J0107a: A Barred Spiral Dusty Star-forming Galaxy at z = 2.467

Huang, Shuo; Kawabe, Ryohei; Kohno, Kotaro; Saito, Toshiki; Mizukoshi, Shoichiro; Iono, Daisuke; Michiyama, Tomonari; Tamura, Yoichi; Hayward, Christopher C.; Umehata, Hideki

doi:10.3847/2041-8213/acff63

Cited by 5 publications

(4 citation statements)

References 80 publications

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“…Our new work is in response to Atacama Large Millimeter/ submillimeter Array (ALMA), Very Large Array, and integralfield spectroscopic observations of gas-rich, star-forming disks in the redshift range z ∼ 1-3 (Chapman et al 2004;Förster Schreiber et al 2006;Genzel et al 2006), supported by subsequent observations (Shapiro et al 2008;Swinbank et al 2012;Hodge et al 2019;Neeleman et al 2021;Rizzo et al 2022). Intriguingly, there are clear cases where the gas entirely dominates the baryon disk fraction (e.g., Hodge et al 2019;Rizzo et al 2022), and even here bar-like features and/or velocity fields are observed (Huang et al 2023;Neeleman et al 2023;Smail et al 2023;Amvrosiadis et al 2024;Tsukui et al 2024). In these instances, stellar bars are either weak or nonexistent.…”

Section: Introductionmentioning

confidence: 91%

“…To date, we are unaware of any claims of a dominated bar residing in a disk potential in the local Universe. The situation may be very different at high redshift, as discussed in the Introduction, with bar-like structures claimed in gas-dominated disks (e.g., Huang et al 2023;Tsukui et al 2024). In the early Universe, gas disks are likely to have formed before star formation commenced in the gas, as judged from the relative thinness of stellar disks at all epochs.…”

Section: Gaseous Bars and Their Evolutionmentioning

confidence: 99%

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Turbulent Gas-rich Disks at High Redshift: Bars and Bulges in a Radial Shear Flow

Bland-Hawthorn,

Tepper-Garcia,

Agertz

et al. 2024

ApJ

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Recent observations of high-redshift galaxies (z ≲ 7) reveal that a substantial fraction have turbulent, gas-rich disks with well-ordered rotation and elevated levels of star formation. In some instances, disks show evidence of spiral arms, with bar-like structures. These remarkable observations have encouraged us to explore a new class of dynamically self-consistent models using our agama/Ramses hydrodynamic N-body simulation framework that mimic a plausible progenitor of the Milky Way at high redshift. We explore disk gas fractions of f gas = 0%, 20%, 40%, 60%, 80%, and 100% and track the creation of stars and metals. The high gas surface densities encourage vigorous star formation, which in turn couples with the gas to drive turbulence. We explore three distinct histories: (i) there is no ongoing accretion and the gas is used up by the star formation, (ii) the star-forming gas is replenished by cooling in the hot halo gas, and (iii) in a companion paper, we revisit these models in the presence of a strong perturbing force. At low f disk (≲0.3), where f disk is the baryon mass fraction of the disk relative to dark matter within 2.2 R disk, a bar does not form in a stellar disk; this remains true even when gas dominates the inner disk potential. For a dominant baryon disk (f disk ≳ 0.5) at all gas fractions, the turbulent gas forms a strong radial shear flow that leads to an intermittent star-forming bar within about 500 Myr; turbulent gas speeds up the formation of bars compared to gas-free models. For f gas ≲ 60%, all bars survive, but for higher gas fractions, the bar devolves into a central bulge after 1 Gyr. The star-forming bars are reminiscent of recent discoveries in high-redshift Atacama Large Millimeter/submillimeter Array observations of gaseous disks.

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Section: Introductionmentioning

confidence: 91%

Section: Gaseous Bars and Their Evolutionmentioning

confidence: 99%

Turbulent Gas-rich Disks at High Redshift: Bars and Bulges in a Radial Shear Flow

Bland-Hawthorn,

Tepper-Garcia,

Agertz

et al. 2024

ApJ

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“…Disk galaxies tend to have spiral arms in the local Universe, and JWST's improved sensitivity compared to HST can possibly detect spiral structures in high-redshifted disk galaxies that HST was unable to provide. A couple of spiral galaxies were recently found at redshifts of z = 2.467 (Huang et al 2023) and z = 3.059 (Wu et al 2023) with the Atacama Large Millimeter/ submillimeter Array (ALMA) and JWST, and one barred spiral galaxy was discovered with JWST at z ; 3 Costantin et al (2023).…”

Section: Introductionmentioning

confidence: 99%

JWST Reveals a Surprisingly High Fraction of Galaxies Being Spiral-like at 0.5 ≤ z ≤ 4

Kuhn,

Guo,

Martin

et al. 2024

ApJL

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Spiral arms are one of the most important features used to classify the morphology of local galaxies. The cosmic epoch when spiral arms first appeared contains essential clues to the evolution of disk galaxies. In this Letter, we used James Webb Space Telescope images from the Cosmic Evolution Early Release Science Survey to visually identify spiral galaxies with redshift 0.5 ≤ z ≤ 4 and stellar mass ≥1010 M ⊙. Out of 873 galaxies, 216 were found to have a spiral structure. The spiral galaxies in our sample have higher star formation rates and larger sizes than nonspiral galaxies. We found the observed spiral fraction decreases from 48% at z ∼ 0.75 to 8% at z ∼ 2.75. These fractions are higher than the fractions observed with the Hubble Space Telescope. We even detect possible spiral-like features at redshifts z > 3. We artificially redshifted low-redshift galaxies to high redshifts and reinspected them to evaluate observational effects. By varying the input spiral fraction of the redshifted sample, we found that the input fraction of ∼35% matches the observed fraction at z = 2–3 the best. We are able to rule out spiral fractions being <20% (2σ) and <10% (3σ) for real galaxies at z ∼ 3. This fraction is surprisingly high and implies that the formation of spiral arms, as well as disks, was earlier in the Universe.

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“…The advent of the James Webb Space Telescope (JWST) is bringing the study of high-z DSFGs to a new level. In merely over a year, the synergy of JWST and ALMA has brought us a lot of details on the connection between dust-obscured and unobscured ("exposed") stellar populations in DSFGs (e.g., Chen et al 2022;Cheng et al 2022Cheng et al , 2023Álvarez-Márquez et al 2023;Barger & Cowie 2023;Boogaard et al 2024;Fujimoto et al 2023;Hashimoto et al 2023;Huang et al 2023;Kamieneski et al 2023;Liu et al 2024;Rujopakarn et al 2023;Tadaki et al 2023;Yoon et al 2023;Killi et al 2024;Sun et al 2024), including a subset among the so-called "HST-dark" galaxies that are faint or even invisible at λ  1.6 μm (e.g., Kokorev et al 2023;Smail et al 2023;Zavala et al 2023).…”

Section: Introductionmentioning

confidence: 99%

A Strongly Lensed Dusty Starburst of an Intrinsic Disk Morphology at a Photometric Redshift of z _ph > 7

Ling,

Sun,

Cheng

et al. 2024

ApJL

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We present COSBO-7, a strong millimeter source known for more than 16 yr that just revealed its near-to-mid-IR counterpart with the James Webb Space Telescope (JWST). The precise pinpointing by the Atacama Large Millimeter/submillimeter Array on the exquisite NIRCam and MIRI images show that it is a background source gravitationally lensed by a single foreground galaxy, and the analysis of its spectral energy distribution by different tools is in favor of photometric redshift at z ph > 7. Strikingly, our lens modeling based on the JWST data shows that it has a regular disk morphology in the source plane. The dusty region giving rise to the far-IR-to-millimeter emission seems to be confined to a limited region to one side of the disk and has a high dust temperature of >90 K. The galaxy is experiencing starburst both within and outside of this dusty region. After taking the lensing magnification of μ ≈ 2.5–3.6 into account, the intrinsic star formation rate is several hundred M ⊙ yr−1 both within the dusty region and across the more extended stellar disk, and the latter already has >1010 M ⊙ of stars in place. If it is indeed at z > 7, COSBO-7 presents an extraordinary case that is against the common wisdom about galaxy formation in the early Universe; simply put, its existence poses a critical question to be answered: how could a massive disk galaxy come into being so early in the Universe and sustain its regular morphology in the middle of an enormous starburst?

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J0107a: A Barred Spiral Dusty Star-forming Galaxy at z = 2.467

Cited by 5 publications

References 80 publications

Turbulent Gas-rich Disks at High Redshift: Bars and Bulges in a Radial Shear Flow

Turbulent Gas-rich Disks at High Redshift: Bars and Bulges in a Radial Shear Flow

JWST Reveals a Surprisingly High Fraction of Galaxies Being Spiral-like at 0.5 ≤ z ≤ 4

A Strongly Lensed Dusty Starburst of an Intrinsic Disk Morphology at a Photometric Redshift of z _ph > 7

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J0107a: A Barred Spiral Dusty Star-forming Galaxy at z = 2.467

Cited by 5 publications

References 80 publications

Turbulent Gas-rich Disks at High Redshift: Bars and Bulges in a Radial Shear Flow

Turbulent Gas-rich Disks at High Redshift: Bars and Bulges in a Radial Shear Flow

JWST Reveals a Surprisingly High Fraction of Galaxies Being Spiral-like at 0.5 ≤ z ≤ 4

A Strongly Lensed Dusty Starburst of an Intrinsic Disk Morphology at a Photometric Redshift of z ph > 7

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A Strongly Lensed Dusty Starburst of an Intrinsic Disk Morphology at a Photometric Redshift of z _ph > 7