing method in three-dimensional cosmologicalsimulations, we self-consistently track the formation of, and radiativefeedback from, individual stars in the course of the formation of aprotogalaxy. We compute in detail the H II regions of each of these sources, aswell as the regions affected by their molecule-dissociating radiation. Wefollow the thermal, chemical, and dynamical evolution of the primordial gas, asit becomes incorporated into the protogalaxy. While the IGM is, in general,optically thick to LW photons only over physical distances of > 30 kpc atredshifts z < 20, the high molecule fraction that is built up in relic H IIregions and their increasing volume-filling fraction renders even the local IGMoptically thick to LW photons over physical distances of the order of a fewkiloparsecs. We find that efficient accretion onto Population III relic blackholes may occur after ~ 60 Myr from the time of their formation, by which timethe photo-heated relic H II region gas can cool and re-collapse into the 10^6M_solar minihalo which hosts the black hole. Also, Pop II.5 stars, postulatedto have masses of the order of 10 M_solar, can likely form from thisre-collapsing relic H II region gas. Overall, we find that the local radiativefeedback from the first generations of stars suppresses the star formation rateby only a factor of, at most, a few.Comment: 29 pages, 7 figures; ApJ in pres

Local Radiative Feedback in the Formation of the First Protogalaxies