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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Autor*in:	Kei Ito [verfasserIn] Francesco Valentino [verfasserIn] Gabriel Brammer [verfasserIn] Andreas L. Faisst [verfasserIn] Steven Gillman [verfasserIn] Carlos Gómez-Guijarro [verfasserIn] Katriona M. L. Gould [verfasserIn] Kasper E. Heintz [verfasserIn] Olivier Ilbert [verfasserIn] Christian Kragh Jespersen [verfasserIn] Vasily Kokorev [verfasserIn] Mariko Kubo [verfasserIn] Georgios E. Magdis [verfasserIn] Conor J. R. McPartland [verfasserIn] Masato Onodera [verfasserIn] Francesca Rizzo [verfasserIn] Masayuki Tanaka [verfasserIn] Sune Toft [verfasserIn] Aswin P. Vijayan [verfasserIn] John R. Weaver [verfasserIn] Katherine E. Whitaker [verfasserIn] Lillian Wright [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2024

Schlagwörter:	Galaxy evolution Galaxy quenching High-redshift galaxies Galaxy radii Quenched galaxies

Übergeordnetes Werk:	In: The Astrophysical Journal - IOP Publishing, 2022, 964(2024), 2, p 192
Übergeordnetes Werk:	volume:964 ; year:2024 ; number:2, p 192

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3847/1538-4357/ad2512

Katalog-ID:	DOAJ097308099

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520			\|a 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.
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allfields	10.3847/1538-4357/ad2512 doi (DE-627)DOAJ097308099 (DE-599)DOAJa8decbb2ca004abfae343bcd8f950144 DE-627 ger DE-627 rakwb eng QB460-466 Kei Ito verfasserin aut Size–Stellar Mass Relation and Morphology of Quiescent Galaxies at z ≥ 3 in Public JWST Fields 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier 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. Galaxy evolution Galaxy quenching High-redshift galaxies Galaxy radii Quenched galaxies Astrophysics Francesco Valentino verfasserin aut Gabriel Brammer verfasserin aut Andreas L. Faisst verfasserin aut Steven Gillman verfasserin aut Carlos Gómez-Guijarro verfasserin aut Katriona M. L. Gould verfasserin aut Kasper E. Heintz verfasserin aut Olivier Ilbert verfasserin aut Christian Kragh Jespersen verfasserin aut Vasily Kokorev verfasserin aut Mariko Kubo verfasserin aut Georgios E. Magdis verfasserin aut Conor J. R. McPartland verfasserin aut Masato Onodera verfasserin aut Francesca Rizzo verfasserin aut Masayuki Tanaka verfasserin aut Sune Toft verfasserin aut Aswin P. Vijayan verfasserin aut John R. Weaver verfasserin aut Katherine E. Whitaker verfasserin aut Lillian Wright verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 964(2024), 2, p 192 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:964 year:2024 number:2, p 192 https://doi.org/10.3847/1538-4357/ad2512 kostenfrei https://doaj.org/article/a8decbb2ca004abfae343bcd8f950144 kostenfrei https://doi.org/10.3847/1538-4357/ad2512 kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 964 2024 2, p 192
spelling	10.3847/1538-4357/ad2512 doi (DE-627)DOAJ097308099 (DE-599)DOAJa8decbb2ca004abfae343bcd8f950144 DE-627 ger DE-627 rakwb eng QB460-466 Kei Ito verfasserin aut Size–Stellar Mass Relation and Morphology of Quiescent Galaxies at z ≥ 3 in Public JWST Fields 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier 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. Galaxy evolution Galaxy quenching High-redshift galaxies Galaxy radii Quenched galaxies Astrophysics Francesco Valentino verfasserin aut Gabriel Brammer verfasserin aut Andreas L. Faisst verfasserin aut Steven Gillman verfasserin aut Carlos Gómez-Guijarro verfasserin aut Katriona M. L. Gould verfasserin aut Kasper E. Heintz verfasserin aut Olivier Ilbert verfasserin aut Christian Kragh Jespersen verfasserin aut Vasily Kokorev verfasserin aut Mariko Kubo verfasserin aut Georgios E. Magdis verfasserin aut Conor J. R. McPartland verfasserin aut Masato Onodera verfasserin aut Francesca Rizzo verfasserin aut Masayuki Tanaka verfasserin aut Sune Toft verfasserin aut Aswin P. Vijayan verfasserin aut John R. Weaver verfasserin aut Katherine E. Whitaker verfasserin aut Lillian Wright verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 964(2024), 2, p 192 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:964 year:2024 number:2, p 192 https://doi.org/10.3847/1538-4357/ad2512 kostenfrei https://doaj.org/article/a8decbb2ca004abfae343bcd8f950144 kostenfrei https://doi.org/10.3847/1538-4357/ad2512 kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 964 2024 2, p 192
allfields_unstemmed	10.3847/1538-4357/ad2512 doi (DE-627)DOAJ097308099 (DE-599)DOAJa8decbb2ca004abfae343bcd8f950144 DE-627 ger DE-627 rakwb eng QB460-466 Kei Ito verfasserin aut Size–Stellar Mass Relation and Morphology of Quiescent Galaxies at z ≥ 3 in Public JWST Fields 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier 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. Galaxy evolution Galaxy quenching High-redshift galaxies Galaxy radii Quenched galaxies Astrophysics Francesco Valentino verfasserin aut Gabriel Brammer verfasserin aut Andreas L. Faisst verfasserin aut Steven Gillman verfasserin aut Carlos Gómez-Guijarro verfasserin aut Katriona M. L. Gould verfasserin aut Kasper E. Heintz verfasserin aut Olivier Ilbert verfasserin aut Christian Kragh Jespersen verfasserin aut Vasily Kokorev verfasserin aut Mariko Kubo verfasserin aut Georgios E. Magdis verfasserin aut Conor J. R. McPartland verfasserin aut Masato Onodera verfasserin aut Francesca Rizzo verfasserin aut Masayuki Tanaka verfasserin aut Sune Toft verfasserin aut Aswin P. Vijayan verfasserin aut John R. Weaver verfasserin aut Katherine E. Whitaker verfasserin aut Lillian Wright verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 964(2024), 2, p 192 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:964 year:2024 number:2, p 192 https://doi.org/10.3847/1538-4357/ad2512 kostenfrei https://doaj.org/article/a8decbb2ca004abfae343bcd8f950144 kostenfrei https://doi.org/10.3847/1538-4357/ad2512 kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 964 2024 2, p 192
allfieldsGer	10.3847/1538-4357/ad2512 doi (DE-627)DOAJ097308099 (DE-599)DOAJa8decbb2ca004abfae343bcd8f950144 DE-627 ger DE-627 rakwb eng QB460-466 Kei Ito verfasserin aut Size–Stellar Mass Relation and Morphology of Quiescent Galaxies at z ≥ 3 in Public JWST Fields 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier 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. Galaxy evolution Galaxy quenching High-redshift galaxies Galaxy radii Quenched galaxies Astrophysics Francesco Valentino verfasserin aut Gabriel Brammer verfasserin aut Andreas L. Faisst verfasserin aut Steven Gillman verfasserin aut Carlos Gómez-Guijarro verfasserin aut Katriona M. L. Gould verfasserin aut Kasper E. Heintz verfasserin aut Olivier Ilbert verfasserin aut Christian Kragh Jespersen verfasserin aut Vasily Kokorev verfasserin aut Mariko Kubo verfasserin aut Georgios E. Magdis verfasserin aut Conor J. R. McPartland verfasserin aut Masato Onodera verfasserin aut Francesca Rizzo verfasserin aut Masayuki Tanaka verfasserin aut Sune Toft verfasserin aut Aswin P. Vijayan verfasserin aut John R. Weaver verfasserin aut Katherine E. Whitaker verfasserin aut Lillian Wright verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 964(2024), 2, p 192 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:964 year:2024 number:2, p 192 https://doi.org/10.3847/1538-4357/ad2512 kostenfrei https://doaj.org/article/a8decbb2ca004abfae343bcd8f950144 kostenfrei https://doi.org/10.3847/1538-4357/ad2512 kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 964 2024 2, p 192
allfieldsSound	10.3847/1538-4357/ad2512 doi (DE-627)DOAJ097308099 (DE-599)DOAJa8decbb2ca004abfae343bcd8f950144 DE-627 ger DE-627 rakwb eng QB460-466 Kei Ito verfasserin aut Size–Stellar Mass Relation and Morphology of Quiescent Galaxies at z ≥ 3 in Public JWST Fields 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier 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. Galaxy evolution Galaxy quenching High-redshift galaxies Galaxy radii Quenched galaxies Astrophysics Francesco Valentino verfasserin aut Gabriel Brammer verfasserin aut Andreas L. Faisst verfasserin aut Steven Gillman verfasserin aut Carlos Gómez-Guijarro verfasserin aut Katriona M. L. Gould verfasserin aut Kasper E. Heintz verfasserin aut Olivier Ilbert verfasserin aut Christian Kragh Jespersen verfasserin aut Vasily Kokorev verfasserin aut Mariko Kubo verfasserin aut Georgios E. Magdis verfasserin aut Conor J. R. McPartland verfasserin aut Masato Onodera verfasserin aut Francesca Rizzo verfasserin aut Masayuki Tanaka verfasserin aut Sune Toft verfasserin aut Aswin P. Vijayan verfasserin aut John R. Weaver verfasserin aut Katherine E. Whitaker verfasserin aut Lillian Wright verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 964(2024), 2, p 192 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:964 year:2024 number:2, p 192 https://doi.org/10.3847/1538-4357/ad2512 kostenfrei https://doaj.org/article/a8decbb2ca004abfae343bcd8f950144 kostenfrei https://doi.org/10.3847/1538-4357/ad2512 kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 964 2024 2, p 192
language	English
source	In The Astrophysical Journal 964(2024), 2, p 192 volume:964 year:2024 number:2, p 192
sourceStr	In The Astrophysical Journal 964(2024), 2, p 192 volume:964 year:2024 number:2, p 192
format_phy_str_mv	Article
institution	findex.gbv.de
topic_facet	Galaxy evolution Galaxy quenching High-redshift galaxies Galaxy radii Quenched galaxies Astrophysics
isfreeaccess_bool	true
container_title	The Astrophysical Journal
authorswithroles_txt_mv	Kei Ito @@aut@@ Francesco Valentino @@aut@@ Gabriel Brammer @@aut@@ Andreas L. Faisst @@aut@@ Steven Gillman @@aut@@ Carlos Gómez-Guijarro @@aut@@ Katriona M. L. Gould @@aut@@ Kasper E. Heintz @@aut@@ Olivier Ilbert @@aut@@ Christian Kragh Jespersen @@aut@@ Vasily Kokorev @@aut@@ Mariko Kubo @@aut@@ Georgios E. Magdis @@aut@@ Conor J. R. McPartland @@aut@@ Masato Onodera @@aut@@ Francesca Rizzo @@aut@@ Masayuki Tanaka @@aut@@ Sune Toft @@aut@@ Aswin P. Vijayan @@aut@@ John R. Weaver @@aut@@ Katherine E. Whitaker @@aut@@ Lillian Wright @@aut@@
publishDateDaySort_date	2024-01-01T00:00:00Z
hierarchy_top_id	269019219
id	DOAJ097308099
language_de	englisch
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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 _⊙ . 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callnumber-first	Q - Science
author	Kei Ito
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topic_title	QB460-466 Size–Stellar Mass Relation and Morphology of Quiescent Galaxies at z ≥ 3 in Public JWST Fields Galaxy evolution Galaxy quenching High-redshift galaxies Galaxy radii Quenched galaxies
topic	misc QB460-466 misc Galaxy evolution misc Galaxy quenching misc High-redshift galaxies misc Galaxy radii misc Quenched galaxies misc Astrophysics
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title	Size–Stellar Mass Relation and Morphology of Quiescent Galaxies at z ≥ 3 in Public JWST Fields
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author_browse	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
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title_sort	size–stellar mass relation and morphology of quiescent galaxies at z ≥ 3 in public jwst fields
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title_auth	Size–Stellar Mass Relation and Morphology of Quiescent Galaxies at z ≥ 3 in Public JWST Fields
abstract	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.
abstractGer	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.
abstract_unstemmed	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.
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title_short	Size–Stellar Mass Relation and Morphology of Quiescent Galaxies at z ≥ 3 in Public JWST Fields
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author2	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
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Size–Stellar Mass Relation and Morphology of Quiescent Galaxies at z ≥ 3 in Public JWST Fields

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