The Evolution of the Galaxy Rest-Frame Ultraviolet Luminosity Function Over the First Two Billion Years

Finkelstein, Steven L.; Ryan, Russell E.; Papovich, Casey; Dickinson, Mark; Song, Mimi; Somerville, Rachel S.; Ferguson, Henry C.; Salmon, Brett; Giavalisco, Mauro; Koekemoer, Anton M.; Ashby, M. L. N.; Behroozi, Peter; Castellano, M.; Dunlop, James; Faber, S. M.; Fazio, G. G.; Fontana, A.; Grogin, Norman A.; Hathi, N. P.; Jaacks, Jason; Kocevski, Dale D.; Livermore, Rachael; McLure, R. J.; Merlin, E.; Mobasher, Bahram; Newman, Jeffrey A.; Rafelski, Marc; Tilvi, Vithal; Willner, S. P.

doi:10.1088/0004-637x/810/1/71

Cited by 701 publications

(1,102 citation statements)

References 169 publications

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“…The model is remarkably consistent with the observed data (Arnouts et al 2005;Oesch et al 2010;Oesch et al 2013bOesch et al , 2014Alavi et al 2014;Bowler et al 2015;Finkelstein et al 2015b;Bouwens et al 2015b,a), which is expected due to the success of our previous implementation of this class of models (Tacchella et al 2013;Trenti et al 2010Trenti et al , 2015. We find the model marginally overpredicts the bright end of the LF at z ∼ 0.3 and z ∼ 2 by ∼ 0.1 dex due to the difficulty in modeling dust extinction at these redshifts, but the observations are still within 2σ of our model.…”

Section: Luminosity Functions and Sfr Densitysupporting

confidence: 89%

“…At z > 7, the model describes the most recent observed data (Oesch et al 2013bFinkelstein et al 2015b;Bouwens et al 2015b,a) well, validating our simple approach. Our model predicts the trend of steepening faint-end slope to continue at z > 10, and number densities to drop rapidly.…”

Section: Luminosity Functions and Sfr Densitysupporting

confidence: 85%

“…The best-fit parameters are in good agreement with observations (Schmidt et al 2014;Bowler et al 2015;Oesch et al 2010;Finkelstein et al 2015b;Bouwens et al 2015b) given the large degeneracies in Schechter function parameters. Encouragingly, we find the evolution of the derived Schechter parameters is in excellent agreement with the observed evolution (Bouwens et al 2015b;Bowler et al 2015): we find dα/dz ∼ −0.1, dM * /dz ∼ 0.1, and d log(Φ * )/dz ∼ −0.3 between z ∼ 4 and z ∼ 8.…”

Section: Luminosity Functions and Sfr Densitysupporting

confidence: 79%

“…However, other studies find either an equally good fit with a double-power law at z ∼ 8 (Finkelstein et al 2015b), or a preference for the double power law at z ∼ 7 (Bowler et al 2014;Bowler et al 2015; but note that the z ∼ 7 investigations are based on ground, rather than space observations). Irrespective of the form of the LF at the bright-end, whose evolution might be linked to changing astrophysical conditions of high-redshift galaxies, such as reduced feedback at early times (Somerville et al 2008), it is clear that overall, the observed population of galaxies (M AB ∼ < − 17) at z > 7 does not produce sufficient photons to ionize the universe.…”

Section: Introductionmentioning

confidence: 96%

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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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Section: Luminosity Functions and Sfr Densitysupporting

confidence: 89%

Section: Luminosity Functions and Sfr Densitysupporting

confidence: 85%

Section: Luminosity Functions and Sfr Densitysupporting

confidence: 79%

Section: Introductionmentioning

confidence: 96%

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The Galaxy UV Luminosity Function Before the Epoch of Reionization

Mason

Trenti²,

Treu

2015

Proc. IAU

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“…The HFF project has been remarkably prolific, with contributions in the structure of galaxy clusters (Jauzac et al 2014;Richard et al 2014;Ogrean et al 2015;Jauzac et al 2015), individual high redshift galaxies (McLeod et al 2015;Kawamata et al 2015;Laporte et al 2016), and high redshift galaxy luminosity function and its evolution (Finkelstein et al 2015;Coe et al 2015;Atek et al 2015) 1 .…”

Section: Introductionmentioning

confidence: 99%

Lens models under the microscope: comparison ofHubble Frontier Fieldcluster magnification maps

Priewe

Williams

Liesenborgs

et al. 2016

Mon. Not. R. Astron. Soc.

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Using the power of gravitational lensing magnification by massive galaxy clusters, the Hubble Frontier Fields provide deep views of six patches of the high redshift Universe. The combination of deep Hubble imaging and exceptional lensing strength has revealed the greatest numbers of multiply-imaged galaxies available to constrain models of cluster mass distributions. However, even with O(100) images per cluster, the uncertainties associated with the reconstructions are not negligible. The goal of this paper is to show the diversity of model magnification predictions. We examine 7 and 9 mass models of Abell 2744 and MACS J0416, respectively, submitted to the Mikulski Archive for Space Telescopes for public distribution in September 2015. The dispersion between model predictions increases from 30% at common low magnifications (µ ∼ 2) to 70% at rare high magnifications (µ ∼ 40). MACS J0416 exhibits smaller dispersions than Abell 2744 for 2 < µ < 10. We show that magnification maps based on different lens inversion techniques typically differ from each other by more than their quoted statistical errors. This suggests that some models underestimate the true uncertainties, which are primarily due to various lensing degeneracies. Though the exact mass sheet degeneracy is broken, its generalized counterpart is not broken at least in Abell 2744. Other, local degeneracies are also present in both clusters. Our comparison of models is complementary to the comparison of reconstructions of known synthetic mass distributions. By focusing on observed clusters, we can identify those that are best constrained, and therefore provide the clearest view of the distant Universe.

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Physics of the Intergalactic Medium During the Epoch of Reionization

Lidz

2016

Understanding the Epoch of Cosmic Reionization

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A major goal of observational and theoretical cosmology is to observe the largely unexplored time period in the history of our universe when the first galaxies form, and to interpret these measurements. Early galaxies dramatically impacted the gas around them in the surrounding intergalactic medium (IGM) by photoionzing the gas during the "Epoch of Reionization" (EoR). This epoch likely spanned an extended stretch in cosmic time: ionized regions formed and grew around early generations of galaxies, gradually filling a larger and larger fraction of the volume of the universe. At some time -thus far uncertain, but within the first billion years or so after the big bang -essentially the entire volume of the universe became filled with ionized gas. The properties of the IGM provide valuable information regarding the formation time and nature of early galaxy populations, and many approaches for studying the first luminous sources are hence based on measurements of the surrounding intergalactic gas. The prospects for improved reionization-era observations of the IGM and early galaxy populations over the next decade are outstanding. Motivated by this, we review the current state of models of the IGM during reionization. We focus on a few key aspects of reionization-era phenomenology and describe: the redshift evolution of the volume-averaged ionization fraction, the properties of the sources and sinks of ionizing photons, along with models describing the spatial variations in the ionization fraction, the ultraviolet radiation field, the temperature of the IGM, and the gas density distribution.

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The Evolution of the Galaxy Rest-Frame Ultraviolet Luminosity Function Over the First Two Billion Years

Cited by 701 publications

References 169 publications

The Galaxy UV Luminosity Function Before the Epoch of Reionization

The Galaxy UV Luminosity Function Before the Epoch of Reionization

Lens models under the microscope: comparison ofHubble Frontier Fieldcluster magnification maps

Physics of the Intergalactic Medium During the Epoch of Reionization

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