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51. COSMOS2020:UV-selected galaxies at z >= 7.5

Author

Kauffmann, O. B., Ilbert, O., Weaver, J. R., McCracken, H. J., Milvang-Jensen, B., Brammer, G., Davidzon, I., Le Fevre, O., Liu, D., Mobasher, B., Moneti, A., Shuntov, M., Toft, S., Casey, C. M., Dunlop, J. S., Kartaltepe, J. S., Koekemoer, A. M., Sanders, D. B., Tresse, L., Kauffmann, O. B., Ilbert, O., Weaver, J. R., McCracken, H. J., Milvang-Jensen, B., Brammer, G., Davidzon, I., Le Fevre, O., Liu, D., Mobasher, B., Moneti, A., Shuntov, M., Toft, S., Casey, C. M., Dunlop, J. S., Kartaltepe, J. S., Koekemoer, A. M., Sanders, D. B., and Tresse, L.

Abstract

This paper presents a new search for z >= 7.5 galaxies using the COSMOS2020 photometric catalogues. Finding galaxies at the reionisation epoch through deep imaging surveys remains observationally challenging. The larger area covered by ground-based surveys such as COSMOS enables the discovery of the brightest galaxies at these high redshifts. Covering 1.4 deg(2), our COSMOS catalogues were constructed from the latest UltraVISTA data release (DR4) combined with the final Spitzer/IRAC COSMOS images and the Hyper-Suprime-Cam Subaru Strategic Program DR2 release. We identified 17 new 7.5 < z < 10 candidate sources, and confirm 15 previously published candidates. Using deblended photometry extracted by fitting surface brightness models on multi-band images, we selected four candidates which would be rejected using fixed aperture photometry. We tested the robustness of all our candidates by comparing six different photometric redshift estimates. Finally, we computed the galaxy UV luminosity function in three redshift bins centred at z = 8, 9, 10. We find no clear evolution of the number density of the brightest galaxies M-UV < 21 .5, in agreement with previous works. Rapid changes in the quenching efficiency or attenuation by dust could explain such a lack of evolution between z similar to 8 and z similar to 9. A spectroscopic confirmation of the redshifts, already planned with JWST and the Keck telescopes, will be essential to confirm our results.

Published
2022

52. COSMOS2020:Manifold learning to estimate physical parameters in large galaxy surveys

Author

Davidzon, I., Jegatheesan, K., Ilbert, O., de la Torre, S., Leslie, S. K., Laigle, C., Hemmati, S., Masters, D. C., Blanquez-Sese, D., Kauffmann, O. B., Magdis, G. E., McCracken, H. J., Mobasher, B., Moneti, A., Sanders, D. B., Shuntov, M., Toft, S., Weaver, J. R., Malek, K., Davidzon, I., Jegatheesan, K., Ilbert, O., de la Torre, S., Leslie, S. K., Laigle, C., Hemmati, S., Masters, D. C., Blanquez-Sese, D., Kauffmann, O. B., Magdis, G. E., McCracken, H. J., Mobasher, B., Moneti, A., Sanders, D. B., Shuntov, M., Toft, S., Weaver, J. R., and Malek, K.

Abstract

We present a novel method for estimating galaxy physical properties from spectral energy distributions (SEDs) as an alternative to template fitting techniques and based on self-organizing maps (SOMs) to learn the high-dimensional manifold of a photometric galaxy catalog. The method has previously been tested with hydrodynamical simulations in Davidzon et al. (2019, MNRAS, 489, 4817), however, here it is applied to real data for the first time. It is crucial for its implementation to build the SOM with a high-quality panchromatic data set, thus we selected "COSMOS2020" galaxy catalog for this purpose. After the training and calibration steps with COSMOS2020, other galaxies can be processed through SOMs to obtain an estimate of their stellar mass and star formation rate (SFR). Both quantities resulted in a good agreement with independent measurements derived from more extended photometric baseline and, in addition, their combination (i.e., the SFR vs. stellar mass diagram) shows a main sequence of star-forming galaxies that is consistent with the findings of previous studies. We discuss the advantages of this method compared to traditional SED fitting, highlighting the impact of replacing the usual synthetic templates with a collection of empirical SEDs built by the SOM in a "data-driven" way. Such an approach also allows, even for extremely large data sets, for an efficient visual inspection to identify photometric errors or peculiar galaxy types. While also considering the computational speed of this new estimator, we argue that it will play a valuable role in the analysis of oncoming large-area surveys such as Euclid of the Legacy Survey of Space and Time at the Vera C. Rubin Telescope.

Published
2022

53. COSMOS2020:Cosmic evolution of the stellar-to-halo mass relation for central and satellite galaxies up to z similar to 5

Author

Shuntov, M., McCracken, H. J., Gavazzi, R., Laigle, C., Weaver, J. R., Davidzon, I., Ilbert, O., Kauffmann, O. B., Faisst, A., Dubois, Y., Koekemoer, A. M., Moneti, A., Milvang-Jensen, B., Mobasher, B., Sanders, D. B., Toft, S., Shuntov, M., McCracken, H. J., Gavazzi, R., Laigle, C., Weaver, J. R., Davidzon, I., Ilbert, O., Kauffmann, O. B., Faisst, A., Dubois, Y., Koekemoer, A. M., Moneti, A., Milvang-Jensen, B., Mobasher, B., Sanders, D. B., and Toft, S.

Abstract

We used the COSMOS2020 catalog to measure the stellar-to-halo mass relation (SHMR) divided by central and satellite galaxies from z = 0.2 to z = 5.5. Starting from accurate photometric redshifts, we measured the near-infrared selected two-point angular correlation and stellar mass functions in ten redshift bins. We used a phenomenological model that parametrizes the stellar-to-halo mass relation for central galaxies and the number of galaxies inside each halo to describe our observations. This model qualitatively reproduces our measurements and their dependence on the stellar mass threshold. Surprisingly, the mean halo occupation distribution only shows a mild evolution with redshift suggesting that galaxies occupy halos similarly throughout cosmic time. At each redshift, we measured the ratio of stellar mass to halo mass, M-*/M-h, which shows the characteristic strong dependence of halo mass with a peak at M-h(peak) similar to 2 x 10(12) M-circle dot. For the first time, using a joint modeling of clustering and abundances, we measured the evolution of M-h(peak) from z = 0.2 to z = 5.5. M-h(peak) increases gradually with redshift from log M-h(peak)/M-circle dot similar to 12.1 at z similar to 0.3 to log M-h(peak)/M-circle dot similar to 12.3 at z similar to 2, and up to log M-h(peak)/M-circle dot similar to 12.9 at z similar to 5. Similarly, the stellar mass peak M-*(peak) increases with redshift from log M-*(peak)/M-circle dot similar to 10.5 at z similar to 0.3 to log M-*(peak)/M-circle dot similar to 10.9 at z similar to 3. The SHMR ratio at the peak halo mass remains almost constant with redshift. These results are in accordance with the scenario in which the peak of star-formation efficiency moves toward more massive halos at higher redshifts. We also measured the fraction of satellites as a function of stellar mass and redshift. For all stellar mass thresholds, the satellite fraction decreases at higher redshifts. At a given redshift, there is a higher frac

Published
2022

54. COSMOS2020:A Panchromatic View of the Universe to z ∼ 10 from Two Complementary Catalogs

Author

Weaver, J. R., Kauffmann, O. B., Ilbert, O., McCracken, H. J., Moneti, A., Toft, S., Brammer, G., Shuntov, M., Davidzon, I., Hsieh, B. C., Laigle, C., Anastasiou, A., Jespersen, C. K., Vinther, J., Capak, P., Casey, C. M., McPartland, C. J.R., Milvang-Jensen, B., Mobasher, B., Sanders, D. B., Zalesky, L., Arnouts, S., Aussel, H., Dunlop, J. S., Faisst, A., Franx, M., Furtak, L. J., Fynbo, J. P.U., Gould, K. M.L., Greve, T. R., Gwyn, S., Kartaltepe, J. S., Kashino, D., Koekemoer, A. M., Kokorev, V., Le Fevre, O., Lilly, S., Masters, D., Magdis, G., Mehta, V., Peng, Y., Riechers, D. A., Salvato, M., Sawicki, M., Scarlata, C., Scoville, N., Shirley, R., Silverman, J. D., Sneppen, A., Smolcić, V., Steinhardt, C., Stern, D., Tanaka, M., Taniguchi, Y., Teplitz, H. I., Vaccari, M., Wang, W. H., Zamorani, G., Weaver, J. R., Kauffmann, O. B., Ilbert, O., McCracken, H. J., Moneti, A., Toft, S., Brammer, G., Shuntov, M., Davidzon, I., Hsieh, B. C., Laigle, C., Anastasiou, A., Jespersen, C. K., Vinther, J., Capak, P., Casey, C. M., McPartland, C. J.R., Milvang-Jensen, B., Mobasher, B., Sanders, D. B., Zalesky, L., Arnouts, S., Aussel, H., Dunlop, J. S., Faisst, A., Franx, M., Furtak, L. J., Fynbo, J. P.U., Gould, K. M.L., Greve, T. R., Gwyn, S., Kartaltepe, J. S., Kashino, D., Koekemoer, A. M., Kokorev, V., Le Fevre, O., Lilly, S., Masters, D., Magdis, G., Mehta, V., Peng, Y., Riechers, D. A., Salvato, M., Sawicki, M., Scarlata, C., Scoville, N., Shirley, R., Silverman, J. D., Sneppen, A., Smolcić, V., Steinhardt, C., Stern, D., Tanaka, M., Taniguchi, Y., Teplitz, H. I., Vaccari, M., Wang, W. H., and Zamorani, G.

Abstract

The Cosmic Evolution Survey (COSMOS) has become a cornerstone of extragalactic astronomy. Since the last public catalog in 2015, a wealth of new imaging and spectroscopic data have been collected in the COSMOS field. This paper describes the collection, processing, and analysis of these new imaging data to produce a new reference photometric redshift catalog. Source detection and multiwavelength photometry are performed for 1.7 million sources across the 2 deg2 of the COSMOS field, ∼966,000 of which are measured with all available broadband data using both traditional aperture photometric methods and a new profile-fitting photometric extraction tool, The Farmer, which we have developed. A detailed comparison of the two resulting photometric catalogs is presented. Photometric redshifts are computed for all sources in each catalog utilizing two independent photometric redshift codes. Finally, a comparison is made between the performance of the photometric methodologies and of the redshift codes to demonstrate an exceptional degree of self-consistency in the resulting photometric redshifts. The i < 21 sources have subpercent photometric redshift accuracy and even the faintest sources at 25 < i < 27 reach a precision of 5%. Finally, these results are discussed in the context of previous, current, and future surveys in the COSMOS field. Compared to COSMOS2015, it reaches the same photometric redshift precision at almost one magnitude deeper. Both photometric catalogs and their photometric redshift solutions and physical parameters will be made available through the usual astronomical archive systems (ESO Phase 3, IPAC-IRSA, and CDS).

Published
2022

55. COSMOS2020: A Panchromatic View of the Universe to z ∼ 10 from Two Complementary Catalogs

Author

Weaver, J. R., Kauffmann, O. B., Ilbert, O., McCracken, H. J., Moneti, A., Toft, S., Brammer, G., Shuntov, M., Davidzon, I., Hsieh, B. C., Laigle, C., Anastasiou, A., Jespersen, C. K., Vinther, J., Capak, P., Casey, C. M., McPartland, C. J. R., Milvang-Jensen, B., Mobasher, B., Sanders, D. B., Zalesky, L., Arnouts, S., Aussel, H., Dunlop, J. S., Faisst, A., Franx, M., Furtak, L. J., Fynbo, J. P. U., Gould, K. M. L., Greve, T. R., Gwyn, S., Kartaltepe, J. S., Kashino, D., Koekemoer, A. M., Kokorev, V., Le Fèvre, O., Lilly, S., Masters, D., Magdis, G., Mehta, V., Peng, Y., Riechers, D. A., Salvato, M., Sawicki, M., Scarlata, C., Scoville, N., Shirley, R., Silverman, J. D., Sneppen, A., Smolc̆ić, V., Steinhardt, C., Stern, D., Tanaka, M., Taniguchi, Y., Teplitz, H. I., Vaccari, M., Wang, W.-H., Zamorani, G., Weaver, J. R., Kauffmann, O. B., Ilbert, O., McCracken, H. J., Moneti, A., Toft, S., Brammer, G., Shuntov, M., Davidzon, I., Hsieh, B. C., Laigle, C., Anastasiou, A., Jespersen, C. K., Vinther, J., Capak, P., Casey, C. M., McPartland, C. J. R., Milvang-Jensen, B., Mobasher, B., Sanders, D. B., Zalesky, L., Arnouts, S., Aussel, H., Dunlop, J. S., Faisst, A., Franx, M., Furtak, L. J., Fynbo, J. P. U., Gould, K. M. L., Greve, T. R., Gwyn, S., Kartaltepe, J. S., Kashino, D., Koekemoer, A. M., Kokorev, V., Le Fèvre, O., Lilly, S., Masters, D., Magdis, G., Mehta, V., Peng, Y., Riechers, D. A., Salvato, M., Sawicki, M., Scarlata, C., Scoville, N., Shirley, R., Silverman, J. D., Sneppen, A., Smolc̆ić, V., Steinhardt, C., Stern, D., Tanaka, M., Taniguchi, Y., Teplitz, H. I., Vaccari, M., Wang, W.-H., and Zamorani, G.

Abstract

The Cosmic Evolution Survey (COSMOS) has become a cornerstone of extragalactic astronomy. Since the last public catalog in 2015, a wealth of new imaging and spectroscopic data have been collected in the COSMOS field. This paper describes the collection, processing, and analysis of these new imaging data to produce a new reference photometric redshift catalog. Source detection and multiwavelength photometry are performed for 1.7 million sources across the 2 deg2 of the COSMOS field, ∼966,000 of which are measured with all available broadband data using both traditional aperture photometric methods and a new profile-fitting photometric extraction tool, The Farmer, which we have developed. A detailed comparison of the two resulting photometric catalogs is presented. Photometric redshifts are computed for all sources in each catalog utilizing two independent photometric redshift codes. Finally, a comparison is made between the performance of the photometric methodologies and of the redshift codes to demonstrate an exceptional degree of self-consistency in the resulting photometric redshifts. The i < 21 sources have subpercent photometric redshift accuracy and even the faintest sources at 25 < i < 27 reach a precision of 5%. Finally, these results are discussed in the context of previous, current, and future surveys in the COSMOS field. Compared to COSMOS2015, it reaches the same photometric redshift precision at almost one magnitude deeper. Both photometric catalogs and their photometric redshift solutions and physical parameters will be made available through the usual astronomical archive systems (ESO Phase 3, IPAC-IRSA, and CDS).

Published
2022

56. COSMOS2020: A Panchromatic View of the Universe to z ∼ 10 from Two Complementary Catalogs

Author

Weaver, J. R., primary, Kauffmann, O. B., additional, Ilbert, O., additional, McCracken, H. J., additional, Moneti, A., additional, Toft, S., additional, Brammer, G., additional, Shuntov, M., additional, Davidzon, I., additional, Hsieh, B. C., additional, Laigle, C., additional, Anastasiou, A., additional, Jespersen, C. K., additional, Vinther, J., additional, Capak, P., additional, Casey, C. M., additional, McPartland, C. J. R., additional, Milvang-Jensen, B., additional, Mobasher, B., additional, Sanders, D. B., additional, Zalesky, L., additional, Arnouts, S., additional, Aussel, H., additional, Dunlop, J. S., additional, Faisst, A., additional, Franx, M., additional, Furtak, L. J., additional, Fynbo, J. P. U., additional, Gould, K. M. L., additional, Greve, T. R., additional, Gwyn, S., additional, Kartaltepe, J. S., additional, Kashino, D., additional, Koekemoer, A. M., additional, Kokorev, V., additional, Le Fèvre, O., additional, Lilly, S., additional, Masters, D., additional, Magdis, G., additional, Mehta, V., additional, Peng, Y., additional, Riechers, D. A., additional, Salvato, M., additional, Sawicki, M., additional, Scarlata, C., additional, Scoville, N., additional, Shirley, R., additional, Silverman, J. D., additional, Sneppen, A., additional, Smolc̆ić, V., additional, Steinhardt, C., additional, Stern, D., additional, Tanaka, M., additional, Taniguchi, Y., additional, Teplitz, H. I., additional, Vaccari, M., additional, Wang, W.-H., additional, and Zamorani, G., additional

Published
2022
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58. COSMOS2020: a panchromatic view of the universe to z 10 from two complementary catalogs

Author

J. R. Weaver, O. B. Kauffmann, O. Ilbert, H. J. McCracken, A. Moneti, S. Toft, G. Brammer, M. Shuntov, I. Davidzon, B. C. Hsieh, C. Laigle, A. Anastasiou, C. K. Jespersen, J. Vinther, P. Capak, C. M. Casey, C. J. R. McPartland, B. Milvang-Jensen, B. Mobasher, D. B. Sanders, L. Zalesky, S. Arnouts, H. Aussel, J. S. Dunlop, A. Faisst, M. Franx, L. J. Furtak, J. P. U. Fynbo, K. M. L. Gould, T. R. Greve, S. Gwyn, J. S. Kartaltepe, D. Kashino, A. M. Koekemoer, V. Kokorev, O. Le Fèvre, S. Lilly, D. Masters, G. Magdis, V. Mehta, Y. Peng, D. A. Riechers, M. Salvato, M. Sawicki, C. Scarlata, N. Scoville, R. Shirley, J. D. Silverman, A. Sneppen, V. Smolc̆ić, C. Steinhardt, D. Stern, M. Tanaka, Y. Taniguchi, H. I. Teplitz, M. Vaccari, W.-H. Wang, G. Zamorani, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Weaver, JR [0000-0003-1614-196X], Kauffmann, OB [0000-0001-5283-4662], Ilbert, O [0000-0002-7303-4397], McCracken, HJ [0000-0002-9489-7765], Toft, S [0000-0003-3631-7176], Brammer, G [0000-0003-2680-005X], Shuntov, M [0000-0002-7087-0701], Davidzon, I [0000-0002-2951-7519], Hsieh, BC [0000-0001-5615-4904], Anastasiou, A [0000-0001-8558-7709], Jespersen, CK [0000-0002-8896-6496], Vinther, J [0000-0002-4418-752X], Capak, P [0000-0003-3578-6843], Casey, CM [0000-0002-0930-6466], McPartland, CJR [0000-0003-0639-025X], Milvang-Jensen, B [0000-0002-2281-2785], Sanders, DB [0000-0002-1233-9998], Zalesky, L [0000-0001-5680-2326], Faisst, A [0000-0002-9382-9832], Franx, M [0000-0002-8871-3026], Furtak, LJ [0000-0001-6278-032X], Fynbo, JPU [0000-0002-8149-8298], Gould, KML [0000-0003-4196-5960], Greve, TR [0000-0002-2554-1837], Gwyn, S [0000-0001-8221-8406], Kartaltepe, JS [0000-0001-9187-3605], Kashino, D [0000-0001-9044-1747], Koekemoer, AM [0000-0002-6610-2048], Kokorev, V [0000-0002-5588-9156], Le Fèvre, O [0000-0001-5891-2596], Lilly, S [0000-0002-6423-3597], Masters, D [0000-0001-5382-6138], Magdis, G [0000-0002-4872-2294], Mehta, V [0000-0001-7166-6035], Riechers, DA [0000-0001-9585-1462], Salvato, M [0000-0001-7116-9303], Sawicki, M [0000-0002-7712-7857], Scarlata, C [0000-0002-9136-8876], Scoville, N [0000-0002-0438-3323], Shirley, R [0000-0002-1114-0135], Sneppen, A [0000-0002-5460-6126], Smolc̆ić, V [0000-0002-3893-8614], Steinhardt, C [0000-0003-3780-6801], Stern, D [0000-0003-2686-9241], Tanaka, M [0000-0002-5011-5178], Taniguchi, Y [0000-0003-2247-3741], Teplitz, HI [0000-0002-7064-5424], Vaccari, M [0000-0002-6748-0577], Wang, W-H [0000-0003-2588-1265], Zamorani, G [0000-0002-2318-301X], and Apollo - University of Cambridge Repository

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics - astrophysics of galaxies, Astrophysics - cosmology and nongalactic astrophysics, FOS: Physical sciences, 5109 Space Sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies and Cosmology, Universe, panchromatic view, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, 51 Physical Sciences
Abstract

The Cosmic Evolution Survey (COSMOS) has become a cornerstone of extragalactic astronomy. Since the last public catalog in 2015, a wealth of new imaging and spectroscopic data has been collected in the COSMOS field. This paper describes the collection, processing, and analysis of this new imaging data to produce a new reference photometric redshift catalog. Source detection and multi-wavelength photometry is performed for 1.7 million sources across the $2\,\mathrm{deg}^{2}$ of the COSMOS field, $\sim$966,000 of which are measured with all available broad-band data using both traditional aperture photometric methods and a new profile-fitting photometric extraction tool, The Farmer, which we have developed. A detailed comparison of the two resulting photometric catalogs is presented. Photometric redshifts are computed for all sources in each catalog utilizing two independent photometric redshift codes. Finally, a comparison is made between the performance of the photometric methodologies and of the redshift codes to demonstrate an exceptional degree of self-consistency in the resulting photometric redshifts. The $i, Comment: 39 pages, 21 figures, accepted for publication in The Astrophysical Journal Supplement Series. Production of IRAC mosaics are presented in Moneti et al. "Euclid Preparation: XVIII. Cosmic Dawn Survey. Spitzer observations of the Euclid deep fields and calibration fields" which has been posted simultaneously. Catalogs can be accessed online now at https://cosmos2020.calet.org

Published
2022
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59. Accelerated formation of ultra-massive galaxies in the first billion years.

Author

Xiao M, Oesch PA, Elbaz D, Bing L, Nelson EJ, Weibel A, Illingworth GD, van Dokkum P, Naidu RP, Daddi E, Bouwens RJ, Matthee J, Wuyts S, Chisholm J, Brammer G, Dickinson M, Magnelli B, Leroy L, Schaerer D, Herard-Demanche T, Lim S, Barrufet L, Endsley R, Fudamoto Y, Gómez-Guijarro C, Gottumukkala R, Labbé I, Magee D, Marchesini D, Maseda M, Qin Y, Reddy NA, Shapley A, Shivaei I, Shuntov M, Stefanon M, Whitaker KE, and Wyithe JSB

Abstract

Recent James Webb Space Telescope (JWST) observations have revealed an unexpected abundance of massive-galaxy candidates in the early Universe, extending further in redshift and to lower luminosity than what had previously been found by submillimetre surveys 1-6 . These JWST candidates have been interpreted as challenging the Λ cold dark-matter cosmology (where Λ is the cosmological constant) 7-9 , but, so far, these studies have mostly relied on only rest-frame ultraviolet data and have lacked spectroscopic confirmation of their redshifts 10-16 . Here we report a systematic study of 36 massive dust-obscured galaxies with spectroscopic redshifts between 5 and 9 from the JWST FRESCO survey. We find no tension with the Λ cold dark-matter model in our sample. However, three ultra-massive galaxies (logM ★ /M ⊙  ≳ 11.0, where M ★ is the stellar mass and M ⊙ is the mass of the Sun) require an exceptional fraction of 50 per cent of baryons converted into stars-two to three times higher than the most efficient galaxies at later epochs. The contribution from an active galactic nucleus is unlikely because of their extended emission. Ultra-massive galaxies account for as much as 17 per cent of the total cosmic star-formation-rate density 17 at redshifts between about five and six., Competing Interests: Competing interests The authors declare no competing interests., (© 2024. The Author(s), under exclusive licence to Springer Nature Limited.)

Published
2024
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