Erratum: “Resolved Neutral Carbon Emission in Nearby Galaxies: [C i] Lines as Total Molecular Gas Tracers” (2019, ApJ, 880, 133)

Jiao, Qian; Zhao, Yi; Lu, N.; Gao, Yu; Salak, Dragan; Zhu, Meiping; Zhang, Zhi-Yu; Jiang, Xue-Jian; Tan, Qinghua

doi:10.3847/1538-4357/ab44cc

Cited by 19 publications

(50 citation statements)

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“…18 in Schreiber et al 2018). The optically thick FIR dust temperature is also in agreement with the observed T ex −T d relation (Jiao et al 2019a) of T ex < T d (Valentino et al 2020). For a comparison with other high-z starbursts, Spilker et al (2016) report a λ 0 − T d correlation based on lensed starburst galaxies at z = 1.9−5.7 with λ 0 = 140 ± 40 µm, derived using free opacity MBB prescription, yielding consistent results with our derived FIR properties of GN20.…”

Section: Resultssupporting

confidence: 86%

Deceptively cold dust in the massive starburst galaxy GN20 at z ∼ 4

Cortzen

Magdis

Valentino

et al. 2020

A&A

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We present new observations, carried out with IRAM NOEMA, of the atomic neutral carbon transitions [C i]( 3 P 1 -3 P 0 ) at 492 GHz and [C i]( 3 P 2 -3 P 1 ) at 809 GHz of GN20, a well-studied star-bursting galaxy at z = 4.05. The high luminosity line ratio [C i]( 3 P 2 -3 P 1 ) /[C i]( 3 P 1 -3 P 0 ) implies an excitation temperature of 48 +14 −9 K, which is significantly higher than the apparent dust temperature of T d =33 ± 2 K (β = 1.9) derived under the common assumption of an optically thin far-infrared dust emission, but fully consistent with T d = 52 ± 5 K of a general opacity model where the optical depth (τ) reaches unity at a wavelength of λ 0 = 170 ± 23 µm. Moreover, the general opacity solution returns a factor of ∼ 2× lower dust mass and, hence, a lower molecular gas mass for a fixed gas-to-dust ratio, than with the optically thin dust model. The derived properties of GN20 thus provide an appealing solution to the puzzling discovery of starbursts appearing colder than main-sequence galaxies above z > 2.5, in addition to a lower dust-to-stellar mass ratio that approaches the physical value predicted for starburst galaxies.

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Section: Resultssupporting

confidence: 86%

Deceptively cold dust in the massive starburst galaxy GN20 at z ∼ 4

Cortzen

Magdis

Valentino

et al. 2020

A&A

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“…Toward a two-pixel aperture of maximum [C I] (1-0) and CO (1-0) integrated intensities at ∼ 2 resolution, we find W [CI] /W CO = 0.22, and the abundance ratio becomes ∼ 7 × 10 −5 . These values are consistent within a factor of two with the estimates of ∼ 3×10 −5 for the Cloverleaf quasar at redshift 2.5 (Weiß et al 2003), (3.9±0.4)×10 −5 in submillimeter galaxies (SMGs) (Alaghband-Zadeh et al 2013), (8.4 ± 3.5) × 10 −5 in SMGs and quasars at redshift 2.5 (Walter et al 2011), 7 × 10 −5 in dusty starforming galaxies at redshift 4 (Bothwell et al 2017), 2 × 10 −5 in the main-sequence galaxies at redshift 1.2 (Valentino et al 2018), and (2.5 ± 1.0) × 10 −5 as the average in a sample of nearby galaxies that includes starbursts and AGN (Jiao et al 2019). These authors used similar methods to calculate the mass.…”

Section: Column Density and Abundancementioning

confidence: 99%

“…In Figure 12(a), we compare the results with the fits obtained by Jiao et al (2019) for a sample of various galaxy types at low resolution. The gray line is the power law log L CO(1−0) = 0.74 + 1.04 log L [CI] for nearby galaxies at ∼ 1 kpc resolution.…”

Section: Co −L [Ci] Correlationsmentioning

confidence: 99%

“…We showed in Figure 11 that the total luminosity of NGC 1808 is in excellent agreement with this fit. Also shown are linear fits log L CO(1−0) = 0.96 + log L [CI] for the same sample of nearby galaxies (red dash-dotted line) and log L CO(1−0) = 0.63 + log L [CI] (blue dash-dotted line) for (U)LIRGs and the Spiderweb Galaxy (Jiao et al 2017(Jiao et al , 2019. Note that the change in slope that we observe at high resolution in NGC 1808 can be regarded as a combination of two regions with different physical conditions: 1 kpc disk, where the slope is comparable to the average for nearby galaxies, and the CND and other hot spots, where the slope is comparable to the 1.488 ± 0.019 0.686 ± 0.010 0.85 CO (2-1) 0.854 ± 0.024 0.948 ± 0.014 0.86 0.738 ± 0.025 0.942 ± 0.014 0.86 13 CO (2-1) 0.401 ± 0.026 0.664 ± 0.014 0.83 C 18 O (2-1) 0.171 ± 0.068 0.580 ± 0.033 0.66…”

Section: Co −L [Ci] Correlationsmentioning

confidence: 99%

“…To increase sensitivity and enable direct comparison, the [C I] data were smoothed to the resolution of CO (1-0) (∼ 100 pc). In panel (a), the gray curve is the fit for nearby galaxies (NGs), the dash-dotted red is a linear fit for nearby galaxies, and the dash-dotted blue is for (U)LIRGs and the Spiderweb Galaxy (Jiao et al 2019). All data are smoothed to the resolution of CO (1-0) (∼ 100 pc); the pixel size (0.…”

Section: Atomic Carbon In the Outflowmentioning

confidence: 99%

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ALMA Observations of Atomic Carbon [C i] (³P₁ → ³P₀) and Low-J CO Lines in the Starburst Galaxy NGC 1808

Salak¹,

Nakai²,

Seta³

et al. 2019

ApJ

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We present [C I] 3 P 1 → 3 P 0 , 12 CO, 13 CO, and C 18 O (J = 2 → 1) observations of the central region (radius 1 kpc) of the starburst galaxy NGC 1808 at 30-50 pc resolution conducted with Atacama Large Millimeter/submillimeter Array. Radiative transfer analysis of multiline data indicates warm (T k ∼ 40−80 K) and dense (n H2 ∼ 10 3−4 cm −3 ) molecular gas with high column density of atomic carbon (N CI ∼ 3 × 10 18 cm −2 ) in the circumnuclear disk (central 100 pc). The C I/H 2 abundance in the central 1 kpc is ∼ 3−7 × 10 −5 , consistent with the values in luminous infrared galaxies. The intensity ratios of [C I]/CO(1-0) and [C I]/CO(3-2), respectively, decrease and increase with radius in the central 1 kpc, whereas [C I]/CO(2-1) is uniform within statistical errors. The result can be explained by excitation and optical depth effects, since the effective critical density of CO (2-1) is comparable to that of [C I]. The distribution of [C I] is similar to that of 13 CO(2-1), and the ratios of [C I] to 13 CO(2-1) and C 18 O(2-1) are uniform within ∼ 30% in the central < 400 pc starburst disk. The results suggest that [C I] 3 P 1 → 3 P 0 luminosity can be used as a CO-equivalent tracer of molecular gas mass, although caution is needed when applied in resolved starburst nuclei (e.g., circumnuclear disk), where the [C I]/CO(1-0) luminosity ratio is enhanced due to high excitation and atomic carbon abundance. The [C I]/CO(1-0) intensity ratio toward the base of the starburst-driven outflow is 0.15, and the upper limits of the mass and kinetic energy of the atomic carbon outflow are ∼ 1 × 10 4 M and ∼ 3 × 10 51 erg, respectively.

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Tracing the total molecular gas in galaxies: [CII] and the CO-dark gas

Madden

Cormier

Hony

et al. 2020

A&A

138

128

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Context. Molecular gas is a necessary fuel for star formation. The CO (1−0) transition is often used to deduce the total molecular hydrogen but is challenging to detect in low-metallicity galaxies in spite of the star formation taking place. In contrast, the [C ii]λ158 µm is relatively bright, highlighting a potentially important reservoir of H 2 that is not traced by CO (1−0) but is residing in the C +-emitting regions. Aims. Here we aim to explore a method to quantify the total H 2 mass (M H 2) in galaxies and to decipher what parameters control the CO-dark reservoir. Methods. We present Cloudy grids of density, radiation field, and metallicity in terms of observed quantities, such as [O i], [C i], CO (1−0), [C ii], L TIR , and the total M H 2. We provide recipes based on these models to derive total M H 2 mass estimates from observations. We apply the models to the Herschel Dwarf Galaxy Survey, extracting the total M H 2 for each galaxy, and compare this to the H 2 determined from the observed CO (1−0) line. This allows us to quantify the reservoir of H 2 that is CO-dark and traced by the [C ii]λ158 µm. Results. We demonstrate that while the H 2 traced by CO (1−0) can be negligible, the [C ii]λ158 µm can trace the total H 2. We find 70 to 100% of the total H 2 mass is not traced by CO (1−0) in the dwarf galaxies, but is well-traced by [C ii]λ158 µm. The CO-dark gas mass fraction correlates with the observed L [C ii] /L CO(1−0) ratio. A conversion factor for [C ii]λ158 µm to total H 2 and a new CO-to-total-M H 2 conversion factor as a function of metallicity are presented. Conclusions. While low-metallicity galaxies may have a feeble molecular reservoir as surmised from CO observations, the presence of an important reservoir of molecular gas that is not detected by CO can exist. We suggest a general recipe to quantify the total mass of H 2 in galaxies, taking into account the CO and [C ii] observations. Accounting for this CO-dark H 2 gas, we find that the star-forming dwarf galaxies now fall on the Schmidt-Kennicutt relation. Their star-forming efficiency is rather normal because the reservoir from which they form stars is now more massive when introducing the [C ii] measures of the total H 2 compared to the small amount of H 2 in the CO-emitting region.

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Erratum: “Resolved Neutral Carbon Emission in Nearby Galaxies: [C i] Lines as Total Molecular Gas Tracers” (2019, ApJ, 880, 133)

Cited by 19 publications

References 0 publications

Deceptively cold dust in the massive starburst galaxy GN20 at z ∼ 4

Deceptively cold dust in the massive starburst galaxy GN20 at z ∼ 4

ALMA Observations of Atomic Carbon [C i] (³P₁ → ³P₀) and Low-J CO Lines in the Starburst Galaxy NGC 1808

Tracing the total molecular gas in galaxies: [CII] and the CO-dark gas

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Erratum: “Resolved Neutral Carbon Emission in Nearby Galaxies: [C i] Lines as Total Molecular Gas Tracers” (2019, ApJ, 880, 133)

Cited by 19 publications

References 0 publications

Deceptively cold dust in the massive starburst galaxy GN20 at z ∼ 4

Deceptively cold dust in the massive starburst galaxy GN20 at z ∼ 4

ALMA Observations of Atomic Carbon [C i] (3P1 → 3P0) and Low-J CO Lines in the Starburst Galaxy NGC 1808

Tracing the total molecular gas in galaxies: [CII] and the CO-dark gas

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Resources

About

ALMA Observations of Atomic Carbon [C i] (³P₁ → ³P₀) and Low-J CO Lines in the Starburst Galaxy NGC 1808