The IRX–β relation of high-redshift galaxies

Liang, Lichen; Feldmann, Robert; Hayward, Christopher C.; Narayanan, Desika; Çatmabacak, Onur; Kereš, Dušan; Faucher-Giguère, Claude-André; Hopkins, Philip F.

doi:10.1093/mnras/stab096

Cited by 30 publications

(33 citation statements)

References 225 publications

(367 reference statements)

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“…Thus, intrinsic red stellar colours could explain the data points lying below the SMC and Calzetti lines in the IRX-β diagram. This result is consistent with previous theoretical studies such as Popping et al (2017), Narayanan et al (2018a) and Liang et al (2021). Burgarella et al (2020), based on their SED fitting analysis, showed that older LBGs tend to occupy the lower part of the IRX-β diagram.…”

Section: Possible Other Effectssupporting

confidence: 93%

“…These data are just used as guides or references for our results, and are not intended for detailed comparison or fitting. We also note that the observational data have large uncertainties; for example, IRX depends on the assumption for the dust temperature (50 K is adopted for the data from Hashimoto et al 2019), whose 1σ uncertainty is typically 10 K. The value of β depends on the choice of the observing wavelengths (Popping et al 2017;Liang et al 2021). Many of the LBGs at z 6 are not detected, even by ALMA (e.g.…”

Section: Irx-β Relationmentioning

confidence: 99%

“…We discuss here the effects of clumpiness, stellar age and dust composition. A recent comprehensive investigation of various effects on the IRX-β relation can be found in Liang et al (2021).…”

Section: Possible Other Effectsmentioning

confidence: 99%

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Geometry effects on dust attenuation curves with different grain sources at high redshift

Lin

Hirashita

Camps

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Dust has been detected in high-redshift (z > 5) galaxies but its origin is still being debated. Dust production in high-redshift galaxies could be dominated by stellar production or by accretion (dust growth) in the interstellar medium. Previous studies have shown that these two dust sources predict different grain-size distributions, which lead to significantly different extinction curves. In this paper, by performing radiative transfer calculations, we investigate how the difference in the extinction curves affects the dust attenuation properties of galaxies. To examine the major effects of the dust–stars distribution geometry, we adopt two representative cases in spherical symmetry: the well-mixed geometry (stars and dust are homogeneously mixed) and the two-layer geometry (young stars are more concentrated in the centre). In both cases, we confirm that the attenuation curve can be drastically steepened by scattering and by different optical depths between young and old stellar populations, and can be flattened by the existence of unobscured stellar populations. We can reproduce similar attenuation curves even with very different extinction curves. Thus, we conclude that it is difficult to distinguish dust sources only with attenuation curves. However, if we include information on dust emission and plot the relation between infrared excess (IRX) and the ultraviolet spectral slope (β), then different dust sources predict different positions in the IRX–β diagram. A larger β is preferred under a similar IRX if dust growth is the dominant dust source.

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Section: Possible Other Effectssupporting

confidence: 93%

Section: Irx-β Relationmentioning

confidence: 99%

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Geometry effects on dust attenuation curves with different grain sources at high redshift

Lin

Hirashita

Camps

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…Fujimoto et al 2017;Hashimoto et al 2019;Novak et al 2020). We examine 𝑅 = 5 kpc for a case of moderate extinction, and shrink This can be directly interpreted as an observed (or luminosity-weighted) dust temperature ('effective dust temperature' in Liang et al 2019). The temperature range is roughly consistent with that assumed in the above mentioned observational studies.…”

Section: Well-mixed Geometrysupporting

confidence: 56%

Geometry effects on dust attenuation curves with different grain sources at high redshift

Lin,

Hirashita,

Camps

et al. 2021

Preprint

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Dust has been detected in high-redshift (𝑧 > 5) galaxies but its origin is still being debated. Dust production in high-redshift galaxies could be dominated by stellar production or by accretion (dust growth) in the interstellar medium. Previous studies have shown that these two dust sources predict different grain size distributions, which lead to significantly different extinction curves. In this paper, we investigate how the difference in the extinction curves affects the dust attenuation properties of galaxies by performing radiative transfer calculations. To examine the major effects of the dust-stars distribution geometry, we adopt two representative cases in spherical symmetry: the well-mixed geometry (stars and dust are homogeneously mixed) and the two-layer geometry (young stars are more concentrated in the centre). In both cases, we confirm that the attenuation curve can be drastically steepened by scattering and by different optical depths between young and old stellar populations, and can be flattened by the existence of unobscured stellar populations. We can reproduce similar attenuation curves even with very different extinction curves. Thus, we conclude that it is difficult to distinguish the dust sources only with attenuation curves. However, if we include information on dust emission and plot the IRX (infrared excess)-𝛽 (ultraviolet spectral slope) relation, different dust sources predict different positions in the IRX-𝛽 diagram. A larger 𝛽 is preferred under a similar IRX if dust growth is the dominant dust source.

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“…The value of the discrepancy depends on the correction factor employed from Suess et al (2019b). We emphasize that Figures 2 and B1 should be understood as illustrations rather than proper com-parisons with observations; we plan to analyse synthetic images of FIREbox galaxies using radiative transfer (e.g., Liang et al 2019Liang et al , 2021 in future work. Shibuya et al (2015) find that a log-normal distribution well approximates the 𝑅 eff distribution in their combined legacy dataset of 3D-HST, CANDELS, Hubble Ultra Deep Fields (HUDF) 09+12 and the Hubble Frontier Fields (HFF) surveys.…”

Section: Comparisons To Observationsmentioning

confidence: 99%

The galaxy-halo size relation of low-mass galaxies in FIRE

Rohr,

Feldmann,

Bullock

et al. 2021

Preprint

Self Cite

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Galaxy sizes correlate closely with the sizes of their parent dark matter haloes, suggesting a link between halo formation and galaxy growth. However, the precise nature of this relation and its scatter remains to be understood fully, especially for low-mass galaxies. We analyse the galaxy-halo size relation for low-mass (𝑀 ★ ∼ 10 7−9 M ) central galaxies over the past 12.5 billion years with the help of cosmological volume simulations (FIREbox) from the Feedback in Realistic Environments (FIRE) project. We find a nearly linear relationship between the half-stellar mass galaxy size 𝑅 1/2 and the parent dark matter halo virial radius 𝑅 vir . This relation evolves only weakly since redshift 𝑧 = 5: 𝑅 1/2 [kpc] = (0.053 ± 0.002) (𝑅 vir /35 kpc) 0.934±0.054 , with a nearly constant scatter 𝜎 = 0.084 [dex]. Whilst this ratio is similar to what is expected from models where galaxy disc sizes are set by halo angular momentum, the low-mass galaxies in our sample are not angular momentum supported, with stellar rotational to circular velocity ratios 𝑣 rot /𝑣 circ ∼ 0.15. Introducing redshift as another parameter to the GHSR does not decrease the scatter. Furthermore, this scatter does not correlate with any of the halo properties we investigate -including spin and concentrationsuggesting that baryonic processes and feedback physics are instead critical in setting the scatter in the galaxy-halo size relation. Given the relatively small scatter and the weak dependence of the galaxy-halo size relation on redshift and halo properties for these low-mass central galaxies, we propose using galaxy sizes as an independent method from stellar masses to infer halo masses.

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The IRX–β relation of high-redshift galaxies

Cited by 30 publications

References 225 publications

Geometry effects on dust attenuation curves with different grain sources at high redshift

Geometry effects on dust attenuation curves with different grain sources at high redshift

Geometry effects on dust attenuation curves with different grain sources at high redshift

The galaxy-halo size relation of low-mass galaxies in FIRE

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