Essential physics of early galaxy formation

Dayal, Pratika; Ferrara, Andrea; Dunlop, James; Pacucci, Fabio

doi:10.1093/mnras/stu1848

Cited by 162 publications

(242 citation statements)

References 86 publications

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“…This last work is most similar in spirit to our approach, though it does not include gas loss from SN winds, which progressively decreases the gas fraction in galaxies as shown in Dayal et al (2014a). A major caveat in many of these existing works is their assumption of a cosmology-independent massto-light ratio (M/L) or ionizing photon production rate-to-mass ratio.…”

Section: Introductionmentioning

confidence: 94%

“…We now briefly summarize the theoretical model and interested readers are referred to Dayal et al (2014aDayal et al ( , 2014b for complete details. We construct 400 merger trees starting at z = 4, linearly distributed across the halo mass range…”

Section: Merger Trees and The Baryonic Implementationmentioning

confidence: 99%

“…Our model is based on the simple premise that any galaxy can form stars with a maximum efficiency ( * f ej ) that provides enough energy to expel all the remaining gas, quenching further star formation, up to a threshold value of f * (see Dayal et al 2014a). This implies that the effective star formation efficiency ( * f eff ) is the minimum between * f ej and f * .…”

Section: Merger Trees and The Baryonic Implementationmentioning

confidence: 99%

“…In this work, our aim is to revisit the constraints allowed on the WDM particle mass by combining these "galaxy" data sets with the latest limits on the cosmological electron scattering optical depth inferred by Planck. We build upon a semi-analytic model that traces both the DM and baryonic assembly of high-z (;5-15) galaxies, reproducing a number of key observables, presented in Dayal et al (2014aDayal et al ( , 2014b to show how the reionization history and sources depend on the DM model considered. The strength of the model lies in the fact that in addition to internal feedback from SN (see Section2.…”

Section: Introductionmentioning

confidence: 99%

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Reionization and Galaxy Formation in Warm Dark Matter Cosmologies

Dayal

Choudhury

Bromm

et al. 2017

ApJ

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We compare model results from a semi-analytic (merger-tree based) framework for high-redshift (z;5-20) galaxy formation against reionization indicators, including the Planck electron scattering optical depth (τ es ) and the ionizing photon emissivity (ṅ ion ), to shed light on the reionization history and sources in Cold (CDM) and Warm Dark Matter (WDM; particle masses of m x =1.5, 3, and 5 keV) cosmologies. This model includes all ofthe key processes of star formation, supernova feedback, the merger/accretion/ejectiondriven evolution of gas and stellar mass and the effect of the ultra-violet background (UVB), created during reionization, in photo-evaporating the gas content of galaxies in halos with M h 10 9  M . We find that the delay in the start of reionization in light (1.5 keV) WDM models can be compensated by a steeper redshift evolution of the ionizing photon escape fraction and a faster mass assembly, resulting in reionization ending at comparable redshifts (z;5.5) in all the dark matter models considered. We find thatthe bulk of the reionization photons come from galaxies with a halo mass of M h 10 9  M and a UV magnitude of −15M UV −10 in CDM. The progressive suppression of low-mass halos with decreasing m x leads to a shift in the "reionization" population to larger halo masses of M h 10 9  M and −17M UV −13 for 1.5 keV WDM. We find that current observations of τ es and the ultra violet luminosity function are equally compatible with all the (cold and warm) dark matter models considered in this work. Quantifying the impact of the UVB on galaxy observables (luminosity functions, stellar mass densities, andstellar to halo mass ratios) for different DM models, we propose that global indicators including the redshift evolution of the stellar mass density and the stellar mass-halo mass relation, observable with the James Webb Space Telescope, can be used to distinguish between CDM and WDM (1.5 keV) cosmologies.

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Section: Introductionmentioning

confidence: 94%

Section: Merger Trees and The Baryonic Implementationmentioning

confidence: 99%

Section: Merger Trees and The Baryonic Implementationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Reionization and Galaxy Formation in Warm Dark Matter Cosmologies

Dayal

Choudhury

Bromm

et al. 2017

ApJ

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“…Lacey et al 2011;Muñoz 2012;Jaacks et al 2013;Behroozi & Silk 2014;Dayal et al 2014;Mashian et al 2015). However, the earlier implementations had two limitations.…”

Section: Introductionmentioning

confidence: 99%

The Galaxy UV Luminosity Function Before the Epoch of Reionization

Mason

Trenti²,

Treu

2015

Proc. IAU

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We present a model for the evolution of the galaxy ultraviolet (UV) luminosity function (LF) across cosmic time where star formation is linked to the assembly of dark matter halos under the assumption of a mass dependent, but redshift independent, efficiency. We introduce a new self-consistent treatment of the halo star formation history, which allows us to make predictions at z > 10 (lookback time ∼ < 500 Myr), when growth is rapid. With a calibration at a single redshift to set the stellar-to-halo mass ratio, and no further degrees of freedom, our model captures the evolution of the UV LF over all available observations (0 ∼ < z ∼ < 10). The significant drop in luminosity density of currently detectable galaxies beyond z ∼ 8 is explained by a shift of star formation toward less massive, fainter galaxies. Assuming that star formation proceeds down to atomic cooling halos, we derive a reionization optical depth τ = 0.056 +0.007 −0.010 , fully consistent with the latest Planck measurement, implying that the universe is fully reionized at z = 7.84 +0.65 −0.98 . In addition, our model naturally produces smoothly rising star formation histories for galaxies with L ∼ < L * in agreement with observations and hydrodynamical simulations. Before the epoch of reionization at z > 10 we predict the LF to remain well-described by a Schechter function, but with an increasingly steep faint-end slope (α ∼ −3.5 at z ∼ 16). Finally, we construct forecasts for surveys with JWST and WFIRST and predict that galaxies out to z ∼ 14 will be observed. Galaxies at z > 15 will likely be accessible to JWST and WFIRST only through the assistance of strong lensing magnification.

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Modeling cosmic reionization

Gnedin

Madau

2022

Living Rev Comput Astrophys

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The transformation of cold neutral intergalactic hydrogen into a highly ionized warm plasma marks the end of the cosmic dark ages and the beginning of the age of galaxies. The details of this process reflect the nature of the early sources of radiation and heat, the statistical characteristics of the large-scale structure of the Universe, the thermodynamics and chemistry of cosmic baryons, and the histories of star formation and black hole accretion. A number of massive data sets from new ground- and space-based instruments and facilities over the next decade are poised to revolutionize our understanding of primeval galaxies, the reionization photon budget, the physics of the intergalactic medium (IGM), and the fine-grained properties of hydrogen gas in the “cosmic web”. In this review, we survey the physics and key aspects of reionization-era modeling and describe the diverse range of computational techniques and tools currently available in this field.

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Essential physics of early galaxy formation

Cited by 162 publications

References 86 publications

Reionization and Galaxy Formation in Warm Dark Matter Cosmologies

Reionization and Galaxy Formation in Warm Dark Matter Cosmologies

The Galaxy UV Luminosity Function Before the Epoch of Reionization

Modeling cosmic reionization

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