A new multifield determination of the galaxy luminosity function at z = 7–9 incorporating the 2012 Hubble Ultra-Deep Field imaging

McLure, R. J.; Dunlop, James; Bowler, R. A. A.; Curtis-Lake, Emma; Schenker, Matthew A.; Ellis, Richard S.; Robertson, Brant; Koekemoer, Anton M.; Rogers, A. B.; Ono, Yoshiyasu; Ouchi, Masami; Charlot, S.; Wild, Vivienne; Stark, Daniel P.; Furlanetto, Steven R.; Cirasuolo, M.; Targett, T. A.

doi:10.1093/mnras/stt627

Cited by 387 publications

(446 citation statements)

References 58 publications

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“…Bouwens et al (2014) and two, the reionization history of the universe through the Thomson scattering optical depth to reionization, τ , measured from large-angle CMB polarization by WMAP (Bennett et al 2013). 5 The extremely deep imaging in bandpasses from the optical to near-IR with the Hubble Space Telescope (HST ) available in several Legacy Fields provides the most fundamental data set for constraining the contribution of galaxies to the reionization of the universe through estimation of the rest-frame UV-luminosity function over the redshift range between z = 4 and 10 (Bouwens et al 2011(Bouwens et al , 2014Oesch et al 2012;Lorenzoni et al 2013;McLure et al 2013). The rest-frame UV-luminosity function is a measure of the number density, per absolute magnitude, of the star-forming galax-4 Another probe that can constrain non-linear scales is galaxy weak lensing, for example through the anticipated data sets from Euclid (Laureijs et al 2011;Amendola et al 2013).…”

Section: The Uv-luminosity Function and Reionizationmentioning

confidence: 99%

Galaxy UV-luminosity function and reionization constraints on axion dark matter

Bozek¹,

Marsh²,

Silk³

et al. 2015

Monthly Notices of the Royal Astronomical Society

173

208

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If the dark matter (DM) were composed of axions, then structure formation in the Universe would be suppressed below the axion Jeans scale. Using an analytic model for the halo mass function of a mixed DM model with axions and cold dark matter, combined with the abundance-matching technique, we construct the UV-luminosity function. Axions suppress high-z galaxy formation and the UV-luminosity function is truncated at a faintest limiting magnitude. From the UV-luminosity function, we predict the reionization history of the universe and find that axion DM causes reionization to occur at lower redshift. We search for evidence of axions using the Hubble Ultra Deep Field UV-luminosity function in the redshift range z = 6-10, and the optical depth to reionization, τ , as measured from cosmic microwave background polarization. All probes we consider consistently exclude m a 10 −23 eV from contributing more than half of the DM, with our strongest constraint ruling this model out at more than 8σ significance. In conservative models of reionization a dominant component of DM with m a = 10 −22 eV is in 3σ tension with the measured value of τ , putting pressure on an axion solution to the cusp-core problem. Tension is reduced to 2σ for the axion contributing only half of the DM. A future measurement of the UV-luminosity function in the range z = 10-13 by JWST would provide further evidence for or against m a = 10 −22 eV. Probing still higher masses of m a = 10 −21 eV will be possible using future measurements of the kinetic Sunyaev-Zel'dovich effect by Advanced ACTPol to constrain the time and duration of reionization.

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Section: The Uv-luminosity Function and Reionizationmentioning

confidence: 99%

Galaxy UV-luminosity function and reionization constraints on axion dark matter

Bozek¹,

Marsh²,

Silk³

et al. 2015

Monthly Notices of the Royal Astronomical Society

173

208

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“…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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“…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.…”

Section: Introductionmentioning

confidence: 99%

Essential physics of early galaxy formation

Dayal

Ferrara

Dunlop

et al. 2014

Monthly Notices of the Royal Astronomical Society

162

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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A new multifield determination of the galaxy luminosity function at z = 7–9 incorporating the 2012 Hubble Ultra-Deep Field imaging

Cited by 387 publications

References 58 publications

Galaxy UV-luminosity function and reionization constraints on axion dark matter

Galaxy UV-luminosity function and reionization constraints on axion dark matter

Reionization and Galaxy Formation in Warm Dark Matter Cosmologies

Essential physics of early galaxy formation

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