CEERS Key Paper. V. Galaxies at 4 < z < 9 Are Bluer than They Appear–Characterizing Galaxy Stellar Populations from Rest-frame ∼1 μm Imaging
We present results from the Cosmic Evolution Early Release Survey on the stellar population parameters for 28 galaxies with redshifts 4 < z < 9 using imaging data from the James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) combined with data from the Hubble Space Telescope and th...
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2023 |
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In: The Astrophysical Journal Letters - IOP Publishing, 2022, 949(2023), 2, p L18 |
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| Übergeordnetes Werk: |
volume:949 ; year:2023 ; number:2, p L18 |
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| DOI / URN: |
10.3847/2041-8213/acc948 |
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| Katalog-ID: |
DOAJ090895851 |
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| 100 | 0 | |a Casey Papovich |e verfasserin |4 aut | |
| 245 | 1 | 0 | |a CEERS Key Paper. V. Galaxies at 4 < z < 9 Are Bluer than They Appear–Characterizing Galaxy Stellar Populations from Rest-frame ∼1 μm Imaging |
| 264 | 1 | |c 2023 | |
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| 520 | |a We present results from the Cosmic Evolution Early Release Survey on the stellar population parameters for 28 galaxies with redshifts 4 < z < 9 using imaging data from the James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) combined with data from the Hubble Space Telescope and the Spitzer Space Telescope. The JWST/MIRI 5.6 and 7.7 μ m data extend the coverage of the rest-frame spectral energy distribution to nearly 1 μ m for galaxies in this redshift range. By modeling the galaxies’ SEDs the MIRI data show that the galaxies have, on average, rest-frame UV (1600 Å)— I -band colors 0.4 mag bluer than derived when using photometry that lacks MIRI. Therefore, the galaxies have lower ratios of stellar mass to light. The MIRI data reduce the stellar masses by $\langle {\rm{\Delta }}\mathrm{log}{M}_{* }\rangle =0.25$ dex at 4 < z < 6 and 0.37 dex at 6 < z < 9. This also reduces the star formation rates (SFRs) by 〈ΔlogSFR〉 = 0.14 dex at 4 < z < 6 and 0.27 dex at 6 < z < 9. The MIRI data also improve constraints on the allowable stellar mass formed in early star formation. We model this using a star formation history that includes both a “burst” at z _f = 100 and a slowly varying (“delayed- τ ”) model. The MIRI data reduce the allowable stellar mass by 0.6 dex at 4 < z < 6 and by ≈1 dex at 6 < z < 9. Applying these results globally, this reduces the cosmic stellar-mass density by an order of magnitude in the early Universe ( z ≈ 9). Therefore, observations of rest-frame ≳1 μ m are paramount for constraining the stellar-mass buildup in galaxies at very high redshifts. | ||
| 650 | 4 | |a Galaxy evolution | |
| 650 | 4 | |a Galaxy formation | |
| 650 | 4 | |a Cosmology | |
| 650 | 4 | |a Galaxy colors | |
| 650 | 4 | |a Galaxy properties | |
| 650 | 4 | |a Galaxy masses | |
| 653 | 0 | |a Astrophysics | |
| 700 | 0 | |a Justin W. Cole |e verfasserin |4 aut | |
| 700 | 0 | |a Guang Yang |e verfasserin |4 aut | |
| 700 | 0 | |a Steven L. Finkelstein |e verfasserin |4 aut | |
| 700 | 0 | |a Guillermo Barro |e verfasserin |4 aut | |
| 700 | 0 | |a Véronique Buat |e verfasserin |4 aut | |
| 700 | 0 | |a Denis Burgarella |e verfasserin |4 aut | |
| 700 | 0 | |a Pablo G. Pérez-González |e verfasserin |4 aut | |
| 700 | 0 | |a Paola Santini |e verfasserin |4 aut | |
| 700 | 0 | |a Lise-Marie Seillé |e verfasserin |4 aut | |
| 700 | 0 | |a Lu Shen |e verfasserin |4 aut | |
| 700 | 0 | |a Pablo Arrabal Haro |e verfasserin |4 aut | |
| 700 | 0 | |a Micaela B. Bagley |e verfasserin |4 aut | |
| 700 | 0 | |a Eric F. Bell |e verfasserin |4 aut | |
| 700 | 0 | |a Laura Bisigello |e verfasserin |4 aut | |
| 700 | 0 | |a Antonello Calabrò |e verfasserin |4 aut | |
| 700 | 0 | |a Caitlin M. Casey |e verfasserin |4 aut | |
| 700 | 0 | |a Marco Castellano |e verfasserin |4 aut | |
| 700 | 0 | |a Katherine Chworowsky |e verfasserin |4 aut | |
| 700 | 0 | |a Nikko J. Cleri |e verfasserin |4 aut | |
| 700 | 0 | |a Luca Costantin |e verfasserin |4 aut | |
| 700 | 0 | |a M. C. Cooper |e verfasserin |4 aut | |
| 700 | 0 | |a Mark Dickinson |e verfasserin |4 aut | |
| 700 | 0 | |a Henry C. Ferguson |e verfasserin |4 aut | |
| 700 | 0 | |a Adriano Fontana |e verfasserin |4 aut | |
| 700 | 0 | |a Mauro Giavalisco |e verfasserin |4 aut | |
| 700 | 0 | |a Andrea Grazian |e verfasserin |4 aut | |
| 700 | 0 | |a Norman A. Grogin |e verfasserin |4 aut | |
| 700 | 0 | |a Nimish P. Hathi |e verfasserin |4 aut | |
| 700 | 0 | |a Benne W. Holwerda |e verfasserin |4 aut | |
| 700 | 0 | |a Taylor A. Hutchison |e verfasserin |4 aut | |
| 700 | 0 | |a Jeyhan S. Kartaltepe |e verfasserin |4 aut | |
| 700 | 0 | |a Lisa J. Kewley |e verfasserin |4 aut | |
| 700 | 0 | |a Allison Kirkpatrick |e verfasserin |4 aut | |
| 700 | 0 | |a Dale D. Kocevski |e verfasserin |4 aut | |
| 700 | 0 | |a Anton M. Koekemoer |e verfasserin |4 aut | |
| 700 | 0 | |a Rebecca L. Larson |e verfasserin |4 aut | |
| 700 | 0 | |a Arianna S. Long |e verfasserin |4 aut | |
| 700 | 0 | |a Ray A. Lucas |e verfasserin |4 aut | |
| 700 | 0 | |a Laura Pentericci |e verfasserin |4 aut | |
| 700 | 0 | |a Nor Pirzkal |e verfasserin |4 aut | |
| 700 | 0 | |a Swara Ravindranath |e verfasserin |4 aut | |
| 700 | 0 | |a Rachel S. Somerville |e verfasserin |4 aut | |
| 700 | 0 | |a Jonathan R. Trump |e verfasserin |4 aut | |
| 700 | 0 | |a Stephanie M. Urbano Stawinski |e verfasserin |4 aut | |
| 700 | 0 | |a Benjamin J. Weiner |e verfasserin |4 aut | |
| 700 | 0 | |a Stephen M. Wilkins |e verfasserin |4 aut | |
| 700 | 0 | |a L. Y. Aaron Yung |e verfasserin |4 aut | |
| 700 | 0 | |a Jorge A. Zavala |e verfasserin |4 aut | |
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10.3847/2041-8213/acc948 doi (DE-627)DOAJ090895851 (DE-599)DOAJdcf51a7e0b354159aee7d0a31fb70d5d DE-627 ger DE-627 rakwb eng QB460-466 Casey Papovich verfasserin aut CEERS Key Paper. V. Galaxies at 4 < z < 9 Are Bluer than They Appear–Characterizing Galaxy Stellar Populations from Rest-frame ∼1 μm Imaging 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present results from the Cosmic Evolution Early Release Survey on the stellar population parameters for 28 galaxies with redshifts 4 < z < 9 using imaging data from the James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) combined with data from the Hubble Space Telescope and the Spitzer Space Telescope. The JWST/MIRI 5.6 and 7.7 μ m data extend the coverage of the rest-frame spectral energy distribution to nearly 1 μ m for galaxies in this redshift range. By modeling the galaxies’ SEDs the MIRI data show that the galaxies have, on average, rest-frame UV (1600 Å)— I -band colors 0.4 mag bluer than derived when using photometry that lacks MIRI. Therefore, the galaxies have lower ratios of stellar mass to light. The MIRI data reduce the stellar masses by $\langle {\rm{\Delta }}\mathrm{log}{M}_{* }\rangle =0.25$ dex at 4 < z < 6 and 0.37 dex at 6 < z < 9. This also reduces the star formation rates (SFRs) by 〈ΔlogSFR〉 = 0.14 dex at 4 < z < 6 and 0.27 dex at 6 < z < 9. The MIRI data also improve constraints on the allowable stellar mass formed in early star formation. We model this using a star formation history that includes both a “burst” at z _f = 100 and a slowly varying (“delayed- τ ”) model. The MIRI data reduce the allowable stellar mass by 0.6 dex at 4 < z < 6 and by ≈1 dex at 6 < z < 9. Applying these results globally, this reduces the cosmic stellar-mass density by an order of magnitude in the early Universe ( z ≈ 9). Therefore, observations of rest-frame ≳1 μ m are paramount for constraining the stellar-mass buildup in galaxies at very high redshifts. Galaxy evolution Galaxy formation Cosmology Galaxy colors Galaxy properties Galaxy masses Astrophysics Justin W. Cole verfasserin aut Guang Yang verfasserin aut Steven L. Finkelstein verfasserin aut Guillermo Barro verfasserin aut Véronique Buat verfasserin aut Denis Burgarella verfasserin aut Pablo G. Pérez-González verfasserin aut Paola Santini verfasserin aut Lise-Marie Seillé verfasserin aut Lu Shen verfasserin aut Pablo Arrabal Haro verfasserin aut Micaela B. Bagley verfasserin aut Eric F. Bell verfasserin aut Laura Bisigello verfasserin aut Antonello Calabrò verfasserin aut Caitlin M. Casey verfasserin aut Marco Castellano verfasserin aut Katherine Chworowsky verfasserin aut Nikko J. Cleri verfasserin aut Luca Costantin verfasserin aut M. C. Cooper verfasserin aut Mark Dickinson verfasserin aut Henry C. Ferguson verfasserin aut Adriano Fontana verfasserin aut Mauro Giavalisco verfasserin aut Andrea Grazian verfasserin aut Norman A. Grogin verfasserin aut Nimish P. Hathi verfasserin aut Benne W. Holwerda verfasserin aut Taylor A. Hutchison verfasserin aut Jeyhan S. Kartaltepe verfasserin aut Lisa J. Kewley verfasserin aut Allison Kirkpatrick verfasserin aut Dale D. Kocevski verfasserin aut Anton M. Koekemoer verfasserin aut Rebecca L. Larson verfasserin aut Arianna S. Long verfasserin aut Ray A. Lucas verfasserin aut Laura Pentericci verfasserin aut Nor Pirzkal verfasserin aut Swara Ravindranath verfasserin aut Rachel S. Somerville verfasserin aut Jonathan R. Trump verfasserin aut Stephanie M. Urbano Stawinski verfasserin aut Benjamin J. Weiner verfasserin aut Stephen M. Wilkins verfasserin aut L. Y. Aaron Yung verfasserin aut Jorge A. Zavala verfasserin aut In The Astrophysical Journal Letters IOP Publishing, 2022 949(2023), 2, p L18 (DE-627)312189028 (DE-600)2006858-X 20418213 nnns volume:949 year:2023 number:2, p L18 https://doi.org/10.3847/2041-8213/acc948 kostenfrei https://doaj.org/article/dcf51a7e0b354159aee7d0a31fb70d5d kostenfrei https://doi.org/10.3847/2041-8213/acc948 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 949 2023 2, p L18 |
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10.3847/2041-8213/acc948 doi (DE-627)DOAJ090895851 (DE-599)DOAJdcf51a7e0b354159aee7d0a31fb70d5d DE-627 ger DE-627 rakwb eng QB460-466 Casey Papovich verfasserin aut CEERS Key Paper. V. Galaxies at 4 < z < 9 Are Bluer than They Appear–Characterizing Galaxy Stellar Populations from Rest-frame ∼1 μm Imaging 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present results from the Cosmic Evolution Early Release Survey on the stellar population parameters for 28 galaxies with redshifts 4 < z < 9 using imaging data from the James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) combined with data from the Hubble Space Telescope and the Spitzer Space Telescope. The JWST/MIRI 5.6 and 7.7 μ m data extend the coverage of the rest-frame spectral energy distribution to nearly 1 μ m for galaxies in this redshift range. By modeling the galaxies’ SEDs the MIRI data show that the galaxies have, on average, rest-frame UV (1600 Å)— I -band colors 0.4 mag bluer than derived when using photometry that lacks MIRI. Therefore, the galaxies have lower ratios of stellar mass to light. The MIRI data reduce the stellar masses by $\langle {\rm{\Delta }}\mathrm{log}{M}_{* }\rangle =0.25$ dex at 4 < z < 6 and 0.37 dex at 6 < z < 9. This also reduces the star formation rates (SFRs) by 〈ΔlogSFR〉 = 0.14 dex at 4 < z < 6 and 0.27 dex at 6 < z < 9. The MIRI data also improve constraints on the allowable stellar mass formed in early star formation. We model this using a star formation history that includes both a “burst” at z _f = 100 and a slowly varying (“delayed- τ ”) model. The MIRI data reduce the allowable stellar mass by 0.6 dex at 4 < z < 6 and by ≈1 dex at 6 < z < 9. Applying these results globally, this reduces the cosmic stellar-mass density by an order of magnitude in the early Universe ( z ≈ 9). Therefore, observations of rest-frame ≳1 μ m are paramount for constraining the stellar-mass buildup in galaxies at very high redshifts. Galaxy evolution Galaxy formation Cosmology Galaxy colors Galaxy properties Galaxy masses Astrophysics Justin W. Cole verfasserin aut Guang Yang verfasserin aut Steven L. Finkelstein verfasserin aut Guillermo Barro verfasserin aut Véronique Buat verfasserin aut Denis Burgarella verfasserin aut Pablo G. Pérez-González verfasserin aut Paola Santini verfasserin aut Lise-Marie Seillé verfasserin aut Lu Shen verfasserin aut Pablo Arrabal Haro verfasserin aut Micaela B. Bagley verfasserin aut Eric F. Bell verfasserin aut Laura Bisigello verfasserin aut Antonello Calabrò verfasserin aut Caitlin M. Casey verfasserin aut Marco Castellano verfasserin aut Katherine Chworowsky verfasserin aut Nikko J. Cleri verfasserin aut Luca Costantin verfasserin aut M. C. Cooper verfasserin aut Mark Dickinson verfasserin aut Henry C. Ferguson verfasserin aut Adriano Fontana verfasserin aut Mauro Giavalisco verfasserin aut Andrea Grazian verfasserin aut Norman A. Grogin verfasserin aut Nimish P. Hathi verfasserin aut Benne W. Holwerda verfasserin aut Taylor A. Hutchison verfasserin aut Jeyhan S. Kartaltepe verfasserin aut Lisa J. Kewley verfasserin aut Allison Kirkpatrick verfasserin aut Dale D. Kocevski verfasserin aut Anton M. Koekemoer verfasserin aut Rebecca L. Larson verfasserin aut Arianna S. Long verfasserin aut Ray A. Lucas verfasserin aut Laura Pentericci verfasserin aut Nor Pirzkal verfasserin aut Swara Ravindranath verfasserin aut Rachel S. Somerville verfasserin aut Jonathan R. Trump verfasserin aut Stephanie M. Urbano Stawinski verfasserin aut Benjamin J. Weiner verfasserin aut Stephen M. Wilkins verfasserin aut L. Y. Aaron Yung verfasserin aut Jorge A. Zavala verfasserin aut In The Astrophysical Journal Letters IOP Publishing, 2022 949(2023), 2, p L18 (DE-627)312189028 (DE-600)2006858-X 20418213 nnns volume:949 year:2023 number:2, p L18 https://doi.org/10.3847/2041-8213/acc948 kostenfrei https://doaj.org/article/dcf51a7e0b354159aee7d0a31fb70d5d kostenfrei https://doi.org/10.3847/2041-8213/acc948 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 949 2023 2, p L18 |
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10.3847/2041-8213/acc948 doi (DE-627)DOAJ090895851 (DE-599)DOAJdcf51a7e0b354159aee7d0a31fb70d5d DE-627 ger DE-627 rakwb eng QB460-466 Casey Papovich verfasserin aut CEERS Key Paper. V. Galaxies at 4 < z < 9 Are Bluer than They Appear–Characterizing Galaxy Stellar Populations from Rest-frame ∼1 μm Imaging 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present results from the Cosmic Evolution Early Release Survey on the stellar population parameters for 28 galaxies with redshifts 4 < z < 9 using imaging data from the James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) combined with data from the Hubble Space Telescope and the Spitzer Space Telescope. The JWST/MIRI 5.6 and 7.7 μ m data extend the coverage of the rest-frame spectral energy distribution to nearly 1 μ m for galaxies in this redshift range. By modeling the galaxies’ SEDs the MIRI data show that the galaxies have, on average, rest-frame UV (1600 Å)— I -band colors 0.4 mag bluer than derived when using photometry that lacks MIRI. Therefore, the galaxies have lower ratios of stellar mass to light. The MIRI data reduce the stellar masses by $\langle {\rm{\Delta }}\mathrm{log}{M}_{* }\rangle =0.25$ dex at 4 < z < 6 and 0.37 dex at 6 < z < 9. This also reduces the star formation rates (SFRs) by 〈ΔlogSFR〉 = 0.14 dex at 4 < z < 6 and 0.27 dex at 6 < z < 9. The MIRI data also improve constraints on the allowable stellar mass formed in early star formation. We model this using a star formation history that includes both a “burst” at z _f = 100 and a slowly varying (“delayed- τ ”) model. The MIRI data reduce the allowable stellar mass by 0.6 dex at 4 < z < 6 and by ≈1 dex at 6 < z < 9. Applying these results globally, this reduces the cosmic stellar-mass density by an order of magnitude in the early Universe ( z ≈ 9). Therefore, observations of rest-frame ≳1 μ m are paramount for constraining the stellar-mass buildup in galaxies at very high redshifts. Galaxy evolution Galaxy formation Cosmology Galaxy colors Galaxy properties Galaxy masses Astrophysics Justin W. Cole verfasserin aut Guang Yang verfasserin aut Steven L. Finkelstein verfasserin aut Guillermo Barro verfasserin aut Véronique Buat verfasserin aut Denis Burgarella verfasserin aut Pablo G. Pérez-González verfasserin aut Paola Santini verfasserin aut Lise-Marie Seillé verfasserin aut Lu Shen verfasserin aut Pablo Arrabal Haro verfasserin aut Micaela B. Bagley verfasserin aut Eric F. Bell verfasserin aut Laura Bisigello verfasserin aut Antonello Calabrò verfasserin aut Caitlin M. Casey verfasserin aut Marco Castellano verfasserin aut Katherine Chworowsky verfasserin aut Nikko J. Cleri verfasserin aut Luca Costantin verfasserin aut M. C. Cooper verfasserin aut Mark Dickinson verfasserin aut Henry C. Ferguson verfasserin aut Adriano Fontana verfasserin aut Mauro Giavalisco verfasserin aut Andrea Grazian verfasserin aut Norman A. Grogin verfasserin aut Nimish P. Hathi verfasserin aut Benne W. Holwerda verfasserin aut Taylor A. Hutchison verfasserin aut Jeyhan S. Kartaltepe verfasserin aut Lisa J. Kewley verfasserin aut Allison Kirkpatrick verfasserin aut Dale D. Kocevski verfasserin aut Anton M. Koekemoer verfasserin aut Rebecca L. Larson verfasserin aut Arianna S. Long verfasserin aut Ray A. Lucas verfasserin aut Laura Pentericci verfasserin aut Nor Pirzkal verfasserin aut Swara Ravindranath verfasserin aut Rachel S. Somerville verfasserin aut Jonathan R. Trump verfasserin aut Stephanie M. Urbano Stawinski verfasserin aut Benjamin J. Weiner verfasserin aut Stephen M. Wilkins verfasserin aut L. Y. Aaron Yung verfasserin aut Jorge A. Zavala verfasserin aut In The Astrophysical Journal Letters IOP Publishing, 2022 949(2023), 2, p L18 (DE-627)312189028 (DE-600)2006858-X 20418213 nnns volume:949 year:2023 number:2, p L18 https://doi.org/10.3847/2041-8213/acc948 kostenfrei https://doaj.org/article/dcf51a7e0b354159aee7d0a31fb70d5d kostenfrei https://doi.org/10.3847/2041-8213/acc948 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 949 2023 2, p L18 |
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10.3847/2041-8213/acc948 doi (DE-627)DOAJ090895851 (DE-599)DOAJdcf51a7e0b354159aee7d0a31fb70d5d DE-627 ger DE-627 rakwb eng QB460-466 Casey Papovich verfasserin aut CEERS Key Paper. V. Galaxies at 4 < z < 9 Are Bluer than They Appear–Characterizing Galaxy Stellar Populations from Rest-frame ∼1 μm Imaging 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present results from the Cosmic Evolution Early Release Survey on the stellar population parameters for 28 galaxies with redshifts 4 < z < 9 using imaging data from the James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) combined with data from the Hubble Space Telescope and the Spitzer Space Telescope. The JWST/MIRI 5.6 and 7.7 μ m data extend the coverage of the rest-frame spectral energy distribution to nearly 1 μ m for galaxies in this redshift range. By modeling the galaxies’ SEDs the MIRI data show that the galaxies have, on average, rest-frame UV (1600 Å)— I -band colors 0.4 mag bluer than derived when using photometry that lacks MIRI. Therefore, the galaxies have lower ratios of stellar mass to light. The MIRI data reduce the stellar masses by $\langle {\rm{\Delta }}\mathrm{log}{M}_{* }\rangle =0.25$ dex at 4 < z < 6 and 0.37 dex at 6 < z < 9. This also reduces the star formation rates (SFRs) by 〈ΔlogSFR〉 = 0.14 dex at 4 < z < 6 and 0.27 dex at 6 < z < 9. The MIRI data also improve constraints on the allowable stellar mass formed in early star formation. We model this using a star formation history that includes both a “burst” at z _f = 100 and a slowly varying (“delayed- τ ”) model. The MIRI data reduce the allowable stellar mass by 0.6 dex at 4 < z < 6 and by ≈1 dex at 6 < z < 9. Applying these results globally, this reduces the cosmic stellar-mass density by an order of magnitude in the early Universe ( z ≈ 9). Therefore, observations of rest-frame ≳1 μ m are paramount for constraining the stellar-mass buildup in galaxies at very high redshifts. Galaxy evolution Galaxy formation Cosmology Galaxy colors Galaxy properties Galaxy masses Astrophysics Justin W. Cole verfasserin aut Guang Yang verfasserin aut Steven L. Finkelstein verfasserin aut Guillermo Barro verfasserin aut Véronique Buat verfasserin aut Denis Burgarella verfasserin aut Pablo G. Pérez-González verfasserin aut Paola Santini verfasserin aut Lise-Marie Seillé verfasserin aut Lu Shen verfasserin aut Pablo Arrabal Haro verfasserin aut Micaela B. Bagley verfasserin aut Eric F. Bell verfasserin aut Laura Bisigello verfasserin aut Antonello Calabrò verfasserin aut Caitlin M. Casey verfasserin aut Marco Castellano verfasserin aut Katherine Chworowsky verfasserin aut Nikko J. Cleri verfasserin aut Luca Costantin verfasserin aut M. C. Cooper verfasserin aut Mark Dickinson verfasserin aut Henry C. Ferguson verfasserin aut Adriano Fontana verfasserin aut Mauro Giavalisco verfasserin aut Andrea Grazian verfasserin aut Norman A. Grogin verfasserin aut Nimish P. Hathi verfasserin aut Benne W. Holwerda verfasserin aut Taylor A. Hutchison verfasserin aut Jeyhan S. Kartaltepe verfasserin aut Lisa J. Kewley verfasserin aut Allison Kirkpatrick verfasserin aut Dale D. Kocevski verfasserin aut Anton M. Koekemoer verfasserin aut Rebecca L. Larson verfasserin aut Arianna S. Long verfasserin aut Ray A. Lucas verfasserin aut Laura Pentericci verfasserin aut Nor Pirzkal verfasserin aut Swara Ravindranath verfasserin aut Rachel S. Somerville verfasserin aut Jonathan R. Trump verfasserin aut Stephanie M. Urbano Stawinski verfasserin aut Benjamin J. Weiner verfasserin aut Stephen M. Wilkins verfasserin aut L. Y. Aaron Yung verfasserin aut Jorge A. Zavala verfasserin aut In The Astrophysical Journal Letters IOP Publishing, 2022 949(2023), 2, p L18 (DE-627)312189028 (DE-600)2006858-X 20418213 nnns volume:949 year:2023 number:2, p L18 https://doi.org/10.3847/2041-8213/acc948 kostenfrei https://doaj.org/article/dcf51a7e0b354159aee7d0a31fb70d5d kostenfrei https://doi.org/10.3847/2041-8213/acc948 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 949 2023 2, p L18 |
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10.3847/2041-8213/acc948 doi (DE-627)DOAJ090895851 (DE-599)DOAJdcf51a7e0b354159aee7d0a31fb70d5d DE-627 ger DE-627 rakwb eng QB460-466 Casey Papovich verfasserin aut CEERS Key Paper. V. Galaxies at 4 < z < 9 Are Bluer than They Appear–Characterizing Galaxy Stellar Populations from Rest-frame ∼1 μm Imaging 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present results from the Cosmic Evolution Early Release Survey on the stellar population parameters for 28 galaxies with redshifts 4 < z < 9 using imaging data from the James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) combined with data from the Hubble Space Telescope and the Spitzer Space Telescope. The JWST/MIRI 5.6 and 7.7 μ m data extend the coverage of the rest-frame spectral energy distribution to nearly 1 μ m for galaxies in this redshift range. By modeling the galaxies’ SEDs the MIRI data show that the galaxies have, on average, rest-frame UV (1600 Å)— I -band colors 0.4 mag bluer than derived when using photometry that lacks MIRI. Therefore, the galaxies have lower ratios of stellar mass to light. The MIRI data reduce the stellar masses by $\langle {\rm{\Delta }}\mathrm{log}{M}_{* }\rangle =0.25$ dex at 4 < z < 6 and 0.37 dex at 6 < z < 9. This also reduces the star formation rates (SFRs) by 〈ΔlogSFR〉 = 0.14 dex at 4 < z < 6 and 0.27 dex at 6 < z < 9. The MIRI data also improve constraints on the allowable stellar mass formed in early star formation. We model this using a star formation history that includes both a “burst” at z _f = 100 and a slowly varying (“delayed- τ ”) model. The MIRI data reduce the allowable stellar mass by 0.6 dex at 4 < z < 6 and by ≈1 dex at 6 < z < 9. Applying these results globally, this reduces the cosmic stellar-mass density by an order of magnitude in the early Universe ( z ≈ 9). Therefore, observations of rest-frame ≳1 μ m are paramount for constraining the stellar-mass buildup in galaxies at very high redshifts. Galaxy evolution Galaxy formation Cosmology Galaxy colors Galaxy properties Galaxy masses Astrophysics Justin W. Cole verfasserin aut Guang Yang verfasserin aut Steven L. Finkelstein verfasserin aut Guillermo Barro verfasserin aut Véronique Buat verfasserin aut Denis Burgarella verfasserin aut Pablo G. Pérez-González verfasserin aut Paola Santini verfasserin aut Lise-Marie Seillé verfasserin aut Lu Shen verfasserin aut Pablo Arrabal Haro verfasserin aut Micaela B. Bagley verfasserin aut Eric F. Bell verfasserin aut Laura Bisigello verfasserin aut Antonello Calabrò verfasserin aut Caitlin M. Casey verfasserin aut Marco Castellano verfasserin aut Katherine Chworowsky verfasserin aut Nikko J. Cleri verfasserin aut Luca Costantin verfasserin aut M. C. Cooper verfasserin aut Mark Dickinson verfasserin aut Henry C. Ferguson verfasserin aut Adriano Fontana verfasserin aut Mauro Giavalisco verfasserin aut Andrea Grazian verfasserin aut Norman A. Grogin verfasserin aut Nimish P. Hathi verfasserin aut Benne W. Holwerda verfasserin aut Taylor A. Hutchison verfasserin aut Jeyhan S. Kartaltepe verfasserin aut Lisa J. Kewley verfasserin aut Allison Kirkpatrick verfasserin aut Dale D. Kocevski verfasserin aut Anton M. Koekemoer verfasserin aut Rebecca L. Larson verfasserin aut Arianna S. Long verfasserin aut Ray A. Lucas verfasserin aut Laura Pentericci verfasserin aut Nor Pirzkal verfasserin aut Swara Ravindranath verfasserin aut Rachel S. Somerville verfasserin aut Jonathan R. Trump verfasserin aut Stephanie M. Urbano Stawinski verfasserin aut Benjamin J. Weiner verfasserin aut Stephen M. Wilkins verfasserin aut L. Y. Aaron Yung verfasserin aut Jorge A. Zavala verfasserin aut In The Astrophysical Journal Letters IOP Publishing, 2022 949(2023), 2, p L18 (DE-627)312189028 (DE-600)2006858-X 20418213 nnns volume:949 year:2023 number:2, p L18 https://doi.org/10.3847/2041-8213/acc948 kostenfrei https://doaj.org/article/dcf51a7e0b354159aee7d0a31fb70d5d kostenfrei https://doi.org/10.3847/2041-8213/acc948 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 949 2023 2, p L18 |
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Casey Papovich @@aut@@ Justin W. Cole @@aut@@ Guang Yang @@aut@@ Steven L. Finkelstein @@aut@@ Guillermo Barro @@aut@@ Véronique Buat @@aut@@ Denis Burgarella @@aut@@ Pablo G. Pérez-González @@aut@@ Paola Santini @@aut@@ Lise-Marie Seillé @@aut@@ Lu Shen @@aut@@ Pablo Arrabal Haro @@aut@@ Micaela B. Bagley @@aut@@ Eric F. Bell @@aut@@ Laura Bisigello @@aut@@ Antonello Calabrò @@aut@@ Caitlin M. Casey @@aut@@ Marco Castellano @@aut@@ Katherine Chworowsky @@aut@@ Nikko J. Cleri @@aut@@ Luca Costantin @@aut@@ M. C. Cooper @@aut@@ Mark Dickinson @@aut@@ Henry C. Ferguson @@aut@@ Adriano Fontana @@aut@@ Mauro Giavalisco @@aut@@ Andrea Grazian @@aut@@ Norman A. Grogin @@aut@@ Nimish P. Hathi @@aut@@ Benne W. Holwerda @@aut@@ Taylor A. Hutchison @@aut@@ Jeyhan S. Kartaltepe @@aut@@ Lisa J. Kewley @@aut@@ Allison Kirkpatrick @@aut@@ Dale D. Kocevski @@aut@@ Anton M. Koekemoer @@aut@@ Rebecca L. Larson @@aut@@ Arianna S. Long @@aut@@ Ray A. Lucas @@aut@@ Laura Pentericci @@aut@@ Nor Pirzkal @@aut@@ Swara Ravindranath @@aut@@ Rachel S. Somerville @@aut@@ Jonathan R. Trump @@aut@@ Stephanie M. Urbano Stawinski @@aut@@ Benjamin J. Weiner @@aut@@ Stephen M. Wilkins @@aut@@ L. Y. Aaron Yung @@aut@@ Jorge A. Zavala @@aut@@ |
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Galaxies at 4 < z < 9 Are Bluer than They Appear–Characterizing Galaxy Stellar Populations from Rest-frame ∼1 μm Imaging</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2023</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">Computermedien</subfield><subfield code="b">c</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Online-Ressource</subfield><subfield code="b">cr</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">We present results from the Cosmic Evolution Early Release Survey on the stellar population parameters for 28 galaxies with redshifts 4 < z < 9 using imaging data from the James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) combined with data from the Hubble Space Telescope and the Spitzer Space Telescope. The JWST/MIRI 5.6 and 7.7 μ m data extend the coverage of the rest-frame spectral energy distribution to nearly 1 μ m for galaxies in this redshift range. By modeling the galaxies’ SEDs the MIRI data show that the galaxies have, on average, rest-frame UV (1600 Å)— I -band colors 0.4 mag bluer than derived when using photometry that lacks MIRI. Therefore, the galaxies have lower ratios of stellar mass to light. The MIRI data reduce the stellar masses by $\langle {\rm{\Delta }}\mathrm{log}{M}_{* }\rangle =0.25$ dex at 4 < z < 6 and 0.37 dex at 6 < z < 9. This also reduces the star formation rates (SFRs) by 〈ΔlogSFR〉 = 0.14 dex at 4 < z < 6 and 0.27 dex at 6 < z < 9. The MIRI data also improve constraints on the allowable stellar mass formed in early star formation. We model this using a star formation history that includes both a “burst” at z _f = 100 and a slowly varying (“delayed- τ ”) model. The MIRI data reduce the allowable stellar mass by 0.6 dex at 4 < z < 6 and by ≈1 dex at 6 < z < 9. Applying these results globally, this reduces the cosmic stellar-mass density by an order of magnitude in the early Universe ( z ≈ 9). 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Casey Papovich Justin W. Cole Guang Yang Steven L. Finkelstein Guillermo Barro Véronique Buat Denis Burgarella Pablo G. Pérez-González Paola Santini Lise-Marie Seillé Lu Shen Pablo Arrabal Haro Micaela B. Bagley Eric F. Bell Laura Bisigello Antonello Calabrò Caitlin M. Casey Marco Castellano Katherine Chworowsky Nikko J. Cleri Luca Costantin M. C. Cooper Mark Dickinson Henry C. Ferguson Adriano Fontana Mauro Giavalisco Andrea Grazian Norman A. Grogin Nimish P. Hathi Benne W. Holwerda Taylor A. Hutchison Jeyhan S. Kartaltepe Lisa J. Kewley Allison Kirkpatrick Dale D. Kocevski Anton M. Koekemoer Rebecca L. Larson Arianna S. Long Ray A. Lucas Laura Pentericci Nor Pirzkal Swara Ravindranath Rachel S. Somerville Jonathan R. Trump Stephanie M. Urbano Stawinski Benjamin J. Weiner Stephen M. Wilkins L. Y. Aaron Yung Jorge A. Zavala |
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ceers key paper. v. galaxies at 4 < z < 9 are bluer than they appear–characterizing galaxy stellar populations from rest-frame ∼1 μm imaging |
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CEERS Key Paper. V. Galaxies at 4 < z < 9 Are Bluer than They Appear–Characterizing Galaxy Stellar Populations from Rest-frame ∼1 μm Imaging |
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We present results from the Cosmic Evolution Early Release Survey on the stellar population parameters for 28 galaxies with redshifts 4 < z < 9 using imaging data from the James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) combined with data from the Hubble Space Telescope and the Spitzer Space Telescope. The JWST/MIRI 5.6 and 7.7 μ m data extend the coverage of the rest-frame spectral energy distribution to nearly 1 μ m for galaxies in this redshift range. By modeling the galaxies’ SEDs the MIRI data show that the galaxies have, on average, rest-frame UV (1600 Å)— I -band colors 0.4 mag bluer than derived when using photometry that lacks MIRI. Therefore, the galaxies have lower ratios of stellar mass to light. The MIRI data reduce the stellar masses by $\langle {\rm{\Delta }}\mathrm{log}{M}_{* }\rangle =0.25$ dex at 4 < z < 6 and 0.37 dex at 6 < z < 9. This also reduces the star formation rates (SFRs) by 〈ΔlogSFR〉 = 0.14 dex at 4 < z < 6 and 0.27 dex at 6 < z < 9. The MIRI data also improve constraints on the allowable stellar mass formed in early star formation. We model this using a star formation history that includes both a “burst” at z _f = 100 and a slowly varying (“delayed- τ ”) model. The MIRI data reduce the allowable stellar mass by 0.6 dex at 4 < z < 6 and by ≈1 dex at 6 < z < 9. Applying these results globally, this reduces the cosmic stellar-mass density by an order of magnitude in the early Universe ( z ≈ 9). Therefore, observations of rest-frame ≳1 μ m are paramount for constraining the stellar-mass buildup in galaxies at very high redshifts. |
| abstractGer |
We present results from the Cosmic Evolution Early Release Survey on the stellar population parameters for 28 galaxies with redshifts 4 < z < 9 using imaging data from the James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) combined with data from the Hubble Space Telescope and the Spitzer Space Telescope. The JWST/MIRI 5.6 and 7.7 μ m data extend the coverage of the rest-frame spectral energy distribution to nearly 1 μ m for galaxies in this redshift range. By modeling the galaxies’ SEDs the MIRI data show that the galaxies have, on average, rest-frame UV (1600 Å)— I -band colors 0.4 mag bluer than derived when using photometry that lacks MIRI. Therefore, the galaxies have lower ratios of stellar mass to light. The MIRI data reduce the stellar masses by $\langle {\rm{\Delta }}\mathrm{log}{M}_{* }\rangle =0.25$ dex at 4 < z < 6 and 0.37 dex at 6 < z < 9. This also reduces the star formation rates (SFRs) by 〈ΔlogSFR〉 = 0.14 dex at 4 < z < 6 and 0.27 dex at 6 < z < 9. The MIRI data also improve constraints on the allowable stellar mass formed in early star formation. We model this using a star formation history that includes both a “burst” at z _f = 100 and a slowly varying (“delayed- τ ”) model. The MIRI data reduce the allowable stellar mass by 0.6 dex at 4 < z < 6 and by ≈1 dex at 6 < z < 9. Applying these results globally, this reduces the cosmic stellar-mass density by an order of magnitude in the early Universe ( z ≈ 9). Therefore, observations of rest-frame ≳1 μ m are paramount for constraining the stellar-mass buildup in galaxies at very high redshifts. |
| abstract_unstemmed |
We present results from the Cosmic Evolution Early Release Survey on the stellar population parameters for 28 galaxies with redshifts 4 < z < 9 using imaging data from the James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) combined with data from the Hubble Space Telescope and the Spitzer Space Telescope. The JWST/MIRI 5.6 and 7.7 μ m data extend the coverage of the rest-frame spectral energy distribution to nearly 1 μ m for galaxies in this redshift range. By modeling the galaxies’ SEDs the MIRI data show that the galaxies have, on average, rest-frame UV (1600 Å)— I -band colors 0.4 mag bluer than derived when using photometry that lacks MIRI. Therefore, the galaxies have lower ratios of stellar mass to light. The MIRI data reduce the stellar masses by $\langle {\rm{\Delta }}\mathrm{log}{M}_{* }\rangle =0.25$ dex at 4 < z < 6 and 0.37 dex at 6 < z < 9. This also reduces the star formation rates (SFRs) by 〈ΔlogSFR〉 = 0.14 dex at 4 < z < 6 and 0.27 dex at 6 < z < 9. The MIRI data also improve constraints on the allowable stellar mass formed in early star formation. We model this using a star formation history that includes both a “burst” at z _f = 100 and a slowly varying (“delayed- τ ”) model. The MIRI data reduce the allowable stellar mass by 0.6 dex at 4 < z < 6 and by ≈1 dex at 6 < z < 9. Applying these results globally, this reduces the cosmic stellar-mass density by an order of magnitude in the early Universe ( z ≈ 9). Therefore, observations of rest-frame ≳1 μ m are paramount for constraining the stellar-mass buildup in galaxies at very high redshifts. |
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| title_short |
CEERS Key Paper. V. Galaxies at 4 < z < 9 Are Bluer than They Appear–Characterizing Galaxy Stellar Populations from Rest-frame ∼1 μm Imaging |
| url |
https://doi.org/10.3847/2041-8213/acc948 https://doaj.org/article/dcf51a7e0b354159aee7d0a31fb70d5d https://doaj.org/toc/2041-8205 |
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Justin W. Cole Guang Yang Steven L. Finkelstein Guillermo Barro Véronique Buat Denis Burgarella Pablo G. Pérez-González Paola Santini Lise-Marie Seillé Lu Shen Pablo Arrabal Haro Micaela B. Bagley Eric F. Bell Laura Bisigello Antonello Calabrò Caitlin M. Casey Marco Castellano Katherine Chworowsky Nikko J. Cleri Luca Costantin M. C. Cooper Mark Dickinson Henry C. Ferguson Adriano Fontana Mauro Giavalisco Andrea Grazian Norman A. Grogin Nimish P. Hathi Benne W. Holwerda Taylor A. Hutchison Jeyhan S. Kartaltepe Lisa J. Kewley Allison Kirkpatrick Dale D. Kocevski Anton M. Koekemoer Rebecca L. Larson Arianna S. Long Ray A. Lucas Laura Pentericci Nor Pirzkal Swara Ravindranath Rachel S. Somerville Jonathan R. Trump Stephanie M. Urbano Stawinski Benjamin J. Weiner Stephen M. Wilkins L. Y. Aaron Yung Jorge A. Zavala |
| author2Str |
Justin W. Cole Guang Yang Steven L. Finkelstein Guillermo Barro Véronique Buat Denis Burgarella Pablo G. Pérez-González Paola Santini Lise-Marie Seillé Lu Shen Pablo Arrabal Haro Micaela B. Bagley Eric F. Bell Laura Bisigello Antonello Calabrò Caitlin M. Casey Marco Castellano Katherine Chworowsky Nikko J. Cleri Luca Costantin M. C. Cooper Mark Dickinson Henry C. Ferguson Adriano Fontana Mauro Giavalisco Andrea Grazian Norman A. Grogin Nimish P. Hathi Benne W. Holwerda Taylor A. Hutchison Jeyhan S. Kartaltepe Lisa J. Kewley Allison Kirkpatrick Dale D. Kocevski Anton M. Koekemoer Rebecca L. Larson Arianna S. Long Ray A. Lucas Laura Pentericci Nor Pirzkal Swara Ravindranath Rachel S. Somerville Jonathan R. Trump Stephanie M. Urbano Stawinski Benjamin J. Weiner Stephen M. Wilkins L. Y. Aaron Yung Jorge A. Zavala |
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| doi_str |
10.3847/2041-8213/acc948 |
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2024-07-03T17:14:27.895Z |
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| score |
7.400613 |