Issue |
A&A
Volume 690, October 2024
|
|
---|---|---|
Article Number | A290 | |
Number of page(s) | 18 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361/202449768 | |
Published online | 17 October 2024 |
Evolution of the star formation rate and ΣSFR of galaxies at cosmic morning (4 < z < 10)
1
INAF – Osservatorio Astronomico di Roma, Via Frascati 33 00078 Monte Porzio Catone, Italy
2
Scuola Normale Superiore, Piazza dei Cavalieri 7, 50126 Pisa, Italy
3
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
4
INAF – Istituto di Radioastronomia, Via Piero Gobetti 101, 40129 Bologna, Italy
5
Dipartimento di Fisica e Astronomia “G. Galilei”, Università di Padova, Via Marzolo 8, I-35131 Padova, Italy
6
Department of Physics and Astronomy, Texas A&M University, College Station, TX 77843-4242, USA
7
George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Texas A& M University, College Station, TX 77843-4242, USA
8
Racah Institute of Physics, The Hebrew University of Jerusalem, Jerusalem 91904, Israel
9
NSF’s National Optical-Infrared Astronomy Research Laboratory, 950 N. Cherry Ave., Tucson, AZ 85719, USA
10
The University of Texas at Austin, 2515 Speedway Blvd Stop, C1400 Austin, TX 78712, USA
11
University of Massachusetts Amherst, 710 North Pleasant Street, Amherst, MA 01003-9305, USA
12
Institute of Physics, Laboratory of Galaxy Evolution, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, 1290 Versoix, Switzerland
13
Department of Physics and Astronomy, University of Louisville, Natural Science Building 102, 40292 KY, Louisville USA
14
, Center for Astrophysics | Harvard & Smithsonian, 60 Garden St., Cambridge, MA 02138, USA
15
Black Hole Initiative at Harvard University, 20 Garden St., Cambridge, MA 02138, USA
16
ESA/AURA, Space Telescope Science Institute, 3800 San Martin Drive, Baltimore, MD 21218, USA
17
Department of Physics and Astronomy, University of California, Los Angeles, 430 Portola Plaza, Los Angeles, 90095 CA, USA
18
Aix Marseille Université, CNRS, CNES, LAM, 38, rue Frédéric Joliot-Curie, 13388 Marseille, CEDEX 13, France
19
Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
20
Cavendish Laboratory, University of Cambridge, 19 JJ Thomson Avenue, Cambridge CB3 0HE, UK
21
Astronomy Centre, University of Sussex, Falmer, Brighton BN1 9QH, UK
22
Institute of Space Sciences and Astronomy, University of Malta, Msida, MSD 2080, Malta
23
Departamento de Astronomía, Universidad de La Serena, Av. Juan Cisternas 1200 Norte, La Serena, Chile
24
ARAID Foundation. Centro de Estudios de Física del Cosmos de Aragón (CEFCA), Unidad Asociada al CSIC, Plaza San Juan 1, E-44001 Teruel, Spain
25
Laboratory for Multiwavelength Astrophysics, School of Physics and Astronomy, Rochester Institute of Technology, 84 Lomb Memorial Drive, Rochester, NY 14623, USA
Received:
27
February
2024
Accepted:
19
June
2024
The galaxy-integrated star formation rate (SFR) surface density measurement (ΣSFR) has been proposed as a valuable diagnostic of the mass accumulation in galaxies given it is more tightly related to the physics of star formation and stellar feedback than other indicators. In this work, we assembled a statistical sample of 230 galaxies observed with JWST in the GLASS and CEERS spectroscopic surveys to estimate Balmer line-based dust attenuations and SFRs (i.e., from Hα, Hβ, and Hγ), along with the UV rest-frame effective radii. We studied the evolution of galaxy SFR and ΣSFR in the first 1.5 billion years of our Universe, from a redshift of z ∼ 4 to z ∼ 10. We found that ΣSFR is mildly increasing with redshift with a linear slope of 0.16 ± 0.06. We explored the dependence of SFR and ΣSFR on stellar mass, showing that a star-forming main sequence and a ΣSFR main sequence are present out to z = 10. This dependence exhibits a similar slope compared to the same relations at lower redshifts, but with a higher normalization. We find that the specific SFR (sSFR) and ΣSFR are correlated with the [O III] λ5007 Å/[O II] λ3727 Å ratio and with indirect estimates of the escape fraction of Lyman continuum photons; hence, they are likely to play an important role in the evolution of ionization conditions at higher redshifts and in the escape of ionizing radiation. We also searched for spectral outflow signatures in the Hα and [O III] emission lines in a subset of galaxies observed at high resolution (R = 2700) by the GLASS survey, finding an outflow incidence of 2/11 (=20%32%9%) at z < 6, but no evidence at z > 6 (0/6, < 26%). Finally, we find a positive correlation between AV and ΣSFR, and a flat trend as a function of sSFR, indicating that there is no evidence of a drop in AV in extremely star-forming galaxies between z ∼ 4 and ∼10. This result might be at odds with a dust-clearing outflow scenario, which may instead take place at redshifts of z ≥ 10, as suggested by some theoretical models.
Key words: galaxies: evolution / galaxies: high-redshift / galaxies: ISM / galaxies: star formation / galaxies: statistics
© The Authors 2024
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.
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