Turbulent Gas in Lensed Planck-selected Starbursts at redshifts 1-3.5

Harrington, Kevin C.; Weiss, Axel; Yun, Min S.; Magnelli, Benjamin; Sharon, C. E.; Leung, T. K. D.; Vishwas, A.; Wang, Q. D.; Jimenez-Andrade, E. F.; Frayer, D. T.; Liu, D.; Garcia, P.; Romano-Diaz, E.; Frye, B. L.; Jarugula, S.; Badescu, T.; Berman, D.; Dannerbauer, H.; Diaz-Sanchez, A.; Grassitelli, L.; Kamieneski, P.; Kim, W. J.; Kirkpatrick, A.; Lowenthal, J. D.; Messias, H.; Puschnig, J.; Stacey, G. J.; Torne, P.; Bertoldi, F.

doi:10.48550/arxiv.2010.16231

Cited by 2 publications

(2 citation statements)

References 325 publications

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“…Despite its narrow linewidth, the total cold gas reservoir inferred from the CO(1-0) emission in SMM J13120 has a mass of (13 ± 3) × 10 10 M , and is extended over ∼16 kpc in diameter. Although the revised CO(1-0) luminosity is significantly lower than previous estimates (R11), we additionally find that the CO SLED still suggests the presence of two gas components to account for all the recovered CO(1-0) emission, including a diffuse component with T kin = 25±5 K and a warmer, denser component with T kin = 40±5 K. These findings are in line with other studies of high-z systems with available low-J CO detections (see e.g., Ivison et al 2011;Riechers et al 2011;Hodge et al 2013, for unlensed galaxies, and Yang et al 2017;Cañameras et al 2018;Harrington et al 2020, for lensed sources), reinforcing the importance of low-J CO observations for establishing the nature of the molecular gas reservoirs in high-z systems and their role in early galaxy evolution.…”

Section: Gas Excitationsupporting

confidence: 90%

Kiloparsec-scale imaging of the CO(1-0)-traced cold molecular gas reservoir in a z~3.4 submillimeter galaxy

Castillo,

Rybak,

Hodge

et al. 2022

Preprint

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We present a high-resolution study of the cold molecular gas as traced by CO(1-0) in the unlensed z∼3.4 submillimeter galaxy SMM J13120+4242, using multi-configuration observations with the Karl G. Jansky Very Large Array (JVLA). The gas reservoir, imaged on 0.39" (∼3 kpc) scales, is resolved into two components separated by ∼11 kpc with a total extent of 16 ± 3 kpc. Despite the large spatial extent of the reservoir, the observations show a CO(1-0) FWHM linewidth of only 267 ± 64 km s −1 . We derive a revised line luminosity of L CO(1-0) = (10 ± 3) × 10 10 K km s −1 pc 2 and a molecular gas mass of M gas = (13 ± 3) × 10 10 (α CO /1) M . Despite the presence of a velocity gradient (consistent with previous resolved CO(6-5) imaging), the CO(1-0) imaging shows evidence for significant turbulent motions which are preventing the gas from fully settling into a disk. The system likely represents a merger in an advanced stage. Although the dynamical mass is highly uncertain, we use it to place an upper limit on the CO-to-H 2 mass conversion factor α CO of 1.4. We revisit the SED fitting, finding that this galaxy lies on the very massive end of the main sequence at z=3.4. Based on the low gas fraction, short gas depletion time and evidence for a central AGN, we propose that SMM J13120 is in a rapid transitional phase between a merger-driven starburst and an unobscured quasar. The case of SMM J13120 highlights the how mergers may drive important physical changes in galaxies without pushing them off the main sequence.

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Section: Gas Excitationsupporting

confidence: 90%

Kiloparsec-scale imaging of the CO(1-0)-traced cold molecular gas reservoir in a z~3.4 submillimeter galaxy

Castillo,

Rybak,

Hodge

et al. 2022

Preprint

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“…Yet their optical to mid-IR SEDs are usually not well sampled. Harrington et al (2020) present a study of CO excitation and far-IR/(sub-)mm dust SED modeling in strongly lensed galaxies, based on a similar gas density PDF modeling.…”

Section: High-z Sb Smgsmentioning

confidence: 99%

CO excitation, molecular gas density and interstellar radiation field in local and high-redshift galaxies

Liu,

Daddi,

Schinnerer

et al. 2021

Preprint

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We study the Carbon Monoxide (CO) excitation, mean molecular gas density and interstellar radiation field (ISRF) intensity in a comprehensive sample of 76 galaxies from local to high redshift (z ∼ 0 − 6), selected based on detections of their CO transitions J = 2 → 1 and 5 → 4 and their optical/infrared/(sub-)millimeter spectral energy distributions (SEDs). We confirm the existence of a tight correlation between CO excitation as traced by the CO(5-4)/(2-1) line ratio R 52 , and the mean ISRF intensity U as derived from infrared SED fitting using dust SED templates. By modeling the molecular gas density probability distribution function (PDF) in galaxies and predicting CO line ratios with large velocity gradient radiative transfer calculations, we present a framework linking global CO line ratios to the mean molecular hydrogen gas density n H2 and kinetic temperature T kin . Mapping in this way observed R 52 ratios to n H2 and T kin probability distributions, we obtain positive Un H2 and U -T kin correlations, which imply a scenario in which the ISRF in galaxies is mainly regulated by T kin and (non-linearly) by n H2 . A small fraction of starburst galaxies showing enhanced n H2 could be due to merger-driven compaction. Our work demonstrates that ISRF and CO excitation are tightly coupled, and that density-PDF modeling is a promising tool for probing detailed ISM properties inside galaxies.

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Turbulent Gas in Lensed Planck-selected Starbursts at redshifts 1-3.5

Cited by 2 publications

References 325 publications

Kiloparsec-scale imaging of the CO(1-0)-traced cold molecular gas reservoir in a z~3.4 submillimeter galaxy

Kiloparsec-scale imaging of the CO(1-0)-traced cold molecular gas reservoir in a z~3.4 submillimeter galaxy

CO excitation, molecular gas density and interstellar radiation field in local and high-redshift galaxies

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