Radiative feedback from high-mass X-ray binaries on the formation of the first galaxies and early reionization

Jeon, Myoungwon; Pawlik, Andreas H.; Milosavljević, Miloš

doi:10.1093/mnras/stu444

Cited by 102 publications

(118 citation statements)

References 203 publications

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“…The fact that we have not tuned any parameters in order to match these observations supports the view that current observations of metal absorbers do not require additional physical inputs such as metals or light from Population III stars (see also Kulkarni et al 2013) or a strong contribution from X-ray binaries to the UVB (Jeon et al 2014). …”

Section: Column Density Distributionsupporting

confidence: 58%

The reionization of carbon

Finlator

Thompson

Huang

et al. 2015

Monthly Notices of the Royal Astronomical Society

109

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Observations suggest that C II was more abundant than C IV in the intergalactic medium towards the end of the hydrogen reionization epoch (z ∼ 6). This transition provides a unique opportunity to study the enrichment history of intergalactic gas and the growth of the ionizing background (UVB) at early times. We study how carbon absorption evolves from z = 10-5 using a cosmological hydrodynamic simulation that includes a self-consistent multifrequency UVB as well as a well-constrained model for galactic outflows to disperse metals. Our predicted UVB is within ∼ 2-4× of that from Haardt & Madau (2012), which is fair agreement given the uncertainties. Nonetheless, we use a calibration in post-processing to account for Lyman-α forest measurements while preserving the predicted spectral slope and inhomogeneity. The UVB fluctuates spatially in such a way that it always exceeds the volume average in regions where metals are found. This implies both that a spatially-uniform UVB is a poor approximation and that metal absorption is not sensitive to the epoch when HII regions overlap globally even at column densites of 10 12 cm −2 . We find, consistent with observations, that the C II mass fraction drops to low redshift while C IV rises owing the combined effects of a growing UVB and continued addition of carbon in low-density regions. This is mimicked in absorption statistics, which broadly agree with observations at z = 6-3 while predicting that the absorber column density distributions rise steeply to the lowest observable columns. Our model reproduces the large observed scatter in the number of low-ionization absorbers per sightline, implying that the scatter does not indicate a partially-neutral Universe at z ∼ 6.

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Section: Column Density Distributionsupporting

confidence: 58%

The reionization of carbon

Finlator

Thompson

Huang

et al. 2015

Monthly Notices of the Royal Astronomical Society

109

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“…Evidently, we can conclude that there were already sufficiently enriched regions at high redshifts to explain the DLA metallicities, which in turn supports our metal enrichment model. accretion rates in Jeon et al (2014). The accreted mass per Pop III-forming minihalo is therefore given by…”

Section: Black Holes and Unresolved X-ray Backgroundmentioning

confidence: 99%

Constraining the primordial initial mass function with stellar archaeology

Hartwig

Bromm

Klessen

et al. 2015

Monthly Notices of the Royal Astronomical Society

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109

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We present a new near-field cosmological probe of the initial mass function (IMF) of the first stars. Specifically, we constrain the lower-mass limit of the Population III (Pop III) IMF with the total number of stars in large, unbiased surveys of the Milky Way. We model the early star formation history in a Milky Way-like halo with a semi-analytic approach, based on Monte-Carlo sampling of dark matter merger trees, combined with a treatment of the most important feedback mechanisms. Assuming a logarithmically flat Pop III IMF and varying its low mass limit, we derive the number of expected survivors of these first stars, using them to estimate the probability to detect any such Pop III fossil in stellar archaeological surveys. Following our analysis, the most promising region to find possible Pop III survivors is the stellar halo of the Milky Way, which is the best target for future surveys. We find that if no genuine Pop III survivor is detected in a sample size of 4 × 10 6 (2 × 10 7 ) halo stars with wellcontrolled selection effects, then we can exclude the hypothesis that the primordial IMF extended down below 0.8M ⊙ at a confidence level of 68% (99%). With the sample size of the Hamburg/ESO survey, we can tentatively exclude Pop III stars with masses below 0.65M ⊙ with a confidence level of 95%, although this is subject to significant uncertainties. To fully harness the potential of our approach, future large surveys are needed that employ uniform, unbiased selection strategies for high-resolution spectroscopic follow-up.

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“…Thanks to a photon packet merging technique in TRAPHIC, the computational cost is independent of the number of ionizing radiation sources, which enables large simulations considering many sources, and as presented here. The RT is controlled by a set of parameters, which we choose identical to those employed in Jeon et al (2014a), except that we here use two frequency bins, Nν = 2 instead of Nν = 4, with bounding energies located at [13.6 eV, 400 eV, 10 keV]. While the main focus of Jeon et al (2014a) is to investigate the impact of X-rays on the gas in haloes and IGM, requiring to track high energy photons denoted by the high characteristic frequencies, in this work we focus on the stellar feedback impact.…”

Section: Photoionization Feedbackmentioning

confidence: 99%

The first galaxies: simulating their feedback-regulated assembly

Jeon¹,

Bromm²,

Pawlik

et al. 2015

Mon. Not. R. Astron. Soc.

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We investigate the formation of a galaxy reaching a virial mass of ≈ 10 8 M at z ≈ 10 by carrying out a zoomed radiation-hydrodynamical cosmological simulation. This simulation traces Population III (Pop III) star formation, characterized by a modestly top-heavy initial mass function (IMF), and considers stellar feedback such as photoionization heating from Pop III and Population II (Pop II) stars, mechanical and chemical feedback from supernovae (SNe), and X-ray feedback from accreting black holes (BHs) and high-mass X-ray binaries (HMXBs). We self-consistently impose a transition in star formation mode from top-heavy Pop III to low-mass Pop II, and find that the star formation rate in the computational box is dominated by Pop III until z ∼ 13, and by Pop II thereafter. The simulated galaxy experiences bursty star formation, with a substantially reduced gas content due to photoionization heating from Pop III and Pop II stars, together with SN feedback. All the gas within the simulated galaxy is metal-enriched above 10 −5 Z , such that there are no remaining pockets of primordial gas. The simulated galaxy has an estimated observed flux of ∼ 10 −3 nJy, which is too low to be detected by the James Webb Space Telescope (JWST) without strong lensing amplification. We also show that our simulated galaxy is similar in terms of stellar mass to Segue 2, the least luminous dwarf known in the Local Group.

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Radiative feedback from high-mass X-ray binaries on the formation of the first galaxies and early reionization

Cited by 102 publications

References 203 publications

The reionization of carbon

The reionization of carbon

Constraining the primordial initial mass function with stellar archaeology

The first galaxies: simulating their feedback-regulated assembly

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