Linguagem, Sociedade e Discurso

Sobral, Gilberto Nazareno Telles; Lopes, Norma da Silva; Ramos, Jânia Martins

doi:10.5151/9788580391176

Cited by 1 publication

(2 citation statements)

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“…The former agree with the local Σ [CII] -Σ SFR relation while HZ1, HZ2, and HZ4 have low Σ [CII] -Σ SFR ratio. This interpretation is also supported by the fact that all CR7 clumps, which have metallicities 12+log(O/H)< 8.2 (see discussion in Sobral et al 2017) , are located well below the local relation. The Σ [CII] deficit is also akin to the simulations by Pallottini et al (2017a) who investigated the physical properties of a simulated galaxy at z = 6, with metallicity 12+log(O/H)=8.35.…”

Section: Surface Brightnessmentioning

confidence: 66%

“…An additional star-forming galaxy with a complex morphology is WHM5 at z = 6.0695, which appears to consist of multiple components in [Cii]: a compact source, seen also in dust emission, and an extended component at the location of the rest-frame UV emission ( At higher redshift, the presence of multiple [Cii] components has recently been reported in CR7 at z=6.6 by Sobral et al (2015Sobral et al ( , 2017 and Matthee et al (2015Matthee et al ( , 2017. Three out of four detected [Cii] clumps coincide with the location of UV clumps.…”

Section: Sfr Estimates and Morphology Analysismentioning

confidence: 95%

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Kiloparsec-scale gaseous clumps and star formation at z = 5–7

Carniani

Maiolino

Amorín

et al. 2018

Monthly Notices of the Royal Astronomical Society

164

242

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We investigate the morphology of the [Cii] emission in a sample of "normal" star-forming galaxies at 5 < z < 7.2 in relation to their UV (rest-frame) counterpart. We use new ALMA observations of galaxies at z ∼ 6−7, as well as a careful re-analysis of archival ALMA data. In total 29 galaxies were analysed, 21 of which are detected in [Cii]. For several of the latter the [Cii] emission breaks into multiple components. Only a fraction of these [Cii] components, if any, is associated with the primary UV systems, while the bulk of the [Cii] emission is associated either with fainter UV components, or not associated with any UV counterpart at the current limits. By taking into account the presence of all these components, we find that the L [CII] -SFR relation at early epochs is fully consistent with the local relation, but it has a dispersion of 0.48±0.07 dex, which is about two times larger than observed locally. We also find that the deviation from the local L [CII] -SFR relation has a weak anti-correlation with the EW(Lyα). The morphological analysis also reveals that [Cii] emission is generally much more extended than the UV emission. As a consequence, these primordial galaxies are characterised by a [Cii] surface brightness generally much lower than expected from the local Σ [CII] − Σ SFR relation. These properties are likely a consequence of a combination of different effects, namely: gas metallicity, [Cii] emission from obscured star-forming regions, strong variations of the ionisation parameter, and circumgalactic gas in accretion or ejected by these primeval galaxies.

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Section: Surface Brightnessmentioning

confidence: 66%

Section: Sfr Estimates and Morphology Analysismentioning

confidence: 95%