A Noncorotating Gas Component in an Extreme Starburst at z = 4.3

Tadaki, Ken-ichi; Iono, Daisuke; Yun, Min S.; Aretxaga, I.; Hatsukade, Bunyo; Lee, Minju; Michiyama, Tomonari; Nakanishi, Koichiro; Saito, Toshiki; Ueda, Junko; Umehata, Hideki

doi:10.3847/1538-4357/ab64f4

Cited by 27 publications

(21 citation statements)

References 73 publications

(91 reference statements)

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“…The sample of SMGs and their proposed cQGs descendants at z ∼ 2 are located in distinct regions of the diagram, but the separation is what is expected given that the SMGs will grow in stellar mass in their current starburst episode and in size due to the observed minor mergers, bringing the location of the populations into agreement and furthering the strength of their evolutionary connection. This evolutionary sequence is also strengthened by recent analysis showing evidence for gaseous rotationally-support disks in some of the SMGs in the sample (e.g., Jones et al 2017;Tadaki et al 2020) and other results on z ∼ 2 cQGs exhibiting rotationally-supported stellar disks (Newman et al 2015;Toft et al 2017).…”

Section: Connecting Submillimeter and Quiescent Galaxiessupporting

confidence: 73%

High-redshift starbursts as progenitors of massive galaxies

Gómez-Guijarro

2019

Proc. IAU

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Starbursting dust-rich galaxies are capable of assembling large amounts of stellar mass very quickly. They have been proposed as progenitors of the population of compact massive quiescent galaxies at z ˜ 2. To test this connection, we present a detailed spatially-resolved study of the stars, dust, and stellar mass in a sample of six submillimeter-bright starburst galaxies at z ˜ 4.5. We found that the systems are undergoing minor mergers and the bulk star formation is located in extremely compact regions. On the other hand, optically-compact star forming galaxies have also been proposed as immediate progenitors of compact massive quiescent galaxies. Were they formed in slow secular processes or in rapid merger-driven starbursts? We explored the location of galaxies with respect to star-forming and structural relations and study the burstiness of star formation. Our results suggest that compact star-forming galaxies could be starbursts winding down and eventually becoming quiescent.

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Section: Connecting Submillimeter and Quiescent Galaxiessupporting

confidence: 73%

High-redshift starbursts as progenitors of massive galaxies

Gómez-Guijarro

2019

Proc. IAU

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“…The significant lower velocity dispersion observed in this component imply that F07599NE may have a different origin from F07599S. Similar gas substructure has been observed in high-z starbursts in [C ii] emission but with a much smaller physical separation (∼ 2 kpc; Tadaki et al 2020), where the formation of subcomponent is expected to be associated with a gravitationally unstable disk or shocks. By contrast, the large physical separation (projected distance of ∼ 19 kpc) observed between F07599NE and the galaxy nucleus indicates that the CO plume feature observed in the NE direction could be a separate component, likely associated with the tidal debris reminiscent of a previous merger.…”

Section: Origin Of the Off-center Co Componentssupporting

confidence: 53%

Deep Observations of CO and Free-Free Emission in Ultraluminous Infrared QSO IRAS F07599+6508

Tan,

Gao,

Daddi

et al. 2021

Preprint

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Infrared quasi-stellar objects (IR QSOs) are a rare subpopulation selected from ultraluminous infrared galaxies (ULIRGs) and have been regarded as promising candidates of ULIRG-to-optical QSO transition objects. Here we present NOEMA observations of the CO(1−0) line and 3 mm continuum emission in an IR QSO IRAS F07599+6508 at z = 0.1486, which has many properties in common with Mrk 231. The CO emission is found to be resolved with a major axis of ∼6.1 kpc that is larger than the size of ∼4.0 kpc derived for 3 mm continuum. We identify two faint CO features located at a projected distance of ∼11.4 and 19.1 kpc from the galaxy nucleus, respectively, both of which are found to have counterparts in the optical and radio bands and may have a merger origin. A systematic velocity gradient is found in the CO main component, suggesting that the bulk of molecular gas is likely rotationally supported. Based on the radio-to-millimeter spectral energy distribution and IR data, we estimate that about 30% of the flux at 3 mm arises from free-free emission and infer a free-free-derived star formation rate of 77 M ⊙ yr −1 , close to the IR estimate corrected for the AGN contribution. We find a high-velocity CO emission feature at the velocity range of about −1300 to −2000 km s −1 . Additional deep CO observations are needed to confirm the presence of a possible very high-velocity CO extension of the OH outflow in this IR QSO.

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“…A vast sample of rotating galaxies has been well studied at < 4 (e.g., Epinat et al 2008;Förster Schreiber et al 2009;Gnerucci et al 2011), revealing dynamical masses and empirical scaling relations. While a number of clumpy or merging galaxies have been detected at > 4 (e.g., Carniani et al 2018;Pavesi et al 2018;Díaz-Santos et al 2018), and a handful of rotating starburst or quasar host galaxies at ∼ 4 − 6 have been well-modelled (e.g., Jones et al 2017;Pensabene et al 2020;Tadaki et al 2020;Fraternali et al 2021;Lelli et al 2021), only two unlensed rotating main sequence galaxies have been observed at ∼ 4 − 6: HZ9 (Capak et al 2015) and J0817 (Neeleman et al 2017(Neeleman et al , 2020 5 . In this section, we add six new ∼ 4 − 6 rotators from the ALPINE sample to this class: CG32, DC396844, DC494057, DC552206, DC881725, and VC.7875.…”

Section: Main Sequence Rotators At Z>4mentioning

confidence: 99%

The ALPINE-ALMA [C ii] Survey: kinematic diversity and rotation in massive star-forming galaxies at z ~ 4.4–5.9

Jones

Vergani

Romano

et al. 2021

Monthly Notices of the Royal Astronomical Society

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While the kinematics of galaxies up to z ∼ 3 have been characterized in detail, only a handful of galaxies at high redshift (z > 4) have been examined in such a way. The Atacama Large Millimeter/submillimeter Array (ALMA) Large Program to INvestigate [CII] at Early times (ALPINE) survey observed a statistically significant sample of 118 star-forming main sequence galaxies at z = 4.4 − 5.9 in [CII]158μm emission, increasing the number of such observations by nearly 10x. A preliminary qualitative classification of these sources revealed a diversity of kinematic types (i.e., rotators, mergers, and dispersion-dominated systems). In this work, we supplement the initial classification by applying quantitative analyses to the ALPINE data: a tilted ring model (TRM) fitting code (3DBarolo), a morphological classification (Gini-M20), and a set of disk identification criteria. Of the 75 [CII]-detected ALPINE galaxies, 29 are detected at sufficient significance and spatial resolution to allow for TRM fitting and the derivation of morphological and kinematic parameters. These 29 sources constitute a high-mass subset of the ALPINE sample (M* > 109.5 M⊙). We robustly classify 14 of these sources (six rotators, five mergers, and three dispersion-dominated systems); the remaining sources showing complex behaviour. By exploring the G-M20 of z > 4 rest-frame FIR and [CII] data for the first time, we find that our 1″ ∼ 6 kpc resolution data alone are insufficient to separate galaxy types. We compare the rotation curves and dynamical mass profiles of the six ALPINE rotators to the two previously detected z ∼ 4 − 6 unlensed main sequence rotators, finding high rotational velocities (∼50 − 250 km s−1) and a diversity of rotation curve shapes.

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A Noncorotating Gas Component in an Extreme Starburst at z = 4.3

Cited by 27 publications

References 73 publications

High-redshift starbursts as progenitors of massive galaxies

High-redshift starbursts as progenitors of massive galaxies

Deep Observations of CO and Free-Free Emission in Ultraluminous Infrared QSO IRAS F07599+6508

The ALPINE-ALMA [C ii] Survey: kinematic diversity and rotation in massive star-forming galaxies at z ~ 4.4–5.9

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