An ALMA survey of the SCUBA-2 cosmology legacy survey UKIDSS/UDS field: Dust attenuation in high-redshift Lyman-break galaxies

Koprowski, M. P.; Coppin, K. E. K.; Dudzevičiūtė, U.; Smail, Ian; Almaini, O.; An, Fangxia; Blain, A. W.; Chapman, Scott; Chen, Chian-Chou; Conselice, C. J.; Dunlop, James; Farrah, D.; Gullberg, B.; Hartley, W. G.; Ivison, R. J.; Karska, A.; Maltby, David T.; Małek, K.; Michałowski, M. J.; Pope, Alexandra; Salim, Samir; Scott, Douglas; Simpson, Chris; Simpson, J. M.; Swinbank, A. M.; Thomson, A. P.; Wardlow, J. L.; Werf, P. P. van der; Whitaker, Katherine E.

doi:10.1093/mnras/staa160

Cited by 12 publications

(9 citation statements)

References 136 publications

(223 reference statements)

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“…When comparing to lower redshift observations at z ∼ 5 − 6, however, we find that our IRLF is more than an order of magnitude lower. Finally, our IRLF shows an interesting evolution with redshift, compared with the literature, not only in number density (as was previously shown in Koprowski et al (2020); Fujimoto et al (2023)), but also in L * . This could be due to our UV-selected sample being biased to bright sources and further study with a similar selection at different redshift should be carried out to confirm the possibility of evolution with L * .…”

Section: Schechter Function Fitssupporting

confidence: 86%

“…Similarly, Wang et al (2019a) shows a decreasing SFRD (light purple area) with large uncertainty in the last bin at z ∼ 4 (dashed light purple area). Koprowski et al (2020) presented a constrained SFRD up to z ∼ 4 (purple area). REBELS results shows the presence of dust at z ∼ 7 even in UV-selected galaxies.…”

Section: What Irlf Is Needed To Reproduce Extreme Sfrd?mentioning

confidence: 99%

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The ALMA REBELS Survey: The First Infrared Luminosity Function Measurement at $\mathbf{z \sim 7}

Barrufet¹,

Oesch²,

Bouwens³

et al. 2023

Preprint

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We present the first observational infrared luminosity function (IRLF) measurement in the Epoch of Reionization (EoR) based on a UV-selected galaxy sample with ALMA spectroscopic observations. Our analysis is based on the ALMA large program Reionization Era Bright Emission Line Survey (REBELS), which targets 42 galaxies at z = 6.4 − 7.7 with [CII] 158µm line scans. 16 sources exhibit a dust detection, 15 of which are also spectroscopically confirmed through the [CII] line. The IR luminosities of the sample range from log L IR /L = 11.4 to 12.2. Using the UVLF as a proxy to derive the effective volume for each of our target sources, we derive IRLF estimates, both for detections and for the full sample including IR luminosity upper limits. The resulting IRLFs are well reproduced by a Schechter function with the characteristic luminosity of log L * /L = 11.6 +0.2 −0.1 . Our observational results are in broad agreement with the average of predicted IRLFs from simulations at z ∼ 7. Conversely, our IRLFs lie significantly below lower redshift estimates, suggesting a rapid evolution from z ∼ 4 to z ∼ 7, into the reionization epoch. The inferred obscured contribution to the cosmic star-formation rate density at z ∼ 7 amounts to log(SFRD/M /yr/Mpc 3 ) = −2.66 +0.17 −0.14 which is at least ∼10% of UV-based estimates. We conclude that the presence of dust is already abundant in the EoR and discuss the possibility of unveiling larger samples of dusty galaxies with future ALMA and JWST observations.

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Section: Schechter Function Fitssupporting

confidence: 86%

Section: What Irlf Is Needed To Reproduce Extreme Sfrd?mentioning

confidence: 99%

The ALMA REBELS Survey: The First Infrared Luminosity Function Measurement at $\mathbf{z \sim 7}

Barrufet¹,

Oesch²,

Bouwens³

et al. 2023

Preprint

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“…The constant starburst is considered as a convenient approximation in SED modelling, but it has a drawback in generating templates with representative intrinsic UV colours (no dust). Koprowski et al (2020) showed that a constant starburst creates spectral templates of different ages with similar intrinsic UV colours, being less sensitive to the life time of the burst (see also Calzetti 2001;Mao et al 2012). In Figure 2 we compare the spectral templates in two extreme cases: one an instantaneous starburst (or a single stellar population) and the other a constant starburst.…”

Section: Star Formation Historiesmentioning

confidence: 99%

“…One can see that by increasing age over 10 − 500 Myr, β0 changes dramatically from −2.4 to 2.2 for the instantaneous starburst, while β0 mildly increases from −2.7 to −2.3 for the constant starburst. This is because the galaxy population is constantly replenished by the youngest stellar populations that dominate the UV radiation and result in an approximately constant UV colour (Koprowski et al 2020;Calzetti et al 2021).…”

Section: Star Formation Historiesmentioning

confidence: 99%

“…It is worth noting that there is a high degree of degeneracy between the star formation histories (SFHs) and dust attenuation curves adopted in SED fitting (Calzetti et al 2021). The determination of the attenuation curve is sensitive to the adopted SFHs in the fitting (Burgarella et al 2005;Koprowski et al 2020;Calzetti et al 2021). Considering the fitting degeneracy is largely unexplored, a thorough investigation is demanded to examine if the AV-slope relation is largely shaped by the fitting degeneracy.…”

Section: Introductionmentioning

confidence: 99%

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Systematic biases in determining dust attenuation curves through galaxy SED fitting

Qin

Zheng

Fang

et al. 2022

Monthly Notices of the Royal Astronomical Society

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While the slope of the dust attenuation curve (δ) is found to correlate with effective dust attenuation (AV) as obtained through spectral energy distribution (SED) fitting, it remains unknown how the fitting degeneracies shape this relation. We examine the degeneracy effects by fitting SEDs of a sample of local star-forming galaxies (SFGs) selected from the Galaxy And Mass Assembly survey, in conjunction with mock galaxy SEDs of known attenuation parameters. A well-designed declining starburst star formation history is adopted to generate model SED templates with intrinsic UV slope (β0) spanning over a reasonably wide range. The best-fitting β0 for our sample SFGs shows a wide coverage, dramatically differing from the limited range of β0 < −2.2 for a starburst of constant star formation. Our results show that strong degeneracies between β0, δ, and AV in the SED fitting induce systematic biases leading to a false AV–δ correlation. Our simulation tests reveal that this relationship can be well reproduced even when a flat AV–δ relation is taken to build the input model galaxy SEDs. The variations in best-fitting δ are dominated by the fitting errors. We show that assuming a starburst with constant star formation in SED fitting will result in a steeper attenuation curve, smaller degeneracy errors, and a stronger AV–δ relation. Our findings confirm that the AV–δ relation obtained through SED fitting is likely driven by the systematic biases induced by the fitting degeneracies between β0, δ, and AV.

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The ALPINE-ALMA [CII] survey

Fudamoto

Oesch

Faisst

et al. 2020

A&A

100

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We present dust attenuation properties of spectroscopically confirmed star forming galaxies on the main sequence at a redshift of ∼4.4 − 5.8. Our analyses are based on the far infrared continuum observations of 118 galaxies at rest-frame 158 μm obtained with the Atacama Large Millimeter Array (ALMA) Large Program to INvestigate [CII] at Early times (ALPINE). We study the connection between the ultraviolet (UV) spectral slope (β), stellar mass (M⋆), and infrared excess (IRX = LIR/LUV). Twenty-three galaxies are individually detected in the continuum at > 3.5σ significance. We perform a stacking analysis using both detections and nondetections to study the average dust attenuation properties at z ∼ 4.4 − 5.8. The individual detections and stacks show that the IRX–β relation at z ∼ 5 is consistent with a steeper dust attenuation curve than typically found at lower redshifts (z < 4). The attenuation curve is similar to or even steeper than that of the extinction curve of the Small Magellanic Cloud. This systematic change of the IRX–β relation as a function of redshift suggests an evolution of dust attenuation properties at z > 4. Similarly, we find that our galaxies have lower IRX values, up to 1 dex on average, at a fixed mass compared to previously studied IRX–M⋆ relations at z ≲ 4, albeit with significant scatter. This implies a lower obscured fraction of star formation than at lower redshifts. Our results suggest that dust properties of UV-selected star forming galaxies at z ≳ 4 are characterised by (i) a steeper attenuation curve than at z ≲ 4, and (ii) a rapidly decreasing dust obscured fraction of star formation as a function of redshift. Nevertheless, even among this UV-selected sample, massive galaxies (log M⋆/M⊙ > 10) at z ∼ 5 − 6 already exhibit an obscured fraction of star formation of ∼45%, indicating a rapid build-up of dust during the epoch of reionization.

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An ALMA survey of the SCUBA-2 cosmology legacy survey UKIDSS/UDS field: Dust attenuation in high-redshift Lyman-break galaxies

Cited by 12 publications

References 136 publications

The ALMA REBELS Survey: The First Infrared Luminosity Function Measurement at $\mathbf{z \sim 7}

The ALMA REBELS Survey: The First Infrared Luminosity Function Measurement at $\mathbf{z \sim 7}

Systematic biases in determining dust attenuation curves through galaxy SED fitting

The ALPINE-ALMA [CII] survey

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