The evolving far-IR galaxy luminosity function and dust-obscured star formation rate density out to ≃

Koprowski, M. P.; Dunlop, James; Michałowski, M. J.; Coppin, K. E. K.; Geach, J. E.; McLure, R. J.; Scott, Douglas; Werf, P. van der

doi:10.1093/mnras/stx1843

Cited by 84 publications

(186 citation statements)

References 103 publications

(241 reference statements)

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“…In general, infrared-selected studies of the dust-obscured contribution at z > 3 show significant scatter compared to rest-frame UV selected studies (e.g. Rowan-Robinson et al 2016;Cowie et al 2018;Koprowski et al 2017;Liu et al 2018;Dunlop et al 2017;Yamaguchi et al 2019), whereas the agreements at z < 3 are much better (Madau & Dickinson 2014, and references therein). The large scatter reflects the difficulty of determining obscured star formation in the early universe.…”

Section: Contribution To Csfrdmentioning

confidence: 98%

“…We add to the compilation of Madau & Dickinson (2014, ; blue circles) with more recent z > 4 measurements by Finkelstein et al (2015); Bouwens et al (2016);McLeod et al (2016); Oesch et al (2018). Red circles are the dust-obscured IR compilation of Madau & Dickinson (2014), to which we add recent z > 2 measurements from Swinbank et al (2014); Koprowski et al (2017); Magnelli et al (2019); Cowie et al (2018); Dunlop et al (2017); Liu et al (2018). The contribution of 3M M -1 is indicated by the black star and shaded region, where the redshift range indicates the estimated selection volume as discussed in §4.5.…”

Section: Comparison To Other "Dark" Galaxiesmentioning

confidence: 99%

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Discovery of a Dark, Massive, ALMA-only Galaxy at z ∼ 5–6 in a Tiny 3 mm Survey

Williams

Labbé

Spilker

et al. 2019

ApJ

108

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We report the serendipitous detection of two 3 mm continuum sources found in deep ALMA Band 3 observations to study intermediate redshift galaxies in the COSMOS field. One is near a foreground galaxy at 1. 3, but is a previously unknown dust-obscured star-forming galaxy (DSFG) at probable z CO = 3.329, illustrating the risk of misidentifying shorter wavelength counterparts. The optical-tomm spectral energy distribution (SED) favors a grey λ −0.4 attenuation curve and results in significantly larger stellar mass and SFR compared to a Calzetti starburst law, suggesting caution when relating progenitors and descendants based on these quantities. The other source is missing from all previous optical/near-infrared/sub-mm/radio catalogs ("ALMA-only"), and remains undetected even in stacked ultradeep optical (> 29.6 AB) and near-infrared (> 27.9 AB) images. Using the ALMA position as a prior reveals faint SN R ∼ 3 measurements in stacked IRAC 3.6+4.5, ultradeep SCUBA2 850µm, and VLA 3GHz, indicating the source is real. The SED is robustly reproduced by a massive M * = 10 10.8 M and M gas = 10 11 M , highly obscured A V ∼ 4, star forming SF R ∼ 300 M yr −1 galaxy at redshift z = 5.5±1.1. The ultrasmall 8 arcmin 2 survey area implies a large yet uncertain contribution to the cosmic star formation rate density CSFRD(z=5) ∼ 0.9 × 10 −2 M yr −1 Mpc −3 , comparable to all ultraviolet-selected galaxies combined. These results indicate the existence of a prominent population of DSFGs at z > 4, below the typical detection limit of bright galaxies found in single-dish sub-mm surveys, but with larger space densities ∼ 3 × 10 −5 Mpc −3 , higher duty cycles 50 − 100%, contributing more to the CSFRD, and potentially dominating the high-mass galaxy stellar mass function.

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Section: Contribution To Csfrdmentioning

confidence: 98%

Section: Comparison To Other "Dark" Galaxiesmentioning

confidence: 99%

Discovery of a Dark, Massive, ALMA-only Galaxy at z ∼ 5–6 in a Tiny 3 mm Survey

Williams

Labbé

Spilker

et al. 2019

ApJ

108

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“…There is, however, considerable uncertainly in this quantity observationally. For example, surveys which select sources on the basis of their mid-or far-infrared luminosity (as a proxy for their SFR) have reported space densities of ∼ 10 −5 to 2×10 −4 cMpc −3 for galaxies with far-infrared luminosities of 10 12 L and inferred SFRs of 100 M yr −1 at z ≈ 1.5-2.5 (e.g., Chapman et al 2005;Magnelli et al 2011;Casey et al 2012;Gruppioni et al 2013;Swinbank et al 2014;Koprowski et al 2017). However, these studies suffer from a combination of AGN contamination of the derived luminosities (a particular problem in the mid-infrared, e.g., Kirkpatrick et al 2012Kirkpatrick et al , 2015Del Moro et al 2013), or blending and misidentification of the correct galaxy counterparts in low-resolution far-infrared and sub-millimeter surveys (e.g., Hodge et al 2013;Simpson et al 2014).…”

Section: Sample 2: Highly Star-forming Submm-faint Galaxiesmentioning

confidence: 99%

The nature of submillimetre and highly star-forming galaxies in the EAGLE simulation

McAlpine

Smail

Bower

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We exploit eagle, a cosmological hydrodynamical simulation, to reproduce the selection of the observed sub-millimeter (submm) galaxy population by selecting the model galaxies at z ≥ 1 with mock submm fluxes S 850µm ≥ 1 mJy (computed in post processing using radiative transfer techniques). There is a reasonable agreement between the galaxies within this sample and the properties of the observed submm population, such as their star formation rates (SFRs) at z < 3, redshift distribution and many integrated galaxy properties. We find that the bulk of the S 850µm ≥ 1 mJy model population is at z ≈ 2.5, and that they are massive galaxies (M * ∼ 10 11 M ) with high dust masses (M dust ∼ 10 8 M ), gas fractions ( f gas ≈ 50%) and SFRs ( M * ≈ 100 M yr −1 ). They have major and minor merger fractions similar to the general population, suggesting that mergers are not the primary driver of the model submm galaxies. Instead, the S 850µm ≥ 1 mJy model galaxies yield high SFRs primarily because they maintain a significant gas reservoir as a result of hosting an undermassive black hole. In addition, we find that not all 'highly star-forming' ( M * ≥ 80 M yr −1 ) eagle galaxies have submm fluxes S 850µm ≥ 1 mJy. Thus, we investigate the nature of z ≥ 1 highly star-forming 'Submm-Faint' galaxies (i.e., M * ≥ 80 M yr −1 but S 850µm < 1 mJy). We find they are similar to the model submm galaxies; being gas rich and hosting undermassive black holes, however they are typically lower mass (M * ∼ 10 10 M ) and are at higher redshifts (z > 4). These typically higher-redshift galaxies show stronger evidence for having been triggered by major mergers, and critically, they are likely missed by current submm surveys due to their higher dust temperatures. This suggests a potentially even larger contribution to the SFR density at z 3 from dust-obscured systems than implied by current observations.

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“…Given the higher than expected radio flux (see Figure 6), and the fact that we do not detect any CO lines, we further suggest that NGP6 D1 hosts an AGN, probably dust enshrouded, which contributes to the radio flux. Figure 13 suggests that SPIRE dropouts can inhabit a much larger range of luminosity-redshift-temperature parameter space than 850 µm risers; the polygon that forms from the constraints that 20 K < T dust < 80 K, and the approximate "knee" of the z > 2 DSFG luminosity function 5 at around 10 13 L (Casey et al 2014;Gruppioni et al 2017;Koprowski et al 2017) encompasses a much larger area of parameter space for the SPIRE dropouts compared to the 850 µm risers. We therefore examine two of the largest extragalactic Figure 13.…”

Section: The Nature Of Ngp6 D1mentioning

confidence: 98%

“…consistently been unable to reproduce the observed number counts of the red, z ≥ 4 DSFGs (Dowell et al 2014;Asboth et al 2016;Ivison et al 2016), and questions remain about whether DSFGs significantly contribute to the global star formation rate (SFR) density at z > 3 ( Rowan-Robinson et al 2016;Liu et al 2017;Novak et al 2017) or not Koprowski et al 2017). We can neither rule out a negligible or dominant contribution to this SFR-density from DSFGs at z > 3.5 (Casey et al 2018).…”

mentioning

confidence: 99%

A SCUBA-2 selected Herschel-SPIRE dropout and the nature of this population

Greenslade

Aguilar

Clements

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Dusty star-forming galaxies (DSFGs) detected at z > 4 provide important examples of the first generations of massive galaxies. However, few examples with spectroscopic confirmation are currently known, with Hershel struggling to detect significant numbers of z > 6 DSFGs. NGP6 D1 is a bright 850 µm source (12.3 ± 2.5 mJy) with no counterparts at shorter wavelengths (a SPIRE dropout). Interferometric observations confirm it is a single source, with no evidence for any optical or NIR emission, or nearby likely foreground lensing sources. No > 3σ detected lines are seen in both LMT RSR and IRAM 30m EMIR spectra of NGP6 D1 across 32 GHz of bandwidth despite reaching detection limits of ∼ 1mJ y/500km s −1 , so the redshift remains unknown. Template fitting suggests that NGP6 D1 is most likely between z = 5.8 and 8.3. SED analysis finds that NGP6 D1 is a ULIRG, with a dust mass ∼ 10 8 -10 9 M and a SFR of ∼ 500 M yr −1 . We place upper limits on the gas mass of NGP6 D1 of M H2 < (1.1 ± 3.5) × 10 11 M , consistent with a gas-to-dust ratio of ∼ 100 -1000. We discuss the nature of NGP6 D1 in the context of the broader submm population, and find that comparable SPIRE dropouts account for ∼ 20% of all SCUBA-2 detected sources, but with a similar flux density distribution to the general population.

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The evolving far-IR galaxy luminosity function and dust-obscured star formation rate density out to ≃

Abstract: The evolving far-IR galaxy luminosity function and dust-obscured star formation rate density out to ≃', Monthly

Cited by 84 publications

References 103 publications

Discovery of a Dark, Massive, ALMA-only Galaxy at z ∼ 5–6 in a Tiny 3 mm Survey

Discovery of a Dark, Massive, ALMA-only Galaxy at z ∼ 5–6 in a Tiny 3 mm Survey

The nature of submillimetre and highly star-forming galaxies in the EAGLE simulation

A SCUBA-2 selected Herschel-SPIRE dropout and the nature of this population

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