The bright end of the galaxy luminosity function at z≃7: before the onset of mass quenching?

Bowler, R. A. A.; Dunlop, James; McLure, R. J.; Rogers, A. B.; McCracken, H. J.; Milvang-Jensen, B.; Furusawa, Hisanori; Fynbo, J. P. U.; Taniguchi, Yoshiaki; Afonso, J.; Bremer, M.; Fèvre, O. Le

doi:10.1093/mnras/stu449

Cited by 215 publications

(509 citation statements)

References 105 publications

(148 reference statements)

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“…2.1. Further, our model naturally predicts that the brightend of the UV LF at z 7 must be flatter than the usuallyassumed Schechter function and is compatible with both the HMF and the double power-law (DPL) slope estimated from the widest-area survey carried out so far at this redshift (Bowler et al 2014). Our model slightly over-predicts the number of bright galaxies at z 5 and z 6, as can be seen from the same figure.…”

Section: Understanding the Uv Lf Evolutionsupporting

confidence: 75%

“…Bouwens et al 2007;McLure et al 2009;Bouwens et al 2010a;McLure et al 2010;Oesch et al 2010b;McLure et al 2013) while ground-based widefield surveys such as UltraVISTA are revealing luminous galaxies populating the bright-end of the UV LF at z 7 (e.g. Ouchi et al 2010;Bowler et al 2012Bowler et al , 2014. Spectral energy distribution (SED) fitting to broad-band photometry has also been used to build galaxy stellar mass functions (SMF; González et al 2011), understand the stellar populations in these sources through their UV (β) slopes (Bouwens et al 2010b;Finkelstein et al 2012;Wilkins et al 2011;Dunlop et al 2012Dunlop et al , 2013Bouwens et al 2013;Rogers et al 2014), infer their physical properties (Oesch et al 2010a;Labbé et al 2010a;McLure et al 2011;Labbé et al 2013) and calculate the growth of stellar mass density (SMD) with redshift (Labbé et al 2010a;González et al 2011;Stark et al 2013).…”

Section: Introductionmentioning

confidence: 99%

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Essential physics of early galaxy formation

Dayal

Ferrara

Dunlop

et al. 2014

Monthly Notices of the Royal Astronomical Society

161

209

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We present a theoretical model embedding the essential physics of early galaxy formation (z 5 − 12) based on the single premise that any galaxy can form stars with a maximal limiting efficiency that provides enough energy to expel all the remaining gas, quenching further star formation. This simple idea is implemented into a merger-tree based semi-analytical model that utilises two mass and redshiftindependent parameters to capture the key physics of supernova feedback in ejecting gas from low-mass halos, and tracks the resulting impact on the subsequent growth of more massive systems via halo mergers and gas accretion. Our model shows that: (i) the smallest halos (halo mass M h 10 10 M ) build up their gas mass by accretion from the intergalactic medium; (ii) the bulk of the gas powering star formation in larger halos (M h 10 11.5 M ) is brought in by merging progenitors; (iii) the faint-end UV luminosity function slope evolves according to α = −1.75 log z − 0.52. In addition, (iv) the stellar mass-to-light ratio is well fit by the functional form log M * = −0.38M U V − 0.13 z + 2.4, which we use to build the evolving stellar mass function to compare to observations. We end with a census of the cosmic stellar mass density (SMD) across galaxies with UV magnitudes over the range −23 M U V −11 spanning redshifts 5 < z < 12: (v) while currently detected LBGs contain ≈ 50% (10%) of the total SMD at z = 5 (8), the JWST will detect up to 25% of the SMD at z 9.5.

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Section: Understanding the Uv Lf Evolutionsupporting

confidence: 75%

Section: Introductionmentioning

confidence: 99%

Essential physics of early galaxy formation

Dayal

Ferrara

Dunlop

et al. 2014

Monthly Notices of the Royal Astronomical Society

161

209

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“…Figure 7. At z;7 and 8, the faint end (M UV −16) data has been collected using the lensed Hubble Frontier fields (HFF; Atek et al 2015;Livermore et al 2016), while the brightest galaxies have been detected using ground-based Ultra-Vista surveys (e.g., Bradley et al 2014;Bowler et al 2014); (unlensed) HST data has been used to obtain the z;9 UV LF as shown in the same figure.…”

Section: Faint End Of the Uv Luminosity Functionsmentioning

confidence: 99%

“…Over the past few years, ground-and space-based observations have allowed a statistically significant data set to be collected for z;6-10 Lyman Break galaxies (LBGs; Bouwens et al 2010Bouwens et al , 2011Bouwens et al , 2015bCastellano et al 2010;McLure et al 2010McLure et al , 2013Oesch et al 2010Oesch et al , 2013Oesch et al , 2016Bradley et al 2012;Bowler et al 2014Bowler et al , 2015Atek et al 2015;Livermore et al 2016). 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.…”

Section: Introductionmentioning

confidence: 99%

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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“…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%

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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The bright end of the galaxy luminosity function at z≃7: before the onset of mass quenching?

Cited by 215 publications

References 105 publications

Essential physics of early galaxy formation

Essential physics of early galaxy formation

Reionization and Galaxy Formation in Warm Dark Matter Cosmologies

The Galaxy UV Luminosity Function Before the Epoch of Reionization

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