Minihalo photoevaporation during cosmic reionization: evaporation times and photon consumption rates

Iliev, Ilian T.; Shapiro, Paul R.; Raga, A. C.

doi:10.1111/j.1365-2966.2005.09155.x

Cited by 156 publications

(209 citation statements)

References 29 publications

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“…In Figure 1, we plot the neutral fraction as a function of time for this halo using the fits from Iliev et al (2005), assuming J21 = 1000 and one ionizing photon per LW photon. This assumption is an overestimate for small pop III stars, but fairly accurate for large ones.…”

Section: Photoevaporationmentioning

confidence: 99%

“…Tidal disruption is unimportant provided that the tidal force is smaller than the gravitational binding force at the surface of the core Neutral gas fraction as a function of time for a 2 × 10 7 M ⊙ halo at z = 10 exposed to J 21 ∼ 1000 (assuming one ionizing photon per LW photon and a T = 10 5 K blackbody spectrum) computed with the fits of Iliev et al (2005).…”

Section: Ram Pressure Stripping and Tidal Disruptionmentioning

confidence: 99%

“…Assuming ∼ 10 ionizing photons released into the IGM for each baryon collapsing into a dark matter halo over 10 percent of the Hubble time and an IGM clumpiness of C = n 2 H / nH 2 ∼ 3 (Pawlik et al 2009;Finlator et al 2012), a 10 11 M⊙ halo will quickly (in < 10 Myr) produce an ionized bubble with r ∼ 65 kpc. Utilizing the fits of Iliev et al (2005) (assuming a T = 5 × 10 4 K blackbody spectra) to determine the photoevaporation time and the spherical collapse model to estimate the maximum distance between the DCBH-forming halo's progenitors and the 10 11 M⊙ halo at z ∼ 15, we find that the progenitors of the DCBH-forming halo can be photoevaporated in less than 200 Myr. The time from z = 10 − 15 corresponds to ∼ 200 Myr, so by z = 10 the DCBH-forming halo is likely to be ionized, effectively raising Jcrit.…”

Section: Introductionmentioning

confidence: 99%

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Direct collapse black hole formation from synchronized pairs of atomic cooling haloes

Visbal¹,

Haiman²,

Bryan³

2014

Monthly Notices of the Royal Astronomical Society

127

118

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High-redshift quasar observations imply that supermassive black holes (SMBHs) larger than ∼ 10 9 M ⊙ formed before z ∼ 6. That such large SMBHs formed so early in the history of the Universe remains an open theoretical problem. One possibility is that gas in atomic cooling halos exposed to strong Lyman-Werner (LW) radiation forms 10 4 − 10 6 M ⊙ supermassive stars which quickly collapse into black holes. We propose a scenario for direct collapse black hole (DCBH) formation based on synchronized pairs of pristine atomic cooling halos. We consider halos at very small separation with one halo being a subhalo of the other. The first halo to surpass the atomic cooling threshold forms stars. Soon after these stars are formed, the other halo reaches the cooling threshold and due to its small distance from the newly formed galaxy, is exposed to the critical LW intensity required to form a DCBH. The main advantage of this scenario is that synchronization can potentially prevent photoevaporation and metal pollution in DCBH-forming halos. We use N-body simulations and an analytic approximation to estimate the abundance of DCBHs formed in this way. The density of DCBHs formed in this scenario could explain the SMBHs implied by z ∼ 6 quasar observations. Metal pollution and photoevaporation could potentially reduce the abundance of DCBHs below that required to explain the observations in other models that rely on a high LW flux.

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Section: Photoevaporationmentioning

confidence: 99%

Section: Ram Pressure Stripping and Tidal Disruptionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Direct collapse black hole formation from synchronized pairs of atomic cooling haloes

Visbal¹,

Haiman²,

Bryan³

2014

Monthly Notices of the Royal Astronomical Society

127

118

View full text Add to dashboard Cite

show abstract

“…[See the electronic edition of the Journal for a color version of this figure. ] the minihalo cross sections will shrink with time before they become completely photoevaporated (Shapiro et al 2004;Iliev et al 2005), and since many minihalos may be photoevaporated by preheating prior to reionization (Oh & Haiman 2003).…”

Section: Model Dependencementioning

confidence: 99%

Detecting the Rise and Fall of 21 cm Fluctuations with the Murchison Widefield Array

Lidz

Zahn

McQuinn

et al. 2008

ApJ

176

280

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We forecast the sensitivity with which the Murchison Widefield Array (MWA) can measure the 21 cm power spectrum of cosmic hydrogen. The MWA is sensitive to roughly a decade in scale (wavenumbers of k $ 0:1Y1 h Mpc À1 ). This amounts primarily to constraints on two numbers: the amplitude and the slope of the 21 cm power spectrum on the scales probed. We find, however, that the redshift evolution in these quantities can yield important information about reionization. We examine a range of theoretical models, spanning uncertainties in the nature of the ionizing sources and the abundance of minihalos during reionization. Although the power spectrum differs substantially among these models, a generic prediction is that the amplitude of the 21 cm power spectrum on MWA scales (k $ 0:4 h Mpc À1 ) peaks near the epoch when the intergalactic medium (IGM) is %50% ionized. Moreover, the slope of the 21 cm power spectrum flattens as the ionization fraction increases and the sizes of the H ii regions grow. With regards to detection sensitivity, we show that the optimal MWA antenna configuration for power spectrum measurements would pack all 500 antenna tiles as closely as possible in a compact core. Detecting the characteristic redshift evolution of our models will help to confirm that observed 21 cm fluctuations originate from the IGM, and not from foregrounds, and will provide an indirect constraint on the evolution of the volume-filling factor of H ii regions during reionization. After two years of observations, the MWA can constrain the filling factor at an epoch when x i h i$ 0:5 to within roughly AE x i h i$ 0:1 at 2 confidence. Subject headingg s: cosmology: theory -intergalactic medium -large-scale structure of universe

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“…Shapiro et al 2004;Iliev et al 2005). To test the impact of reionization in our simulations we ran two different sets of models.…”

Section: Implementation Of Reionizationmentioning

confidence: 99%

Low-mass galaxy formation and the ionizing photon budget during reionization

Duffy

Wyithe

Mutch

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We use high-resolution simulations of cosmological volumes to model galaxy formation at high-redshift, with the goal of studying the photon budget for reionization. We demonstrate that galaxy formation models that include a strong, thermally coupled supernovae scheme reproduce current observations of star formation rates and specific star formation rates, both during and after the reionization era. These models produce enough UV photons to sustain reionization at z 8 (z 6) through a significant population of faint, unobserved, galaxies for an assumed escape fraction of 20% (5%). This predicted population is consistent with extrapolation of the faint end of observed UV luminosity functions. We find that heating from a global UV/X-ray background after reionization causes a dip in the total global star formation rate density in galaxies below the current observational threshold. Finally, while the currently observed specific star formation rates are incapable of differentiating between supernovae feedback models, sufficiently deep observations will be able to use this diagnostic in the future to investigate galaxy formation at high-redshift.

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Minihalo photoevaporation during cosmic reionization: evaporation times and photon consumption rates

Cited by 156 publications

References 29 publications

Direct collapse black hole formation from synchronized pairs of atomic cooling haloes

Direct collapse black hole formation from synchronized pairs of atomic cooling haloes

Detecting the Rise and Fall of 21 cm Fluctuations with the Murchison Widefield Array

Low-mass galaxy formation and the ionizing photon budget during reionization

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