ALMA observations of atomic carbon in<i>z</i> ∼ 4 dusty star-forming galaxies

Bothwell, M. S.; Aguirre, James E.; Aravena, M.; Béthermin, M.; Bisbas, Thomas G.; Chapman, Scott; Breuck, C. De; Gonzalez, Anthony H.; Greve, T. R.; Hezaveh, Yashar; Ma, Jingzhe; Malkan, Matthew A.; Marrone, Daniel P.; Murphy, E. J.; Spilker, Justin; Strandet, M.; Vieira, J. D.; Weiß, A.

doi:10.1093/mnras/stw3270

Cited by 134 publications

(197 citation statements)

References 70 publications

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“…The mid and high−J CO lines (J = 6 − 5 and above) are shown to have increasingly sub-linear slopes with L FIR which suggests that denser and much warmer gas than star forming regions (possibly due to shocks or turbulence) is needed for CO excitation (Narayanan et al 2008;Greve et al 2014). Thus, variations in star formation efficiency, or other physical properties within the molecular gas such Bothwell et al (2017). SPT0538-50 and other two SPT sources (SPT0125-47 and SPT0346-52) are detailed in Aravena et al (2016).…”

Section: H 2 O and Comentioning

confidence: 99%

“…Σ gas is calculated by dividing gas mass by the effective area of the source. The gas mass values from Bothwell et al (2017) The black data points are obtained by combining all the pixels from the five sources and the fit to these points by fixing the slope to zero is shown as thick black line with the 1σ uncertainty on the fit shown in grey. The dotted line is the best fit by allowing the slope to vary and it is within the grey error region.…”

Section: Correlation Of L H2o /L F Ir With Physical Propertiesmentioning

confidence: 99%

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Spatially Resolved Water Emission from Gravitationally Lensed Dusty Star-forming Galaxies at z ∼ 3

Jarugula

Vieira

Spilker

et al. 2019

ApJ

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Water (H 2 O), one of the most ubiquitous molecules in the universe, has bright millimeter-wave emission lines easily observed at high-redshift with the current generation of instruments. The low excitation transition of H 2 O, p-H 2 O(2 0,2 − 1 1,1 ) (ν rest = 987.927 GHz) is known to trace the far-infrared (FIR) radiation field independent of the presence of active galactic nuclei (AGN) over many ordersof-magnitude in FIR luminosity (L FIR ). This indicates that this transition arises mainly due to star formation. In this paper, we present spatially (∼0.5 ′′ corresponding to ∼1 kiloparsec) and spectrally resolved (∼100 kms −1 ) observations of p-H 2 O(2 0,2 − 1 1,1 ) in a sample of four strong gravitationally lensed high-redshift galaxies with the Atacama Large Millimeter/submillimeter Array (ALMA). In addition to increasing the sample of luminous (> 10 12 L ⊙ ) galaxies observed with H 2 O, this paper examines the L H2O /L FIR relation on resolved scales for the first time at high-redshift. We find that L H2O is correlated with L FIR on both global and resolved kiloparsec scales within the galaxy in starbursts and AGN with average L H2O /L FIR = 2.76 +2.15 −1.21 × 10 −5 . We find that the scatter in the observed L H2O /L FIR relation does not obviously correlate with the effective temperature of the dust spectral energy distribution (SED) or the molecular gas surface density. This is a first step in developing p-H 2 O(2 0,2 − 1 1,1 ) as a resolved star formation rate (SFR) calibrator.

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Section: H 2 O and Comentioning

confidence: 99%

Section: Correlation Of L H2o /L F Ir With Physical Propertiesmentioning

confidence: 99%

Spatially Resolved Water Emission from Gravitationally Lensed Dusty Star-forming Galaxies at z ∼ 3

Jarugula

Vieira

Spilker

et al. 2019

ApJ

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“…Such findings were previously dismissed as the result of not correcting αCO for the effects of metallicity variations (Leroy et al 2011), but later studies which are able to make these corrections still find the same trends. 16 There remains an active debate over the most appropriate α CO value to use for higher redshift systems and SMGs, with recent work finding values intermediate between the ULIRG and Milky Way values (Weiß et al 2005;Ivison et al 2011;Carleton et al 2017;Bothwell et al 2017) but see also Aravena et al (2016). If we instead used the α CO = 0.8 ULIRG value for the SMGs at high redshift, this shifts the open cyan squares up to lie closer to the ULIRGS but it does not affect the discussion related to the BADGRS.…”

Section: Molecular Gas-to-dust Ratios and Star Formation Efficiencymentioning

confidence: 99%

The unusual ISM in blue and dusty gas-rich galaxies (BADGRS)

Dunne

Zhang

Vis

et al. 2018

Monthly Notices of the Royal Astronomical Society

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The Herschel-ATLAS unbiased survey of cold dust in the local Universe is dominated by a surprising population of very blue (F U V − K < 3.5), dust-rich galaxies with high gas fractions (f HI = M HI /( M * + M HI ) > 0.5). Dubbed 'Blue and Dusty Gas Rich Sources' (BADGRS) they have cold diffuse dust temperatures, and the highest dustto-stellar mass ratios of any galaxies in the local Universe. Here, we explore the molecular ISM in a representative sample of BADGRS, using very deep CO(J up = 1, 2, 3) observations across the central and outer disk regions. We find very low CO brightnesses (T p = 5 − 30 mK), despite the bright far-infrared emission and metallicities in the range 0.5 < Z/Z < 1.0. The CO line ratios indicate a range of conditions with R 21 = T 21 b /T 10 b = 0.6 − 2.1 and R 31 = T 32 b /T 10 b = 0.2 − 1.2. Using a metallicity dependent conversion from CO luminosity to molecular gas mass we find M H2 / M d ∼ 7 − 27 and Σ H2 = 0.5 − 6 M pc −2 , around an order of magnitude lower than expected. The BADGRS have lower molecular gas depletion timescales (τ d ∼ 0.5 Gyr) than other local spirals, lying offset from the Kennicutt-Schmidt relation by a similar factor to Blue Compact Dwarf galaxies. The cold diffuse dust temperature in BADGRS (13-16 K) requires an interstellar radiation field 10-20 times lower than that inferred from their observed surface brightness. We speculate that the dust in these sources has either a very clumpy geometry or a very different opacity in order to explain the cold temperatures and lack of CO emission. BADGRS also have low UV attenuation for their UV colour suggestive of an SMC-type dust attenuation curve, different star formation histories or different dust/star geometry. They lie in a similar part of the IRX-β space as z ∼ 5 galaxies and may be useful as local analogues for high gas fraction galaxies in the early Universe.

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“…; 10 -Velocity-integrated CO (2 − 1) fluxes; 11 -Dust mass; 12 -Mass of [C I] (from L Tex = 30 K); 13 -Atomic carbon abundances computed assuming Mgas(dust, δ GDR = 30) and removing the 1.36× contribution of helium; 14 -Atomic carbon abundances computed assuming Mgas(CO, αCO = 0.8 M /(K km s −1pc 2 ), r 21 = 0.84) and removing the 1.36× contribution of helium; 15 -Fraction infrared AGN emission:L AGN+SF = L IR /(1 − f AGN ).Upper limits are at 3σ.All values have been corrected for gravitational magnification. † : We report the nominal flux measurements presented inBothwell et al (2017), but we adopt the 3σ upper limits for the analysis.References: Cols 1-3, 9: Bothwell et al (2017); Col 4: Ma et al (2015); Cols 5, 6 (photometry): Weiß et al (2013); Col 10: Aravena et al (2016).…”

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confidence: 99%

A Survey of Atomic Carbon [C i] in High-redshift Main-sequence Galaxies

Valentino

Magdis

Daddi

et al. 2018

ApJ

125

168

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We present the first results of an ALMA survey of the lower fine structure line of atomic carbon [C I]( 3 P 1 − 3 P 0 ) in far infrared-selected galaxies on the main sequence at z ∼ 1.2 in the COSMOS field. We compare our sample with a comprehensive compilation of data available in literature for local and high-redshift starbursting systems and quasars. We show that the [C I]( 3 P 1 → 3 P 0 ) luminosity correlates on global scales with the infrared luminosity L IR similarly to low-J CO transitions. We report a systematic variation of L [C I] 3 P1 − 3 P0 /L IR as a function of the galaxy type, with the ratio being larger for main-sequence galaxies than for starbursts and sub-millimeter galaxies at fixed L IR . The L [C I] 3 P1 − 3 P0 /L CO(2−1) and M [C I] /M dust mass ratios are similar for main-sequence galaxies and for local and high-redshift starbursts within a 0.2 dex intrinsic scatter, suggesting that [C I] is a good tracer of molecular gas mass as CO and dust. We derive a fraction of f [C I] = M [C I] /M C ∼ 3 − 13% of the total carbon mass in the atomic neutral phase. Moreover, we estimate the neutral atomic carbon abundance, the fundamental ingredient to calibrate [C I] as a gas tracer, by comparing L [C I] 3 P1 − 3 P0 and available gas masses from CO lines and dust emission. We find lower [C I] abundances in mainsequence galaxies than in starbursting systems and sub-millimeter galaxies, as a consequence of the canonical α CO and gas-to-dust conversion factors. This argues against the application to different galaxy populations of a universal standard [C I] abundance derived from highly biased samples.

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ALMA observations of atomic carbon inz ∼ 4 dusty star-forming galaxies

Cited by 134 publications

References 70 publications

Spatially Resolved Water Emission from Gravitationally Lensed Dusty Star-forming Galaxies at z ∼ 3

Spatially Resolved Water Emission from Gravitationally Lensed Dusty Star-forming Galaxies at z ∼ 3

The unusual ISM in blue and dusty gas-rich galaxies (BADGRS)

A Survey of Atomic Carbon [C i] in High-redshift Main-sequence Galaxies

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