Cosmological H II Bubble Growth during Reionization

摘要: We present general properties of ionized hydrogen (H II) bubbles and their growth based on a state-of-the-art, large-scale (100 Mpc h−1) cosmological radiative transfer simulation. The simulation resolves all halos with atomic cooling at the relevant redshifts simultaneously performs dynamical evolution structure formation. Our major conclusions include following: (1) For significant H II bubbles, number distribution is peaked volume ~0.6 Mpc3 h−3 redshifts. But -->z ≤ 10, one large, connected network dominates entire volume. (2) are highly nonspherical. (3) regions biased respect to underlying matter distribution, bias decreasing time. (4) non-Gaussianity region small when universe becomes 50% ionized. reaches its maximum near end reionization epoch ~ 6. interest there in field. (5) Population III galaxies may play role process. Small initially largely produced by stars. At ≥ 10 even largest have balanced ionizing photon contribution from stars, while 8 stars start dominate overall production for large although continue make nonnegligible contribution. (6) relationship between halo density bubble size complicated, but strong correlation found bubbles.