KAOSS: turbulent, but disc-like kinematics in dust-obscured star-forming galaxies at $z\sim$1.3-2.6

Birkin, Jack E.; Smail, Ian; M., Swinbank, A.; An, Fang Xia; Chapman, S. C.; Chen, Chian-Chou; Conselice, C. J.; Dudzevičiūtė, U.; D., Farrah,; Matsuda, Y.; Puglisi, A.; Schinnerer, E.; Scott, D.; Wardlow, J. L.; Werf, P. van der

doi:10.48550/arxiv.2301.05720

Cited by 3 publications

(2 citation statements)

References 97 publications

(196 reference statements)

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“…In addition to showing clear rotation, the low velocity dispersion of Az9 (26 km s −1 ) suggests that it is stable. Dusty star-forming galaxies at z ∼ 2 from the KAOSS survey have average rotational velocities and velocity dispersions from ionized gas of 190 and 90 km s −1 , respectively (Birkin et al 2023). Even though these dusty galaxies are technically rotation-dominated, their high dispersion suggests turbulent rotating disks.…”

Section: A Stable Rotating Gas Diskmentioning

confidence: 99%

ALMA Reveals a Stable Rotating Gas Disk in a Paradoxical Low-mass, Ultradusty Galaxy at z = 4.274

Pope

McKinney

Kamieneski

et al. 2023

ApJL

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We report ALMA detections of [C ii] and a dust continuum in Az9, a multiply imaged galaxy behind the Frontier Field cluster MACS J0717.5+3745. The bright [C ii] emission line provides a spectroscopic redshift of z = 4.274. This strongly lensed (μ = 7 ± 1) galaxy has an intrinsic stellar mass of only 2 × 109 M ⊙ and a total star formation rate of 26 M ⊙ yr−1 (∼80% of which is dust-obscured). Using public magnification maps, we reconstruct the [C ii] emission in the source plane to reveal a stable, rotation-dominated disk with V/σ = 5.3, which is >2× higher than predicted from simulations for similarly high-redshift, low-mass galaxies. In the source plane, the [C ii] disk has a half-light radius of 1.8 kpc and, along with the dust, is spatially offset from the peak of the stellar light by 1.4 kpc. Az9 is not deficient in [C ii]; L [C II]/L IR = 0.0027, consistent with local and high-redshift normal star-forming galaxies. While dust-obscured star formation is expected to dominate in higher-mass galaxies, such a large reservoir of dust and gas in a lower-mass disk galaxy 1.4 Gyr after the Big Bang challenges our picture of early galaxy evolution. Furthermore, the prevalence of such low-mass dusty galaxies has important implications for the selection of the highest-redshift dropout galaxies with JWST. As one of the lowest stellar mass galaxies at z > 4 to be detected in a dust continuum and [C ii], Az9 is an excellent laboratory in which to study early dust enrichment in the interstellar medium.

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Section: A Stable Rotating Gas Diskmentioning

confidence: 99%

ALMA Reveals a Stable Rotating Gas Disk in a Paradoxical Low-mass, Ultradusty Galaxy at z = 4.274

Pope

McKinney

Kamieneski

et al. 2023

ApJL

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“…Extensive observations with the kiloparsec-scale nearinfrared Integral-Field-Unit (IFU) of SFGs around cosmic noon (1 ≤ z ≤ 3, e.g., Law et al 2009;Stott et al 2016;Förster Schreiber et al 2018;Mieda et al 2016;Mason et al 2017;Turner et al 2017;Wisnioski et al 2019;Birkin et al 2023) have found a significant increase in the gas velocity dispersion (∼50−100 km s −1 ) compared to local SFG values (∼20−25 km s −1 , Andersen et al 2006;Epinat et al 2010). Notably, the rotation-to-dispersion ratio (V rot /σ) for cosmicnoon disks typically falls in the range 1−10 (Law et al 2009;Gnerucci et al 2011;Genzel et al 2011;Johnson et al 2018;Birkin et al 2023), in contrast to the value of 10−20 observed in Milky Way and other local spiral disks (Epinat et al 2010). As a result, a significant conclusion drawn by these studies was that SFGs become dynamically hotter, featuring substantial pressure support, toward high-z.…”

Section: Introductionmentioning

confidence: 99%

Dynamically cold disks in the early Universe: Myth or reality?

Kohandel,

Pallottini,

Ferrara

et al. 2024

A&A

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Theoretical models struggle to reproduce dynamically cold disks with significant rotation-to-dispersion support ($V_ rot observed in star-forming galaxies in the early Universe at redshift $z>4$. We aim to explore the possible emergence of dynamically cold disks in cosmological simulations and to understand whether different kinematic tracers can help reconcile the tension between theory and observations. We used 3218 galaxies from the serra suite of zoom-in simulations, with $8 (M_ odot) 10.3$ and star formation rates $ SFR within the $4 z 9$ range. We generated hyperspectral data cubes for $2 synthetic observations of Halpha and CII We find that the choice of kinematic tracer strongly influences gas velocity dispersion (sigma ) estimates. In Halpha ( synthetic observations, we observe a strong (mild) correlation between sigma and $M_ This difference mostly arises for $M_ galaxies, for which $ for a significant fraction of the sample. Regardless of the tracer, our predictions suggest the existence of massive ($M_ galaxies with rot > 10$ at $z>4$, maintaining cold disks for $>10$ orbital periods ($ Myr $). Furthermore, we find no significant redshift dependence for the $V_ rot ratio in our sample. Our simulations predict the existence of dynamically cold disks in the early Universe. However, different tracers are sensitive to different kinematic properties. While effectively traces the thin gaseous disk of galaxies, Halpha includes the contribution from ionized gas beyond the disk region, characterized by prevalent vertical or radial motions that may be associated with outflows. We show that Halpha halos could be a signature of these galactic outflows. This result emphasizes the importance of combining ALMA and JWST/NIRspec studies of high-$z$ galaxies.

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Disc settling and dynamical heating: histories of Milky Way-mass stellar discs across cosmic time in the FIRE simulations

McCluskey,

Wetzel,

Loebman

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We study the kinematics of stars both at their formation and today within 14 Milky Way (MW)-mass galaxies from the FIRE-2 cosmological zoom-in simulations. We quantify the relative importance of cosmological disc settling and post-formation dynamical heating. We identify three eras: a Pre-Disc Era (typically ≳ 8 Gyr ago), when stars formed on dispersion-dominated orbits; an Early-Disc Era (≈8–4 Gyr ago), when stars started to form on rotation-dominated orbits but with high velocity dispersion, σform; and a Late-Disc Era (≲ 4 Gyr ago), when stars formed with low σform. σform increased with time during the Pre-Disc Era, peaking ≈8 Gyr ago, then decreased throughout the Early-Disc Era as the disc settled and remained low throughout the Late-Disc Era. By contrast, the dispersion measured today, σnow, increases monotonically with age because of stronger post-formation heating for Pre-Disc stars. Importantly, most of σnow was in place at formation, not added post-formation, for stars younger than ≈10 Gyr. We compare the evolution of the three velocity components: at all times, σR, form > σϕ, form > σZ, form. Post-formation heating primarily increased σR at ages ≲ 4 Gyr but acted nearly isotropically for older stars. The kinematics of young stars in FIRE-2 broadly agree with the range observed across the MW, M31, M33, and PHANGS-MUSE galaxies. The lookback time that the disc began to settle correlates with its dynamical state today: earlier-settling galaxies currently form colder discs. Including stellar cosmic-ray feedback does not significantly change disc rotational support at fixed stellar mass.

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KAOSS: turbulent, but disc-like kinematics in dust-obscured star-forming galaxies at $z\sim$1.3-2.6

Cited by 3 publications

References 97 publications

ALMA Reveals a Stable Rotating Gas Disk in a Paradoxical Low-mass, Ultradusty Galaxy at z = 4.274

ALMA Reveals a Stable Rotating Gas Disk in a Paradoxical Low-mass, Ultradusty Galaxy at z = 4.274

Dynamically cold disks in the early Universe: Myth or reality?

Disc settling and dynamical heating: histories of Milky Way-mass stellar discs across cosmic time in the FIRE simulations

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