Burgarella, D. and Bogdanoska, J. and Nanni, A. and Bardelli, S. and Béthermin, M. and Boquien, M. and Buat, V. and Faisst, A. L. and Dessauges-Zavadsky, M. and Fudamoto, Y. and Fujimoto, S. and Giavalisco, M. and Ginolfi, M. and Gruppioni, C. and Hathi, N. P. and Ibar, E. and Jones, G. C. and Koekemoer, A. M. and Kohno, K. and Lemaux, B. C. and Narayanan, D. and Oesch, P. and Ouchi, M. and Riechers, D. A. and Pozzi, F. and Romano, M. and Schaerer, D. and Talia, M. and Theulé, P. and Vergani, D. and Zamorani, G. and Zucca, E. and Cassata, P. (2022) The ALMA-ALPINE [CII] survey - The star formation history and the dust emission of star-forming galaxies at 4.5 < z < 6.2°. Astronomy and Astrophysics, 664 . Art. No. A73. ISSN 0004-6361. doi:10.1051/0004-6361/202142554. https://resolver.caltech.edu/CaltechAUTHORS:20220805-204876000
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Abstract
Star-forming galaxies are composed of various types of galaxies. However, the luminosity functions at z ≳ 4–5 suggest that most galaxies have a relatively low stellar mass (log M_(star) ∼ 10) and a low dust attenuation (A_(FUV) ∼ 1.0). The physical properties of these objects are quite homogeneous. We used an approach where we combined their rest-frame far-infrared and submillimeter emissions and utilized the universe and the redshift as a spectrograph to increase the amount of information in a collective way. From a subsample of 27 ALMA-detected galaxies at z > 4.5, we built an infrared spectral energy distribution composite template. It was used to fit, with CIGALE, the 105 galaxies (detections and upper limits) in the sample from the far-ultraviolet to the far-infrared. The derived physical parameters provide information to decipher the nature of the dust cycle and of the stellar populations in these galaxies. The derived IR composite template is consistent with the galaxies in the studied sample. A delayed star formation history with τ_(main) = 500 Myr is slightly favored by the statistical analysis as compared to a delayed with a final burst or a continuous star formation history. The position of the sample in the star formation rate (SFR) versus M_(star) diagram is consistent with previous papers. The redshift evolution of the log M_(star) versus A_(FUV) relation is in agreement with an evolution in redshift of this relation. This evolution is necessary to explain the cosmic evolution of the average dust attenuation of galaxies. Evolution is also observed in the L_(dust)/L_(FUV) (IRX) versus UV slope β_(FUV) diagram: younger galaxies have bluer β_(FUV). We modeled the shift of galaxies in the IRX versus the β_(FUV) diagram with the mass-weighted age as a free parameter, and we provide an equation to make predictions. The large sample studied in this paper is generally consistent with models that assume rapid dust formation from supernovae and removal of dust by outflows and supernovae blasts. However, we find that high mass dusty star-forming galaxies cannot be explained by the models.
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| Alternate Title: | The ALMA-ALPINE [CII] survey. The star formation history and the dust emission of star-forming galaxies at 4.5 < z < 6.2⋆, IR characteristic emission and dust properties of star-forming galaxies at 4.5 < z < 6.2 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Additional Information: | © D. Burgarella et al. 2022. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Received: 30 October 2021 Accepted: 8 February 2022. This program receives funding from the CNRS national program Cosmology and Galaxies. D.R. acknowledges support from the National Science Foundation under grant No. AST-1910107. D.R. also acknowledges support from the Alexander von Humboldt Foundation through a Humboldt Research Fellowship for Experienced Researchers. M.T. acknowledges the support from grant PRIN MIUR 2017 20173ML3WW 001. A.N. acknowledges support from the Narodowe Centrum Nauki (UMO-2018/30/E/ST9/00082 and UMO-2020/38/E/ST9/00077). G.C.J. acknowledges ERC Advanced Grant 695671 “QUENCH” and support by the Science and Technology Facilities Council (STFC). Y.F. further acknowledges support from NAOJ ALMA Scientific Research Grant number 2020-16B. M.R. acknowledges support from the Narodowe Centrum Nauki (UMO-2020/38/E/ST9/00077). M.B. gratefully acknowledges support by the ANID BASAL project FB210003 and from the FONDECYT regular grant 1211000. E.I. acknowledges partial support from FONDECYT through grant N° 1171710. | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Group: | Infrared Processing and Analysis Center (IPAC) | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
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| Subject Keywords: | galaxies: formation / galaxies: evolution / early Universe / submillimeter: galaxies / ultraviolet: galaxies / infrared: galaxies | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| DOI: | 10.1051/0004-6361/202142554 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Record Number: | CaltechAUTHORS:20220805-204876000 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Persistent URL: | https://resolver.caltech.edu/CaltechAUTHORS:20220805-204876000 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Official Citation: | The ALMA-ALPINE [CII] survey - The star formation history and the dust emission of star-forming galaxies at 4.5 < z < 6.2 D. Burgarella, J. Bogdanoska, A. Nanni, S. Bardelli, M. Béthermin, M. Boquien, V. Buat, A. L. Faisst, M. Dessauges-Zavadsky, Y. Fudamoto, S. Fujimoto, M. Giavalisco, M. Ginolfi, C. Gruppioni, N. P. Hathi, E. Ibar, G. C. Jones, A. M. Koekemoer, K. Kohno, B. C. Lemaux, D. Narayanan, P. Oesch, M. Ouchi, D. A. Riechers, F. Pozzi, M. Romano, D. Schaerer, M. Talia, P. Theulé, D. Vergani, G. Zamorani, E. Zucca, P. Cassata and the ALPINE team A&A, 664 (2022) A73 DOI: https://doi.org/10.1051/0004-6361/202142554 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Usage Policy: | No commercial reproduction, distribution, display or performance rights in this work are provided. | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| ID Code: | 116153 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Collection: | CaltechAUTHORS | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Deposited By: | George Porter | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Deposited On: | 11 Aug 2022 22:36 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Last Modified: | 17 Aug 2022 16:48 |
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