A$^{3}$COSMOS: A census on the molecular gas mass and extent of main-sequence galaxies across cosmic time

Wang, Tsan-Ming; Magnelli, Benjamin; Schinnerer, Eva; Liu, Daizhong; Modak, Ziad Aziz; Jiménez-Andrade, Eric Faustino; Karoumpis, Christos; Kokorev, Vasily; Bertoldi, Frank

doi:10.48550/arxiv.2201.12070

Cited by 3 publications

(3 citation statements)

References 157 publications

(267 reference statements)

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“…In Figure 11, we include only molecular gas mass density estimates based on the untargeted CO observations (both in emission and absorption). There are references in the literature providing the estimates on the molecular gas mass density based on a different approach, which we did not include on the plot, e.g., scaled dust continuum, based on empirical gas-to-dust conversion (Scoville et al 2017;Liu et al 2019;Magnelli et al 2020;Garratt et al 2021;Wang et al 2022), radio continuum to CO luminosity conversion (Orellana-González et al 2020) or CO intensity mapping (see discussion in Popping & Péroux 2022).…”

Section: Methodsmentioning

confidence: 99%

ALMACAL VIII: A pilot survey for untargeted extragalactic CO emission lines in deep ALMA calibration data

Hamanowicz¹,

Péroux²,

Lagos³

et al. 2022

Preprint

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We present a pilot, untargeted extragalactic carbon monoxide (CO) emission-line survey using ALMACAL, a project utilizing ALMA calibration data for scientific purposes. In 33 deep (𝑇 exp > 40 min) ALMACAL fields we report six CO emission-line detections above 𝑆/𝑁 > 4, one third confirmed by MUSE observations. With this pilot survey, we probe a cosmologically significant volume of ∼ 10 5 cMpc 3 , widely distributed over many pointings in the southern sky, making the survey largely insusceptible to the effects of cosmic variance. We derive the redshift probability of the CO detections using probability functions from the S semianalytical model of galaxy formation. By assuming typical CO excitations for the detections, we put constraints on the cosmic molecular gas mass density evolution over the redshift range 0 < 𝑧 < 1.5. The results of our pilot survey are consistent with the findings of other untargeted emission-line surveys and the theoretical model predictions and currently cannot rule out a non-evolving molecular gas mass density. Our study demonstrates the potential of using ALMA calibrator fields as a multi-sightline untargeted CO emission line survey. Applying this approach to the full ALMACAL database will provide an accurate, free of cosmic variance, measurement of the molecular luminosity function as a function of redshift.

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Section: Methodsmentioning

confidence: 99%

ALMACAL VIII: A pilot survey for untargeted extragalactic CO emission lines in deep ALMA calibration data

Hamanowicz¹,

Péroux²,

Lagos³

et al. 2022

Preprint

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“…4.4. Cold gas content scaling relations at z ∼ 2 Recent studies have calibrated scaling relations of M mol , µ mol , and t depl as a function of redshift, M * , and SFR (or, equivalently, offset from the MS) by combining samples with Rayleigh-Jeans dust continuum and/or CO line emission observations spanning z = 0 − 4 (Genzel et al 2015;Scoville et al 2017;Tacconi et al 2018Tacconi et al , 2020Liu et al 2019;Wang et al 2022). These scaling relations potentially have great utility by providing estimates of the cold gas content of galaxies based on galaxy properties that are easier to directly constrain.…”

Section: A Budget Of Metals In Massive Z ∼ 2 Star-forming Galaxiesmentioning

confidence: 99%

CO Emission, Molecular Gas, and Metallicity in Main-Sequence Star-Forming Galaxies at $z\sim2.3$

Shapley¹,

Jones²,

Shivaei³

et al. 2022

Preprint

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We present observations of CO(3−2) in 13 main-sequence z = 2.0 − 2.5 star-forming galaxies at log(M * /M ) = 10.2 − 10.6 that span a wide range in metallicity (O/H) based on rest-optical spectroscopy. We find that L CO(3−2) /SFR decreases with decreasing metallicity, implying that the CO luminosity per unit gas mass is lower in low-metallicity galaxies at z ∼ 2. We constrain the CO-to-H 2 conversion factor (α CO ) and find that α CO inversely correlates with metallicity at z ∼ 2. We derive molecular gas masses (M mol ) and characterize the relations among M * , SFR, M mol , and metallicity. At z ∼ 2, M mol increases and molecular gas fraction (M mol /M * ) decrease with increasing M * , with a significant secondary dependence on SFR. Galaxies at z ∼ 2 lie on a near-linear molecular KS law that is well-described by a constant depletion time of 700 Myr. We find that the scatter about the mean SFR−M * , O/H−M * , and M mol −M * relations is correlated such that, at fixed M * , z ∼ 2 galaxies with larger M mol have higher SFR and lower O/H. We thus confirm the existence of a fundamental metallicity relation at z ∼ 2 where O/H is inversely correlated with both SFR and M mol at fixed M * . These results suggest that the scatter of the z ∼ 2 star-forming main sequence, mass-metallicity relation, and M mol -M * relation are primarily driven by stochastic variations in gas inflow rates. We place constraints on the mass loading of galactic outflows and perform a metal budget analysis, finding that massive z ∼ 2 star-forming galaxies retain only 30% of metals produced, implying that a large mass of metals resides in the circumgalactic medium.

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“…In recent years, single millimeter dust-continuum measurements in particular have been used as estimators of galaxy cold gas masses (see for example Scoville et al 2017, Kaasinen et al 2019. In some cases these recipes account for changes in the DTG as a function of metallicity (Bertemes et al 2018;Wang et al 2022), but not always. The robustness of such dust-based gas mass estimates will be improved by using the DTG-metallicity relation tabulated in Table 1.…”

Section: No Cosmic Evolution In Galaxy Dust Properties With Metallicitymentioning

confidence: 99%

Observed cosmic evolution of galaxy dust properties with metallicity and tensions with models

Popping,

Péroux

2022

Preprint

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The dust abundance of the interstellar medium plays an important role in galaxy physics, the chemical evolution of matter and the absorption and re-emission of stellar light. The last years have seen a surge in observational and theoretical studies constraining the dust-abundance of galaxies up to 𝑧 ∼ 5. In this work we gather the latest observational measurements (with a focus on absorption studies covering metallicities in the range 6.8 < 12 + log (𝑂/𝐻) < 9) and theoretical predictions (from six different galaxy formation models) for the dust-to-gas (DTG) and dust-to-metal (DTM) ratio of galaxies. The observed trend between DTG and DTM and gas-phase metallicity can be described by a linear relation and shows no evolution from 0 < 𝑧 < 5. Importantly, the fit to the DTG-metallicity relation provides a refined tool for robust dust-based gas mass estimates inferred from millimeter dust-continuum observations. The lack of evolution in the observed relations are indicative of a quickly reached balance (already when the Universe was 1.2 Gyr old) between the formation and destruction of dust and a constant timescale for star-formation at fixed metallicities over cosmic time. None of the models is able to reproduce the observed trends over the entire range in metallicity and redshift probed. The comparison between models and simulations furthermore rules out some of the current implementations for the growth and destruction of dust in galaxy formation models and places tight constraints on the predicted timescale for star-formation.

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A$^{3}$COSMOS: A census on the molecular gas mass and extent of main-sequence galaxies across cosmic time

Cited by 3 publications

References 157 publications

ALMACAL VIII: A pilot survey for untargeted extragalactic CO emission lines in deep ALMA calibration data

ALMACAL VIII: A pilot survey for untargeted extragalactic CO emission lines in deep ALMA calibration data

CO Emission, Molecular Gas, and Metallicity in Main-Sequence Star-Forming Galaxies at $z\sim2.3$

Observed cosmic evolution of galaxy dust properties with metallicity and tensions with models

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