CEERS Key Paper. II. A First Look at the Resolved Host Properties of AGN at 3 < z < 5 with JWST
We report on the host properties of five X-ray-luminous active galactic nuclei (AGN) identified at 3 < z < 5 in the first epoch of imaging from the Cosmic Evolution Early Release Science Survey. Each galaxy has been imaged with the JWST Near-Infrared Camera, which provides rest-frame optical m...
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| Veröffentlicht in: | Astrophysical journal. Letters 2023-03, Vol.946 (1), p.L14 |
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| creator | Kocevski, Dale D. Barro, Guillermo McGrath, Elizabeth J. Finkelstein, Steven L. Bagley, Micaela B. Ferguson, Henry C. Jogee, Shardha Yang, Guang Dickinson, Mark Hathi, Nimish P. Backhaus, Bren E. Bell, Eric F. Bisigello, Laura Buat, Véronique Burgarella, Denis Casey, Caitlin M. Cleri, Nikko J. Cooper, M. C. Costantin, Luca Croton, Darren Daddi, Emanuele Fontana, Adriano Fujimoto, Seiji Gardner, Jonathan P. Gawiser, Eric Giavalisco, Mauro Grazian, Andrea Grogin, Norman A. Guo, Yuchen Arrabal Haro, Pablo Hirschmann, Michaela Holwerda, Benne W. Huertas-Company, Marc Hutchison, Taylor A. Iyer, Kartheik G. Jones, Brenda Juneau, Stéphanie Kartaltepe, Jeyhan S. Kewley, Lisa J. Kirkpatrick, Allison Koekemoer, Anton M. Kurczynski, Peter Bail, Aurélien Le Long, Arianna S. Lotz, Jennifer M. Lucas, Ray A. Papovich, Casey Pentericci, Laura Pérez-González, Pablo G. Pirzkal, Nor Rafelski, Marc Ravindranath, Swara Somerville, Rachel S. Straughn, Amber N. Tacchella, Sandro Trump, Jonathan R. Wilkins, Stephen M. Wuyts, Stijn Yung, L. Y. Aaron Zavala, Jorge A. |
| description | We report on the host properties of five X-ray-luminous active galactic nuclei (AGN) identified at 3 <
z
< 5 in the first epoch of imaging from the Cosmic Evolution Early Release Science Survey. Each galaxy has been imaged with the JWST Near-Infrared Camera, which provides rest-frame optical morphologies at these redshifts. We also derive stellar masses and star formation rates for each host by fitting its spectral energy distribution using a combination of galaxy and AGN templates. We find that three of the AGN hosts have spheroidal morphologies, one is a bulge-dominated disk, and one is dominated by pointlike emission. None are found to show strong morphological disturbances that might indicate a recent interaction or merger event. When compared to a sample of mass-matched inactive galaxies, we find that the AGN hosts have morphologies that are less disturbed and more bulge-dominated. Notably, all four of the resolved hosts have rest-frame optical colors consistent with a quenched or poststarburst stellar population. The presence of AGN in passively evolving galaxies at
z
> 3 is significant because a rapid feedback mechanism is required in most semianalytic models and cosmological simulations to explain the growing population of massive quiescent galaxies observed at these redshifts. Our findings show that AGN can continue to inject energy into these systems after their star formation is curtailed, potentially heating their halos and preventing renewed star formation. Additional observations will be needed to determine what role this feedback may play in helping to quench these systems and/or maintain their quiescent state. |
| doi_str_mv | 10.3847/2041-8213/acad00 |
| format | Article |
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z
< 5 in the first epoch of imaging from the Cosmic Evolution Early Release Science Survey. Each galaxy has been imaged with the JWST Near-Infrared Camera, which provides rest-frame optical morphologies at these redshifts. We also derive stellar masses and star formation rates for each host by fitting its spectral energy distribution using a combination of galaxy and AGN templates. We find that three of the AGN hosts have spheroidal morphologies, one is a bulge-dominated disk, and one is dominated by pointlike emission. None are found to show strong morphological disturbances that might indicate a recent interaction or merger event. When compared to a sample of mass-matched inactive galaxies, we find that the AGN hosts have morphologies that are less disturbed and more bulge-dominated. Notably, all four of the resolved hosts have rest-frame optical colors consistent with a quenched or poststarburst stellar population. The presence of AGN in passively evolving galaxies at
z
> 3 is significant because a rapid feedback mechanism is required in most semianalytic models and cosmological simulations to explain the growing population of massive quiescent galaxies observed at these redshifts. Our findings show that AGN can continue to inject energy into these systems after their star formation is curtailed, potentially heating their halos and preventing renewed star formation. Additional observations will be needed to determine what role this feedback may play in helping to quench these systems and/or maintain their quiescent state.</description><identifier>ISSN: 2041-8205</identifier><identifier>EISSN: 2041-8213</identifier><identifier>DOI: 10.3847/2041-8213/acad00</identifier><language>eng</language><publisher>Austin: The American Astronomical Society</publisher><subject>Active galactic nuclei ; AGN host galaxies ; Astronomical models ; Feedback ; Galactic evolution ; Galaxies ; Galaxy distribution ; Halos ; Infrared cameras ; Morphology ; Sciences of the Universe ; Spectral energy distribution ; Star & galaxy formation ; Star formation ; Stars ; Stars & galaxies ; Supermassive black holes</subject><ispartof>Astrophysical journal. Letters, 2023-03, Vol.946 (1), p.L14</ispartof><rights>2023. The Author(s). Published by the American Astronomical Society.</rights><rights>2023. The Author(s). Published by the American Astronomical Society. 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Y. Aaron</creatorcontrib><creatorcontrib>Zavala, Jorge A.</creatorcontrib><title>CEERS Key Paper. II. A First Look at the Resolved Host Properties of AGN at 3 < z < 5 with JWST</title><title>Astrophysical journal. Letters</title><addtitle>APJL</addtitle><addtitle>Astrophys. J. Lett</addtitle><description>We report on the host properties of five X-ray-luminous active galactic nuclei (AGN) identified at 3 <
z
< 5 in the first epoch of imaging from the Cosmic Evolution Early Release Science Survey. Each galaxy has been imaged with the JWST Near-Infrared Camera, which provides rest-frame optical morphologies at these redshifts. We also derive stellar masses and star formation rates for each host by fitting its spectral energy distribution using a combination of galaxy and AGN templates. We find that three of the AGN hosts have spheroidal morphologies, one is a bulge-dominated disk, and one is dominated by pointlike emission. None are found to show strong morphological disturbances that might indicate a recent interaction or merger event. When compared to a sample of mass-matched inactive galaxies, we find that the AGN hosts have morphologies that are less disturbed and more bulge-dominated. Notably, all four of the resolved hosts have rest-frame optical colors consistent with a quenched or poststarburst stellar population. The presence of AGN in passively evolving galaxies at
z
> 3 is significant because a rapid feedback mechanism is required in most semianalytic models and cosmological simulations to explain the growing population of massive quiescent galaxies observed at these redshifts. Our findings show that AGN can continue to inject energy into these systems after their star formation is curtailed, potentially heating their halos and preventing renewed star formation. Additional observations will be needed to determine what role this feedback may play in helping to quench these systems and/or maintain their quiescent state.</description><subject>Active galactic nuclei</subject><subject>AGN host galaxies</subject><subject>Astronomical models</subject><subject>Feedback</subject><subject>Galactic evolution</subject><subject>Galaxies</subject><subject>Galaxy distribution</subject><subject>Halos</subject><subject>Infrared cameras</subject><subject>Morphology</subject><subject>Sciences of the Universe</subject><subject>Spectral energy distribution</subject><subject>Star & galaxy formation</subject><subject>Star formation</subject><subject>Stars</subject><subject>Stars & galaxies</subject><subject>Supermassive black holes</subject><issn>2041-8205</issn><issn>2041-8213</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2023</creationdate><recordtype>article</recordtype><sourceid>O3W</sourceid><sourceid>DOA</sourceid><recordid>eNp9kduLEzEUhwdRcK2--xgQfBDbzW1yAV9K6W6rgy67BR8PaS526riZTaYr619v6khFEB9Cwsl3vpPwq6qXBM-Y4vKcYk6mihJ2bqxxGD-qzk6lx6czrp9Wz3LeY0yxIOqsgsVyeX2DPvgHdGV6n2ZovZ6hObpoUx5QE-NXZAY07Dy69jl2996hVSw3VykWemh9RjGg-eXHI8bQO_SjrBp9b4cdev_5ZvO8ehJMl_2L3_uk2lwsN4vVtPl0uV7Mm6nlig7TrSJBKC-CVU7o4LTmXhlZM7sNtcdGSmsU16xwXHEbgiNmKxUzlkpaWzap1qPWRbOHPrXfTHqAaFr4VYjpC5jyWtt5kLU0giq79YFy4WvlpHeaEU21cKLMmFRvRtfOdH-pVvMG2tt8AMy51Fire1LgVyPcp3h38HmAfTyk2_JVoFITUYSqLhQeKZtizsmHk5dgOMYHx3zgmBWM8ZWWt2NLG_s_zv_gr_-Bm37fgeYCCDSEQ-8C-wlz9aNK</recordid><startdate>20230301</startdate><enddate>20230301</enddate><creator>Kocevski, Dale D.</creator><creator>Barro, Guillermo</creator><creator>McGrath, Elizabeth J.</creator><creator>Finkelstein, Steven L.</creator><creator>Bagley, Micaela B.</creator><creator>Ferguson, Henry C.</creator><creator>Jogee, Shardha</creator><creator>Yang, Guang</creator><creator>Dickinson, Mark</creator><creator>Hathi, Nimish P.</creator><creator>Backhaus, Bren E.</creator><creator>Bell, Eric F.</creator><creator>Bisigello, Laura</creator><creator>Buat, Véronique</creator><creator>Burgarella, Denis</creator><creator>Casey, Caitlin M.</creator><creator>Cleri, Nikko J.</creator><creator>Cooper, M. 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II. A First Look at the Resolved Host Properties of AGN at 3 < z < 5 with JWST</title><author>Kocevski, Dale D. ; Barro, Guillermo ; McGrath, Elizabeth J. ; Finkelstein, Steven L. ; Bagley, Micaela B. ; Ferguson, Henry C. ; Jogee, Shardha ; Yang, Guang ; Dickinson, Mark ; Hathi, Nimish P. ; Backhaus, Bren E. ; Bell, Eric F. ; Bisigello, Laura ; Buat, Véronique ; Burgarella, Denis ; Casey, Caitlin M. ; Cleri, Nikko J. ; Cooper, M. C. ; Costantin, Luca ; Croton, Darren ; Daddi, Emanuele ; Fontana, Adriano ; Fujimoto, Seiji ; Gardner, Jonathan P. ; Gawiser, Eric ; Giavalisco, Mauro ; Grazian, Andrea ; Grogin, Norman A. ; Guo, Yuchen ; Arrabal Haro, Pablo ; Hirschmann, Michaela ; Holwerda, Benne W. ; Huertas-Company, Marc ; Hutchison, Taylor A. ; Iyer, Kartheik G. ; Jones, Brenda ; Juneau, Stéphanie ; Kartaltepe, Jeyhan S. ; Kewley, Lisa J. ; Kirkpatrick, Allison ; Koekemoer, Anton M. ; Kurczynski, Peter ; Bail, Aurélien Le ; Long, Arianna S. ; Lotz, Jennifer M. ; Lucas, Ray A. ; Papovich, Casey ; Pentericci, Laura ; Pérez-González, Pablo G. ; Pirzkal, Nor ; Rafelski, Marc ; Ravindranath, Swara ; Somerville, Rachel S. ; Straughn, Amber N. ; Tacchella, Sandro ; Trump, Jonathan R. ; Wilkins, Stephen M. ; Wuyts, Stijn ; Yung, L. Y. Aaron ; Zavala, Jorge A.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c482t-b81f68e6fc8d69fd994e8a753cbf5e0a77ca8493b81484cffd1ab783ac2725c3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2023</creationdate><topic>Active galactic nuclei</topic><topic>AGN host galaxies</topic><topic>Astronomical models</topic><topic>Feedback</topic><topic>Galactic evolution</topic><topic>Galaxies</topic><topic>Galaxy distribution</topic><topic>Halos</topic><topic>Infrared cameras</topic><topic>Morphology</topic><topic>Sciences of the Universe</topic><topic>Spectral energy distribution</topic><topic>Star & galaxy formation</topic><topic>Star formation</topic><topic>Stars</topic><topic>Stars & galaxies</topic><topic>Supermassive black holes</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Kocevski, Dale D.</creatorcontrib><creatorcontrib>Barro, Guillermo</creatorcontrib><creatorcontrib>McGrath, Elizabeth J.</creatorcontrib><creatorcontrib>Finkelstein, Steven L.</creatorcontrib><creatorcontrib>Bagley, Micaela B.</creatorcontrib><creatorcontrib>Ferguson, Henry C.</creatorcontrib><creatorcontrib>Jogee, Shardha</creatorcontrib><creatorcontrib>Yang, Guang</creatorcontrib><creatorcontrib>Dickinson, Mark</creatorcontrib><creatorcontrib>Hathi, Nimish P.</creatorcontrib><creatorcontrib>Backhaus, Bren E.</creatorcontrib><creatorcontrib>Bell, Eric F.</creatorcontrib><creatorcontrib>Bisigello, Laura</creatorcontrib><creatorcontrib>Buat, Véronique</creatorcontrib><creatorcontrib>Burgarella, Denis</creatorcontrib><creatorcontrib>Casey, Caitlin M.</creatorcontrib><creatorcontrib>Cleri, Nikko J.</creatorcontrib><creatorcontrib>Cooper, M. 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Y. Aaron</creatorcontrib><creatorcontrib>Zavala, Jorge A.</creatorcontrib><collection>Institute of Physics Open Access Journal Titles</collection><collection>IOPscience (Open Access)</collection><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Hyper Article en Ligne (HAL)</collection><collection>Hyper Article en Ligne (HAL) (Open Access)</collection><collection>Directory of Open Access Journals</collection><jtitle>Astrophysical journal. Letters</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Kocevski, Dale D.</au><au>Barro, Guillermo</au><au>McGrath, Elizabeth J.</au><au>Finkelstein, Steven L.</au><au>Bagley, Micaela B.</au><au>Ferguson, Henry C.</au><au>Jogee, Shardha</au><au>Yang, Guang</au><au>Dickinson, Mark</au><au>Hathi, Nimish P.</au><au>Backhaus, Bren E.</au><au>Bell, Eric F.</au><au>Bisigello, Laura</au><au>Buat, Véronique</au><au>Burgarella, Denis</au><au>Casey, Caitlin M.</au><au>Cleri, Nikko J.</au><au>Cooper, M. C.</au><au>Costantin, Luca</au><au>Croton, Darren</au><au>Daddi, Emanuele</au><au>Fontana, Adriano</au><au>Fujimoto, Seiji</au><au>Gardner, Jonathan P.</au><au>Gawiser, Eric</au><au>Giavalisco, Mauro</au><au>Grazian, Andrea</au><au>Grogin, Norman A.</au><au>Guo, Yuchen</au><au>Arrabal Haro, Pablo</au><au>Hirschmann, Michaela</au><au>Holwerda, Benne W.</au><au>Huertas-Company, Marc</au><au>Hutchison, Taylor A.</au><au>Iyer, Kartheik G.</au><au>Jones, Brenda</au><au>Juneau, Stéphanie</au><au>Kartaltepe, Jeyhan S.</au><au>Kewley, Lisa J.</au><au>Kirkpatrick, Allison</au><au>Koekemoer, Anton M.</au><au>Kurczynski, Peter</au><au>Bail, Aurélien Le</au><au>Long, Arianna S.</au><au>Lotz, Jennifer M.</au><au>Lucas, Ray A.</au><au>Papovich, Casey</au><au>Pentericci, Laura</au><au>Pérez-González, Pablo G.</au><au>Pirzkal, Nor</au><au>Rafelski, Marc</au><au>Ravindranath, Swara</au><au>Somerville, Rachel S.</au><au>Straughn, Amber N.</au><au>Tacchella, Sandro</au><au>Trump, Jonathan R.</au><au>Wilkins, Stephen M.</au><au>Wuyts, Stijn</au><au>Yung, L. Y. Aaron</au><au>Zavala, Jorge A.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>CEERS Key Paper. II. A First Look at the Resolved Host Properties of AGN at 3 < z < 5 with JWST</atitle><jtitle>Astrophysical journal. Letters</jtitle><stitle>APJL</stitle><addtitle>Astrophys. J. Lett</addtitle><date>2023-03-01</date><risdate>2023</risdate><volume>946</volume><issue>1</issue><spage>L14</spage><pages>L14-</pages><issn>2041-8205</issn><eissn>2041-8213</eissn><abstract>We report on the host properties of five X-ray-luminous active galactic nuclei (AGN) identified at 3 <
z
< 5 in the first epoch of imaging from the Cosmic Evolution Early Release Science Survey. Each galaxy has been imaged with the JWST Near-Infrared Camera, which provides rest-frame optical morphologies at these redshifts. We also derive stellar masses and star formation rates for each host by fitting its spectral energy distribution using a combination of galaxy and AGN templates. We find that three of the AGN hosts have spheroidal morphologies, one is a bulge-dominated disk, and one is dominated by pointlike emission. None are found to show strong morphological disturbances that might indicate a recent interaction or merger event. When compared to a sample of mass-matched inactive galaxies, we find that the AGN hosts have morphologies that are less disturbed and more bulge-dominated. Notably, all four of the resolved hosts have rest-frame optical colors consistent with a quenched or poststarburst stellar population. The presence of AGN in passively evolving galaxies at
z
> 3 is significant because a rapid feedback mechanism is required in most semianalytic models and cosmological simulations to explain the growing population of massive quiescent galaxies observed at these redshifts. Our findings show that AGN can continue to inject energy into these systems after their star formation is curtailed, potentially heating their halos and preventing renewed star formation. Additional observations will be needed to determine what role this feedback may play in helping to quench these systems and/or maintain their quiescent state.</abstract><cop>Austin</cop><pub>The American Astronomical Society</pub><doi>10.3847/2041-8213/acad00</doi><tpages>14</tpages><orcidid>https://orcid.org/0000-0001-8688-2443</orcidid><orcidid>https://orcid.org/0000-0003-3130-5643</orcidid><orcidid>https://orcid.org/0000-0003-1581-7825</orcidid><orcidid>https://orcid.org/0000-0001-8835-7722</orcidid><orcidid>https://orcid.org/0000-0001-9187-3605</orcidid><orcidid>https://orcid.org/0000-0001-8519-1130</orcidid><orcidid>https://orcid.org/0000-0001-7151-009X</orcidid><orcidid>https://orcid.org/0000-0002-1410-0470</orcidid><orcidid>https://orcid.org/0000-0001-8534-7502</orcidid><orcidid>https://orcid.org/0000-0003-4528-5639</orcidid><orcidid>https://orcid.org/0000-0001-7113-2738</orcidid><orcidid>https://orcid.org/0000-0002-0786-7307</orcidid><orcidid>https://orcid.org/0000-0001-9298-3523</orcidid><orcidid>https://orcid.org/0000-0002-8224-4505</orcidid><orcidid>https://orcid.org/0000-0003-3903-6935</orcidid><orcidid>https://orcid.org/0000-0001-6251-4988</orcidid><orcidid>https://orcid.org/0000-0002-7959-8783</orcidid><orcidid>https://orcid.org/0000-0002-4162-6523</orcidid><orcidid>https://orcid.org/0000-0002-4772-7878</orcidid><orcidid>https://orcid.org/0000-0002-1416-8483</orcidid><orcidid>https://orcid.org/0000-0002-9946-4731</orcidid><orcidid>https://orcid.org/0000-0002-0000-2394</orcidid><orcidid>https://orcid.org/0000-0002-3301-3321</orcidid><orcidid>https://orcid.org/0000-0002-7831-8751</orcidid><orcidid>https://orcid.org/0000-0002-5564-9873</orcidid><orcidid>https://orcid.org/0000-0003-0492-4924</orcidid><orcidid>https://orcid.org/0000-0002-7051-1100</orcidid><orcidid>https://orcid.org/0000-0003-3735-1931</orcidid><orcidid>https://orcid.org/0000-0001-8152-3943</orcidid><orcidid>https://orcid.org/0000-0002-9921-9218</orcidid><orcidid>https://orcid.org/0000-0001-6820-0015</orcidid><orcidid>https://orcid.org/0000-0001-6145-5090</orcidid><orcidid>https://orcid.org/0000-0003-3382-5941</orcidid><orcidid>https://orcid.org/0000-0003-2098-9568</orcidid><orcidid>https://orcid.org/0000-0002-1306-1545</orcidid><orcidid>https://orcid.org/0000-0002-6610-2048</orcidid><orcidid>https://orcid.org/0000-0003-3466-035X</orcidid><orcidid>https://orcid.org/0000-0001-5414-5131</orcidid><orcidid>https://orcid.org/0000-0002-8360-3880</orcidid><orcidid>https://orcid.org/0000-0002-1590-0568</orcidid><orcidid>https://orcid.org/0000-0002-5009-512X</orcidid><orcidid>https://orcid.org/0000-0002-4193-2539</orcidid><orcidid>https://orcid.org/0000-0001-7201-5066</orcidid><orcidid>https://orcid.org/0000-0002-7530-8857</orcidid><orcidid>https://orcid.org/0000-0002-9466-2763</orcidid><orcidid>https://orcid.org/0000-0002-4884-6756</orcidid><orcidid>https://orcid.org/0000-0002-5269-6527</orcidid><orcidid>https://orcid.org/0000-0003-1371-6019</orcidid><orcidid>https://orcid.org/0000-0002-5688-0663</orcidid><orcidid>https://orcid.org/0000-0001-8940-6768</orcidid><orcidid>https://orcid.org/0000-0001-7503-8482</orcidid><orcidid>https://orcid.org/0000-0002-8816-5146</orcidid><orcidid>https://orcid.org/0000-0003-3441-903X</orcidid><orcidid>https://orcid.org/0000-0002-0930-6466</orcidid><orcidid>https://orcid.org/0000-0001-9440-8872</orcidid><orcidid>https://orcid.org/0000-0003-1530-8713</orcidid><orcidid>https://orcid.org/0000-0003-3820-2823</orcidid><orcidid>https://orcid.org/0000-0002-3331-9590</orcidid><orcidid>https://orcid.org/0000-0002-6748-6821</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 2041-8205 |
| ispartof | Astrophysical journal. Letters, 2023-03, Vol.946 (1), p.L14 |
| issn | 2041-8205 2041-8213 |
| language | eng |
| recordid | cdi_hal_primary_oai_HAL_insu_04479098v1 |
| source | IOPscience journals; Institute of Physics Open Access Journal Titles; Directory of Open Access Journals; Alma/SFX Local Collection; EZB Electronic Journals Library |
| subjects | Active galactic nuclei AGN host galaxies Astronomical models Feedback Galactic evolution Galaxies Galaxy distribution Halos Infrared cameras Morphology Sciences of the Universe Spectral energy distribution Star & galaxy formation Star formation Stars Stars & galaxies Supermassive black holes |
| title | CEERS Key Paper. II. A First Look at the Resolved Host Properties of AGN at 3 < z < 5 with JWST |
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