Probing the high-redshift universe with SPICA: Toward the epoch of reionisation and beyond

Egami, Eiichi; Gallerani, S.; Schneider, Raffaella; Pallottini, Andrea; Vallini, L.; Sobacchi, Emanuele; Ferrara, Andrea; Bianchi, S.; Bocchio, Marco; Marassi, Stefania; Armus, L.; Spinoglio, L.; Blain, A. W.; Bradford, M.; Clements, D. L.; Dannerbauer, H.; Fernández-Ontiveros, J. A.; González-Alfonso, E.; Griffin, Matthew Joseph; Gruppioni, C.; Kaneda, Hidehiro; Kohno, Kotaro; Madden, S.; Matsuhara, Hideo; Najarro, F.; Oliver, Seb; Omukai, Kazuyuki; Onaka, Takashi; Pearson, Chris; Pérez-Fournón, I.; Pérez‐González, Pablo G.; Scott, Douglas; Serjeant, S.; Smith, J. D.; Tak, F. F. S. van der; Wada, Takehiko; Yajima, Hidenobu

doi:10.1017/pasa.2018.41

Cited by 22 publications

(18 citation statements)

References 241 publications

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“…[OIII] (Inoue et al 2016;Vallini et al 2017), dust continuum (Behrens et al 2018, to constrain D), CO lines (Vallini et al 2018), or even H 2 lines, hopefully becoming available at these redshifts with SPICA (Spinoglio et al 2017;Egami et al 2018). An interesting, and more readily available alternative are optical nebular lines, such as Lyα and C III] , used in combination with machine learning strategies (Ucci et al 2019).…”

Section: Discussionmentioning

confidence: 99%

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

Ferrara

Vallini

Pallottini

et al. 2019

Monthly Notices of the Royal Astronomical Society

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114

139

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A tight relation between the [C ii] 158 $\mu$m line luminosity and star formation rate is measured in local galaxies. At high redshift (z > 5), though, a much larger scatter is observed, with a considerable (15–20 per cent) fraction of the outliers being [C ii]-deficient. Moreover, the [C ii] surface brightness ($\Sigma_{\rm [C\, \small {II}]}$) of these sources is systematically lower than expected from the local relation. To clarify the origin of such [C ii]-deficiency, we have developed an analytical model that fits local [C ii] data and has been validated against radiative transfer simulations performed with cloudy. The model predicts an overall increase of $\Sigma_{\rm [C\, \small {II}]}$ with ΣSFR. However, for ΣSFR ${\gtrsim} 1 \, \mathrm{M}_\odot \,{\rm yr}^{-1}\,{\rm kpc}^{-2}$, $\Sigma_{\rm [C\, \small {II}]}$ saturates. We conclude that underluminous [C ii] systems can result from a combination of three factors: (a) large upward deviations from the Kennicutt–Schmidt relation (κs ≫ 1), parametrized by the ‘burstiness’ parameter κs; (b) low metallicity; (c) low gas density, at least for the most extreme sources (e.g. CR7). Observations of [C ii] emission alone cannot break the degeneracy among the above three parameters; this requires additional information coming from other emission lines (e.g. [O iii]88 $\mu$m, C iii]1909 Å, CO lines). Simple formulae are given to interpret available data for low- and high-z galaxies.

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Section: Discussionmentioning

confidence: 99%

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

Ferrara

Vallini

Pallottini

et al. 2019

Monthly Notices of the Royal Astronomical Society

Self Cite

114

139

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“…Schaerer et al 2013Schaerer et al , 2020Faisst et al 2020). In this context, future observations in the near-and mid-IR with JWST (Gardner et al 2006;Williams et al 2018;Chevallard et al 2019), and SPICA (Spinoglio et al 2017;Egami et al 2018) will be crucial to better constrain the SED shape and, thus, determine galaxy properties as SFR. In the rest of the work, we use the SFR from UV+FIR luminosity since it is the same method used to determine the local L [CII] -SFR relation (De Looze et al 2014).…”

Section: [Cii] As Tracer Of Sfr In the Eor?mentioning

confidence: 98%

Missing [C ii] emission from early galaxies

Carniani

Ferrara

Maiolino

et al. 2020

Monthly Notices of the Royal Astronomical Society

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155

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ALMA observations have revealed that [C$\scriptstyle \rm II$]158μm line emission in high-z galaxies is ≈2 − 3 × more extended than the UV continuum emission. Here we explore whether surface brightness dimming (SBD) of the [C$\scriptstyle \rm II$] line is responsible for the reported [C$\scriptstyle \rm II$] deficit, and the large L[OIII]/L[CII] luminosity ratio measured in early galaxies. We first analyse archival ALMA images of nine z > 6 galaxies observed in both [C$\scriptstyle \rm II$] and [O$\scriptstyle \rm III$]. After performing several uv-tapering experiments to optimize the identification of extended line emission, we detect [C$\scriptstyle \rm II$] emission in the whole sample, with an extent systematically larger than the [O$\scriptstyle \rm III$] emission. Next, we use interferometric simulations to study the effect of SBD on the line luminosity estimate. About 40% of the extended [C$\scriptstyle \rm II$] component might be missed at an angular resolution of 0.8″, implying that L[CII] is underestimated by a factor ≈2 in data at low (<7) signal-to-noise ratio. By combining these results, we conclude that L[CII] of z > 6 galaxies lies, on average, slightly below the local L[CII] − SFR relation (Δz = 6 − 9 = −0.07 ± 0.3), but within the intrinsic dispersion of the relation. SBD correction also yields L[OIII]/L[CII] < 10, i.e. more in line with current hydrodynamical simulations.

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“…Future infrared space telescope (e.g. SPICA, Spinoglio et al 2017;Egami et al 2018) spanning similar wavelength range and with higher sensitivity may help improve the constraint near emission peak and hence the observationally-derived dust temperatures.…”

Section: Comparing Simulation To Observationmentioning

confidence: 99%

On the dust temperatures of high-redshift galaxies

Liang

Feldmann

Kereš

et al. 2019

Monthly Notices of the Royal Astronomical Society

148

173

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Dust temperature is an important property of the interstellar medium (ISM) of galaxies. It is required when converting (sub)millimetre broad-band flux to total infrared luminosity (LIR), and hence star formation rate, in high-redshift galaxies. However, different definitions of dust temperatures have been used in the literature, leading to different physical interpretations of how ISM conditions change with, e.g. redshift and star formation rate. In this paper, we analyse the dust temperatures of massive ($M_{\rm star} \gt 10^{10}\, \mathrm{M}_{\odot }$) $z$ = 2–6 galaxies with the help of high-resolution cosmological simulations from the Feedback in Realistic Environments (fire) project. At $z$ ∼ 2, our simulations successfully predict dust temperatures in good agreement with observations. We find that dust temperatures based on the peak emission wavelength increase with redshift, in line with the higher star formation activity at higher redshift, and are strongly correlated with the specific star formation rate. In contrast, the mass-weighted dust temperature, which is required to accurately estimate the total dust mass, does not strongly evolve with redshift over $z$ = 2–6 at fixed IR luminosity but is tightly correlated with LIR at fixed $z$. We also analyse an ‘equivalent’ dust temperature for converting (sub)millimetre flux density to total IR luminosity, and provide a fitting formula as a function of redshift and dust-to-metal ratio. We find that galaxies of higher equivalent (or higher peak) dust temperature (‘warmer dust’) do not necessarily have higher mass-weighted temperatures. A ‘two-phase’ picture for interstellar dust can explain the different scaling relations of the various dust temperatures.

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Probing the high-redshift universe with SPICA: Toward the epoch of reionisation and beyond

Cited by 22 publications

References 241 publications

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

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

Missing [C ii] emission from early galaxies

On the dust temperatures of high-redshift galaxies

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