The ALPINE-ALMA [CII] survey

Pozzi, F.; Calura, F.; Fudamoto, Y.; Dessauges‐Zavadsky, M.; Gruppioni, C.; Talia, M.; Zamorani, G.; Béthermin, M.; Cimatti, A.; Khusanova, Y.; Decarli, Roberto; Fèvre, O. Le; Capak, P.; Cassata, P.; Faisst, Andreas L.; Yan, Lin; Silverman, John D.; Bardelli, S.; Boquien, M.; Enia, A.; Narayanan, Desika; Ginolfi, M.; Hathi, N. P.; Jones, G. C.; Koekemoer, Anton M.; Lemaux, Brian C.; Loiacono, F.; Maiolino, R.; Riechers, D.; Rodighiero, G.; Romano, Michael; Vallini, L.; Vergani, D.; Zucca, E.

doi:10.1051/0004-6361/202040258

Cited by 27 publications

(21 citation statements)

References 121 publications

(159 reference statements)

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“…The continuum surrounding this line lies close to the peak of the FIR dust emission, † Deceased. making detections easier and helping to constrain the total FIR luminosity and obscured star formation (e.g., Gruppioni et al 2020;Khusanova et al 2021;Pozzi et al 2021). Moreover, the [CII] emission can provide important information on a variety of ISM properties, such as the star-formation rate (SFR; e.g., De Looze et al 2014;Olsen et al 2017), the presence of outflows (e.g., Gallerani et al 2018;Ginolfi et al 2020), and the kinematics of the ISM (e.g., Jones et al 2021;Romano et al 2021).…”

Section: Introductionmentioning

confidence: 99%

The ALPINE-ALMA [CII] survey: The population of [CII]-undetected galaxies and their role in the L_[CII]-SFR relation

Romano

Morselli

Cassata

et al. 2022

A&A

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The [CII] 158 μm emission line represents one of the most profitable tools for the investigation of the high-redshift galaxies in the early Universe so far. 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 the 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] nondetected galaxies. In this work, we characterize the population of [CII] nondetections in ALPINE. By stacking their ALMA spectra, we obtained 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 found a L[CII]-SFR relation with a slope b = 1.14 ± 0.11, which is 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 deviate from the observed L[CII]-SFR relation most 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 favor of a deficit of [CII] content in high-z galaxies, in contrast with earlier studies.

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Section: Introductionmentioning

confidence: 99%

The ALPINE-ALMA [CII] survey: The population of [CII]-undetected galaxies and their role in the L_[CII]-SFR relation

Romano

Morselli

Cassata

et al. 2022

A&A

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“…Even though the average dust content of galaxies in the EoR is expected to be lower compared to the low-redshift Universe (z < 4, e.g. Li et al 2019;Magnelli et al 2020;Pozzi et al 2021), it still has a significant impact on shaping observations by attenuating the emitted source radiation (see review by Salim & Narayanan 2020), particularly on the most massive galaxies. Recent observations have also found dust-obscured galaxies (as early as z ∼ 7, e.g.…”

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confidence: 99%

First Light And Reionisation Epoch Simulations (FLARES) – III. The properties of massive dusty galaxies at cosmic dawn

Vijayan

Wilkins

Lovell

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Using the First Light And Reionisation Epoch Simulations (Flares) we explore the dust driven properties of massive high-redshift galaxies at z ∈ [5, 10]. By post-processing the galaxy sample using the radiative transfer code skirt we obtain the full spectral energy distribution. We explore the resultant luminosity functions, IRX-β relations as well as the luminosity-weighted dust temperatures in the Epoch of Reionisation (EoR). We find that most of our results are in agreement with the current set of observations, but under-predict the number densities of bright IR galaxies, which are extremely biased towards the most overdense regions. We see that the Flares IRX-β relation (for 5 ≤ z ≤ 8) predominantly follows the local starburst relation. The IRX shows an increase with stellar mass, plateauing at the high-mass end (∼1010 M⊙) and shows no evolution in the median normalization with redshift. We also look at the dependence of the peak dust temperature (Tpeak) on various galaxy properties including the stellar mass, IR luminosity and sSFR, finding the correlation to be strongest with sSFR. The luminosity-weighted dust temperatures increase towards higher redshifts, with the slope of the Tpeak - redshift relation showing a higher slope than the lower redshift relations obtained from previous observational and theoretical works. The results from Flares, which is able to provide a better statistical sample of high-redshift galaxies compared to other simulations, provides a distinct vantage point for the high-redshift Universe.

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“…Being the largest targeted survey of high-redshift galaxies with ALMA, ALPINE is a real treasure trove to study outflows (Ginolfi et al 2020), mergers and morpho-kinematic diversity (Le Fèvre et al 2020;Jones et al 2020Jones et al , 2021Romano et al 2021), Ly-α emitters (Cassata et al 2020), [C ii] as an SFR tracer (Schaerer et al 2020), [C ii] sizes (Fujimoto et al 2020), molecular gas (Dessauges-Zavadsky et al 2020), [C ii] luminosity functions (Yan et al 2020;Gruppioni et al 2020;Loiacono et al 2021), the main sequence (Khusanova et al 2021), the dust mass budget (Pozzi et al 2021), and even the study of serendipitously discovered objects (Gruppioni et al 2020;Romano et al 2020;Loiacono et al 2021). Of particular interest to this article, Fudamoto et al (2020a) delved into the attenuation properties of ALPINE galaxies.…”

Section: The Alpine Surveymentioning

confidence: 99%

The ALPINE-ALMA [CII] survey: dust attenuation curves at z=4.4-5.5

Boquien,

Buat,

Burgarella

et al. 2022

Preprint

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Context. There is now ample evidence that dust is already present in abundance at high redshift. However, given the faintness of distant galaxies in the optical and the near-infrared, datasets are still limited and how the dust affects the emerging radiation of galaxies at very high redshift is not yet fully understood. Aims. Using the ALMA Large Program to INvestigate [C ii] at Early times (ALPINE), our objective is to quantify the dust attenuation properties in galaxies at z = 4.4-5.5, and in particular the shape of their attenuation curve. Methods. Using the CIGALE Spectral Energy Distribution (SED) code, we model the stellar populations and their interaction with the dust in order to measure some of the physical properties of the ALPINE sample. We select a subsample of 23 main-sequence galaxies requiring a detection in at least 6 bands in the rest-frame UV and optical, as well as in the dust continuum around 158 µm and/or the [C ii] fine structure line, whose inclusion is important to improve the constraints on the physical properties, while having a reasonably small uncertainty on the slope of the attenuation curves. Results. We find that the attenuation curves span a broad range of properties, from curves that are much steeper than the SMC extinction curve, to shallower than the starburst attenuation curve. The shape of the attenuation curves strongly depends on the Vband attenuation. Galaxies with the lowest attenuation also present the steepest curves. The steepness of such curves is probably the consequence of the combination of the intrinsic physical properties of the dust, the relative distribution of stars and dust in the interstellar medium, and the differential reddening, with an important fraction of the dust concentrated in star-forming regions. The broad range of attenuation curves found at z ∼ 5 shows that no single attenuation curve is appropriate for main sequence galaxies and that assuming a fixed curve can lead to large errors, for instance in the interpretation and use of the IRX-β diagram, if SED modeling is not feasible. Conclusions. Great caution should be exercised when correcting high redshift galaxies for the presence of dust using the UV slope β as it can affect the estimation of both star-formation rate and stellar mass even at low V-band attenuation due to the steepness of the attenuation curve. However, when SED modeling can be used, the impact of the choice of the attenuation curve on the star formation rate and the stellar mass is limited.

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The ALPINE-ALMA [CII] survey

Cited by 27 publications

References 121 publications

The ALPINE-ALMA [CII] survey: The population of [CII]-undetected galaxies and their role in the L_[CII]-SFR relation

The ALPINE-ALMA [CII] survey: The population of [CII]-undetected galaxies and their role in the L_[CII]-SFR relation

First Light And Reionisation Epoch Simulations (FLARES) – III. The properties of massive dusty galaxies at cosmic dawn

The ALPINE-ALMA [CII] survey: dust attenuation curves at z=4.4-5.5

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The ALPINE-ALMA [CII] survey

Cited by 27 publications

References 121 publications

The ALPINE-ALMA [CII] survey: The population of [CII]-undetected galaxies and their role in the L[CII]-SFR relation

The ALPINE-ALMA [CII] survey: The population of [CII]-undetected galaxies and their role in the L[CII]-SFR relation

First Light And Reionisation Epoch Simulations (FLARES) – III. The properties of massive dusty galaxies at cosmic dawn

The ALPINE-ALMA [CII] survey: dust attenuation curves at z=4.4-5.5

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The ALPINE-ALMA [CII] survey: The population of [CII]-undetected galaxies and their role in the L_[CII]-SFR relation

The ALPINE-ALMA [CII] survey: The population of [CII]-undetected galaxies and their role in the L_[CII]-SFR relation