THE SPECTRAL EVOLUTION OF THE FIRST GALAXIES. I.<i>JAMES WEBB SPACE TELESCOPE</i>DETECTION LIMITS AND COLOR CRITERIA FOR POPULATION III GALAXIES

Zackrisson, Erik; Rydberg, Claes-Erik; Schaerer, D.; Östlin, Göran; Tuli, Mahmoud

doi:10.1088/0004-637x/740/1/13

Cited by 307 publications

(395 citation statements)

References 94 publications

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“…5 shows this plot for the YMC sample of M83. The model plotted over the points is the cluster evolutionary model for M83 at solar metallicity that includes nebular and continuum emission and uses a Kroupa IMF from Zackrisson et al (2011), which was also used for SED fitting of the clusters. The orange circles correspond to embedded clusters, the purple diamonds to partially embedded clusters and green stars to exposed clusters.…”

Section: Colour-colour Plotmentioning

confidence: 99%

Studying the YMC population of M83: how long clusters remain embedded, their interaction with the ISM and implications for GC formation theories

Hollyhead

Bastian

Adamo

et al. 2015

Monthly Notices of the Royal Astronomical Society

149

129

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The study of young massive clusters can provide key information for the formation of globular clusters, as they are often considered analogues. A currently unanswered question in this field is how long these massive clusters remain embedded in their natal gas, with important implications for the formation of multiple populations that have been used to explain phenomena observed in globular clusters. We present an analysis of ages and masses of the young massive cluster population of M83. Through visual inspection of the clusters, and comparison of their spectral energy distributions (SEDs) and position in colour-colour space, the clusters are all exposed (no longer embedded) by <4 Myr, most likely less, indicating that current proposed age spreads within older clusters are unlikely. We also present several methods of constraining the ages of very young massive clusters. This can often be difficult using SED fitting due to a lack of information to disentangle age-extinction degeneracies and possible inaccurate assumptions in the models used for the fitting. The individual morphology of the Hα around each cluster has a significant effect on the measured fluxes, which contributes to inaccuracies in the age estimates for clusters younger than 10 Myr using SED fitting. This is due to model uncertainties and aperture effects. Our methods to help constrain ages of young clusters include using the near-infrared and spectral features, such as Wolf-Rayet stars.

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Section: Colour-colour Plotmentioning

confidence: 99%

Studying the YMC population of M83: how long clusters remain embedded, their interaction with the ISM and implications for GC formation theories

Hollyhead

Bastian

Adamo

et al. 2015

Monthly Notices of the Royal Astronomical Society

149

129

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“…4.1.1 Zackrisson et al (2013) Using stellar SEDs from the Yggdrasil population synthesis code (Zackrisson et al 2011) and Cloudy, Zackrisson et al (2013) explore the evolution of the UV slope of galaxies over time and with respect to Hβ EW for a range Lyman continuum escape fractions. They argue that for high escape fractions, galaxies with M ≥ 10 7 M should be detectable with JWST up to z 9 where our entire sample of galaxies with M ≥ 10 7 M is visible to redshift 12 with µ = 10.…”

Section: Comparable Workmentioning

confidence: 99%

First light: exploring the spectra of high-redshift galaxies in the Renaissance Simulations

Barrow

Wise

Norman

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present synthetic observations for the first generations of galaxies in the Universe and make predictions for future deep field observations for redshifts greater than 6. Due to the strong impact of nebular emission lines and the relatively compact scale of H ii regions, high resolution cosmological simulations and a robust suite of analysis tools are required to properly simulate spectra. We created a software pipeline consisting of FSPS, Hyperion, Cloudy and our own tools to generate synthetic IR observations from a fully three-dimensional arrangement of gas, dust, and stars. Our prescription allows us to include emission lines for a complete chemical network and tackle the effect of dust extinction and scattering in the various lines of sight. We provide spectra, 2-D binned photon imagery for both HST and JWST IR filters, luminosity relationships, and emission line strengths for a large sample of high redshift galaxies in the Renaissance Simulations. Our resulting synthetic spectra show high variability between galactic halos with a strong dependence on stellar mass, metallicity, gas mass fraction, and formation history. haloes with the lowest stellar mass have the greatest variability in [O iii]/Hβ, [O iii] and C iii] while haloes with higher masses are seen to show consistency in their spectra and [O iii] equivalent widths (EW) between 1Å and 10Å. Viewing angle accounted for three-fold difference in flux due to the presence of ionized gas channels in a halo. Furthermore, JWST colour plots show a discernible relationship between redshift, colour, and mean stellar age.

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“…Its evolution is followed via a moment method that couples with the opacity field from the gas in a way that captures the UVB's feedback effect (Finlator et al 2011). The emissivity of starforming gas particles is proportional to their star formation rate, with a metallicity dependence that is computed from a modified version of Yggdrasil (Zackrisson et al 2011). The emissivity is tabulated at 7 distinct metallicities between Z = 0-0.04, and each gas particle's actual emissivity is computed by interpolating to its Z.…”

Section: Radiation Transportmentioning

confidence: 99%

The reionization of carbon

Finlator

Thompson

Huang

et al. 2015

Monthly Notices of the Royal Astronomical Society

109

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Observations suggest that C II was more abundant than C IV in the intergalactic medium towards the end of the hydrogen reionization epoch (z ∼ 6). This transition provides a unique opportunity to study the enrichment history of intergalactic gas and the growth of the ionizing background (UVB) at early times. We study how carbon absorption evolves from z = 10-5 using a cosmological hydrodynamic simulation that includes a self-consistent multifrequency UVB as well as a well-constrained model for galactic outflows to disperse metals. Our predicted UVB is within ∼ 2-4× of that from Haardt & Madau (2012), which is fair agreement given the uncertainties. Nonetheless, we use a calibration in post-processing to account for Lyman-α forest measurements while preserving the predicted spectral slope and inhomogeneity. The UVB fluctuates spatially in such a way that it always exceeds the volume average in regions where metals are found. This implies both that a spatially-uniform UVB is a poor approximation and that metal absorption is not sensitive to the epoch when HII regions overlap globally even at column densites of 10 12 cm −2 . We find, consistent with observations, that the C II mass fraction drops to low redshift while C IV rises owing the combined effects of a growing UVB and continued addition of carbon in low-density regions. This is mimicked in absorption statistics, which broadly agree with observations at z = 6-3 while predicting that the absorber column density distributions rise steeply to the lowest observable columns. Our model reproduces the large observed scatter in the number of low-ionization absorbers per sightline, implying that the scatter does not indicate a partially-neutral Universe at z ∼ 6.

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THE SPECTRAL EVOLUTION OF THE FIRST GALAXIES. I.JAMES WEBB SPACE TELESCOPEDETECTION LIMITS AND COLOR CRITERIA FOR POPULATION III GALAXIES

Cited by 307 publications

References 94 publications

Studying the YMC population of M83: how long clusters remain embedded, their interaction with the ISM and implications for GC formation theories

Studying the YMC population of M83: how long clusters remain embedded, their interaction with the ISM and implications for GC formation theories

First light: exploring the spectra of high-redshift galaxies in the Renaissance Simulations

The reionization of carbon

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