Compact Dust Emission in a Gravitationally Lensed Massive Quiescent Galaxy at z = 2.15 Revealed in ∼130 pc Resolution Observations by the Atacama Large Millimeter/submillimeter Array

Morishita, Takahiro; Abdurrouf,; Hirashita, Hiroyuki; Newman, Andrew B.; Stiavelli, M.; Chiaberge, M.

doi:10.3847/1538-4357/ac9055

Cited by 7 publications

(2 citation statements)

References 86 publications

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“…This suggests distinct regions of high and low dust obscuration. Similar conditions have been observed in quiescent galaxies at later times (e.g., Morishita et al 2022;Lee et al 2024;Setton et al 2024).…”

Section: Impact Of Dust Attenuation On Observed Quiescencesupporting

confidence: 83%

Dead or Alive? How Bursty Star Formation and Patchy Dust Can Cause Temporary Quiescence in High-redshift Galaxies

Faisst,

Morishita

2024

ApJ

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The recent discovery of a galaxy at z = 7.3 with undetected optical emission lines and a blue UV-to-optical continuum ratio in JWST spectroscopy is surprising and needs to be explained physically. Here, we explore two possibilities that could cause such a seemingly quiescent ∼5 × 108 M ⊙ galaxy in the early Universe: (i) stochastic variations in the star formation history (SFH) and (ii) the effect of spatially varying dust attenuation on the measured line and continuum emission properties. Both scenarios can play out at the same time to amplify the effect. A stochastic star formation model (similar to realistic SFHs from hydrodynamical simulations of similar-mass galaxies) can create such observed properties if star formation is fast-varying with a correlation time of <150 Myr given a reasonable burst amplitude of ∼0.6 dex. The total time spent in this state is less than 20 Myr, and the likelihood of such a state to occur over 500 Myr at z = 7 is ∼50% (consistent with current observations). On the other hand, we show that a spectrum with blue UV continuum and lack of emission lines can be reproduced by a blue+red composite spectrum. The UV continuum is emitted from dust-free density-bounded H ii regions (blue component), while the red component is a dust-obscured starburst with weakened emission lines due to strong differential dust attenuation between stellar and nebular emission. Future resolving far-infrared observations with the Atacama Large Millimeter/submillimeter Array will shed light on the latter scenario.

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Section: Impact Of Dust Attenuation On Observed Quiescencesupporting

confidence: 83%

Dead or Alive? How Bursty Star Formation and Patchy Dust Can Cause Temporary Quiescence in High-redshift Galaxies

Faisst,

Morishita

2024

ApJ

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“…Indeed, spatially resolved studies of quiescent galaxies at slightly lower redshift (z ∼ 2, about 1 billion yr later) show a diverse range of formation pathways, with examples of both inside-out and outside-in quenching (Akhshik et al 2023). Evidence for residual dustobscured star formation in the cores of these early massive galaxies is confirmed through high-resolution millimeter wavelength detections in some cases (Morishita et al 2022;Lee et al 2023), but ruled out in others (Whitaker et al 2021).…”

Section: Discussionmentioning

confidence: 95%

Remarkably Compact Quiescent Candidates at 3 < z < 5 in JWST-CEERS

Wright,

Whitaker,

Weaver

et al. 2024

ApJL

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In this Letter, we measure the rest-frame optical and near-infrared sizes of 10 quiescent candidates at 3 < z < 5, first reported by Carnall et al. We use James Webb Space Telescope Near-Infrared Camera F277W and F444W imaging obtained through the public CEERS Early Release Science program and imcascade, an astronomical fitting code that utilizes multi-Gaussian expansion, to carry out our size measurements. When compared to the extrapolation of rest-optical size–mass relations for quiescent galaxies at lower redshift, 8 out of 10 candidates in our sample (80%) are on average more compact by ∼40%. A total of 7 out of 10 candidates (70%) exhibit rest-frame infrared sizes ∼10% smaller than rest-frame optical sizes, indicative of negative color gradients. Two candidates (20%) have rest-frame infrared sizes ∼1.4× larger than rest-frame optical sizes; one of these candidates exhibits signs of ongoing or residual star formation, suggesting this galaxy may not be fully quenched. The remaining candidate is unresolved in both filters, which may indicate an active galactic nucleus. Strikingly, we observe three of the most massive galaxies in the sample (log(M ⋆/M ⊙) = 10.74–10.95) are extremely compact, with effective radii ∼0.7 kpc. Our findings provide no indication that the size evolution relation flattens out, and may indicate that the size evolution of quiescent galaxies is steeper than previously anticipated beyond z > 3.

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The gas mass reservoir of quiescent galaxies at cosmic noon

Blánquez¹,

Gómez-Guijarro²,

Magdis³

et al. 2023

A&A

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We present a 1.1 mm stacking analysis of moderately massive (log(M*/M⊙) = 10.7 ± 0.2) quiescent galaxies (QGs) at ⟨z⟩∼1.5, searching for cold dust continuum emission, which serves as an excellent tracer of dust and gas mass. Using both the recent GOODS-ALMA survey, as well as the full suite of ALMA Band-6 ancillary data in the GOODS-S field, we report the tentative detection of a dust continuum equivalent of the dust mass log(Mdust/M⊙) = 7.47 ± 0.13 and gas mass log(Mgas/M⊙) = 9.42 ± 0.14. The emerging gas fraction is fgas = 5.3 ± 1.8%, consistent with the results of previous stacking analyses based on lower resolution sub(mm) observations. Our results support the scenario where high-z QGs exhibit a larger fgas value by one order of magnitude compared to their local counterparts and have experienced quenching with a non-negligible gas reservoir in their interstellar medium, namely, with gas retention. Our subsequent analysis yields an anti-correlation between the fgas and the stellar mass of QGs, especially in the high-mass end where galaxies reside in the most massive halos. The fgas − M* anti-correlation promotes the selection bias as a possible solution to the tension between the stacking results pointing towards gas retention in high-z QGs of moderate M* and studies of individual targets that favour a fully depleted ISM in massive (log(M*/M⊙) > 11.2) high-z QGs.

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Compact Dust Emission in a Gravitationally Lensed Massive Quiescent Galaxy at z = 2.15 Revealed in ∼130 pc Resolution Observations by the Atacama Large Millimeter/submillimeter Array

Cited by 7 publications

References 86 publications

Dead or Alive? How Bursty Star Formation and Patchy Dust Can Cause Temporary Quiescence in High-redshift Galaxies

Dead or Alive? How Bursty Star Formation and Patchy Dust Can Cause Temporary Quiescence in High-redshift Galaxies

Remarkably Compact Quiescent Candidates at 3 < z < 5 in JWST-CEERS

The gas mass reservoir of quiescent galaxies at cosmic noon

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