Investigating the [C ii]-to-H i Conversion Factor and the H i Gas Budget of Galaxies at z ≈ 6 with Hydrodynamic Simulations

Vizgan, David; Heintz, K. E.; Greve, T. R.; Narayanan, Desika; Davé, Romeel; Olsen, Karen P.; Popping, Gergö; Watson, Derrick G.

doi:10.3847/2041-8213/ac982c

Cited by 8 publications

(3 citation statements)

References 48 publications

(102 reference statements)

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“…However, [C II] can also be used as a proxy for the neutral atomic H I gas mass (Heintz et al 2021(Heintz et al , 2022aVizgan et al 2022a) since it has been shown observationally to predominantly originate from the neutral gas phase in the Milky Way and nearby galaxies (Madden et al 1993(Madden et al , 1997Pineda et al 2014;Croxall et al 2017), with supporting evidence from high-redshift galaxy observations (e.g., Novak et al 2019;Meyer et al 2022) and simulations (Katz et al 2017;Ramos Padilla et al 2022) as well. We adopt the [C II]-to-H I calibration from Heintz et al (2021), prescribed as…”

Section: Disentangling the Baryonic Matter Budgetmentioning

confidence: 93%

The Gas and Stellar Content of a Metal-poor Galaxy at z = 8.496 as Revealed by JWST and ALMA

Heintz

Giménez-Arteaga

Fujimoto

et al. 2023

ApJL

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We present a joint analysis of the galaxy S04590 at z = 8.496 based on NIRSpec, NIRCam, and NIRISS observations obtained as part of the Early Release Observations program of the James Webb Space Telescope (JWST) and the far-infrared [C ii] 158 μm emission line detected by dedicated Atacama Large Millimeter/submillimeter Array (ALMA) observations. We determine the physical properties of S04590 from modeling of the spectral energy distribution (SED) and through the redshifted optical nebular emission lines detected with JWST/NIRSpec. The best-fit SED model reveals a low-mass (M ⋆ = 107.2–108 M ⊙) galaxy with a low oxygen abundance of 12 + log ( O / H ) = 7.16 − 0.12 + 0.10 derived from the strong nebular and auroral emission lines. Assuming that [C ii] effectively traces the interstellar medium, we estimate the total gas mass of the galaxy to be M gas = (8.0 ± 4.0) × 108 M ⊙ based on the luminosity and spatial extent of [C ii]. This yields an exceptionally high gas fraction, f gas = M gas/(M gas + M ⋆) ≳ 90%, though one still consistent with the range expected for low metallicity. We further derive the metal mass of the galaxy based on the gas mass and gas-phase metallicity, which we find to be consistent with the expected metal production from Type II supernovae. Finally, we make the first constraints on the dust-to-gas (DTG) and dust-to-metal (DTM) ratios of galaxies in the epoch of reionization at z ≳ 6, showing overall low mass ratios of logDTG < −3.8 and logDTM < −0.5, though they are consistent with established scaling relations and in particular with those of the local metal-poor galaxy I Zwicky 18. Our analysis highlights the synergy between ALMA and JWST in characterizing the gas, metal, and stellar content of the first generation of galaxies.

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Section: Disentangling the Baryonic Matter Budgetmentioning

confidence: 93%

The Gas and Stellar Content of a Metal-poor Galaxy at z = 8.496 as Revealed by JWST and ALMA

Heintz

Giménez-Arteaga

Fujimoto

et al. 2023

ApJL

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“…While these narrow pencil-beam sightlines do not provide information about the total gas mass of the absorbing galaxies, they can accurately determine the relative abundance between [C ii] and H i. This [C ii]-to-H i calibration has also been investigated with hydrodynamical simulations of galaxies at z ∼ 0−6, which were found to be in good agreement (Pallottini et al 2017;Vizgan et al 2022;Liang et al 2024).…”

Section: Introductionmentioning

confidence: 69%

A high-redshift calibration of the [O I]-to-H I conversion factor in star-forming galaxies

Wilson,

Heintz,

Jakobsson

et al. 2024

A&A

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The assembly and build-up of neutral atomic hydrogen ( in galaxies is one of the most fundamental processes in galaxy formation and evolution. Studying this process directly in the early universe is hindered by the weakness of the hyperfine 21-cm line transition, impeding direct detections and measurements of the gas masses HI $). Here we present a new method to infer $M_ HI $ of high-redshift galaxies using neutral, atomic oxygen as a proxy. Specifically, we derive metallicity-dependent conversion factors relating the far-infrared oi and oi emission line luminosities and HI $ in star-forming galaxies at $z 2-6$ using gamma-ray bursts (GRBs) as probes. We calibrate the oi -to- conversion factor relying on a sample of local galaxies with direct measurements of HI $ and oi and oi line luminosities in addition to the Sigamé hydrodynamical simulation framework at similar epochs ($ z $). We find that the oi m $-to- and oi m $-to- conversion factors, here denoted $ OI m $ and $ OI m $, respectively, universally appear to be anti-correlated with the gas-phase metallicity. The GRB measurements further predict a mean ratio of $L_ OI m / L_ OI m 0.12$ and reveal generally less excited cii over oi compared to the local galaxy sample. The $z 0$ galaxy sample also shows systematically higher $ OI m $ and $ OI m $ conversion factors than the GRB sample, indicating either suppressed oi emission in local galaxies likely due to their lower hydrogen densities or more extended, diffuse gas reservoirs traced by the 21-cm. Finally, we apply these empirical calibrations to the few detections of oi and oi line transitions at $ z $ from the literature and further discuss the applicability of these conversion factors to probe the gas content in the dense, star-forming interstellar medium (ISM) of galaxies well into the epoch of reionization.

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“…The bulk of its emission comes from neutral atomic gas arising in photo-dissociation regions (PDRs) surrounding young stars (Hollenbach & Tielens 1999) but, given its low ionization potential (11.3 eV, compared to the 13.6 eV of neutral hydrogen), it can also be emitted by the partly ionized (e.g., Cormier et al 2012;Pineda et al 2014) and molecular medium (e.g., Zanella et al 2018;Madden et al 2020). Furthermore, [CII] has been recently used to infer the neutral hydrogen (HI) gas mass in galaxies out to z ∼ 6 both with observations and simulations (e.g., Heintz et al 2021;Vizgan et al 2022). High-velocity outflows have been detected in the broad wings of the [CII] line profile in individual high-redshift luminous quasars (QSOs; e.g., Maiolino et al 2012;Cicone et al 2015) and in normal SFGs at z > 4 (e.g., Ginolfi et al 2020;Herrera-Camus et al 2021) thanks to the IRAM Plateau de Bure Interferometer and ALMA observations, respectively.…”

Section: Introductionmentioning

confidence: 99%

Star-formation-driven outflows in local dwarf galaxies as revealed from [CII] observations by Herschel

Romano¹,

Nanni²,

D.³

et al. 2023

A&A

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We characterize the physical properties of star-formation driven outflows in a sample of 29 local dwarf galaxies drawn from the Dwarf Galaxy Survey. We make use of Herschel/PACS archival data to search for atomic outflow signatures in the wings of individual [CII] 158 µm spectra and in their stacked line profile. We find a clear excess of emission in the high-velocity tails of 11 sources which can be explained with an additional broad component (tracing the outflowing gas) in the modeling of their spectra. The remaining objects are likely hosts of weaker outflows that can still be detected in the average stacked spectrum. In both cases, we estimate the atomic mass outflow rates which result to be comparable with the star-formation rates of the galaxies, implying mass-loading factors (i.e., outflow efficiencies) of the order of unity. Outflow velocities in all the 11 galaxies with individual detections are larger than (or compatible with) the escape velocities of their dark matter halos, with an average fraction of 40% of gas escaping into the intergalactic medium (IGM). Depletion timescales due to outflows are lower than those due to gas consumption by star formation in most of our sources, ranging from hundred million to a few billion years. From the energetic point of view, our outflows are mostly consistent with momentum-driven winds generated by the radiation pressure of young stellar populations on dust grains, although the energydriven scenario is not excluded if considering a coupling efficiency up to 20% between the energy injected by supernova (SN) and the interstellar medium. Overall, our results suggest that, despite their low efficiencies, galactic outflows can regulate the star formation history of dwarf galaxies. Specifically, they are able to enrich with metals the circumgalactic medium of these sources, bringing on average a non-negligible amount of gas into the IGM, where it will not be available anymore for new star formation. Our findings are suitable for tuning chemical evolution models attempting to describe the physical processes shaping the evolution of dwarf galaxies.

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Investigating the [C ii]-to-H i Conversion Factor and the H i Gas Budget of Galaxies at z ≈ 6 with Hydrodynamic Simulations

Cited by 8 publications

References 48 publications

The Gas and Stellar Content of a Metal-poor Galaxy at z = 8.496 as Revealed by JWST and ALMA

The Gas and Stellar Content of a Metal-poor Galaxy at z = 8.496 as Revealed by JWST and ALMA

A high-redshift calibration of the [O I]-to-H I conversion factor in star-forming galaxies

Star-formation-driven outflows in local dwarf galaxies as revealed from [CII] observations by Herschel

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