Vales

Hughes, T. M.; Ibar, E.; Villanueva, V.; Aravena, M.; Baes, M.; Bourne, N.; Cooray, Asantha; Dunne, L.; Dye, S.; Eales, Stephen Anthony; Furlanetto, C.; Herrera-Camus, Rodrigo; Ivison, R. J.; Kampen, E. van; Lara-López, M. A.; Maddox, Steve; Michałowski, M. J.; Smith, M.; Valiante, Elisabetta; Werf, P. van der; Xue, Yongquan

doi:10.1051/0004-6361/201629588

Cited by 25 publications

(36 citation statements)

References 72 publications

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“…We note that our sample is not significantly contaminated by active galactic nuclei (V17) and the [C II] emission is likely to be optically thin within the galaxies of our sample as based on photodissociation region (PDR) modelling (Hughes et al 2017a), suggesting that these two possible effects are not substantially affecting the trend observed in Fig. 7.…”

Section: Ir Luminosity and The L [C Ii] /L Ir Deficitmentioning

confidence: 73%

“…Nevertheless, physical properties of the gaseous components of the ISM may be characterized by studying correlations between the [C II] emission and various galaxy properties [e.g. CO(1-0), L IR ; Ibar et al 2015;Hughes et al 2017a].…”

Section: [C Ii] Luminositymentioning

confidence: 99%

“…In this model, the gas is assumed to be collisionally heated via the ejection of photoelectrons from dust grains and polycyclic aromatic hydrocarbon (PAH) molecules by FUV photons, and gas cooling from line emission is predicted by simultaneously solving the chemical and energy equilibrium in the slab. Hughes et al (2017a) assumed that the galactic emission comes from a single PDR. They compare the predicted L [C II] /L IR and L CO /L IR luminosity ratios with the observed quantities.…”

Section: Pdr Modelling and Molecular Gas Kinematicsmentioning

confidence: 99%

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VALES V: a kinematic analysis of the molecular gas content inH-ATLAS galaxies atz ∼ 0.03–0.35 using ALMA

Molina

Ibar

Villanueva

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present Atacama Large Millimeter/submillimeter Array (ALMA) resolved observations of molecular gas in galaxies up to z = 0.35 to characterize the role of global galactic dynamics on the global interstellar medium properties. These observations consist of a sub-sample of 39 galaxies taken from the Valparaíso ALMA Line Emission Survey (VALES). From the CO(J = 1-0) emission line, we quantify the kinematic parameters by modelling the velocity fields. We find that the infrared (IR) luminosity increases with the rotational to dispersion velocity ratio (V rot /σ v , corrected for inclination). We find a dependence between V rot /σ v and the [C II]/IR ratio, suggesting that the so-called [C II] deficit is related to the dynamical state of the galaxies. We find that global pressure support is needed to reconcile the dynamical mass estimates with the stellar masses in our systems with low V rot /σ v values. The star formation rate (SFR) is weakly correlated with the molecular gas fraction (f H 2) in our sample, suggesting that the release of gravitational energy from cold gas may not be the main energy source of the turbulent motions seen in the VALES galaxies. By defining a proxy of the 'star formation efficiency' (SFE) parameter as the SFR divided by the CO luminosity (SFE ≡ SFR/L CO), we find a constant SFE per crossing time (t cross). We suggest that t cross may be the controlling timescale in which the star formation occurs in dusty z ∼ 0.03-0.35 galaxies.

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Section: Ir Luminosity and The L [C Ii] /L Ir Deficitmentioning

confidence: 73%

Section: [C Ii] Luminositymentioning

confidence: 99%

Section: Pdr Modelling and Molecular Gas Kinematicsmentioning

confidence: 99%

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VALES V: a kinematic analysis of the molecular gas content inH-ATLAS galaxies atz ∼ 0.03–0.35 using ALMA

Molina

Ibar

Villanueva

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…As this SPT sample is likely a mix of main-sequence and starburst galaxies (Weiß et al 2013), we suggest that the [C II]-to-H 2 conversion factor is unique and independent of the source mode of star formation. Similarly, we considered the starbursts at z ∼ 0.2 analyzed by Magdis et al (2014) with available [C II] and CO observations and the sample of main-sequence and starbursts from the VALES survey Hughes et al (2017). The M mol /L [C II] ratios of these samples are on average consistent with that of local and high-redshift main-sequence galaxies, as shown in Figure 8.…”

Section: Starburst Galaxiesmentioning

confidence: 97%

“…To explore a larger parameter space and gain a more comprehensive view, we complemented our observations with multiple [C II] datasets from the literature, both at low and high redshift , Gullberg et al 2015, Huynh et al 2014, Schaerer et al 2015, Brisbin et al 2015, Hughes et al 2017. In Appendix C we briefly present these additional samples and discuss how the physical parameters that are relevant for our analysis (namely the redshift, [C II], IR, and CO luminosity, molecular gas mass, sSFR, and gasphase metallicity) have been derived; in Table C1 we report them.…”

Section: Other Samples From the Literaturementioning

confidence: 99%

The [C ii] emission as a molecular gas mass tracer in galaxies at low and high redshifts

Zanella

Daddi

Magdis

et al. 2018

Monthly Notices of the Royal Astronomical Society

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197

217

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We present ALMA Band 9 observations of the [C II]158µ m emission for a sample of 10 main-sequence galaxies at redshift z∼2, with typical stellar masses (log M /M ∼10.0-10.9) and star formation rates (∼35-115 M yr −1 ). Given the strong and well understood evolution of the interstellar medium from the present to z = 2, we investigate the behaviour of the [C II] emission and empirically identify its primary driver. We detect [C II] from six galaxies (four secure, two tentative) and estimate ensemble averages including non detections. The [C II]-to-infrared luminosity ratio (L [C II] /L IR ) of our sample is similar to that of local main-sequence galaxies (∼ 2 × 10 −3 ), and ∼ 10 times higher than that of starbursts. The [C II] emission has an average spatial extent of 4 -7 kpc, consistent with the optical size. Complementing our sample with literature data, we find that the [C II] luminosity correlates with galaxies' molecular gas mass, with a mean absolute deviation of 0.2 dex and without evident systematics: the [C II]-to-H 2 conversion factor (α [C II] ∼ 30 M /L ) is largely independent of galaxies' depletion time, metallicity, and redshift. [C II] seems therefore a convenient tracer to estimate galaxies' molecular gas content regardless of their starburst or main-sequence nature, and extending to metal-poor galaxies at low-and high-redshifts. The dearth of [C II] emission reported for z > 6-7 galaxies might suggest either a high star formation efficiency or a small fraction of UV light from star formation reprocessed by dust.

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The ALPINE-ALMA [CII] survey

Fèvre

Béthermin

Faisst

et al. 2020

A&A

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167

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The ALMA-ALPINE [CII] survey is aimed at characterizing the properties of a sample of normal star-forming galaxies (SFGs). The ALMA Large Program to INvestigate (ALPINE) features 118 galaxies observed in the [CII]-158 μm line and far infrared (FIR) continuum emission during the period of rapid mass assembly, right after the end of the HI reionization, at redshifts of 4 < z < 6. We present the survey science goals, the observational strategy, and the sample selection of the 118 galaxies observed with ALMA, with an average beam minor axis of about 0.85″, or ∼5 kpc at the median redshift of the survey. The properties of the sample are described, including spectroscopic redshifts derived from the UV-rest frame, stellar masses, and star-formation rates obtained from a spectral energy distribution (SED) fitting. The observed properties derived from the ALMA data are presented and discussed in terms of the overall detection rate in [CII] and FIR continuum, with the observed signal-to-noise distribution. The sample is representative of the SFG population in the main sequence at these redshifts. The overall detection rate in [CII] is 64% for a signal-to-noise ratio (S/N) threshold larger than 3.5 corresponding to a 95% purity (40% detection rate for S/N > 5). Based on a visual inspection of the [CII] data cubes together with the large wealth of ancillary data, we find a surprisingly wide range of galaxy types, including 40% that are mergers, 20% extended and dispersion-dominated, 13% compact, and 11% rotating discs, with the remaining 16% too faint to be classified. This diversity indicates that a wide array of physical processes must be at work at this epoch, first and foremost, those of galaxy mergers. This paper sets a reference sample for the gas distribution in normal SFGs at 4 < z < 6, a key epoch in galaxy assembly, which is ideally suited for studies with future facilities, such as the James Webb Space Telescope (JWST) and the Extremely Large Telescopes (ELTs).

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Vales

Cited by 25 publications

References 72 publications

VALES V: a kinematic analysis of the molecular gas content inH-ATLAS galaxies atz ∼ 0.03–0.35 using ALMA

VALES V: a kinematic analysis of the molecular gas content inH-ATLAS galaxies atz ∼ 0.03–0.35 using ALMA

The [C ii] emission as a molecular gas mass tracer in galaxies at low and high redshifts

The ALPINE-ALMA [CII] survey

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