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Wilkins, David E.; Shemmings, David; Shemmings, Yvonne

doi:10.1057/978-1-137-00827-5_17

Cited by 4 publications

(6 citation statements)

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“…At z = 12 the number of objects identified falls to around 20 million, and only around 700 have stellar masses greater than 10 8 M . The galaxy stellar mass and rest-frame UV luminosity functions predicted by the simulation (see Feng et al 2016;Wilkins et al 2016) match observational constraints available at z ≈ 8 (e.g. Bouwens, Oesch, Labbe 2015a;Song, Finkelstein, Ashby 2015).…”

Section: The Bluetides Simulationsupporting

confidence: 72%

“…The intrinsic rest-frame UV luminosities, and thus the model expectations, are sensitive to various assumptions including the choice of IMF, SPS model, and Lyman continuum escape fraction. The impact of these assumptions on the SED of galaxies at high-redshift are explored in detail in Wilkins et al (2016). Figure 1 shows that observational constraints at 2015) are consistent with these predictions, largely lying between the z = 10 and z = 11 lines.…”

Section: Luminosity Function and Volume Densitymentioning

confidence: 68%

“…Galaxy spectral energy distributions (SED) were calculated by coupling the simulation with the Pegase (Fioc & Rocca-Volmerange 1997) stellar population synthesis (SPS) model assuming a Chabrier (2003) initial mass function (IMF) combined with reprocessing by both gas and dust (see Wilkins et al, 2016 for details).…”

Section: The Bluetides Simulationmentioning

confidence: 99%

“…We note, however, that the predicted intrinsic UV continuum slope is also sensitive to the choice of SPS model, IMF, and assumed Lyman continuum escape fraction. Alternative choices can result in bluer intrinsic UV continuum slopes leaving open the possibility of some dust attenuation (see Wilkins et al 2016).…”

Section: Uv Continuum Slopementioning

confidence: 99%

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Monsters in the dark: predictions for luminous galaxies in the early Universe from the BlueTides simulation

Waters

Wilkins

Matteo

et al. 2016

Monthly Notices of the Royal Astronomical Society: Letters

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Using deep Hubble and Spitzer observations Oesch et al. (2016) have identified a bright (M UV ≈ −22) star forming galaxy candidate at z ≈ 11. The presence of GN-z11 implies a number density ∼ 10 −6 Mpc −3 , roughly an order of magnitude higher than the expected value based on extrapolations from lower redshift. Using the unprecedented volume and high resolution of the BlueTides cosmological hydrodynamical simulation, we study the population of luminous rare objects at z > 10. The luminosity function in BlueTides implies an enhanced number of massive galaxies, consistent with the observation of GN-z11. We find about 30 galaxies at M UV ≈ −22 at z = 11 in the BlueTides volume, including a few objects about 1.5 magnitudes brighter. The probability of observing GN-z11 in the volume probed by Oesch et al. (2016) is ∼ 13 per cent. The predicted properties of the rare bright galaxies at z = 11 in BlueTides closely match those inferred from the observations of GN-z11. BlueTides predicts a negligible contribution from faint AGN in the observed SED. The enormous increase in volume surveyed by WFIRST will provide observations of ∼ 1000 galaxies with M UV < −22 beyond z = 11 out to z = 13.5.

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Section: The Bluetides Simulationsupporting

confidence: 72%

Section: Luminosity Function and Volume Densitymentioning

confidence: 68%

Section: The Bluetides Simulationmentioning

confidence: 99%

Section: Uv Continuum Slopementioning

confidence: 99%

See 2 more Smart Citations

Monsters in the dark: predictions for luminous galaxies in the early Universe from the BlueTides simulation

Waters

Wilkins

Matteo

et al. 2016

Monthly Notices of the Royal Astronomical Society: Letters

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“…20 QLaue was used to simulate the Laue diffraction pattern. 21 A schematic diagram of the seeded CVT set up is shown in Fig. 1(a), with the charge and transport agent shown on the source end and a single seed crystal on the deposition end.…”

Section: Characterizationmentioning

confidence: 99%

Seeded Chemical Vapor Transport Growth of Cu₂OSeO₃

Panella

Trump

Marcus

et al. 2017

Crystal Growth & Design

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We present an optimized seeded chemical vapor transport method for the growth of Cu 2 OSeO 3 that allows for chemical control in a system with many stable phases to selectively produce large phase pure single crystals. This method is shown to consistently produce single crystals in the range of 120 to 180 mg. A Wulff construction model of a representative crystal shows that the minimum energy surface is {1 1 0}, followed by {1 0 0}. Analysis of the lowest index planes revealed that cleavage of Se-O bonds has a large energy cost, leading to an overall high surface energy. The seeded chemical vapor transport demonstrated here shows promise for large single crystal growth of other functional materials such as Weyl semimetals, frustrated magnets, and superconductors.

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