Star Formation for Predictive Primordial Galaxy Formation

Milosavljević, Miloš; Safranek-Shrader, Chalence

doi:10.1007/978-3-319-21957-8_3

Cited by 2 publications

(1 citation statement)

References 305 publications

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“…With these facilities on the near horizon, it is a particularly valuable time to summarize the physical picture that has emerged following the past five years of observations. This manuscript builds on the review of and complements several recent theoretical reviews on reionization (e.g., Lidz 2016) and early galaxy formation (e.g., Bromm & Yoshida 2011, Milosavljević & Safranek-Shrader 2016. The plan is as follows.…”

Section: Introductionmentioning

confidence: 99%

Galaxies in the First Billion Years After the Big Bang

Stark

2016

Annu. Rev. Astron. Astrophys.

269

158

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In the past five years, deep imaging campaigns conducted with the Hubble Space Telescope (HST) and ground-based observatories have delivered large samples of galaxies at 6.5<z<10, providing our first glimpse of the census of star formation activity in what is thought to be the heart of the reionization era. The space density of luminous galaxies has been shown to decrease by 15–20× over 4<z<8. Over this same redshift interval, the faint-end slope of the UV luminosity function becomes steeper (α≃−2.0 at z≃7−8), revealing a dominant population of low-luminosity galaxies. Analysis of multiwavelength imaging from HST and the Spitzer Space Telescope demonstrates that z>6 UV-selected galaxies are relatively compact with blue UV continuum slopes, low stellar masses, and large specific star formation rates. In the last year, ALMA (the Atacama Large Millimeter Array) and ground-based infrared spectrographs have begun to complement this picture, revealing minimal dust obscuration and hard radiation fields, and providing evidence for metal-poor ionized gas. Weak low-ionization absorption lines suggest a patchy distribution of neutral gas surrounds O and B stars, possibly aiding in the escape of ionizing radiation. Gamma ray burst afterglows and Lyman-α surveys have provided evidence that the intergalactic medium (IGM) evolves from mostly ionized at z≃6−6.5 ([Formula: see text]) to considerably neutral at z≃7−8 ([Formula: see text]). The reionization history that emerges from considering the UV output of galaxies over 6<z<10 is consistent with these constraints on the IGM ionization state. The latest measurements suggest that galaxies can complete reionization by z≃6 and reproduce the Thomson scattering optical depth faced by cosmic microwave background photons if the luminosity function extends ≃4 mag below current surveys and a moderate fraction ([Formula: see text]) of ionizing radiation escapes from galaxies.

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Section: Introductionmentioning

confidence: 99%

Galaxies in the First Billion Years After the Big Bang

Stark

2016

Annu. Rev. Astron. Astrophys.

269

158

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Towardsab initioextremely metal-poor stars

Ritter¹,

Safranek-Shrader²,

Milosavljević³

2016

Mon. Not. R. Astron. Soc.

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Extremely metal poor stars have been the focus of much recent attention owing to the expectation that their chemical abundances can shed light on the metal and dust yields of the earliest supernovae. We present our most realistic simulation to date of the astrophysical pathway to the first metal enriched stars. We simulate the radiative and supernova hydrodynamic feedback of a 60 M Population III star starting from cosmological initial conditions realizing Gaussian density fluctuations. We follow the gravitational hydrodynamics of the supernova remnant at high spatial resolution through its freely-expanding, adiabatic, and radiative phases, until gas, now metal-enriched, has resumed runaway gravitational collapse. Our findings are surprising: while the Population III progenitor exploded with a low energy of 10 51 erg and injected an ample metal mass of 6 M , the first cloud to collapse after the supernova explosion is a dense surviving primordial cloud on which the supernova blast wave deposited metals only superficially, in a thin, unresolved layer. The first metal-enriched stars can form at a very low metallicity, of only 2 − 5 × 10 −4 Z , and can inherit the parent cloud's highly elliptical, radially extended orbit in the dark matter gravitational potential.

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Star Formation for Predictive Primordial Galaxy Formation

Cited by 2 publications

References 305 publications

Galaxies in the First Billion Years After the Big Bang

Galaxies in the First Billion Years After the Big Bang

Towardsab initioextremely metal-poor stars

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