<i>z</i>∼ 7 GALAXIES IN THE HUDF: FIRST EPOCH WFC3/IR RESULTS

Oesch, Pascal; Bouwens, Rychard; Illingworth, G. D.; Carollo, C. M.; Franx, Marijn; Labbé, Ivo; Magee, D.; Stiavelli, M.; Trenti, Michele; Dokkum, Pieter van

doi:10.1088/2041-8205/709/1/l16

Cited by 283 publications

(542 citation statements)

References 38 publications

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“…This is determined by observed rest-frame ultraviolet luminosity functions (e.g. Bouwens et al, 2006;Reddy et al, 2008;Oesch et al, 2010) at high redshift and the observed main sequence (Noeske et al, 2007b;Stark et al, 2013).…”

Section: Relationship To Normal Galaxies: the Infrared Main Sequencementioning

confidence: 97%

Dusty star-forming galaxies at high redshift

2014

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Far-infrared and submillimeter wavelength surveys have now established the important role of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of massive galaxies in the Universe. The brightest of these galaxies have infrared luminosities in excess of 10 13 L with implied star-formation rates of thousands of solar masses per year. They represent the most intense starbursts in the Universe, yet many are completely optically obscured. Their easy detection at submm wavelengths is due to dust heated by ultraviolet radiation of newly forming stars. When summed up, all of the dusty, star-forming galaxies in the Universe produce an infrared radiation field that has an equal energy density as the direct starlight emission from all galaxies visible at ultraviolet and optical wavelengths. The bulk of this infrared extragalactic background light emanates from galaxies as diverse as gas-rich disks to mergers of intense starbursting galaxies. Major advances in far-infrared instrumentation in recent years, both spacebased and ground-based, has led to the detection of nearly a million DSFGs, yet our understanding of the underlying astrophysics that govern the start and end of the dusty starburst phase is still in nascent stage. This review is aimed at summarizing the current status of DSFG studies, focusing especially on the detailed characterization of the bestunderstood subset (submillimeter galaxies, who were summarized in the last review of this field over a decade ago, Blain et al. 2002), but also the selection and characterization of more recently discovered DSFG populations. We review DSFG population statistics, their physical properties including dust, gas and stellar contents, their environments, and current theoretical models related to the formation and evolution of these galaxies.

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Section: Relationship To Normal Galaxies: the Infrared Main Sequencementioning

confidence: 97%

Dusty star-forming galaxies at high redshift

2014

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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

152

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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z∼ 7 GALAXIES IN THE HUDF: FIRST EPOCH WFC3/IR RESULTS

Cited by 283 publications

References 38 publications

Dusty star-forming galaxies at high redshift

Dusty star-forming galaxies at high redshift

Reionization and Galaxy Formation in Warm Dark Matter Cosmologies

Essential physics of early galaxy formation

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