A physical model for [C ii] line emission from galaxies

Ferrara, Andrea; Vallini, L.; Pallottini, Andrea; Gallerani, S.; Carniani, Stefano; Kohandel, M.; Decataldo, D.; Behrens, Christoph

doi:10.1093/mnras/stz2031

Cited by 114 publications

(159 citation statements)

References 69 publications

(83 reference statements)

Supporting

Mentioning

139

Contrasting

Unclassified

Order By: Relevance

“…Over the past several years, numerous theoretical studies have focused on the exact contribution of the various gas phases (e.g., Olsen et al 2017;Pallottini et al 2019) and the effects of metallicity (Vallini et al 2015; Lagache et al 2018), gas dynamics (Kohandel et al 2019), and star-formation feedback (Katz et al 2017;Vallini et al 2017;Ferrara et al 2019) on the [CII] emission, which nowadays is the most studied longwavelength line at z > 4.…”

Section: Introductionmentioning

confidence: 99%

The ALPINE-ALMA [CII] survey: Data processing, catalogs, and statistical source properties

Béthermin

Fudamoto

Ginolfi

et al. 2020

A&A

184

154

View full text Add to dashboard Cite

The Atacama Large Millimeter Array (ALMA) Large Program to INvestigate [CII] at Early times (ALPINE) targets the [CII] 158 μm line and the far-infrared continuum in 118 spectroscopically confirmed star-forming galaxies between z = 4.4 and z = 5.9. It represents the first large [CII] statistical sample built in this redshift range. We present details regarding the data processing and the construction of the catalogs. We detected 23 of our targets in the continuum. To derive accurate infrared luminosities and obscured star formation rates (SFRs), we measured the conversion factor from the ALMA 158 μm rest-frame dust continuum luminosity to the total infrared luminosity (LIR) after constraining the dust spectral energy distribution by stacking a photometric sample similar to ALPINE in ancillary single-dish far-infrared data. We found that our continuum detections have a median LIR of 4.4 × 1011 L⊙. We also detected 57 additional continuum sources in our ALMA pointings. They are at a lower redshift than the ALPINE targets, with a mean photometric redshift of 2.5 ± 0.2. We measured the 850 μm number counts between 0.35 and 3.5 mJy, thus improving the current interferometric constraints in this flux density range. We found a slope break in the number counts around 3 mJy with a shallower slope below this value. More than 40% of the cosmic infrared background is emitted by sources brighter than 0.35 mJy. Finally, we detected the [CII] line in 75 of our targets. Their median [CII] luminosity is 4.8 × 108 L⊙ and their median full width at half maximum is 252 km s−1. After measuring the mean obscured SFR in various [CII] luminosity bins by stacking ALPINE continuum data, we find a good agreement between our data and the local and predicted SFR–L[CII] relations.

show abstract

Section: Introductionmentioning

confidence: 99%

The ALPINE-ALMA [CII] survey: Data processing, catalogs, and statistical source properties

Béthermin

Fudamoto

Ginolfi

et al. 2020

A&A

184

154

View full text Add to dashboard Cite

show abstract

“…6 we see the [C ii] deficit when we compare the observational sample with the power law derived by De Looze et al 2014: at higher SFR 10 M yr −1 the slope with L [C ii] is less steep than at low SFR 10 M yr −1 (FIR luminosities 10 11 L ). The L [C ii] -SFR relation is complex and a simple power law (like the one implemented by De Looze et al (2014)) cannot describe it (Ferrara et al 2019). This trend is also observed in other FIR lines as presented by Díaz-Santos et al (2017).…”

Section: Molecularmentioning

confidence: 99%

“…Muñoz & Oh 2016;Narayanan & Krumholz 2017;Smith et al 2017;Díaz-Santos et al 2017;Ferrara et al 2019) pointing mainly to local conditions of the interstellar gas as the drivers of this deficit, such as the intensity of the radiation field, metallicity A&A proofs: manuscript no. main…”

mentioning

confidence: 99%

Diagnosing the interstellar medium of galaxies with far-infrared emission lines

Padilla

Wang

Ploeckinger

et al. 2021

A&A

View full text Add to dashboard Cite

Context. Atomic fine structure lines have been detected in the local Universe and at high redshifts over the past decades. The [C ii] emission line at 158 µm is an important observable as it provides constraints on the interstellar medium (ISM) cooling processes. Aims. We develop a physically motivated framework to simulate the production of far-infrared line emission from galaxies in a cosmological context. This first paper sets out our methodology and describes its first application: simulating the [C ii] 158 µm line emission in the local Universe. Methods. We combine the output from EAGLE cosmological hydrodynamical simulations with a multi-phase model of the ISM. Gas particles are divided into three phases: dense molecular gas, neutral atomic gas, and diffuse ionised gas (DIG). We estimate the [C ii] line emission from the three phases using a set of Cloudy cooling tables. Results. Our results agree with previous findings regarding the contribution of these three ISM phases to the [C ii] emission. Our model shows good agreement with the observed L [C ii]-star formation rate (SFR) relation in the local Universe within 0.4 dex scatter. Conclusions. The fractional contribution to the [C ii] line from different ISM phases depends on the total SFR and metallicity. The neutral gas phase dominates the [C ii] emission in galaxies with SFR ∼ 0.01-1 M yr −1 , but the ionised phase dominates at lower SFRs. Galaxies above solar metallicity exhibit lower L [C ii] /SFR ratios for the neutral phase. In comparison, the L [C ii] /SFR ratio in the DIG is stable when metallicity varies. We suggest that the reduced size of the neutral clouds, caused by increased SFRs, is the likely cause for the L [C ii] deficit at high infrared luminosities, although EAGLE simulations do not reach these luminosities at z = 0.

show abstract

“…On the other hand, low density gas (n < 10 2 cm −3 ) typically shows G 0 > 10-100 and ionization parameter U ion 10 −2 , as this gas is associated with H II regions. According to Pallottini et al (2019) [C II] emission mostly comes from regions in which n 2 × 10 2 cm −3 , G 0 20, and U ion is relatively low, implying that they are neutral (see also Ferrara et al 2019). Lines as [N II] and [O III] are instead emitted from ionized regions with densities around 50-100 cm −3 and U ion > 10 −3 .…”

Section: Radiation In the Gmcmentioning

confidence: 99%

Shaping the structure of a GMC with radiation and winds

Decataldo

Lupi

Ferrara

et al. 2020

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

We study the effect of stellar feedback (photodissociation/ionization, radiation pressure and winds) on the evolution of a Giant Molecular Cloud (GMC), by means of a 3D radiative transfer, hydro-simulation implementing a complex chemical network featuring H2 formation and destruction. We track the formation of individual stars with mass M > 1 M⊙ with a stochastic recipe. Each star emits radiation according to its spectrum, sampled with 10 photon bins from near-infrared to extreme ultra-violet bands; winds are implemented by energy injection in the neighbouring cells. We run a simulation of a GMC with mass M = 105 M⊙, following the evolution of different gas phases. Thanks to the simultaneous inclusion of different stellar feedback mechanisms, we identify two stages in the cloud evolution: (1) radiation and winds carve ionized, low-density bubbles around massive stars, while FUV radiation dissociates most H2 in the cloud, apart from dense, self-shielded clumps; (2) rapid star formation (SFR≃ 0.1 M⊙ − 1) consumes molecular gas in the dense clumps, so that UV radiation escapes and ionizes the remaining HI gas in the GMC. H2 is exhausted in 1.6 Myr, yielding a final star formation efficiency of 36 per cent. The average intensity of FUV and ionizing fields increases almost steadily with time; by the end of the simulation (t = 2.5 Myr) we find 〈G0〉 ≃ 103 (in Habing units), and a ionization parameter 〈Uion〉 ≃ 102, respectively. The ionization field has also a more patchy distribution than the FUV one within the GMC. Throughout the evolution, the escape fraction of ionizing photons from the cloud is fion, esc ≲ 0.03.

show abstract

A physical model for [C ii] line emission from galaxies

Cited by 114 publications

References 69 publications

The ALPINE-ALMA [CII] survey: Data processing, catalogs, and statistical source properties

The ALPINE-ALMA [CII] survey: Data processing, catalogs, and statistical source properties

Diagnosing the interstellar medium of galaxies with far-infrared emission lines

Shaping the structure of a GMC with radiation and winds

Contact Info

Product

Resources

About