The ALMA-ALPINE [CII] survey

Burgarella, D.; Bogdanoska, J.; Nanni, Ambra; Bardelli, S.; Béthermin, M.; Boquien, M.; Buat, V.; Faisst, Andreas L.; Dessauges‐Zavadsky, M.; Fudamoto, Yoshinobu; Fujimoto, Seiji; Giavalisco, Mauro; Ginolfi, M.; Gruppioni, C.; Hathi, Nimish P.; Ibar, E.; Jones, G. C.; Koekemoer, Anton M.; Kohno, Kotaro; Lemaux, Brian C.; Narayanan, Desika; Oesch, Pascal; Ouchi, Masami; Riechers, Dominik A.; Pozzi, F.; Romano, Michael; Talia, M.; Theulé, Patrice; Vergani, D.; Zamorani, G.; Zucca, E.; Cassata, P.

doi:10.1051/0004-6361/202142554

Cited by 8 publications

(5 citation statements)

References 138 publications

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“…Yellow points correspond to the CANDELS catalog. Purple pointing-down triangles depict ALMA-detected galaxies (Scoville et al 2016;Bowler et al 2018;Tadaki et al 2020;Burgarella et al 2022;Schouws et al 2022). Orange crosses show near-IR-faint, mid-IR-bright sources (i.e., red galaxies) discovered in the Spitzer/HST era (Huang et al 2011;Wang et al 2016;Alcalde Pampliega et al 2019).…”

Section: Star Formation Historiesmentioning

confidence: 99%

CEERS Key Paper. IV. A Triality in the Nature of HST-dark Galaxies

Pérez‐González

Barro

Annunziatella

et al. 2023

ApJL

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The new capabilities that JWST offers in the near- and mid-infrared (IR) are used to investigate in unprecedented detail the nature of optical/near-IR-faint, mid-IR-bright sources, with HST-dark galaxies among them. We gather JWST data from the CEERS survey in the Extended Groth Strip, jointly with HST data, and analyze spatially resolved optical-to-mid-IR spectral energy distributions to estimate photometric redshifts in two dimensions and stellar population properties on a pixel-by-pixel basis for red galaxies detected by NIRCam. We select 138 galaxies with F150W − F356W > 1.5 mag and F356W < 27.5 mag. The nature of these sources is threefold: (1) 71% are dusty star-forming galaxies (SFGs) at 2 < z < 6 with 9 < log M ⋆ / M ⊙ < 11 and a variety of specific SFRs (<1 to >100 Gyr−1); (2) 18% are quiescent/dormant (i.e., subject to reignition/rejuvenation) galaxies (QGs) at 3 < z < 5, with log M ⋆ / M ⊙ ∼ 10 and poststarburst mass-weighted ages (0.5–1.0 Gyr); and (3) 11% are strong young starbursts with indications of high equivalent width emission lines (typically, [O iii]+Hβ) at 6 < z < 7 (XELG-z6) and log M ⋆ / M ⊙ ∼ 9.5 . The sample is dominated by disk-like galaxies with remarkable compactness for XELG-z6 (effective radii smaller than 0.4 kpc). Large attenuations in SFGs, 2 < A(V) < 5 mag, are found within 1.5 times the effective radius, approximately 2 kpc, while QGs present A(V) ∼ 0.2 mag. Our SED-fitting technique reproduces the expected dust emission luminosities of IR-bright and submillimeter galaxies. This study implies high levels of star formation activity between z ∼ 20 and z ∼ 10, where virtually 100% of our galaxies had already formed 108 M ⊙, 60% had assembled 109 M ⊙, and 10% up to 1010 M ⊙ (in situ or ex situ).

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Section: Star Formation Historiesmentioning

confidence: 99%

CEERS Key Paper. IV. A Triality in the Nature of HST-dark Galaxies

Pérez‐González

Barro

Annunziatella

et al. 2023

ApJL

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“…Most notably we do not account for dust extinction. Recent ALMA surveys report the existence of a substantial amount of dust in star-forming galaxies at z ∼ 6−8 (Fudamoto et al 2020;Burgarella et al 2022;Bakx et al 2021;Schouws et al 2022;Tamura et al 2019;Inami et al 2022). Given the importance of emission line ratios including [Oiii] 5007 Å, accurate modeling of dust extinction may be needed for future studies.…”

Section: Discussionmentioning

confidence: 99%

Simulations of high-redshift [OIII] emitters: Chemical evolution and multi-line diagnostics

Nakazato¹,

Yoshida²,

Ceverino³

2023

Preprint

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Recent observations by James Webb Space Telescope discovered a number of high-redshift galaxies with strong emission lines from doubly ionized oxygen. Combined with ALMA observations of farinfrared lines, multi-line diagnostics can be applied to the high-redshift galaxies in order to probe the physical conditions of the inter-stellar medium. We study the formation and evolution of galaxies using the FirstLight simulation suite, which provides outputs of 62 high-resolution, zoom-in galaxy simulations. We devise a physical model of Hii regions and calculate spatially resolved [Oiii] line emission. We show that massive galaxies with stellar masses of M * > 10 9 M chemically evolve rapidly to z = 9. Young stellar populations in the star-forming galaxies boost the [Oiii] line emission, rendering the ratio of line luminosity to star formation rate larger than that for low-redshift galaxies, which is consistent with recent observations. Measuring the flux ratios of rest-frame optical and far-infrared lines allows us to estimate the physical conditions such as density and metallicity of the star-forming gas in high-redshift [Oiii] emitters.

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“…Most notably, weonly account for simplified dust extinction. Recent ALMA surveys report the existence of a substantial amount of dust in star-forming galaxies at z ∼ 6-8 (Tamura et al 2019;Fudamoto et al 2020;Bakx et al 2021;Burgarella et al 2022;Inami et al 2022;Schouws et al 2022). Given the importance of emission line ratios including [O III] 5007 Å, accurate modeling of dust extinction may be needed for future studies.…”

Section: Discussionmentioning

confidence: 99%

Simulations of High-redshift [O iii] Emitters: Chemical Evolution and Multiline Diagnostics

Nakazato

Yoshida

Ceverino

2023

ApJ

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Recent observations by the James Webb Space Telescope discovered a number of high-redshift galaxies with strong emission lines from doubly ionized oxygen. Combined with Atacama Large Millimeter/submillimeter Array observations of far-infrared lines, multiline diagnostics can be applied to the high-redshift galaxies in order to probe the physical conditions of the interstellar medium. We study the formation and evolution of galaxies using the FirstLight simulation suite, which provides outputs of 62 high-resolution, zoom-in galaxy simulations. We devise a physical model of H ii regions and calculate spatially resolved [O iii] line emission. We show that massive galaxies with stellar masses of M * > 109 M ⊙ chemically evolve rapidly to z = 9. Young stellar populations in the star-forming galaxies boost the [O iii] line emission, rendering the ratio of line luminosity to star formation rate larger than that for low-redshift galaxies, which is consistent with recent observations. Measuring the flux ratios of rest-frame optical and far-infrared lines allows us to estimate the physical conditions such as density and metallicity of the star-forming gas in high-redshift [O iii] emitters.

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The ALMA-ALPINE [CII] survey

Cited by 8 publications

References 138 publications

CEERS Key Paper. IV. A Triality in the Nature of HST-dark Galaxies

CEERS Key Paper. IV. A Triality in the Nature of HST-dark Galaxies

Simulations of high-redshift [OIII] emitters: Chemical evolution and multi-line diagnostics

Simulations of High-redshift [O iii] Emitters: Chemical Evolution and Multiline Diagnostics

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