ALMA Lensing Cluster Survey: Bright [C ii] 158 μm Lines from a Multiply Imaged Sub-L
               <sup>⋆</sup> Galaxy at z = 6.0719

Fujimoto, Seiji; Oguri, Masamune; Brammer, Gabriel; Yoshimura, Yuki; Laporte, Nicolas; González-López, Jorge; Caminha, G. B.; Kohno, Kotaro; Zitrin, Adi; Richard, Johan; Ouchi, Masami; Bauer, F. E.; Smail, Ian; Hatsukade, Bunyo; Ono, Yoshiyasu; Kokorev, Vasily; Umehata, Hideki; Schaerer, D.; Knudsen, K. K.; Sun, Fengwu; Magdis, G.; Valentino, F.; Ao, Yiping; Toft, Sune; Dessauges‐Zavadsky, M.; Shimasaku, Kazuhiro; Caputi, K.; Kusakabe, Haruka; Morokuma-Matsui, Kana; Kikuchihara, Shotaro; Egami, Eiichi; Lee, Minju; Rawle, Timothy D.; Espada, Daniel

doi:10.3847/1538-4357/abd7ec

Cited by 44 publications

(41 citation statements)

References 138 publications

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“…We relate the observed [C ii] luminosity to the total dust mass via the gas mass and a gas-to-dust ratio (assumed to scale linearly with the metallicity, which is justified down to . Two parameters are added in the expression for α CII in order to account for both (i) the expected offset from the KS-relation (i.e., the burstiness of the SF of a galaxy parametrized by κ s ) and (ii) the observed larger extension of [C ii] with respect to stellar emission at high-z (up to 1.5-3 times larger; Carniani et al 2017bCarniani et al , 2018Carniani et al , 2020Matthee et al 2017Matthee et al , 2019Fujimoto et al 2019Fujimoto et al , 2020Fujimoto et al , 2021Ginolfi et al 2020;Herrera-Camus et al 2021).…”

Section: Dust Temperature From [C Ii] Emissionmentioning

confidence: 99%

Accurate dust temperature determination in a $z = 7.13$ galaxy

Bakx,

Sommovigo,

Carniani

et al. 2021

Preprint

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We report ALMA Band 9 continuum observations of the normal, dusty star-forming galaxy A1689-zD1 at z = 7.13, resulting in a ∼4.6 σ detection at 702 GHz. For the first time these observations probe the far infrared (FIR) spectrum shortward of the emission peak of a galaxy in the Epoch of Reionization (EoR). Together with ancillary data from earlier works, we derive the dust temperature, T d , and mass, M d , of A1689-zD1 using both traditional modified blackbody spectral energy density fitting, and a new method that relies only on the [C ii] 158 µm line and underlying continuum data. The two methods give T d = (42 +13 −7 , 40 +13 −7 ) K, and M d = (1.7 +1.3 −0.7 , 2.0 +1.8 −1.0 ) × 10 7 M . Band 9 observations improve the accuracy of the dust temperature (mass) estimate by ∼ 50% (6 times). The derived temperatures confirm the reported increasing T d -redshift trend between z = 0 and 8; the dust mass is consistent with a supernova origin. Although A1689-zD1 is a normal UV-selected galaxy, our results, implying that ∼85% of its star formation rate is obscured, underline the non-negligible effects of dust in EoR galaxies.

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Section: Dust Temperature From [C Ii] Emissionmentioning

confidence: 99%

Accurate dust temperature determination in a $z = 7.13$ galaxy

Bakx,

Sommovigo,

Carniani

et al. 2021

Preprint

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“…At high redshifts, the number of [CII] detections is increasing, but there are still few constraints from the low SFR, stellar mass regime, which are fundamental to properly characterize the L [CII] -SFR relation over cosmic time. Indeed, only a handful of low-SFR, high-z sources have been detected (or undetected) so far in [CII], most of them as strongly lensed galaxies (e.g., Knudsen et al 2016;Carniani et al 2017;Laporte et al 2019;Fujimoto et al 2021;Jolly et al 2021;Laporte et al 2021).…”

Section: Discussionmentioning

confidence: 99%

“…However, further and deeper observations are needed in order to confirm these results, especially in the low SFR regime, where the L [CII] -SFR relation is consistent from the spatiallyresolved and the entire galaxy scales, and where only a handful of strongly lensed galaxies have been detected so far at log(SFR/M yr −1 ) 0.5 (e.g., Knudsen et al 2016;Fujimoto et al 2021). Current simulations provide different results at high redshift, suggesting that many physical mechanisms could be in place in the ISM of distant galaxies (e.g., Lagache et al 2018;Arata et al 2020).…”

Section: Discussionmentioning

confidence: 99%

The ALPINE-ALMA [CII] Survey: the population of [CII]-undetected galaxies and their role in the $\mathrm{L_{[CII]}}$-SFR relation

Romano,

Morselli,

Cassata

et al. 2022

Preprint

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The [CII] 158 µm emission line represents so far one of the most profitable tools for the investigation of the high-redshift galaxies in the early Universe. Being one of the brightest cooling lines in the rest-frame far-infrared regime of star-forming galaxies, it has been successfully exploited as a tracer of star-formation rate (SFR) in local sources. The picture is more complex at higher redshifts, where its usability in this context is still under investigation. Recent results from the ALMA Large Program to INvestigate [CII] at Early times (ALPINE) survey suggest that there is no (or weak) evolution of the L [CII] -SFR relation up to z ∼ 6 but their reliability is hampered by the presence of a large population of [CII] non-detected galaxies. In this work, we characterize the population of [CII] non-detections in ALPINE. By stacking their ALMA spectra, we obtain a signal detected at ∼ 5.1σ, resulting in a [CII] luminosity of log(L [CII] /L ) ∼ 7.8. When combining this value with those from the [CII] detections, we find a L [CII] -SFR relation with a slope b = 1.14 ± 0.11, in agreement within the uncertainties both with the linear relation found in the local Universe, and with the previous findings from ALPINE at z ∼ 5. This suggests that the [CII] line can be considered a good tracer of star formation up to the distant Universe. Finally, we show that the galaxies of our sample that most deviate from the observed L [CII] -SFR relation could suffer from a less precise redshift estimation, perhaps artificially reducing their [CII] luminosity. In this respect, we claim that there is no evidence in favour of a deficit of [CII] content in high-z galaxies, in contrast with earlier studies.

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“…In Figure 3 we present the measured [C ] luminosity as a function of SFR UV and include sources from the literature for comparison (Matthee et al 2019;Knudsen et al 2016;Bradač et al 2017;Fujimoto et al 2021). The UV SFRs are calculated using the Kennicutt & Evans (2012) 3.…”

Section: 𝐿 [Cii] Vs Sfr Relationmentioning

confidence: 99%

“…However, much less is known about galaxies at these high redshifts which are more representative of the galaxy population as a whole (𝐿 ≤ 𝐿 * z=7 ). Our best insights into this fainter population are rare, apparently bright sources, which have been gravitationally lensed (Knudsen et al 2016;Bradač et al 2017;Fujimoto et al 2021;Laporte et al 2021). Despite the capability of ALMA to probe galaxies in the EoR, it has limited sky coverage in the Northern Hemisphere and so interesting targets might be missed.…”

Section: Introductionmentioning

confidence: 99%

Spectroscopic confirmation of a gravitationally lensed Lyman-break galaxy at z[C ii] = 6.827 using NOEMA

Molyneux

Smit

Bradley

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We present the spectroscopic confirmation of the brightest known gravitationally lensed Lyman break galaxy in the Epoch of Reionisation, A1703-zD1, through the detection of [C ii]158 μm at a redshift of z = 6.8269 ± 0.0004. This source was selected behind the strong lensing cluster Abell 1703, with an intrinsic $L_{\rm UV} \sim L^*_{\rm z=7}$ luminosity and a very blue Spitzer/IRAC [3.6]–[4.5] colour, implying high equivalent width line emission of [O iii]+Hβ. [C ii] is reliably detected at 6.1σ co-spatial with the rest-frame UV counterpart, showing similar spatial extent. Correcting for the lensing magnification, the [C ii] luminosity in A1703-zD1 is broadly consistent with the local $L_{\rm [C\, \small {II}]}$ – SFR relation. We find a clear velocity gradient of 103 ± 22 km $\rm s^{-1}$ across the source which possibly indicates rotation or an ongoing merger. We furthermore present spectral scans with no detected [C ii] above 4.6σ in two unlensed Lyman break galaxies in the EGS-CANDELS field at z ∼ 6.6–6.9. This is the first time that NOEMA has been successfully used to observe [C ii] in a ‘normal’ star-forming galaxy at z > 6, and our results demonstrate its capability to complement ALMA in confirming galaxies in the Epoch of Reionisation.

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ALMA Lensing Cluster Survey: Bright [C ii] 158 μm Lines from a Multiply Imaged Sub-L ^⋆ Galaxy at z = 6.0719

Cited by 44 publications

References 138 publications

Accurate dust temperature determination in a $z = 7.13$ galaxy

Accurate dust temperature determination in a $z = 7.13$ galaxy

The ALPINE-ALMA [CII] Survey: the population of [CII]-undetected galaxies and their role in the $\mathrm{L_{[CII]}}$-SFR relation

Spectroscopic confirmation of a gravitationally lensed Lyman-break galaxy at z[C ii] = 6.827 using NOEMA

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ALMA Lensing Cluster Survey: Bright [C ii] 158 μm Lines from a Multiply Imaged Sub-L ⋆ Galaxy at z = 6.0719

Cited by 44 publications

References 138 publications

Accurate dust temperature determination in a $z = 7.13$ galaxy

Accurate dust temperature determination in a $z = 7.13$ galaxy

The ALPINE-ALMA [CII] Survey: the population of [CII]-undetected galaxies and their role in the $\mathrm{L_{[CII]}}$-SFR relation

Spectroscopic confirmation of a gravitationally lensed Lyman-break galaxy at z[C ii] = 6.827 using NOEMA

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ALMA Lensing Cluster Survey: Bright [C ii] 158 μm Lines from a Multiply Imaged Sub-L ^⋆ Galaxy at z = 6.0719