Spatial Extent of Molecular Gas, Dust, and Stars in Massive Galaxies at z ∼ 2.2–2.5 Determined with ALMA and JWST

We present the results of 0.″6-resolution observations of CO J = 3 − 2 line emission in 10 massive star-forming galaxies at z ∼ 2.2–2.5 with the Atacama Large Millimeter/submillimeter Array (ALMA). We compare the spatial extent of molecular gas with those of dust and stars, traced by the 870 and 4.4...
Ausführliche Beschreibung

Gespeichert in:

Autor*in:	Ken-ichi Tadaki [verfasserIn] Tadayuki Kodama [verfasserIn] Yusei Koyama [verfasserIn] Tomoko L. Suzuki [verfasserIn] Ikki Mitsuhashi [verfasserIn] Ryota Ikeda [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2023

Schlagwörter:	Starburst galaxies High-redshift galaxies

Übergeordnetes Werk:	In: The Astrophysical Journal Letters - IOP Publishing, 2022, 957(2023), 2, p L15
Übergeordnetes Werk:	volume:957 ; year:2023 ; number:2, p L15

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3847/2041-8213/ad03f2

Katalog-ID:	DOAJ096917512

Internformat


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allfields	10.3847/2041-8213/ad03f2 doi (DE-627)DOAJ096917512 (DE-599)DOAJ331427764f2b408ca9de54c6d2929696 DE-627 ger DE-627 rakwb eng QB460-466 Ken-ichi Tadaki verfasserin aut Spatial Extent of Molecular Gas, Dust, and Stars in Massive Galaxies at z ∼ 2.2–2.5 Determined with ALMA and JWST 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present the results of 0.″6-resolution observations of CO J = 3 − 2 line emission in 10 massive star-forming galaxies at z ∼ 2.2–2.5 with the Atacama Large Millimeter/submillimeter Array (ALMA). We compare the spatial extent of molecular gas with those of dust and stars, traced by the 870 and 4.4 μ m continuum emissions, respectively. The average effective radius of the CO emission is 1.75 ± 0.34 kpc, which is about 60% larger than that of the 870 μ m emission and is comparable with that of the 4.4 μ m emission. Utilizing the best-fit parametric models, we derive the radial gradients of the specific star formation rate (sSFR), gas depletion timescale, and gas-mass fraction within the observed galaxies. We find a more intense star formation activity with a higher sSFR and a shorter depletion timescale in the inner region than in the outer region. The central starburst may be the primary process for massive galaxies to build up a core. Furthermore, the gas-mass fraction is high, independent of the galactocentric radius in the observed galaxies, suggesting that the galaxies have not begun to quench star formation. Given the shorter gas depletion timescale in the center compared to the outer region, quenching is expected to occur in the center first and then propagate outward. We may be witnessing the observed galaxies in the formation phase of a core prior to the forthcoming phase of star formation propagating outward. Starburst galaxies High-redshift galaxies Astrophysics Tadayuki Kodama verfasserin aut Yusei Koyama verfasserin aut Tomoko L. Suzuki verfasserin aut Ikki Mitsuhashi verfasserin aut Ryota Ikeda verfasserin aut In The Astrophysical Journal Letters IOP Publishing, 2022 957(2023), 2, p L15 (DE-627)312189028 (DE-600)2006858-X 20418213 nnns volume:957 year:2023 number:2, p L15 https://doi.org/10.3847/2041-8213/ad03f2 kostenfrei https://doaj.org/article/331427764f2b408ca9de54c6d2929696 kostenfrei https://doi.org/10.3847/2041-8213/ad03f2 kostenfrei https://doaj.org/toc/2041-8205 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_213 GBV_ILN_230 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 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 957 2023 2, p L15
spelling	10.3847/2041-8213/ad03f2 doi (DE-627)DOAJ096917512 (DE-599)DOAJ331427764f2b408ca9de54c6d2929696 DE-627 ger DE-627 rakwb eng QB460-466 Ken-ichi Tadaki verfasserin aut Spatial Extent of Molecular Gas, Dust, and Stars in Massive Galaxies at z ∼ 2.2–2.5 Determined with ALMA and JWST 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present the results of 0.″6-resolution observations of CO J = 3 − 2 line emission in 10 massive star-forming galaxies at z ∼ 2.2–2.5 with the Atacama Large Millimeter/submillimeter Array (ALMA). We compare the spatial extent of molecular gas with those of dust and stars, traced by the 870 and 4.4 μ m continuum emissions, respectively. The average effective radius of the CO emission is 1.75 ± 0.34 kpc, which is about 60% larger than that of the 870 μ m emission and is comparable with that of the 4.4 μ m emission. Utilizing the best-fit parametric models, we derive the radial gradients of the specific star formation rate (sSFR), gas depletion timescale, and gas-mass fraction within the observed galaxies. We find a more intense star formation activity with a higher sSFR and a shorter depletion timescale in the inner region than in the outer region. The central starburst may be the primary process for massive galaxies to build up a core. Furthermore, the gas-mass fraction is high, independent of the galactocentric radius in the observed galaxies, suggesting that the galaxies have not begun to quench star formation. Given the shorter gas depletion timescale in the center compared to the outer region, quenching is expected to occur in the center first and then propagate outward. We may be witnessing the observed galaxies in the formation phase of a core prior to the forthcoming phase of star formation propagating outward. Starburst galaxies High-redshift galaxies Astrophysics Tadayuki Kodama verfasserin aut Yusei Koyama verfasserin aut Tomoko L. Suzuki verfasserin aut Ikki Mitsuhashi verfasserin aut Ryota Ikeda verfasserin aut In The Astrophysical Journal Letters IOP Publishing, 2022 957(2023), 2, p L15 (DE-627)312189028 (DE-600)2006858-X 20418213 nnns volume:957 year:2023 number:2, p L15 https://doi.org/10.3847/2041-8213/ad03f2 kostenfrei https://doaj.org/article/331427764f2b408ca9de54c6d2929696 kostenfrei https://doi.org/10.3847/2041-8213/ad03f2 kostenfrei https://doaj.org/toc/2041-8205 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_213 GBV_ILN_230 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 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 957 2023 2, p L15
allfields_unstemmed	10.3847/2041-8213/ad03f2 doi (DE-627)DOAJ096917512 (DE-599)DOAJ331427764f2b408ca9de54c6d2929696 DE-627 ger DE-627 rakwb eng QB460-466 Ken-ichi Tadaki verfasserin aut Spatial Extent of Molecular Gas, Dust, and Stars in Massive Galaxies at z ∼ 2.2–2.5 Determined with ALMA and JWST 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present the results of 0.″6-resolution observations of CO J = 3 − 2 line emission in 10 massive star-forming galaxies at z ∼ 2.2–2.5 with the Atacama Large Millimeter/submillimeter Array (ALMA). We compare the spatial extent of molecular gas with those of dust and stars, traced by the 870 and 4.4 μ m continuum emissions, respectively. The average effective radius of the CO emission is 1.75 ± 0.34 kpc, which is about 60% larger than that of the 870 μ m emission and is comparable with that of the 4.4 μ m emission. Utilizing the best-fit parametric models, we derive the radial gradients of the specific star formation rate (sSFR), gas depletion timescale, and gas-mass fraction within the observed galaxies. We find a more intense star formation activity with a higher sSFR and a shorter depletion timescale in the inner region than in the outer region. The central starburst may be the primary process for massive galaxies to build up a core. Furthermore, the gas-mass fraction is high, independent of the galactocentric radius in the observed galaxies, suggesting that the galaxies have not begun to quench star formation. Given the shorter gas depletion timescale in the center compared to the outer region, quenching is expected to occur in the center first and then propagate outward. We may be witnessing the observed galaxies in the formation phase of a core prior to the forthcoming phase of star formation propagating outward. Starburst galaxies High-redshift galaxies Astrophysics Tadayuki Kodama verfasserin aut Yusei Koyama verfasserin aut Tomoko L. Suzuki verfasserin aut Ikki Mitsuhashi verfasserin aut Ryota Ikeda verfasserin aut In The Astrophysical Journal Letters IOP Publishing, 2022 957(2023), 2, p L15 (DE-627)312189028 (DE-600)2006858-X 20418213 nnns volume:957 year:2023 number:2, p L15 https://doi.org/10.3847/2041-8213/ad03f2 kostenfrei https://doaj.org/article/331427764f2b408ca9de54c6d2929696 kostenfrei https://doi.org/10.3847/2041-8213/ad03f2 kostenfrei https://doaj.org/toc/2041-8205 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_213 GBV_ILN_230 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 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 957 2023 2, p L15
allfieldsGer	10.3847/2041-8213/ad03f2 doi (DE-627)DOAJ096917512 (DE-599)DOAJ331427764f2b408ca9de54c6d2929696 DE-627 ger DE-627 rakwb eng QB460-466 Ken-ichi Tadaki verfasserin aut Spatial Extent of Molecular Gas, Dust, and Stars in Massive Galaxies at z ∼ 2.2–2.5 Determined with ALMA and JWST 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present the results of 0.″6-resolution observations of CO J = 3 − 2 line emission in 10 massive star-forming galaxies at z ∼ 2.2–2.5 with the Atacama Large Millimeter/submillimeter Array (ALMA). We compare the spatial extent of molecular gas with those of dust and stars, traced by the 870 and 4.4 μ m continuum emissions, respectively. The average effective radius of the CO emission is 1.75 ± 0.34 kpc, which is about 60% larger than that of the 870 μ m emission and is comparable with that of the 4.4 μ m emission. Utilizing the best-fit parametric models, we derive the radial gradients of the specific star formation rate (sSFR), gas depletion timescale, and gas-mass fraction within the observed galaxies. We find a more intense star formation activity with a higher sSFR and a shorter depletion timescale in the inner region than in the outer region. The central starburst may be the primary process for massive galaxies to build up a core. Furthermore, the gas-mass fraction is high, independent of the galactocentric radius in the observed galaxies, suggesting that the galaxies have not begun to quench star formation. Given the shorter gas depletion timescale in the center compared to the outer region, quenching is expected to occur in the center first and then propagate outward. We may be witnessing the observed galaxies in the formation phase of a core prior to the forthcoming phase of star formation propagating outward. Starburst galaxies High-redshift galaxies Astrophysics Tadayuki Kodama verfasserin aut Yusei Koyama verfasserin aut Tomoko L. Suzuki verfasserin aut Ikki Mitsuhashi verfasserin aut Ryota Ikeda verfasserin aut In The Astrophysical Journal Letters IOP Publishing, 2022 957(2023), 2, p L15 (DE-627)312189028 (DE-600)2006858-X 20418213 nnns volume:957 year:2023 number:2, p L15 https://doi.org/10.3847/2041-8213/ad03f2 kostenfrei https://doaj.org/article/331427764f2b408ca9de54c6d2929696 kostenfrei https://doi.org/10.3847/2041-8213/ad03f2 kostenfrei https://doaj.org/toc/2041-8205 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_213 GBV_ILN_230 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 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 957 2023 2, p L15
allfieldsSound	10.3847/2041-8213/ad03f2 doi (DE-627)DOAJ096917512 (DE-599)DOAJ331427764f2b408ca9de54c6d2929696 DE-627 ger DE-627 rakwb eng QB460-466 Ken-ichi Tadaki verfasserin aut Spatial Extent of Molecular Gas, Dust, and Stars in Massive Galaxies at z ∼ 2.2–2.5 Determined with ALMA and JWST 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present the results of 0.″6-resolution observations of CO J = 3 − 2 line emission in 10 massive star-forming galaxies at z ∼ 2.2–2.5 with the Atacama Large Millimeter/submillimeter Array (ALMA). We compare the spatial extent of molecular gas with those of dust and stars, traced by the 870 and 4.4 μ m continuum emissions, respectively. The average effective radius of the CO emission is 1.75 ± 0.34 kpc, which is about 60% larger than that of the 870 μ m emission and is comparable with that of the 4.4 μ m emission. Utilizing the best-fit parametric models, we derive the radial gradients of the specific star formation rate (sSFR), gas depletion timescale, and gas-mass fraction within the observed galaxies. We find a more intense star formation activity with a higher sSFR and a shorter depletion timescale in the inner region than in the outer region. The central starburst may be the primary process for massive galaxies to build up a core. Furthermore, the gas-mass fraction is high, independent of the galactocentric radius in the observed galaxies, suggesting that the galaxies have not begun to quench star formation. Given the shorter gas depletion timescale in the center compared to the outer region, quenching is expected to occur in the center first and then propagate outward. We may be witnessing the observed galaxies in the formation phase of a core prior to the forthcoming phase of star formation propagating outward. Starburst galaxies High-redshift galaxies Astrophysics Tadayuki Kodama verfasserin aut Yusei Koyama verfasserin aut Tomoko L. Suzuki verfasserin aut Ikki Mitsuhashi verfasserin aut Ryota Ikeda verfasserin aut In The Astrophysical Journal Letters IOP Publishing, 2022 957(2023), 2, p L15 (DE-627)312189028 (DE-600)2006858-X 20418213 nnns volume:957 year:2023 number:2, p L15 https://doi.org/10.3847/2041-8213/ad03f2 kostenfrei https://doaj.org/article/331427764f2b408ca9de54c6d2929696 kostenfrei https://doi.org/10.3847/2041-8213/ad03f2 kostenfrei https://doaj.org/toc/2041-8205 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_213 GBV_ILN_230 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 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 957 2023 2, p L15
language	English
source	In The Astrophysical Journal Letters 957(2023), 2, p L15 volume:957 year:2023 number:2, p L15
sourceStr	In The Astrophysical Journal Letters 957(2023), 2, p L15 volume:957 year:2023 number:2, p L15
format_phy_str_mv	Article
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authorswithroles_txt_mv	Ken-ichi Tadaki @@aut@@ Tadayuki Kodama @@aut@@ Yusei Koyama @@aut@@ Tomoko L. Suzuki @@aut@@ Ikki Mitsuhashi @@aut@@ Ryota Ikeda @@aut@@
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callnumber-first	Q - Science
author	Ken-ichi Tadaki
spellingShingle	Ken-ichi Tadaki misc QB460-466 misc Starburst galaxies misc High-redshift galaxies misc Astrophysics Spatial Extent of Molecular Gas, Dust, and Stars in Massive Galaxies at z ∼ 2.2–2.5 Determined with ALMA and JWST
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topic_title	QB460-466 Spatial Extent of Molecular Gas, Dust, and Stars in Massive Galaxies at z ∼ 2.2–2.5 Determined with ALMA and JWST Starburst galaxies High-redshift galaxies
topic	misc QB460-466 misc Starburst galaxies misc High-redshift galaxies misc Astrophysics
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title	Spatial Extent of Molecular Gas, Dust, and Stars in Massive Galaxies at z ∼ 2.2–2.5 Determined with ALMA and JWST
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title_full	Spatial Extent of Molecular Gas, Dust, and Stars in Massive Galaxies at z ∼ 2.2–2.5 Determined with ALMA and JWST
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author_browse	Ken-ichi Tadaki Tadayuki Kodama Yusei Koyama Tomoko L. Suzuki Ikki Mitsuhashi Ryota Ikeda
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title_sort	spatial extent of molecular gas, dust, and stars in massive galaxies at z ∼ 2.2–2.5 determined with alma and jwst
callnumber	QB460-466
title_auth	Spatial Extent of Molecular Gas, Dust, and Stars in Massive Galaxies at z ∼ 2.2–2.5 Determined with ALMA and JWST
abstract	We present the results of 0.″6-resolution observations of CO J = 3 − 2 line emission in 10 massive star-forming galaxies at z ∼ 2.2–2.5 with the Atacama Large Millimeter/submillimeter Array (ALMA). We compare the spatial extent of molecular gas with those of dust and stars, traced by the 870 and 4.4 μ m continuum emissions, respectively. The average effective radius of the CO emission is 1.75 ± 0.34 kpc, which is about 60% larger than that of the 870 μ m emission and is comparable with that of the 4.4 μ m emission. Utilizing the best-fit parametric models, we derive the radial gradients of the specific star formation rate (sSFR), gas depletion timescale, and gas-mass fraction within the observed galaxies. We find a more intense star formation activity with a higher sSFR and a shorter depletion timescale in the inner region than in the outer region. The central starburst may be the primary process for massive galaxies to build up a core. Furthermore, the gas-mass fraction is high, independent of the galactocentric radius in the observed galaxies, suggesting that the galaxies have not begun to quench star formation. Given the shorter gas depletion timescale in the center compared to the outer region, quenching is expected to occur in the center first and then propagate outward. We may be witnessing the observed galaxies in the formation phase of a core prior to the forthcoming phase of star formation propagating outward.
abstractGer	We present the results of 0.″6-resolution observations of CO J = 3 − 2 line emission in 10 massive star-forming galaxies at z ∼ 2.2–2.5 with the Atacama Large Millimeter/submillimeter Array (ALMA). We compare the spatial extent of molecular gas with those of dust and stars, traced by the 870 and 4.4 μ m continuum emissions, respectively. The average effective radius of the CO emission is 1.75 ± 0.34 kpc, which is about 60% larger than that of the 870 μ m emission and is comparable with that of the 4.4 μ m emission. Utilizing the best-fit parametric models, we derive the radial gradients of the specific star formation rate (sSFR), gas depletion timescale, and gas-mass fraction within the observed galaxies. We find a more intense star formation activity with a higher sSFR and a shorter depletion timescale in the inner region than in the outer region. The central starburst may be the primary process for massive galaxies to build up a core. Furthermore, the gas-mass fraction is high, independent of the galactocentric radius in the observed galaxies, suggesting that the galaxies have not begun to quench star formation. Given the shorter gas depletion timescale in the center compared to the outer region, quenching is expected to occur in the center first and then propagate outward. We may be witnessing the observed galaxies in the formation phase of a core prior to the forthcoming phase of star formation propagating outward.
abstract_unstemmed	We present the results of 0.″6-resolution observations of CO J = 3 − 2 line emission in 10 massive star-forming galaxies at z ∼ 2.2–2.5 with the Atacama Large Millimeter/submillimeter Array (ALMA). We compare the spatial extent of molecular gas with those of dust and stars, traced by the 870 and 4.4 μ m continuum emissions, respectively. The average effective radius of the CO emission is 1.75 ± 0.34 kpc, which is about 60% larger than that of the 870 μ m emission and is comparable with that of the 4.4 μ m emission. Utilizing the best-fit parametric models, we derive the radial gradients of the specific star formation rate (sSFR), gas depletion timescale, and gas-mass fraction within the observed galaxies. We find a more intense star formation activity with a higher sSFR and a shorter depletion timescale in the inner region than in the outer region. The central starburst may be the primary process for massive galaxies to build up a core. Furthermore, the gas-mass fraction is high, independent of the galactocentric radius in the observed galaxies, suggesting that the galaxies have not begun to quench star formation. Given the shorter gas depletion timescale in the center compared to the outer region, quenching is expected to occur in the center first and then propagate outward. We may be witnessing the observed galaxies in the formation phase of a core prior to the forthcoming phase of star formation propagating outward.
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title_short	Spatial Extent of Molecular Gas, Dust, and Stars in Massive Galaxies at z ∼ 2.2–2.5 Determined with ALMA and JWST
url	https://doi.org/10.3847/2041-8213/ad03f2 https://doaj.org/article/331427764f2b408ca9de54c6d2929696 https://doaj.org/toc/2041-8205
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author2	Tadayuki Kodama Yusei Koyama Tomoko L. Suzuki Ikki Mitsuhashi Ryota Ikeda
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up_date	2024-07-03T22:57:04.935Z
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Spatial Extent of Molecular Gas, Dust, and Stars in Massive Galaxies at z ∼ 2.2–2.5 Determined with ALMA and JWST

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