The evolution of the UV-to-mm extragalactic background light: evidence for a top-heavy initial mass function?

Cowley, William I.; Lacey, Cedric G.; Baugh, C. M.; Cole, Shaun; Frenk, Carlos S.; Lagos, Claudia del P.

doi:10.1093/mnras/stz1398

Cited by 29 publications

(18 citation statements)

References 125 publications

(220 reference statements)

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“…There are also no bright sources (> 4 mJy) in E at > 0.5. Our number counts derived for E are in agreement with those presented by Wang et al (2019); Cowley et al (2019).…”

Section: Model Comparisonssupporting

confidence: 90%

“…S 's level of agreement is unprecedented from cosmological hydrodynamic simulations (for a review, see Casey et al 2014). For comparison, we also show the results from the E simulation (McAlpine et al 2019), which illustrates that E does not come as close to matching the 850 µm number counts (see also Wang et al 2019;Cowley et al 2019). In particular, E does not produce any bright (> 4 mJy) sources at > 0.5.…”

Section: Integrated Number Countssupporting

confidence: 54%

“…This is required to produce sufficiently bright sub-mm emission during frequent low-mass merger events. Later versions of the model used a more moderately top-heavy IMF in starbursts, triggered by disk instabilities rather than mergers, and found similarly good agreement with the number counts (Cowley et al 2015;Park et al 2016;Lacey et al 2016;Cowley et al 2019). However, such IMF variability is still controversial, particularly extreme forms and any dependence on merger state (Bastian et al 2010;Hopkins 2013;Krumholz 2014), and is inconsistent with the constraints on the IMF in massive star-forming galaxies which is significantly less extreme (e.g.…”

Section: Introductionmentioning

confidence: 98%

“…They used the E simulations (Schaye et al 2015;Crain et al 2015) combined with the S RT code (Camps et al 2018) and found good agreement between E and the observed SMG redshift distribution. However, they form very few high flux density (> 3 mJy) sources, and the luminosity function at IR-wavelengths has been shown to be in tension with observational constraints (Wang et al 2019;Cowley et al 2019).…”

Section: Introductionmentioning

confidence: 99%

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Reproducing submillimetre galaxy number counts with cosmological hydrodynamic simulations

Lovell

Geach

Davé

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Matching the number counts of high-z submillimetre-selected galaxies (SMGs) has been a long-standing problem for galaxy formation models. In this paper, we use 3D dust radiative transfer to model the submm emission from galaxies in the simba cosmological hydrodynamic simulations, and compare predictions to the latest single-dish observational constraints on the abundance of 850 μm-selected sources. We find good agreement with the shape of the integrated 850 μm luminosity function, and the normalization is within 0.25 dex at >3 mJy, unprecedented for a fully cosmological hydrodynamic simulation, along with good agreement in the redshift distribution of bright SMGs. The agreement is driven primarily by simba’s good match to infrared measures of the star formation rate (SFR) function between z = 2 and 4 at high SFRs. Also important is the self-consistent on-the-fly dust model in simba, which predicts, on average, higher dust masses (by up to a factor of 2.5) compared to using a fixed dust-to-metals ratio of 0.3. We construct a light-cone to investigate the effect of far-field blending, and find that 52 per cent of sources are blends of multiple components, which makes a small contribution to the normalization of the bright end of the number counts. We provide new fits to the 850 μm luminosity as a function of SFR and dust mass. Our results demonstrate that solutions to the discrepancy between submm counts in simulations and observations, such as a top-heavy initial mass function, are unnecessary, and that submillimetre-bright phases are a natural consequence of massive galaxy evolution.

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“…There are also no bright sources (> 4 mJy) in E at > 0.5. Our number counts derived for E are in agreement with those presented by Wang et al (2019); Cowley et al (2019).…”

Section: Model Comparisonssupporting

confidence: 90%

Section: Integrated Number Countssupporting

confidence: 54%

Section: Introductionmentioning

confidence: 98%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Reproducing submillimetre galaxy number counts with cosmological hydrodynamic simulations

Lovell

Geach

Davé

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…This is not necessarily surprising given the discrepancy in the predicted number counts of EAGLE and observations in the FIR bands (e.g. Cowley et al 2019;Wang et al 2019).…”

Section: The Final Ebl and Comparison To Modelsmentioning

confidence: 98%

GAMA/DEVILS: constraining the cosmic star formation history from improved measurements of the 0.3–2.2 μm extragalactic background light

Koushan

Driver

Bellstedt

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present a revised measurement of the optical extragalactic background light (EBL), based on the contribution of resolved galaxies to the integrated galaxy light (IGL). The cosmic optical background radiation (COB), encodes the light generated by star-formation, and provides a wealth of information about the cosmic star formation history (CSFH). We combine wide and deep galaxy number counts from the Galaxy And Mass Assembly survey (GAMA) and Deep Extragalactic VIsible Legacy Survey (DEVILS), along with the Hubble Space Telescope (HST) archive and other deep survey datasets, in 9 multi-wavelength filters to measure the COB in the range from 0.35 μm to 2.2 μm. We derive the luminosity density in each band independently and show good agreement with recent and complementary estimates of the optical-EBL from very high-energy (VHE) experiments. Our error analysis suggests that the IGL and γ-ray measurements are now fully consistent to within $\sim 10{{\ \rm per\ cent}}$, suggesting little need for any additional source of diffuse light beyond the known galaxy population. We use our revised IGL measurements to constrain the cosmic star-formation history, and place amplitude constraints on a number of recent estimates. As a consistency check, we can now demonstrate convincingly, that the CSFH, stellar mass growth, and the optical-EBL provide a fully consistent picture of galaxy evolution. We conclude that the peak of star-formation rate lies in the range 0.066–0.076 M⊙ yr−1 Mpc−3 at a lookback time of 9.1 to 10.9 Gyrs.

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Probing the evolution of the EBL photon density out to $z\sim 1$ via $\gamma $-ray propagation measurements with Fermi

Singh

Yadav

Meintjes

2021

Astrophys Space Sci

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The evolution of the UV-to-mm extragalactic background light: evidence for a top-heavy initial mass function?

Cited by 29 publications

References 125 publications

Reproducing submillimetre galaxy number counts with cosmological hydrodynamic simulations

Reproducing submillimetre galaxy number counts with cosmological hydrodynamic simulations

GAMA/DEVILS: constraining the cosmic star formation history from improved measurements of the 0.3–2.2 μm extragalactic background light

Probing the evolution of the EBL photon density out to $z\sim 1$ via $\gamma $-ray propagation measurements with Fermi

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