Normal, dust-obscured galaxies in the epoch of reionization

Fudamoto, Yoshinobu; Oesch, Pascal; Schouws, Sander; Stefanon, Mauro; Smit, Renske; Bouwens, Rychard; Bowler, R. A. A.; Endsley, Ryan; González, Valentino; Inami, Hanae; Labbé, Ivo; Stark, Daniel P.; Aravena, M.; Barrufet, L.; Cunha, Elisabete da; Dayal, Pratika; Ferrara, Andrea; Graziani, Luca; Hodge, J. A.; Hutter, Anne; Li, Y.; Looze, I. De; Nanayakkara, Themiya; Pallottini, Andrea; Riechers, Dominik A.; Schneider, R.; Ucci, Graziano; Werf, P. van der; White, Courtney

doi:10.1038/s41586-021-03846-z

Cited by 96 publications

(84 citation statements)

References 65 publications

(80 reference statements)

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“…The [CII]158µm line is especially interesting as it is the strongest cooling line of warm gas (T < 10 4 K) in galaxies. This line has already been detected in a significant number of galaxies out to z ∼ 7-8 (e.g., Walter et al 2009;Wagg et al 2010;Riechers et al 2014;Willott et al 2015;Capak et al 2015;Maiolino et al 2015;Pentericci et al 2016;Knudsen et al 2016;Bradač et al 2017;Smit et al 2018;Matthee et al 2017Matthee et al , 2019Harikane et al 2020;Carniani et al 2020;Le Fèvre et al 2020;Béthermin et al 2020;Venemans et al 2020;Fudamoto et al 2021). In addition to the immediate utility of [CII] to spectroscopically confirm galaxies in the reionization era and obtain a precise measurement of their redshift, the strength of this line makes it one of the prime features for studying the kinematics of high-z galaxies (e.g., Smit et al 2018;Hashimoto et al 2019;.…”

Section: Introductionmentioning

confidence: 94%

ALMA as a Redshift Machine: Using [CII] to Efficiently Confirm Galaxies in the Epoch of Reionization

Schouws¹,

Smit²,

Hodge³

et al. 2022

Preprint

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The [CII] 158µm line has long been proposed as a promising line to spectroscopically confirm galaxies in the epoch of reionization. In this paper we present the results of new ALMA observations spectral scanning for [CII] in six particularly luminous Lyman Break Galaxies at z ∼ 7. The six sources were drawn from a sample of bright z ∼ 7 galaxies identified using the wide-area optical, near-IR, and Spitzer /IRAC data over the COSMOS/UltraVISTA field and were targeted on the basis of tight constraints on their redshifts from their IRAC [3.6]-[4.5] colors. We detect significant (> 9σ) [CII] lines in three of our six targets (50%) co-spatial with the rest-U V emission from the ground/space-based near-IR imaging. The luminosities of the [CII] lines lie in the range 5.6 to 8.8 × 10 8 L , consistent with the local [CII]-SFR relation. Meanwhile, their [CII]/L IR ∼ 1 − 3 × 10 −3 ratios are slightly elevated compared to local (U)LIRGS. This could be due to lower dust-to-gas or dust-to-metal ratios. We also find that our sources display a large kinematic diversity, with one source showing signs of rotation, one source a likely major merger and one dispersion dominated source that might contain a bright star-forming clump. Our results highlight the effectiveness of spectral scans with ALMA in spectroscopically confirming luminous galaxies in the epoch of reionization, something that is being be applied on a significantly larger sample in the on-going REBELS large program.

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Section: Introductionmentioning

confidence: 94%

ALMA as a Redshift Machine: Using [CII] to Efficiently Confirm Galaxies in the Epoch of Reionization

Schouws¹,

Smit²,

Hodge³

et al. 2022

Preprint

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“…2022) indicate that TSED increases towards high redshifts. Thus, the IRX value of the currently available targets might be underestimated, perhaps indicating that at least some of the galaxies in the EoR are already highly obscured (Fudamoto et al 2021). More robust dust temperature measurements, only made possible through high-frequency ALMA observations (e.g.…”

Section: Continuum Propertiesmentioning

confidence: 99%

“…10), a feature shared by many high-z observed targets. Also, some of the rebels galaxies appear as scaled-down versions of dusty star forming galaxies (Fudamoto et al 2021).…”

Section: Loozementioning

confidence: 99%

A survey of high-$z$ galaxies: SERRA simulations

Pallottini,

Ferrara,

Gallerani

et al. 2022

Preprint

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We introduce serra, a suite of zoom-in high-resolution (∼ 10 pc) cosmological simulations including non-equilibrium chemistry and on-the-fly radiative transfer. The outputs are post-processed to derive galaxy UV+FIR continuum and emission line properties. Results are compared with available multi-wavelength data to constrain the physical properties (e.g., star formation rates, stellar/gas/dust mass, metallicity) of high-redshift 6 < ∼ z < ∼ 15 galaxies. This flagship paper focuses on the z = 7.7 sub-sample, including 207 galaxies with stellar mass 10 7 M < ∼ M < ∼ 5×10 10 M , and specific star formation ranging from sSFR ∼ 100 Gyr −1 in young, low-mass galaxies to ∼ 10 Gyr −1 for older, massive ones. At this redshift, serra galaxies are typically bursty, i.e. they are located above the Schmidt-Kennicutt relation by a factor κ s = 3.03 +4.9 −1.8 , consistent with recent findings for [O III] and [C II] emitters at high-z. They also show relatively large IRX = L FIR /L UV values as a result of their compact/clumpy morphology effectively blocking the stellar UV luminosity. Note that this conclusion might be affected by insufficient spatial resolution at the molecular cloud level. We confirm that early galaxies lie on the standard [C II]−SFR relation; their observed L [OIII] /L [CII] 1−10 ratios are reproduced without the need of a top-heavy IMF and/or anomalous C/O abundances. [O I] line intensities are similar to local ones, making ALMA high-z detections challenging but feasible (∼ 6 hr for an SFR of 50 M yr −1 ).

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“…Indeed, FIR observations have now been used to estimate dust-to-stellar mass ratios ranging between 0.012 − 3% for "normal" star forming galaxies, with stellar masses M * ∼ 10 8.3−10.5 M , at z > ∼ 7 (e.g. Watson et al 2015;Laporte et al 2017;Marrone et al 2018;Hashimoto et al 2019;Bakx et al 2020;Reuter et al 2020;Fudamoto et al 2021;Schouws et al 2021).…”

Section: Introductionmentioning

confidence: 99%

“…REBELS focuses on studying 40 of the brightest galaxies at z > ∼ 6.5 over a 7 deg 2 area which are being scanned for both bright ISM cooling lines (such as those from [CII] 158 µm and [OIII] 88 µm) and dust continuum emission, as detailed in Bouwens et al (2021a). This survey has already serendipitously revealed two dusty star forming galaxies at z ∼ 7 (Fudamoto et al 2021) in addition to yielding a sample of 13 (continuum and CII detected) z ∼ 7 LBGs (Inami et al 2022, in prep;Schouws et al 2022, in prep. ) with M * ∼ 10 8.8−10.6 M (Stefanon et al 2022, in prep;Topping et al 2022, in prep.…”

Section: Introductionmentioning

confidence: 99%

The ALMA REBELS survey: the dust content of z ∼ 7 Lyman break galaxies

Dayal

Ferrara

Sommovigo

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We include a fully coupled treatment of metal and dust enrichment into the Delphi semi-analytic model of galaxy formation to explain the dust content of 13 Lyman Break Galaxies (LBGs) detected by the Atacama Large millimetre Array (ALMA) REBELS Large Program at z ≃ 7. We find that the galaxy dust mass, Md, is regulated by the combination of SNII dust production, astration, shock destruction, and ejection in outflows; grain growth (with a standard timescale τ0 = 30 Myr) plays a negligible role. The model predicts a dust-to-stellar mass ratio of $\sim 0.07-0.1{{\ \rm per\ cent}}$ and a UV-to-total star formation rate relation such that log(ψUV) = −0.05 [log(ψ)]2 + 0.86 log(ψ) − 0.05 (implying that 55-80 per cent of the star formation is obscured) for REBELS galaxies with stellar mass $M_* = 10^{9-10} \rm M_\odot$. This relation reconciles the intrinsic UV luminosity of LBGs with their observed luminosity function at z = 7. However, 2 out of the 13 systems show dust-to-stellar mass ratios ($\sim 0.94-1.1{{\ \rm per\ cent}}$) that are up to 18 × larger than expected from the fiducial relation. Due to the physical coupling between dust and metal enrichment, even decreasing τ0 to very low values (0.3 Myr) only increases the dust-to-stellar mass ratio by a factor ∼2. Given that grain growth is not a viable explanation for such high observed ratios of the dust-to-stellar mass, we propose alternative solutions.

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Normal, dust-obscured galaxies in the epoch of reionization

Cited by 96 publications

References 65 publications

ALMA as a Redshift Machine: Using [CII] to Efficiently Confirm Galaxies in the Epoch of Reionization

ALMA as a Redshift Machine: Using [CII] to Efficiently Confirm Galaxies in the Epoch of Reionization

A survey of high-$z$ galaxies: SERRA simulations

The ALMA REBELS survey: the dust content of z ∼ 7 Lyman break galaxies

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