Size–Stellar Mass Relation and Morphology of Quiescent Galaxies at z ≥ 3 in Public JWST Fields
We present the results of a systematic study of the rest-frame optical morphology of quiescent galaxies at z ≥ 3 using the Near-Infrared Camera (NIRCam) on board the James Webb Space Telescope (JWST). Based on a sample selected by UVJ color or NUVUVJ color, we focus on 26 quiescent galaxies with $9....
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IOP Publishing
2024-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ad2512 |
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| author | Kei Ito Francesco Valentino Gabriel Brammer Andreas L. Faisst Steven Gillman Carlos Gómez-Guijarro Katriona M. L. Gould Kasper E. Heintz Olivier Ilbert Christian Kragh Jespersen Vasily Kokorev Mariko Kubo Georgios E. Magdis Conor J. R. McPartland Masato Onodera Francesca Rizzo Masayuki Tanaka Sune Toft Aswin P. Vijayan John R. Weaver Katherine E. Whitaker Lillian Wright |
| author_facet | Kei Ito Francesco Valentino Gabriel Brammer Andreas L. Faisst Steven Gillman Carlos Gómez-Guijarro Katriona M. L. Gould Kasper E. Heintz Olivier Ilbert Christian Kragh Jespersen Vasily Kokorev Mariko Kubo Georgios E. Magdis Conor J. R. McPartland Masato Onodera Francesca Rizzo Masayuki Tanaka Sune Toft Aswin P. Vijayan John R. Weaver Katherine E. Whitaker Lillian Wright |
| author_sort | Kei Ito |
| collection | DOAJ |
| description | We present the results of a systematic study of the rest-frame optical morphology of quiescent galaxies at z ≥ 3 using the Near-Infrared Camera (NIRCam) on board the James Webb Space Telescope (JWST). Based on a sample selected by UVJ color or NUVUVJ color, we focus on 26 quiescent galaxies with $9.8\lt \mathrm{log}({M}_{\star }/{M}_{\odot })\lt 11.4$ at 2.8 < z _phot < 4.6 with publicly available JWST data. Their sizes are constrained by fitting the Sérsic profile to all available NIRCam images. We see a negative correlation between the observed wavelength and the size and derive their size at the rest frame 0.5 μ m using size measurements in multiple bands. Our quiescent galaxies show a significant correlation between the rest-frame 0.5 μ m size and the stellar mass at z ≥ 3. The analytical fit for them at $\mathrm{log}({M}_{\star }/{M}_{\odot })\gt 10.3$ implies that our size–stellar mass relations are below those at lower redshifts, with the amplitude of ∼0.6 kpc at M _⋆ = 5 × 10 ^10 M _⊙ . This value agrees with the extrapolation of the size evolution of quiescent galaxies at z < 3 in the literature, implying that the size of quiescent galaxies increases monotonically from z ∼ 3–5. Our sample mainly comprises galaxies with bulge-like structures according to their median Sérsic index and axis ratio of n ∼ 3–4 and q ∼ 0.6–0.8, respectively. On the other hand, there is a trend of increasing fraction of galaxies with low Sérsic index at higher redshift, suggesting 3 < z < 5 might be the epoch of onset of morphological transformation with a fraction of very notable disky quenched galaxies. |
| first_indexed | 2024-04-24T16:36:16Z |
| format | Article |
| id | doaj.art-a8decbb2ca004abfae343bcd8f950144 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-04-24T16:36:16Z |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-a8decbb2ca004abfae343bcd8f9501442024-03-29T15:27:03ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-01964219210.3847/1538-4357/ad2512Size–Stellar Mass Relation and Morphology of Quiescent Galaxies at z ≥ 3 in Public JWST FieldsKei Ito0https://orcid.org/0000-0002-9453-0381Francesco Valentino1https://orcid.org/0000-0001-6477-4011Gabriel Brammer2https://orcid.org/0000-0003-2680-005XAndreas L. Faisst3https://orcid.org/0000-0002-9382-9832Steven Gillman4https://orcid.org/0000-0001-9885-4589Carlos Gómez-Guijarro5https://orcid.org/0000-0002-4085-9165Katriona M. L. Gould6Kasper E. Heintz7https://orcid.org/0000-0002-9389-7413Olivier Ilbert8https://orcid.org/0000-0002-7303-4397Christian Kragh Jespersen9https://orcid.org/0000-0002-8896-6496Vasily Kokorev10https://orcid.org/0000-0002-5588-9156Mariko Kubo11https://orcid.org/0000-0002-7598-5292Georgios E. Magdis12https://orcid.org/0000-0002-4872-2294Conor J. R. McPartland13https://orcid.org/0000-0003-0639-025XMasato Onodera14https://orcid.org/0000-0003-3228-7264Francesca Rizzo15Masayuki Tanaka16Sune Toft17https://orcid.org/0000-0003-3631-7176Aswin P. Vijayan18John R. Weaver19https://orcid.org/0000-0003-1614-196XKatherine E. Whitaker20https://orcid.org/0000-0001-7160-3632Lillian Wright21https://orcid.org/0000-0002-3722-322XDepartment of Astronomy, School of Science, The University of Tokyo , 7-3-1, Hongo, Bunkyo-ku, Tokyo, 113-0033, Japan ; kei.ito@astron.s.u-tokyo.ac.jp, kei.ito.astro@gmail.comEuropean Southern Observatory , Karl-Schwarzschild-Str. 2, D-85748 Garching bei Munchen, Germany; Cosmic Dawn Center (DAWN) , Copenhagen, DenmarkCosmic Dawn Center (DAWN) , Copenhagen, Denmark; Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK-2200 Copenhagen N, DenmarkCaltech/IPAC , 1200 E. California Boulevard, Pasadena, CA 91125, USACosmic Dawn Center (DAWN) , Copenhagen, Denmark; DTU-Space, Technical University of Denmark , Elektrovej 327, DK-2800 Kgs. Lyngby, DenmarkUniversité Paris-Saclay, Université Paris Cité , CEA, CNRS, AIM, 91191, Gif-sur-Yvette, FranceCosmic Dawn Center (DAWN) , Copenhagen, Denmark; Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK-2200 Copenhagen N, DenmarkCosmic Dawn Center (DAWN) , Copenhagen, Denmark; Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK-2200 Copenhagen N, DenmarkAix Marseille Univ , CNRS, CNES, LAM, Marseille, FranceDepartment of Astrophysical Sciences, Princeton University , Princeton, NJ 08544, USACosmic Dawn Center (DAWN) , Copenhagen, Denmark; Kapteyn Astronomical Institute, University of Groningen , P.O. Box 800, 9700AV Groningen, The NetherlandsAstronomical Institute, Tohoku University , 6-3, Aramaki Aoba, Aoba-ku, Sendai 980-8578, JapanCosmic Dawn Center (DAWN) , Copenhagen, Denmark; Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK-2200 Copenhagen N, Denmark; DTU-Space, Technical University of Denmark , Elektrovej 327, DK-2800 Kgs. Lyngby, DenmarkCosmic Dawn Center (DAWN) , Copenhagen, Denmark; Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK-2200 Copenhagen N, DenmarkDepartment of Astronomical Science, The Graduate University for Advanced Studies , SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, Japan; Subaru Telescope, National Astronomical Observatory of Japan , National Institutes of Natural Sciences (NINS), 650 North A’ohoku Place, Hilo, HI 96720, USACosmic Dawn Center (DAWN) , Copenhagen, Denmark; Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK-2200 Copenhagen N, DenmarkDepartment of Astronomical Science, The Graduate University for Advanced Studies , SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, Japan; National Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, JapanCosmic Dawn Center (DAWN) , Copenhagen, Denmark; Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK-2200 Copenhagen N, DenmarkCosmic Dawn Center (DAWN) , Copenhagen, Denmark; DTU-Space, Technical University of Denmark , Elektrovej 327, DK-2800 Kgs. Lyngby, DenmarkDepartment of Astronomy, University of Massachusetts , Amherst, MA 01003, USACosmic Dawn Center (DAWN) , Copenhagen, Denmark; Department of Astronomy, University of Massachusetts , Amherst, MA 01003, USADepartment of Astronomy, University of Massachusetts , Amherst, MA 01003, USA; Department of Physics and Astronomy, Seoul National University , 1 Gwanak-ro, Gwanak-gu, Seoul, Republic of KoreaWe present the results of a systematic study of the rest-frame optical morphology of quiescent galaxies at z ≥ 3 using the Near-Infrared Camera (NIRCam) on board the James Webb Space Telescope (JWST). Based on a sample selected by UVJ color or NUVUVJ color, we focus on 26 quiescent galaxies with $9.8\lt \mathrm{log}({M}_{\star }/{M}_{\odot })\lt 11.4$ at 2.8 < z _phot < 4.6 with publicly available JWST data. Their sizes are constrained by fitting the Sérsic profile to all available NIRCam images. We see a negative correlation between the observed wavelength and the size and derive their size at the rest frame 0.5 μ m using size measurements in multiple bands. Our quiescent galaxies show a significant correlation between the rest-frame 0.5 μ m size and the stellar mass at z ≥ 3. The analytical fit for them at $\mathrm{log}({M}_{\star }/{M}_{\odot })\gt 10.3$ implies that our size–stellar mass relations are below those at lower redshifts, with the amplitude of ∼0.6 kpc at M _⋆ = 5 × 10 ^10 M _⊙ . This value agrees with the extrapolation of the size evolution of quiescent galaxies at z < 3 in the literature, implying that the size of quiescent galaxies increases monotonically from z ∼ 3–5. Our sample mainly comprises galaxies with bulge-like structures according to their median Sérsic index and axis ratio of n ∼ 3–4 and q ∼ 0.6–0.8, respectively. On the other hand, there is a trend of increasing fraction of galaxies with low Sérsic index at higher redshift, suggesting 3 < z < 5 might be the epoch of onset of morphological transformation with a fraction of very notable disky quenched galaxies.https://doi.org/10.3847/1538-4357/ad2512Galaxy evolutionGalaxy quenchingHigh-redshift galaxiesGalaxy radiiQuenched galaxies |
| spellingShingle | Kei Ito Francesco Valentino Gabriel Brammer Andreas L. Faisst Steven Gillman Carlos Gómez-Guijarro Katriona M. L. Gould Kasper E. Heintz Olivier Ilbert Christian Kragh Jespersen Vasily Kokorev Mariko Kubo Georgios E. Magdis Conor J. R. McPartland Masato Onodera Francesca Rizzo Masayuki Tanaka Sune Toft Aswin P. Vijayan John R. Weaver Katherine E. Whitaker Lillian Wright Size–Stellar Mass Relation and Morphology of Quiescent Galaxies at z ≥ 3 in Public JWST Fields The Astrophysical Journal Galaxy evolution Galaxy quenching High-redshift galaxies Galaxy radii Quenched galaxies |
| title | Size–Stellar Mass Relation and Morphology of Quiescent Galaxies at z ≥ 3 in Public JWST Fields |
| title_full | Size–Stellar Mass Relation and Morphology of Quiescent Galaxies at z ≥ 3 in Public JWST Fields |
| title_fullStr | Size–Stellar Mass Relation and Morphology of Quiescent Galaxies at z ≥ 3 in Public JWST Fields |
| title_full_unstemmed | Size–Stellar Mass Relation and Morphology of Quiescent Galaxies at z ≥ 3 in Public JWST Fields |
| title_short | Size–Stellar Mass Relation and Morphology of Quiescent Galaxies at z ≥ 3 in Public JWST Fields |
| title_sort | size stellar mass relation and morphology of quiescent galaxies at z ≥ 3 in public jwst fields |
| topic | Galaxy evolution Galaxy quenching High-redshift galaxies Galaxy radii Quenched galaxies |
| url | https://doi.org/10.3847/1538-4357/ad2512 |
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