Semi-analytic forecasts forJWST– I. UV luminosity functions atz = 4–10

Yung, L. Y. Aaron; Somerville, Rachel S.; Finkelstein, Steven L.; Popping, Gergö; Davé, Romeel

doi:10.1093/mnras/sty3241

Cited by 178 publications

(202 citation statements)

References 199 publications

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“…In the literature, dust optical depths are often linked to the gas column density, which is then converted to the dust column density using the dust-to-gas (DTG) ratio (De Lucia & Blaizot 2007;Guo et al 2011;Somerville et al 2012;Yung et al 2019). In this model, optical depths are expressed by…”

Section: Dust-to-gas Ratio Modelmentioning

confidence: 99%

Dark-age reionization and galaxy formation simulation – XIX. Predictions of infrared excess and cosmic star formation rate density from UV observations

Qiu

Mutch

Cunha

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present a new analysis of high-redshift UV observations using a semi-analytic galaxy formation model, and provide self-consistent predictions of the infrared excess (IRX) -β relations and cosmic star formation rate density. We combine the Charlot & Fall dust attenuation model with the meraxes semi-analytic model, and explore three different parametrisations for the dust optical depths, linked to star formation rate, dust-to-gas ratio and gas column density respectively. A Bayesian approach is employed to statistically calibrate model free parameters including star formation efficiency, mass loading factor, dust optical depths and reddening slope directly against UV luminosity functions and colour-magnitude relations at z ∼ 4 − 7. The best-fit models show excellent agreement with the observations. We calculate IRX using energy balance arguments, and find that the large intrinsic scatter in the IRX -β plane is driven by the specific star formation rate. Additionally, the difference among the three dust models suggests a factor of two systematic uncertainty in the dust-corrected star formation rate when using the Meurer IRX -β relation at z 4.

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Section: Dust-to-gas Ratio Modelmentioning

confidence: 99%

Dark-age reionization and galaxy formation simulation – XIX. Predictions of infrared excess and cosmic star formation rate density from UV observations

Qiu

Mutch

Cunha

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…For z = 6 − 9, the data (at M UV ≥ −17) is from the analysis of HFF program applying the gravitational lensing techniques (Atek et al 2015(Atek et al , 2018Livermore et al 2017;Ishigaki et al 2018). We use Livermore's Eddington-corrected data points shown in Yung et al (2019b). yielded intriguing results for the faint-end LF observations. In particular, the HFF program has been able to identify sources that are intrinsically fainter than the limits of the current unlensed surveys, extending the observed UV LFs to M UV ∼ -13 − -15 (Atek et al 2015;Livermore et al 2017;Ishigaki et al 2018).…”

Section: Galaxy Luminosity Functionmentioning

confidence: 99%

“…In Fig. 13, the horizontal lines indicate the median (the solid lines), 1σ, 2σ, and 3σ lower bounds (the dash, the dotted, and the dashdotted lines) of n obs obtained from Atek et al (2018) at z = 6 (left panel) and Livermore et al (2017) (Eddington-corrected version from Yung et al (2019b)) at z = 7 (right panel). The data points marked by the red cross are cumulative number densities (n M UV ) obtained from different FDM simulations, while CDM models are indicated by the rightmost points.…”

Section: Comparison With Observationsmentioning

confidence: 99%

“…However, we also note that it is possible that the predictions for the UV LFs might be affected by different sub-grid physical models. For example, recently Yung et al (2019b) have explored how different galaxy formation recipes (in semi-analytic models) can influence faint-end LFs. In this section, we broadly test some of the effects of a few different sub-grid models and examine whether the details of sub-grid models may potentially lead to weaker constraints on FDM.…”

Section: Possible Effects From the Sub-grid Modelingmentioning

confidence: 99%

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Predictions for the abundance of high-redshift galaxies in a fuzzy dark matter universe

Feng

Matteo

2019

Monthly Notices of the Royal Astronomical Society

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During the last decades, rapid progress has been made in measurements of the rest-frame ultraviolet (UV) luminosity function (LF) for high-redshift galaxies (z ≥ 6). The faint-end of the galaxy LF at these redshifts provides powerful constraints on different dark matter models that suppress small-scale structure formation. In this work we perform full hydrodynamical cosmological simulations of galaxy formation using an alternative DM model composed of extremely light bosonic particles (m ∼ 10 −22 eV), also known as fuzzy dark matter (FDM), and examine the predictions for the galaxy stellar mass function and luminosity function at z ≥ 6 for a range of FDM masses. We find that for FDM models with bosonic mass m = 5 × 10 −22 eV, the number density of galaxies with stellar mass M * ∼ 10 7 M is suppressed by ∼ 40% at z = 9, ∼ 20% at z = 5, and the UV LFs within magnitude range of -16 < M UV < -14 is suppressed by ∼ 60% at z = 9, ∼ 20% at z = 5 comparing to the CDM counterpart simulation. Comparing our predictions with current measurements of the faint-end LFs (−18 M UV −14), we find that FDM models with m 22 < 5 × 10 −22 are ruled out at 3σ confidence level. We expect that future LF measurements by James Webb Space Telescope (JWST), which will extend down to M UV ∼ −13 for z 10, with a survey volume that is comparable to the Hubble Ultra Deep Field (HUDF) would have the capability to constrain FDM models to m 10 −21 eV.

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“…In recent years, a number of such 'JWST prediction' papers have appeared, typically analysing mock JWST catalogues built using semi-analytic models, or numerical cosmological hydrodynamical simulations of galaxy formation and evolution (e.g. FIBY Paardekooper et al 2013, Blue-Tides Feng et al 2016Wilkins et al 2017, GALFORM Lacey et al 2016, Barrow et al 2017, Lovell et al 2018, Yung et al 2019.…”

Section: Introductionmentioning

confidence: 99%

Maximizing the power of deep extragalactic imaging surveys with the James Webb Space Telescope

Kemp

Dunlop

McLure

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present a new analysis of the potential power of deep, near-infrared, imaging surveys with the James Webb Space Telescope (JWST) to improve our knowledge of galaxy evolution. In this work we properly simulate what can be achieved with realistic survey strategies, and utilise rigorous signal:noise calculations to calculate the resulting posterior constraints on the physical properties of galaxies. We explore a broad range of assumed input galaxy types (> 20,000 models, including extremely dusty objects) across a wide redshift range (out to z 12), while at the same time considering a realistic mix of galaxy properties based on our current knowledge of the evolving population (as quantified through the Empirical Galaxy Generator: EGG). While our main focus is on imaging surveys with NIRCam, spanning λ obs = 0.8−5.0 µm, an important goal of this work is to quantify the impact/added-value of: i) parallel imaging observations with MIRI at longer wavelengths, and ii) deeper supporting optical/UV imaging with HST (potentially prior to JWST launch) in maximising the power and robustness of a major extragalactic NIRCam survey. We show that MIRI parallel 7.7-µm imaging is of most value for better constraining the redshifts and stellar masses of the dustiest (A V > 3) galaxies, while deep B-band imaging (reaching 28.5 AB mag) with ACS on HST is vital for determining the redshifts of the large numbers of faint/low-mass, z < 5 galaxies that will be detected in a deep JWST NIRCam survey.

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Semi-analytic forecasts forJWST– I. UV luminosity functions atz = 4–10

Cited by 178 publications

References 199 publications

Dark-age reionization and galaxy formation simulation – XIX. Predictions of infrared excess and cosmic star formation rate density from UV observations

Dark-age reionization and galaxy formation simulation – XIX. Predictions of infrared excess and cosmic star formation rate density from UV observations

Predictions for the abundance of high-redshift galaxies in a fuzzy dark matter universe

Maximizing the power of deep extragalactic imaging surveys with the James Webb Space Telescope

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