The ALPINE-ALMA [C <scp>ii</scp>] Survey: kinematic diversity and rotation in massive star-forming galaxies at <i>z</i> ~ 4.4–5.9

Jones, G. C.; Vergani, D.; Romano, Michael; Ginolfi, M.; Fudamoto, Yoshinobu; Béthermin, M.; Fujimoto, Seiji; Lemaux, B. C.; Morselli, L.; Capak, P.; Cassata, P.; Faisst, Andreas L.; Fèvre, O. Le; Schaerer, D.; Silverman, J. D.; Yan, Lin; Boquien, M.; Cimatti, A.; Dessauges‐Zavadsky, M.; Ibar, E.; Maiolino, R.; Rizzo, Francesca; Talia, M.; Zamorani, G.

doi:10.1093/mnras/stab2226

Cited by 52 publications

(52 citation statements)

References 105 publications

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“…Fortunately, thanks to the improving capabilities of the Atacama Large Millimeter Array (ALMA), we can make significant progress characterizing the physical properties of massive star-forming sources in the early universe (e.g., Hodge & da Cunha 2020). ALMA efficiently allows for a probe of the redshift and dynamical state of galaxies in the reionization epoch using bright interstellar medium (ISM)-cooling lines like 157.74 μm [C II] and 88.36 μm [O III] (e.g., Smit et al 2018;Hashimoto et al 2019;Tamura et al 2019;Jones et al 2021), while simultaneously probing the far-IR dust-continuum radiation (e.g., Capak et al 2015;Bowler et al 2018;Fudamoto et al 2020;Schouws et al 2022a). This provides us with an essential measure of the star formation in galaxies obscured by dust.…”

Section: Introductionmentioning

confidence: 99%

Reionization Era Bright Emission Line Survey: Selection and Characterization of Luminous Interstellar Medium Reservoirs in the z > 6.5 Universe

Bouwens

Smit

Schouws

et al. 2022

ApJ

127

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The Reionization Era Bright Emission Line Survey (REBELS) is a cycle-7 ALMA Large Program (LP) that is identifying and performing a first characterization of many of the most luminous star-forming galaxies known in the z > 6.5 universe. REBELS is providing this probe by systematically scanning 40 of the brightest UV-selected galaxies identified over a 7 deg2 area for bright [C ii]158 μm and [O iii]88 μm lines and dust-continuum emission. Selection of the 40 REBELS targets was done by combining our own and other photometric selections, each of which is subject to extensive vetting using three completely independent sets of photometry and template-fitting codes. Building on the observational strategy deployed in two pilot programs, we are increasing the number of massive interstellar medium (ISM) reservoirs known at z > 6.5 by ∼4–5× to >30. In this manuscript, we motivate the observational strategy deployed in the REBELS program and present initial results. Based on the first-year observations, 18 highly significant ≥ 7σ [C ii]158 μm lines have already been discovered, the bulk of which (13/18) also show ≥3.3σ dust-continuum emission. These newly discovered lines more than triple the number of bright ISM-cooling lines known in the z > 6.5 universe, such that the number of ALMA-derived redshifts at z > 6.5 rival Lyα discoveries. An analysis of the completeness of our search results versus star formation rate (SFR) suggests an ∼79% efficiency in scanning for [C ii]158 μm when the SFRUV+IR is >28 M ⊙ yr−1. These new LP results further demonstrate ALMA’s efficiency as a “redshift machine,” particularly in the Epoch of Reionization.

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Section: Introductionmentioning

confidence: 99%

Reionization Era Bright Emission Line Survey: Selection and Characterization of Luminous Interstellar Medium Reservoirs in the z > 6.5 Universe

Bouwens

Smit

Schouws

et al. 2022

ApJ

127

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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%

“…However, as shown in Fujimoto et al (2020) the offsets in ALPINE galaxies appear small or altogether absent, so displacements should not play a major role in the evolution of attenuation curves in our sample. This being said, a number of ALPINE galaxies are mergers (Le Fèvre et al 2020;Jones et al 2020Jones et al , 2021 and most of these sources are likely undergoing inflow and/or unresolved minor mergers. This is also true for our subsample.…”

Section: Dust Properties and The δ-A V Relationmentioning

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 combination of ALMA and sub-kpc resolution HST imaging can mitigate these issues. Importantly, C + emission provides kinematic information of UV and optically dust-obscured merger components (see e.g., [151,152]).…”

Section: Contribution Of Mergers To Mass Assembly and The Emergence O...mentioning

confidence: 99%

ALPINE: A Large Survey to Understand Teenage Galaxies

et al. 2022

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A multiwavelength study of galaxies is important to understand their formation and evolution. Only in the recent past, thanks to the Atacama Large (Sub) Millimeter Array (ALMA), were we able to study the far-infrared (IR) properties of galaxies at high redshifts. In this article, we summarize recent research highlights and their significance to our understanding of early galaxy evolution from the ALPINE survey, a large program with ALMA to observe the dust continuum and 158μm C+ emission of normal star-forming galaxies at z= 4–6. Combined with ancillary data at UV through near-IR wavelengths, ALPINE provides the currently largest multiwavelength sample of post-reionization galaxies and has advanced our understanding of (i) the demographics of C+ emission; (ii) the relation of star formation and C+ emission; (iii) the gas content; (iv) outflows and enrichment of the intergalactic medium; and (v) the kinematics, emergence of disks, and merger rates in galaxies at z>4. ALPINE builds the basis for more detailed measurements with the next generation of telescopes, and places itself as an important post-reionization baseline sample to allow a continuous study of galaxies over 13 billion years of cosmic time.

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The ALPINE-ALMA [C ii] Survey: kinematic diversity and rotation in massive star-forming galaxies at z ~ 4.4–5.9

Cited by 52 publications

References 105 publications

Reionization Era Bright Emission Line Survey: Selection and Characterization of Luminous Interstellar Medium Reservoirs in the z > 6.5 Universe

Reionization Era Bright Emission Line Survey: Selection and Characterization of Luminous Interstellar Medium Reservoirs in the z > 6.5 Universe

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

ALPINE: A Large Survey to Understand Teenage Galaxies

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