Stellar Half-mass Radii of 0.5 z < 2.3 Galaxies: Comparison with JWST/NIRCam Half-light Radii

We use CEERS JWST/NIRCam imaging to measure rest-frame near-IR light profiles of 435 M _⋆ < 10 ^10 M _⊙ galaxies in the redshift range of 0.5 < z < 2.3. We compare the resulting rest-frame 1.5–2 μ m half-light radii ( R _NIR ) with stellar half-mass radii ( ${R}_{{{M}}_{\star }}$ ) derived...
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Autor*in:	Arjen van der Wel [verfasserIn] Marco Martorano [verfasserIn] Boris Häußler [verfasserIn] Kalina V. Nedkova [verfasserIn] Tim B. Miller [verfasserIn] Gabriel B. Brammer [verfasserIn] Glenn van de Ven [verfasserIn] Joel Leja [verfasserIn] Rachel S. Bezanson [verfasserIn] Adam Muzzin [verfasserIn] Danilo Marchesini [verfasserIn] Anna de Graaff [verfasserIn] Erica J. Nelson [verfasserIn] Mariska Kriek [verfasserIn] Eric F. Bell [verfasserIn] Marijn Franx [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2023

Schlagwörter:	Galaxy evolution

Übergeordnetes Werk:	In: The Astrophysical Journal - IOP Publishing, 2022, 960(2023), 1, p 53
Übergeordnetes Werk:	volume:960 ; year:2023 ; number:1, p 53

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3847/1538-4357/ad02ee

Katalog-ID:	DOAJ098971263

Internformat


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245	1	0	\|a Stellar Half-mass Radii of 0.5 z < 2.3 Galaxies: Comparison with JWST/NIRCam Half-light Radii
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520			\|a We use CEERS JWST/NIRCam imaging to measure rest-frame near-IR light profiles of 435 M _⋆ < 10 ^10 M _⊙ galaxies in the redshift range of 0.5 < z < 2.3. We compare the resulting rest-frame 1.5–2 μ m half-light radii ( R _NIR ) with stellar half-mass radii ( ${R}_{{{M}}_{\star }}$ ) derived with multicolor light profiles from CANDELS Hubble Space Telescope imaging. In general agreement with previous work, we find that R _NIR and ${R}_{{{M}}_{\star }}$ are up to 40% smaller than the rest-frame optical half-light radius R _opt . The agreement between R _NIR and ${R}_{{{M}}_{\star }}$ is excellent, with a negligible systematic offset (<0.03 dex) up to z = 2 for quiescent galaxies and up to z = 1.5 for star-forming galaxies. We also deproject the profiles to estimate ${R}_{{{M}}_{\star },3{\rm{D}}}$ , the radius of a sphere containing 50% of the stellar mass. We present the R − M _⋆ distribution of galaxies at 0.5 < z < 1.5, comparing R _opt , ${R}_{{{M}}_{\star }}$ , and ${R}_{{{M}}_{\star },3{\rm{D}}}$ . The slope is significantly flatter for ${R}_{{{M}}_{\star }}$ and ${R}_{{{M}}_{\star },3{\rm{D}}}$ compared to R _opt , mostly due to downward shifts in size for massive star-forming galaxies, while ${R}_{{{M}}_{\star }}$ and ${R}_{{{M}}_{\star },3{\rm{D}}}$ do not show markedly different trends. Finally, we show rapid evolution of the size ( R ∝ (1 + z ) ^−1.7±0.1 ) of massive ( M _⋆ < 10 ^11 M _⊙ ) quiescent galaxies between z = 0.5 and z = 2.3, again comparing R _opt , ${R}_{{{M}}_{\star }}$ , and ${R}_{{{M}}_{\star },3{\rm{D}}}$ . We conclude that the main tenets of the evolution of the size narrative established over the past 20 yr, based on rest-frame optical light profile analysis, still hold in the era of JWST/NIRCam observations in the rest-frame near-IR.
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700	0		\|a Boris Häußler \|e verfasserin \|4 aut
700	0		\|a Kalina V. Nedkova \|e verfasserin \|4 aut
700	0		\|a Tim B. Miller \|e verfasserin \|4 aut
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700	0		\|a Marijn Franx \|e verfasserin \|4 aut
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Indexfelder

author_variant	a v d w avdw m m mm b h bh k v n kvn t b m tbm g b b gbb g v d v gvdv j l jl r s b rsb a m am d m dm a d g adg e j n ejn m k mk e f b efb m f mf
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allfields	10.3847/1538-4357/ad02ee doi (DE-627)DOAJ098971263 (DE-599)DOAJ39f06aed39b5496892538eddb70896fe DE-627 ger DE-627 rakwb eng QB460-466 Arjen van der Wel verfasserin aut Stellar Half-mass Radii of 0.5 z < 2.3 Galaxies: Comparison with JWST/NIRCam Half-light Radii 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We use CEERS JWST/NIRCam imaging to measure rest-frame near-IR light profiles of 435 M _⋆ < 10 ^10 M _⊙ galaxies in the redshift range of 0.5 < z < 2.3. We compare the resulting rest-frame 1.5–2 μ m half-light radii ( R _NIR ) with stellar half-mass radii ( ${R}_{{{M}}_{\star }}$ ) derived with multicolor light profiles from CANDELS Hubble Space Telescope imaging. In general agreement with previous work, we find that R _NIR and ${R}_{{{M}}_{\star }}$ are up to 40% smaller than the rest-frame optical half-light radius R _opt . The agreement between R _NIR and ${R}_{{{M}}_{\star }}$ is excellent, with a negligible systematic offset (<0.03 dex) up to z = 2 for quiescent galaxies and up to z = 1.5 for star-forming galaxies. We also deproject the profiles to estimate ${R}_{{{M}}_{\star },3{\rm{D}}}$ , the radius of a sphere containing 50% of the stellar mass. We present the R − M _⋆ distribution of galaxies at 0.5 < z < 1.5, comparing R _opt , ${R}_{{{M}}_{\star }}$ , and ${R}_{{{M}}_{\star },3{\rm{D}}}$ . The slope is significantly flatter for ${R}_{{{M}}_{\star }}$ and ${R}_{{{M}}_{\star },3{\rm{D}}}$ compared to R _opt , mostly due to downward shifts in size for massive star-forming galaxies, while ${R}_{{{M}}_{\star }}$ and ${R}_{{{M}}_{\star },3{\rm{D}}}$ do not show markedly different trends. Finally, we show rapid evolution of the size ( R ∝ (1 + z ) ^−1.7±0.1 ) of massive ( M _⋆ < 10 ^11 M _⊙ ) quiescent galaxies between z = 0.5 and z = 2.3, again comparing R _opt , ${R}_{{{M}}_{\star }}$ , and ${R}_{{{M}}_{\star },3{\rm{D}}}$ . We conclude that the main tenets of the evolution of the size narrative established over the past 20 yr, based on rest-frame optical light profile analysis, still hold in the era of JWST/NIRCam observations in the rest-frame near-IR. Galaxy evolution Astrophysics Marco Martorano verfasserin aut Boris Häußler verfasserin aut Kalina V. Nedkova verfasserin aut Tim B. Miller verfasserin aut Gabriel B. Brammer verfasserin aut Glenn van de Ven verfasserin aut Joel Leja verfasserin aut Rachel S. Bezanson verfasserin aut Adam Muzzin verfasserin aut Danilo Marchesini verfasserin aut Anna de Graaff verfasserin aut Erica J. Nelson verfasserin aut Mariska Kriek verfasserin aut Eric F. Bell verfasserin aut Marijn Franx verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 960(2023), 1, p 53 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:960 year:2023 number:1, p 53 https://doi.org/10.3847/1538-4357/ad02ee kostenfrei https://doaj.org/article/39f06aed39b5496892538eddb70896fe kostenfrei https://doi.org/10.3847/1538-4357/ad02ee 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 960 2023 1, p 53
spelling	10.3847/1538-4357/ad02ee doi (DE-627)DOAJ098971263 (DE-599)DOAJ39f06aed39b5496892538eddb70896fe DE-627 ger DE-627 rakwb eng QB460-466 Arjen van der Wel verfasserin aut Stellar Half-mass Radii of 0.5 z < 2.3 Galaxies: Comparison with JWST/NIRCam Half-light Radii 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We use CEERS JWST/NIRCam imaging to measure rest-frame near-IR light profiles of 435 M _⋆ < 10 ^10 M _⊙ galaxies in the redshift range of 0.5 < z < 2.3. We compare the resulting rest-frame 1.5–2 μ m half-light radii ( R _NIR ) with stellar half-mass radii ( ${R}_{{{M}}_{\star }}$ ) derived with multicolor light profiles from CANDELS Hubble Space Telescope imaging. In general agreement with previous work, we find that R _NIR and ${R}_{{{M}}_{\star }}$ are up to 40% smaller than the rest-frame optical half-light radius R _opt . The agreement between R _NIR and ${R}_{{{M}}_{\star }}$ is excellent, with a negligible systematic offset (<0.03 dex) up to z = 2 for quiescent galaxies and up to z = 1.5 for star-forming galaxies. We also deproject the profiles to estimate ${R}_{{{M}}_{\star },3{\rm{D}}}$ , the radius of a sphere containing 50% of the stellar mass. We present the R − M _⋆ distribution of galaxies at 0.5 < z < 1.5, comparing R _opt , ${R}_{{{M}}_{\star }}$ , and ${R}_{{{M}}_{\star },3{\rm{D}}}$ . The slope is significantly flatter for ${R}_{{{M}}_{\star }}$ and ${R}_{{{M}}_{\star },3{\rm{D}}}$ compared to R _opt , mostly due to downward shifts in size for massive star-forming galaxies, while ${R}_{{{M}}_{\star }}$ and ${R}_{{{M}}_{\star },3{\rm{D}}}$ do not show markedly different trends. Finally, we show rapid evolution of the size ( R ∝ (1 + z ) ^−1.7±0.1 ) of massive ( M _⋆ < 10 ^11 M _⊙ ) quiescent galaxies between z = 0.5 and z = 2.3, again comparing R _opt , ${R}_{{{M}}_{\star }}$ , and ${R}_{{{M}}_{\star },3{\rm{D}}}$ . We conclude that the main tenets of the evolution of the size narrative established over the past 20 yr, based on rest-frame optical light profile analysis, still hold in the era of JWST/NIRCam observations in the rest-frame near-IR. Galaxy evolution Astrophysics Marco Martorano verfasserin aut Boris Häußler verfasserin aut Kalina V. Nedkova verfasserin aut Tim B. Miller verfasserin aut Gabriel B. Brammer verfasserin aut Glenn van de Ven verfasserin aut Joel Leja verfasserin aut Rachel S. Bezanson verfasserin aut Adam Muzzin verfasserin aut Danilo Marchesini verfasserin aut Anna de Graaff verfasserin aut Erica J. Nelson verfasserin aut Mariska Kriek verfasserin aut Eric F. Bell verfasserin aut Marijn Franx verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 960(2023), 1, p 53 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:960 year:2023 number:1, p 53 https://doi.org/10.3847/1538-4357/ad02ee kostenfrei https://doaj.org/article/39f06aed39b5496892538eddb70896fe kostenfrei https://doi.org/10.3847/1538-4357/ad02ee 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 960 2023 1, p 53
allfields_unstemmed	10.3847/1538-4357/ad02ee doi (DE-627)DOAJ098971263 (DE-599)DOAJ39f06aed39b5496892538eddb70896fe DE-627 ger DE-627 rakwb eng QB460-466 Arjen van der Wel verfasserin aut Stellar Half-mass Radii of 0.5 z < 2.3 Galaxies: Comparison with JWST/NIRCam Half-light Radii 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We use CEERS JWST/NIRCam imaging to measure rest-frame near-IR light profiles of 435 M _⋆ < 10 ^10 M _⊙ galaxies in the redshift range of 0.5 < z < 2.3. We compare the resulting rest-frame 1.5–2 μ m half-light radii ( R _NIR ) with stellar half-mass radii ( ${R}_{{{M}}_{\star }}$ ) derived with multicolor light profiles from CANDELS Hubble Space Telescope imaging. In general agreement with previous work, we find that R _NIR and ${R}_{{{M}}_{\star }}$ are up to 40% smaller than the rest-frame optical half-light radius R _opt . The agreement between R _NIR and ${R}_{{{M}}_{\star }}$ is excellent, with a negligible systematic offset (<0.03 dex) up to z = 2 for quiescent galaxies and up to z = 1.5 for star-forming galaxies. We also deproject the profiles to estimate ${R}_{{{M}}_{\star },3{\rm{D}}}$ , the radius of a sphere containing 50% of the stellar mass. We present the R − M _⋆ distribution of galaxies at 0.5 < z < 1.5, comparing R _opt , ${R}_{{{M}}_{\star }}$ , and ${R}_{{{M}}_{\star },3{\rm{D}}}$ . The slope is significantly flatter for ${R}_{{{M}}_{\star }}$ and ${R}_{{{M}}_{\star },3{\rm{D}}}$ compared to R _opt , mostly due to downward shifts in size for massive star-forming galaxies, while ${R}_{{{M}}_{\star }}$ and ${R}_{{{M}}_{\star },3{\rm{D}}}$ do not show markedly different trends. Finally, we show rapid evolution of the size ( R ∝ (1 + z ) ^−1.7±0.1 ) of massive ( M _⋆ < 10 ^11 M _⊙ ) quiescent galaxies between z = 0.5 and z = 2.3, again comparing R _opt , ${R}_{{{M}}_{\star }}$ , and ${R}_{{{M}}_{\star },3{\rm{D}}}$ . We conclude that the main tenets of the evolution of the size narrative established over the past 20 yr, based on rest-frame optical light profile analysis, still hold in the era of JWST/NIRCam observations in the rest-frame near-IR. Galaxy evolution Astrophysics Marco Martorano verfasserin aut Boris Häußler verfasserin aut Kalina V. Nedkova verfasserin aut Tim B. Miller verfasserin aut Gabriel B. Brammer verfasserin aut Glenn van de Ven verfasserin aut Joel Leja verfasserin aut Rachel S. Bezanson verfasserin aut Adam Muzzin verfasserin aut Danilo Marchesini verfasserin aut Anna de Graaff verfasserin aut Erica J. Nelson verfasserin aut Mariska Kriek verfasserin aut Eric F. Bell verfasserin aut Marijn Franx verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 960(2023), 1, p 53 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:960 year:2023 number:1, p 53 https://doi.org/10.3847/1538-4357/ad02ee kostenfrei https://doaj.org/article/39f06aed39b5496892538eddb70896fe kostenfrei https://doi.org/10.3847/1538-4357/ad02ee 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 960 2023 1, p 53
allfieldsGer	10.3847/1538-4357/ad02ee doi (DE-627)DOAJ098971263 (DE-599)DOAJ39f06aed39b5496892538eddb70896fe DE-627 ger DE-627 rakwb eng QB460-466 Arjen van der Wel verfasserin aut Stellar Half-mass Radii of 0.5 z < 2.3 Galaxies: Comparison with JWST/NIRCam Half-light Radii 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We use CEERS JWST/NIRCam imaging to measure rest-frame near-IR light profiles of 435 M _⋆ < 10 ^10 M _⊙ galaxies in the redshift range of 0.5 < z < 2.3. We compare the resulting rest-frame 1.5–2 μ m half-light radii ( R _NIR ) with stellar half-mass radii ( ${R}_{{{M}}_{\star }}$ ) derived with multicolor light profiles from CANDELS Hubble Space Telescope imaging. In general agreement with previous work, we find that R _NIR and ${R}_{{{M}}_{\star }}$ are up to 40% smaller than the rest-frame optical half-light radius R _opt . The agreement between R _NIR and ${R}_{{{M}}_{\star }}$ is excellent, with a negligible systematic offset (<0.03 dex) up to z = 2 for quiescent galaxies and up to z = 1.5 for star-forming galaxies. We also deproject the profiles to estimate ${R}_{{{M}}_{\star },3{\rm{D}}}$ , the radius of a sphere containing 50% of the stellar mass. We present the R − M _⋆ distribution of galaxies at 0.5 < z < 1.5, comparing R _opt , ${R}_{{{M}}_{\star }}$ , and ${R}_{{{M}}_{\star },3{\rm{D}}}$ . The slope is significantly flatter for ${R}_{{{M}}_{\star }}$ and ${R}_{{{M}}_{\star },3{\rm{D}}}$ compared to R _opt , mostly due to downward shifts in size for massive star-forming galaxies, while ${R}_{{{M}}_{\star }}$ and ${R}_{{{M}}_{\star },3{\rm{D}}}$ do not show markedly different trends. Finally, we show rapid evolution of the size ( R ∝ (1 + z ) ^−1.7±0.1 ) of massive ( M _⋆ < 10 ^11 M _⊙ ) quiescent galaxies between z = 0.5 and z = 2.3, again comparing R _opt , ${R}_{{{M}}_{\star }}$ , and ${R}_{{{M}}_{\star },3{\rm{D}}}$ . We conclude that the main tenets of the evolution of the size narrative established over the past 20 yr, based on rest-frame optical light profile analysis, still hold in the era of JWST/NIRCam observations in the rest-frame near-IR. Galaxy evolution Astrophysics Marco Martorano verfasserin aut Boris Häußler verfasserin aut Kalina V. Nedkova verfasserin aut Tim B. Miller verfasserin aut Gabriel B. Brammer verfasserin aut Glenn van de Ven verfasserin aut Joel Leja verfasserin aut Rachel S. Bezanson verfasserin aut Adam Muzzin verfasserin aut Danilo Marchesini verfasserin aut Anna de Graaff verfasserin aut Erica J. Nelson verfasserin aut Mariska Kriek verfasserin aut Eric F. Bell verfasserin aut Marijn Franx verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 960(2023), 1, p 53 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:960 year:2023 number:1, p 53 https://doi.org/10.3847/1538-4357/ad02ee kostenfrei https://doaj.org/article/39f06aed39b5496892538eddb70896fe kostenfrei https://doi.org/10.3847/1538-4357/ad02ee 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 960 2023 1, p 53
allfieldsSound	10.3847/1538-4357/ad02ee doi (DE-627)DOAJ098971263 (DE-599)DOAJ39f06aed39b5496892538eddb70896fe DE-627 ger DE-627 rakwb eng QB460-466 Arjen van der Wel verfasserin aut Stellar Half-mass Radii of 0.5 z < 2.3 Galaxies: Comparison with JWST/NIRCam Half-light Radii 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We use CEERS JWST/NIRCam imaging to measure rest-frame near-IR light profiles of 435 M _⋆ < 10 ^10 M _⊙ galaxies in the redshift range of 0.5 < z < 2.3. We compare the resulting rest-frame 1.5–2 μ m half-light radii ( R _NIR ) with stellar half-mass radii ( ${R}_{{{M}}_{\star }}$ ) derived with multicolor light profiles from CANDELS Hubble Space Telescope imaging. In general agreement with previous work, we find that R _NIR and ${R}_{{{M}}_{\star }}$ are up to 40% smaller than the rest-frame optical half-light radius R _opt . The agreement between R _NIR and ${R}_{{{M}}_{\star }}$ is excellent, with a negligible systematic offset (<0.03 dex) up to z = 2 for quiescent galaxies and up to z = 1.5 for star-forming galaxies. We also deproject the profiles to estimate ${R}_{{{M}}_{\star },3{\rm{D}}}$ , the radius of a sphere containing 50% of the stellar mass. We present the R − M _⋆ distribution of galaxies at 0.5 < z < 1.5, comparing R _opt , ${R}_{{{M}}_{\star }}$ , and ${R}_{{{M}}_{\star },3{\rm{D}}}$ . The slope is significantly flatter for ${R}_{{{M}}_{\star }}$ and ${R}_{{{M}}_{\star },3{\rm{D}}}$ compared to R _opt , mostly due to downward shifts in size for massive star-forming galaxies, while ${R}_{{{M}}_{\star }}$ and ${R}_{{{M}}_{\star },3{\rm{D}}}$ do not show markedly different trends. Finally, we show rapid evolution of the size ( R ∝ (1 + z ) ^−1.7±0.1 ) of massive ( M _⋆ < 10 ^11 M _⊙ ) quiescent galaxies between z = 0.5 and z = 2.3, again comparing R _opt , ${R}_{{{M}}_{\star }}$ , and ${R}_{{{M}}_{\star },3{\rm{D}}}$ . We conclude that the main tenets of the evolution of the size narrative established over the past 20 yr, based on rest-frame optical light profile analysis, still hold in the era of JWST/NIRCam observations in the rest-frame near-IR. Galaxy evolution Astrophysics Marco Martorano verfasserin aut Boris Häußler verfasserin aut Kalina V. Nedkova verfasserin aut Tim B. Miller verfasserin aut Gabriel B. Brammer verfasserin aut Glenn van de Ven verfasserin aut Joel Leja verfasserin aut Rachel S. Bezanson verfasserin aut Adam Muzzin verfasserin aut Danilo Marchesini verfasserin aut Anna de Graaff verfasserin aut Erica J. Nelson verfasserin aut Mariska Kriek verfasserin aut Eric F. Bell verfasserin aut Marijn Franx verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 960(2023), 1, p 53 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:960 year:2023 number:1, p 53 https://doi.org/10.3847/1538-4357/ad02ee kostenfrei https://doaj.org/article/39f06aed39b5496892538eddb70896fe kostenfrei https://doi.org/10.3847/1538-4357/ad02ee 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 960 2023 1, p 53
language	English
source	In The Astrophysical Journal 960(2023), 1, p 53 volume:960 year:2023 number:1, p 53
sourceStr	In The Astrophysical Journal 960(2023), 1, p 53 volume:960 year:2023 number:1, p 53
format_phy_str_mv	Article
institution	findex.gbv.de
topic_facet	Galaxy evolution Astrophysics
isfreeaccess_bool	true
container_title	The Astrophysical Journal
authorswithroles_txt_mv	Arjen van der Wel @@aut@@ Marco Martorano @@aut@@ Boris Häußler @@aut@@ Kalina V. Nedkova @@aut@@ Tim B. Miller @@aut@@ Gabriel B. Brammer @@aut@@ Glenn van de Ven @@aut@@ Joel Leja @@aut@@ Rachel S. Bezanson @@aut@@ Adam Muzzin @@aut@@ Danilo Marchesini @@aut@@ Anna de Graaff @@aut@@ Erica J. Nelson @@aut@@ Mariska Kriek @@aut@@ Eric F. Bell @@aut@@ Marijn Franx @@aut@@
publishDateDaySort_date	2023-01-01T00:00:00Z
hierarchy_top_id	269019219
id	DOAJ098971263
language_de	englisch
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We compare the resulting rest-frame 1.5–2 μ m half-light radii ( R _NIR ) with stellar half-mass radii ( ${R}_{{{M}}_{\star }}$ ) derived with multicolor light profiles from CANDELS Hubble Space Telescope imaging. In general agreement with previous work, we find that R _NIR and ${R}_{{{M}}_{\star }}$ are up to 40% smaller than the rest-frame optical half-light radius R _opt . The agreement between R _NIR and ${R}_{{{M}}_{\star }}$ is excellent, with a negligible systematic offset (<0.03 dex) up to z = 2 for quiescent galaxies and up to z = 1.5 for star-forming galaxies. We also deproject the profiles to estimate ${R}_{{{M}}_{\star },3{\rm{D}}}$ , the radius of a sphere containing 50% of the stellar mass. We present the R − M _⋆ distribution of galaxies at 0.5 < z < 1.5, comparing R _opt , ${R}_{{{M}}_{\star }}$ , and ${R}_{{{M}}_{\star },3{\rm{D}}}$ . The slope is significantly flatter for ${R}_{{{M}}_{\star }}$ and ${R}_{{{M}}_{\star },3{\rm{D}}}$ compared to R _opt , mostly due to downward shifts in size for massive star-forming galaxies, while ${R}_{{{M}}_{\star }}$ and ${R}_{{{M}}_{\star },3{\rm{D}}}$ do not show markedly different trends. Finally, we show rapid evolution of the size ( R ∝ (1 + z ) ^−1.7±0.1 ) of massive ( M _⋆ < 10 ^11 M _⊙ ) quiescent galaxies between z = 0.5 and z = 2.3, again comparing R _opt , ${R}_{{{M}}_{\star }}$ , and ${R}_{{{M}}_{\star },3{\rm{D}}}$ . 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callnumber-first	Q - Science
author	Arjen van der Wel
spellingShingle	Arjen van der Wel misc QB460-466 misc Galaxy evolution misc Astrophysics Stellar Half-mass Radii of 0.5 z < 2.3 Galaxies: Comparison with JWST/NIRCam Half-light Radii
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topic_title	QB460-466 Stellar Half-mass Radii of 0.5 z < 2.3 Galaxies: Comparison with JWST/NIRCam Half-light Radii Galaxy evolution
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title	Stellar Half-mass Radii of 0.5 z < 2.3 Galaxies: Comparison with JWST/NIRCam Half-light Radii
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title_full	Stellar Half-mass Radii of 0.5 z < 2.3 Galaxies: Comparison with JWST/NIRCam Half-light Radii
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author_browse	Arjen van der Wel Marco Martorano Boris Häußler Kalina V. Nedkova Tim B. Miller Gabriel B. Brammer Glenn van de Ven Joel Leja Rachel S. Bezanson Adam Muzzin Danilo Marchesini Anna de Graaff Erica J. Nelson Mariska Kriek Eric F. Bell Marijn Franx
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title_sort	stellar half-mass radii of 0.5 z < 2.3 galaxies: comparison with jwst/nircam half-light radii
callnumber	QB460-466
title_auth	Stellar Half-mass Radii of 0.5 z < 2.3 Galaxies: Comparison with JWST/NIRCam Half-light Radii
abstract	We use CEERS JWST/NIRCam imaging to measure rest-frame near-IR light profiles of 435 M _⋆ < 10 ^10 M _⊙ galaxies in the redshift range of 0.5 < z < 2.3. We compare the resulting rest-frame 1.5–2 μ m half-light radii ( R _NIR ) with stellar half-mass radii ( ${R}_{{{M}}_{\star }}$ ) derived with multicolor light profiles from CANDELS Hubble Space Telescope imaging. In general agreement with previous work, we find that R _NIR and ${R}_{{{M}}_{\star }}$ are up to 40% smaller than the rest-frame optical half-light radius R _opt . The agreement between R _NIR and ${R}_{{{M}}_{\star }}$ is excellent, with a negligible systematic offset (<0.03 dex) up to z = 2 for quiescent galaxies and up to z = 1.5 for star-forming galaxies. We also deproject the profiles to estimate ${R}_{{{M}}_{\star },3{\rm{D}}}$ , the radius of a sphere containing 50% of the stellar mass. We present the R − M _⋆ distribution of galaxies at 0.5 < z < 1.5, comparing R _opt , ${R}_{{{M}}_{\star }}$ , and ${R}_{{{M}}_{\star },3{\rm{D}}}$ . The slope is significantly flatter for ${R}_{{{M}}_{\star }}$ and ${R}_{{{M}}_{\star },3{\rm{D}}}$ compared to R _opt , mostly due to downward shifts in size for massive star-forming galaxies, while ${R}_{{{M}}_{\star }}$ and ${R}_{{{M}}_{\star },3{\rm{D}}}$ do not show markedly different trends. Finally, we show rapid evolution of the size ( R ∝ (1 + z ) ^−1.7±0.1 ) of massive ( M _⋆ < 10 ^11 M _⊙ ) quiescent galaxies between z = 0.5 and z = 2.3, again comparing R _opt , ${R}_{{{M}}_{\star }}$ , and ${R}_{{{M}}_{\star },3{\rm{D}}}$ . We conclude that the main tenets of the evolution of the size narrative established over the past 20 yr, based on rest-frame optical light profile analysis, still hold in the era of JWST/NIRCam observations in the rest-frame near-IR.
abstractGer	We use CEERS JWST/NIRCam imaging to measure rest-frame near-IR light profiles of 435 M _⋆ < 10 ^10 M _⊙ galaxies in the redshift range of 0.5 < z < 2.3. We compare the resulting rest-frame 1.5–2 μ m half-light radii ( R _NIR ) with stellar half-mass radii ( ${R}_{{{M}}_{\star }}$ ) derived with multicolor light profiles from CANDELS Hubble Space Telescope imaging. In general agreement with previous work, we find that R _NIR and ${R}_{{{M}}_{\star }}$ are up to 40% smaller than the rest-frame optical half-light radius R _opt . The agreement between R _NIR and ${R}_{{{M}}_{\star }}$ is excellent, with a negligible systematic offset (<0.03 dex) up to z = 2 for quiescent galaxies and up to z = 1.5 for star-forming galaxies. We also deproject the profiles to estimate ${R}_{{{M}}_{\star },3{\rm{D}}}$ , the radius of a sphere containing 50% of the stellar mass. We present the R − M _⋆ distribution of galaxies at 0.5 < z < 1.5, comparing R _opt , ${R}_{{{M}}_{\star }}$ , and ${R}_{{{M}}_{\star },3{\rm{D}}}$ . The slope is significantly flatter for ${R}_{{{M}}_{\star }}$ and ${R}_{{{M}}_{\star },3{\rm{D}}}$ compared to R _opt , mostly due to downward shifts in size for massive star-forming galaxies, while ${R}_{{{M}}_{\star }}$ and ${R}_{{{M}}_{\star },3{\rm{D}}}$ do not show markedly different trends. Finally, we show rapid evolution of the size ( R ∝ (1 + z ) ^−1.7±0.1 ) of massive ( M _⋆ < 10 ^11 M _⊙ ) quiescent galaxies between z = 0.5 and z = 2.3, again comparing R _opt , ${R}_{{{M}}_{\star }}$ , and ${R}_{{{M}}_{\star },3{\rm{D}}}$ . We conclude that the main tenets of the evolution of the size narrative established over the past 20 yr, based on rest-frame optical light profile analysis, still hold in the era of JWST/NIRCam observations in the rest-frame near-IR.
abstract_unstemmed	We use CEERS JWST/NIRCam imaging to measure rest-frame near-IR light profiles of 435 M _⋆ < 10 ^10 M _⊙ galaxies in the redshift range of 0.5 < z < 2.3. We compare the resulting rest-frame 1.5–2 μ m half-light radii ( R _NIR ) with stellar half-mass radii ( ${R}_{{{M}}_{\star }}$ ) derived with multicolor light profiles from CANDELS Hubble Space Telescope imaging. In general agreement with previous work, we find that R _NIR and ${R}_{{{M}}_{\star }}$ are up to 40% smaller than the rest-frame optical half-light radius R _opt . The agreement between R _NIR and ${R}_{{{M}}_{\star }}$ is excellent, with a negligible systematic offset (<0.03 dex) up to z = 2 for quiescent galaxies and up to z = 1.5 for star-forming galaxies. We also deproject the profiles to estimate ${R}_{{{M}}_{\star },3{\rm{D}}}$ , the radius of a sphere containing 50% of the stellar mass. We present the R − M _⋆ distribution of galaxies at 0.5 < z < 1.5, comparing R _opt , ${R}_{{{M}}_{\star }}$ , and ${R}_{{{M}}_{\star },3{\rm{D}}}$ . The slope is significantly flatter for ${R}_{{{M}}_{\star }}$ and ${R}_{{{M}}_{\star },3{\rm{D}}}$ compared to R _opt , mostly due to downward shifts in size for massive star-forming galaxies, while ${R}_{{{M}}_{\star }}$ and ${R}_{{{M}}_{\star },3{\rm{D}}}$ do not show markedly different trends. Finally, we show rapid evolution of the size ( R ∝ (1 + z ) ^−1.7±0.1 ) of massive ( M _⋆ < 10 ^11 M _⊙ ) quiescent galaxies between z = 0.5 and z = 2.3, again comparing R _opt , ${R}_{{{M}}_{\star }}$ , and ${R}_{{{M}}_{\star },3{\rm{D}}}$ . We conclude that the main tenets of the evolution of the size narrative established over the past 20 yr, based on rest-frame optical light profile analysis, still hold in the era of JWST/NIRCam observations in the rest-frame near-IR.
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title_short	Stellar Half-mass Radii of 0.5 z < 2.3 Galaxies: Comparison with JWST/NIRCam Half-light Radii
url	https://doi.org/10.3847/1538-4357/ad02ee https://doaj.org/article/39f06aed39b5496892538eddb70896fe https://doaj.org/toc/1538-4357
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Stellar Half-mass Radii of 0.5 z < 2.3 Galaxies: Comparison with JWST/NIRCam Half-light Radii

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