Rest-frame far-ultraviolet to far-infrared view of Lyman break galaxies at <i>z</i> = 3: Templates and dust attenuation

Álvarez-Márquez, J.; Burgarella, D.; Buat, V.; Ilbert, O.; Pérez‐González, Pablo G.

doi:10.1051/0004-6361/201935719

Cited by 42 publications

(43 citation statements)

References 124 publications

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“…We find a median excess of 240 +100 −25 and 1160 +180 −140 , respectively, where the errors are calculated from the 16-84th percentile range of the rest-frame SEDs. These ratios are much higher than those for similar stellar mass UVselected galaxies (∼4-90; Heinis et al 2013;Bouwens et al 2016;Alvarez-Márquez et al 2019).…”

Section: Optical/near-infrared Propertiescontrasting

confidence: 54%

Tracing the evolution of dust-obscured activity using sub-millimetre galaxy populations from STUDIES and AS2UDS

Dudzevičiūtė

Smail

Swinbank

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We analyse the physical properties of 121 SNR ≥ 5 sub-millimetre galaxies (SMGs) from the STUDIES 450-μm survey. We model their UV-to-radio spectral energy distributions using magphys+photo-z and compare the results to similar modelling of 850-μm-selected SMG sample from AS2UDS, to understand the fundamental physical differences between the two populations at the observed depths. The redshift distribution of the 450-μm sample has a median of z = 1.85 ± 0.12 and can be described by strong evolution of the far-infrared luminosity function. The fainter 450-μm sample has ∼ 14 times higher space density than the brighter 850-μm sample at z ≲ 2, and a comparable space density at z = 2–3, before rapidly declining, suggesting LIRGs are the main obscured population at z ∼ 1–2, while ULIRGs dominate at higher redshifts. We construct rest-frame ∼ 180-μm-selected and dust-mass-matched samples at z = 1–2 and z = 3–4 from the 450-μm and 850-μm samples, respectively, to probe the evolution of a uniform sample of galaxies spanning the cosmic noon era. Using far-infrared luminosity, dust masses and an optically-thick dust model, we suggest that higher-redshift sources have higher dust densities due to inferred dust continuum sizes which are roughly half of those for the lower-redshift population at a given dust mass, leading to higher dust attenuation. We track the evolution in the cosmic dust mass density and suggest that the dust content of galaxies is governed by a combination of both the variation of gas content and dust destruction timescale.

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Section: Optical/near-infrared Propertiescontrasting

confidence: 54%

Tracing the evolution of dust-obscured activity using sub-millimetre galaxy populations from STUDIES and AS2UDS

Dudzevičiūtė

Smail

Swinbank

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…We focus on determinations at z∼1.5-3.5 since this is where our results are the most significant and where most of previous results have been obtained. In Figure 15, we compare the IRX-stellar mass relationship we find at z∼1.5-3.5 with what we obtained in our pilot study (Bouwens et al 2016) and many other determinations in the literature (Heinis et al 2014;Pannella et al 2015;Álvarez-Márquez et al 2016Álvarez-Márquez et al , 2019Bourne et al 2017;Fudamoto et al 2017Fudamoto et al , 2020aKoprowski et al 2018;McLure et al 2018;Reddy et al 2018).…”

Section: Comparison With Previous Determinations Of the Infrared Excessmentioning

confidence: 52%

“…In Figure 17, we compare the IRX-β relationship we derive for higher-mass, z∼1.5-3.5 galaxies with the results obtained in our pilot study (Bouwens et al 2016) as well as a wide variety of different determinations in the literature (Heinis et al 2013;Álvarez-Márquez et al 2016Álvarez-Márquez et al , 2019Bourne et al 2017;Fudamoto et al 2017Fudamoto et al , 2020aKoprowski et al 2018;McLure et al 2018;Reddy et al 2018). Similar to what we found for the IRX-stellar mass relation, the larger number of dustcontinuum detections found here (versus from the smaller-area ASPECS pilot) results in the recovery of a steeper IRX-β relation than in our pilot, i.e., -+ 1.48 0.11 0.09 versus -+…”

Section: Comparison With Previous Determinations Of the Infrared Excessmentioning

confidence: 83%

“…by McLure et al (2018) using the shallower ALMA observations over the HUDF (Dunlop et al 2017) Álvarez-Márquez et al 2019). Given the current strong constraints on the obscured SFR at low masses (<10 9.25 M e ) and the challenge that source confusion presents for the lowest mass sources with Herschel, it seems likely that the slope of the IRX is approximately unity or steeper, as essentially all analyses relying on ALMA data have found.…”

Section: Comparison With Previous Determinations Of the Infrared Excessmentioning

confidence: 98%

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The ALMA Spectroscopic Survey Large Program: The Infrared Excess of z = 1.5–10 UV-selected Galaxies and the Implied High-redshift Star Formation History

Bouwens

González-López

Aravena

et al. 2020

ApJ

129

156

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We make use of sensitive (9.3 μJy beam −1 rms) 1.2 mm continuum observations from the Atacama Large Millimeter/submillimeter Array (ALMA) Spectroscopic Survey in the Hubble Ultra-Deep Field (ASPECS) large program to probe dust-enshrouded star formation from 1362 Lyman-break galaxies spanning the redshift range z=1.5-10 (to ∼7-28 M e yr −1 at 4σ over the entire range). We find that the fraction of ALMA-detected galaxies in our z=1.5-10 samples increases steeply with stellar mass, with the detection fraction rising from 0% at 10 9.0 M e to-+ 85 18 9 % at >10 10 M e. Moreover, on stacking all 1253 low-mass (<10 9.25 M e) galaxies over the ASPECS footprint, we find a mean continuum flux of −0.1±0.4 μJy beam −1 , implying a hard upper limit on the obscured star formation rate of <0.6 M e yr −1 (4σ) in a typical low-mass galaxy. The correlation between the infrared excess (IRX) of UV-selected galaxies (L IR /L UV) and the UV-continuum slope is also seen in our ASPECS data and shows consistency with a Calzetti-like relation at >  M 10 9.5 and an SMC-like relation at lower masses. Using stellar mass and β measurements for z∼2 galaxies over the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey, we derive a new empirical relation between β and stellar mass and then use this correlation to show that our IRX-β and IRX-stellar mass relations are consistent with each other. We then use these constraints to express the IRX as a bivariate function of β and stellar mass. Finally, we present updated estimates of star formation rate density determinations at z>3, leveraging present improvements in the measured IRX and recent probes of ultraluminous far-IR galaxies at z>2. Unified Astronomy Thesaurus concepts: Lyman-break galaxies (979); Infrared excess (788); High-redshift galaxies (734); Dust continuum emission (412); Far infrared astronomy (529)

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“…From our SEDs, γ, the fraction of the dust heated by starlight above the lower cutoff U min (the minimum of the distribution of starlight intensity relative to the local interstellar radiation field), in Draine and Li's models cannot be constrained. We assume that the best value for the DGS sample is valid for the Hi-z LBGs (but the impact of this parameter on our result is limited to ±8%, estimated using the range found by (Álvarez-Márquez et al 2019) on a sample of 22000 LBGs at z ∼ 3.0). In addition to the dust continuum information, we use the emission in the restframe FUV and optical range to model the stellar populations.…”

Section: Building Spectral Energy Distributionsmentioning

confidence: 99%

Observational and theoretical constraints on the formation and early evolution of the first dust grains in galaxies at 5 < z < 10

Burgarella

Nanni

Hirashita

et al. 2020

A&A

Self Cite

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Context. The first generation of stars were born a few hundred million years after the big bang. These stars synthesized elements heavier than H and He, that are later expelled into the interstellar medium, initiating the rise of metals. Within this enriched medium, the first dust grains formed. This event is cosmological crucial for molecule formation as dust plays a major role by cooling lowmetallicity star-forming clouds which can fragment to create lower mass stars. Collecting information on these first dust grains is difficult because of the negative alliance of large distances and low dust masses. Aims. We combine the observational information from galaxies at redshifts 5 z 10 to constrain their dust emission and theoretically understand the first evolutionary phases of the dust cycle. Methods. Spectral energy distributions (SEDs) are fitted with CIGALE and the physical parameters and their evolution are modelled. From this SED fitting, we build a dust emission template for this population of galaxies in the epoch of reionization. Results. Our new models explain why some early galaxies are observed and others are not. We follow in time the formation of the first grains by supernovae later destroyed by other supernova blasts and expelled in the circumgalactic and intergalactic media. Conclusions. We have found evidence for the first dust grains formed in the universe. But, above all, this paper underlines the need to collect more data and to develop new facilities to further constrain the dust cycle in galaxies in the epoch of reionization.

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Rest-frame far-ultraviolet to far-infrared view of Lyman break galaxies at z = 3: Templates and dust attenuation

Cited by 42 publications

References 124 publications

Tracing the evolution of dust-obscured activity using sub-millimetre galaxy populations from STUDIES and AS2UDS

Tracing the evolution of dust-obscured activity using sub-millimetre galaxy populations from STUDIES and AS2UDS

The ALMA Spectroscopic Survey Large Program: The Infrared Excess of z = 1.5–10 UV-selected Galaxies and the Implied High-redshift Star Formation History

Observational and theoretical constraints on the formation and early evolution of the first dust grains in galaxies at 5 < z < 10

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