Early Release Science of the exoplanet WASP-39b with JWST NIRCam

Measuring the metallicity and carbon-to-oxygen (C/O) ratio in exoplanet atmospheres is a fundamental step towards constraining the dominant chemical processes at work and, if in equilibrium, revealing planet formation histories. Transmission spectroscopy provides the necessary means by constraining...

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Veröffentlicht in:arXiv.org 2022-11
Hauptverfasser: Eva-Maria Ahrer, Stevenson, Kevin B, Mansfield, Megan, Moran, Sarah E, Brande, Jonathan, Morello, Giuseppe, Murray, Catriona A, Nikolov, Nikolay K, Dominique J M Petit dit de la Roche, Everett Schlawin, Wheatley, Peter J, Zieba, Sebastian, Batalha, Natasha E, Damiano, Mario, Goyal, Jayesh M, Lendl, Monika, Lothringer, Joshua D, Mukherjee, Sagnick, Ohno, Kazumasa, Batalha, Natalie M, Battley, Matthew P, Bean, Jacob L, Beatty, Thomas G, Benneke, Björn, Berta-Thompson, Zachory K, Carter, Aarynn L, Cubillos, Patricio E, Daylan, Tansu, Espinoza, Néstor, Gao, Peter, Gibson, Neale P, Gill, Samuel, Harrington, Joseph, Hu, Renyu, Kreidberg, Laura, Lewis, Nikole K, Line, Michael R, López-Morales, Mercedes, Parmentier, Vivien, Powell, Diana K, Sing, David K, Shang-Min Tsai, Wakeford, Hannah R, Welbanks, Luis, Alam, Munazza K, Alderson, Lili, Allen, Natalie H, Anderson, David R, Barstow, Joanna K, Bayliss, Daniel, Bell, Taylor J, Blecic, Jasmina, Bryant, Edward M, Burleigh, Matthew R, Carone, Ludmila, Casewell, S L, Changeat, Quentin, Chubb, Katy L, Crossfield, Ian J M, Crouzet, Nicolas, Decin, Leen, Jean-Michel Désert, Feinstein, Adina D, Flagg, Laura, tney, Jonathan J, Gizis, John E, Heng, Kevin, Iro, Nicolas, Kempton, Eliza M -R, Kendrew, Sarah, Kirk, James, Knutson, Heather A, Komacek, Thaddeus D, Pierre-Olivier Lagage, Leconte, Jérémy, Lustig-Yaeger, Jacob, MacDonald, Ryan J, Mancini, Luigi, May, E M, Mayne, N J, Yamila Miguel, Mikal-Evans, Thomas, Molaverdikhani, Karan, Palle, Enric, Piaulet, Caroline, Rackham, Benjamin V, Redfield, Seth, Rogers, Laura K, Pierre-Alexis, Roy, Rustamkulov, Zafar, Shkolnik, Evgenya L, Sotzen, Kristin S, Taylor, Jake, Tremblin, P, Tucker, Gregory S, Turner, Jake D, Miguel de Val-Borro, Venot, Olivia, Zhang, Xi
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container_title arXiv.org
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creator Eva-Maria Ahrer
Stevenson, Kevin B
Mansfield, Megan
Moran, Sarah E
Brande, Jonathan
Morello, Giuseppe
Murray, Catriona A
Nikolov, Nikolay K
Dominique J M Petit dit de la Roche
Everett Schlawin
Wheatley, Peter J
Zieba, Sebastian
Batalha, Natasha E
Damiano, Mario
Goyal, Jayesh M
Lendl, Monika
Lothringer, Joshua D
Mukherjee, Sagnick
Ohno, Kazumasa
Batalha, Natalie M
Battley, Matthew P
Bean, Jacob L
Beatty, Thomas G
Benneke, Björn
Berta-Thompson, Zachory K
Carter, Aarynn L
Cubillos, Patricio E
Daylan, Tansu
Espinoza, Néstor
Gao, Peter
Gibson, Neale P
Gill, Samuel
Harrington, Joseph
Hu, Renyu
Kreidberg, Laura
Lewis, Nikole K
Line, Michael R
López-Morales, Mercedes
Parmentier, Vivien
Powell, Diana K
Sing, David K
Shang-Min Tsai
Wakeford, Hannah R
Welbanks, Luis
Alam, Munazza K
Alderson, Lili
Allen, Natalie H
Anderson, David R
Barstow, Joanna K
Bayliss, Daniel
Bell, Taylor J
Blecic, Jasmina
Bryant, Edward M
Burleigh, Matthew R
Carone, Ludmila
Casewell, S L
Changeat, Quentin
Chubb, Katy L
Crossfield, Ian J M
Crouzet, Nicolas
Decin, Leen
Jean-Michel Désert
Feinstein, Adina D
Flagg, Laura
tney, Jonathan J
Gizis, John E
Heng, Kevin
Iro, Nicolas
Kempton, Eliza M -R
Kendrew, Sarah
Kirk, James
Knutson, Heather A
Komacek, Thaddeus D
Pierre-Olivier Lagage
Leconte, Jérémy
Lustig-Yaeger, Jacob
MacDonald, Ryan J
Mancini, Luigi
May, E M
Mayne, N J
Yamila Miguel
Mikal-Evans, Thomas
Molaverdikhani, Karan
Palle, Enric
Piaulet, Caroline
Rackham, Benjamin V
Redfield, Seth
Rogers, Laura K
Pierre-Alexis, Roy
Rustamkulov, Zafar
Shkolnik, Evgenya L
Sotzen, Kristin S
Taylor, Jake
Tremblin, P
Tucker, Gregory S
Turner, Jake D
Miguel de Val-Borro
Venot, Olivia
Zhang, Xi
description Measuring the metallicity and carbon-to-oxygen (C/O) ratio in exoplanet atmospheres is a fundamental step towards constraining the dominant chemical processes at work and, if in equilibrium, revealing planet formation histories. Transmission spectroscopy provides the necessary means by constraining the abundances of oxygen- and carbon-bearing species; however, this requires broad wavelength coverage, moderate spectral resolution, and high precision that, together, are not achievable with previous observatories. Now that JWST has commenced science operations, we are able to observe exoplanets at previously uncharted wavelengths and spectral resolutions. Here we report time-series observations of the transiting exoplanet WASP-39b using JWST's Near InfraRed Camera (NIRCam). The long-wavelength spectroscopic and short-wavelength photometric light curves span 2.0 - 4.0 \(\mu\)m, exhibit minimal systematics, and reveal well-defined molecular absorption features in the planet's spectrum. Specifically, we detect gaseous H\(_2\)O in the atmosphere and place an upper limit on the abundance of CH\(_4\). The otherwise prominent CO\(_2\) feature at 2.8 \(\mu\)m is largely masked by H\(_2\)O. The best-fit chemical equilibrium models favour an atmospheric metallicity of 1-100\(\times\) solar (i.e., an enrichment of elements heavier than helium relative to the Sun) and a sub-stellar carbon-to-oxygen (C/O) ratio. The inferred high metallicity and low C/O ratio may indicate significant accretion of solid materials during planet formation or disequilibrium processes in the upper atmosphere.
doi_str_mv 10.48550/arxiv.2211.10489
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Stevenson, Kevin B ; Mansfield, Megan ; Moran, Sarah E ; Brande, Jonathan ; Morello, Giuseppe ; Murray, Catriona A ; Nikolov, Nikolay K ; Dominique J M Petit dit de la Roche ; Everett Schlawin ; Wheatley, Peter J ; Zieba, Sebastian ; Batalha, Natasha E ; Damiano, Mario ; Goyal, Jayesh M ; Lendl, Monika ; Lothringer, Joshua D ; Mukherjee, Sagnick ; Ohno, Kazumasa ; Batalha, Natalie M ; Battley, Matthew P ; Bean, Jacob L ; Beatty, Thomas G ; Benneke, Björn ; Berta-Thompson, Zachory K ; Carter, Aarynn L ; Cubillos, Patricio E ; Daylan, Tansu ; Espinoza, Néstor ; Gao, Peter ; Gibson, Neale P ; Gill, Samuel ; Harrington, Joseph ; Hu, Renyu ; Kreidberg, Laura ; Lewis, Nikole K ; Line, Michael R ; López-Morales, Mercedes ; Parmentier, Vivien ; Powell, Diana K ; Sing, David K ; Shang-Min Tsai ; Wakeford, Hannah R ; Welbanks, Luis ; Alam, Munazza K ; Alderson, Lili ; Allen, Natalie H ; Anderson, David R ; Barstow, Joanna K ; Bayliss, Daniel ; Bell, Taylor J ; Blecic, Jasmina ; Bryant, Edward M ; Burleigh, Matthew R ; Carone, Ludmila ; Casewell, S L ; Changeat, Quentin ; Chubb, Katy L ; Crossfield, Ian J M ; Crouzet, Nicolas ; Decin, Leen ; Jean-Michel Désert ; Feinstein, Adina D ; Flagg, Laura ; tney, Jonathan J ; Gizis, John E ; Heng, Kevin ; Iro, Nicolas ; Kempton, Eliza M -R ; Kendrew, Sarah ; Kirk, James ; Knutson, Heather A ; Komacek, Thaddeus D ; Pierre-Olivier Lagage ; Leconte, Jérémy ; Lustig-Yaeger, Jacob ; MacDonald, Ryan J ; Mancini, Luigi ; May, E M ; Mayne, N J ; Yamila Miguel ; Mikal-Evans, Thomas ; Molaverdikhani, Karan ; Palle, Enric ; Piaulet, Caroline ; Rackham, Benjamin V ; Redfield, Seth ; Rogers, Laura K ; Pierre-Alexis, Roy ; Rustamkulov, Zafar ; Shkolnik, Evgenya L ; Sotzen, Kristin S ; Taylor, Jake ; Tremblin, P ; Tucker, Gregory S ; Turner, Jake D ; Miguel de Val-Borro ; Venot, Olivia ; Zhang, Xi</creator><creatorcontrib>Eva-Maria Ahrer ; Stevenson, Kevin B ; Mansfield, Megan ; Moran, Sarah E ; Brande, Jonathan ; Morello, Giuseppe ; Murray, Catriona A ; Nikolov, Nikolay K ; Dominique J M Petit dit de la Roche ; Everett Schlawin ; Wheatley, Peter J ; Zieba, Sebastian ; Batalha, Natasha E ; Damiano, Mario ; Goyal, Jayesh M ; Lendl, Monika ; Lothringer, Joshua D ; Mukherjee, Sagnick ; Ohno, Kazumasa ; Batalha, Natalie M ; Battley, Matthew P ; Bean, Jacob L ; Beatty, Thomas G ; Benneke, Björn ; Berta-Thompson, Zachory K ; Carter, Aarynn L ; Cubillos, Patricio E ; Daylan, Tansu ; Espinoza, Néstor ; Gao, Peter ; Gibson, Neale P ; Gill, Samuel ; Harrington, Joseph ; Hu, Renyu ; Kreidberg, Laura ; Lewis, Nikole K ; Line, Michael R ; López-Morales, Mercedes ; Parmentier, Vivien ; Powell, Diana K ; Sing, David K ; Shang-Min Tsai ; Wakeford, Hannah R ; Welbanks, Luis ; Alam, Munazza K ; Alderson, Lili ; Allen, Natalie H ; Anderson, David R ; Barstow, Joanna K ; Bayliss, Daniel ; Bell, Taylor J ; Blecic, Jasmina ; Bryant, Edward M ; Burleigh, Matthew R ; Carone, Ludmila ; Casewell, S L ; Changeat, Quentin ; Chubb, Katy L ; Crossfield, Ian J M ; Crouzet, Nicolas ; Decin, Leen ; Jean-Michel Désert ; Feinstein, Adina D ; Flagg, Laura ; tney, Jonathan J ; Gizis, John E ; Heng, Kevin ; Iro, Nicolas ; Kempton, Eliza M -R ; Kendrew, Sarah ; Kirk, James ; Knutson, Heather A ; Komacek, Thaddeus D ; Pierre-Olivier Lagage ; Leconte, Jérémy ; Lustig-Yaeger, Jacob ; MacDonald, Ryan J ; Mancini, Luigi ; May, E M ; Mayne, N J ; Yamila Miguel ; Mikal-Evans, Thomas ; Molaverdikhani, Karan ; Palle, Enric ; Piaulet, Caroline ; Rackham, Benjamin V ; Redfield, Seth ; Rogers, Laura K ; Pierre-Alexis, Roy ; Rustamkulov, Zafar ; Shkolnik, Evgenya L ; Sotzen, Kristin S ; Taylor, Jake ; Tremblin, P ; Tucker, Gregory S ; Turner, Jake D ; Miguel de Val-Borro ; Venot, Olivia ; Zhang, Xi</creatorcontrib><description>Measuring the metallicity and carbon-to-oxygen (C/O) ratio in exoplanet atmospheres is a fundamental step towards constraining the dominant chemical processes at work and, if in equilibrium, revealing planet formation histories. Transmission spectroscopy provides the necessary means by constraining the abundances of oxygen- and carbon-bearing species; however, this requires broad wavelength coverage, moderate spectral resolution, and high precision that, together, are not achievable with previous observatories. Now that JWST has commenced science operations, we are able to observe exoplanets at previously uncharted wavelengths and spectral resolutions. Here we report time-series observations of the transiting exoplanet WASP-39b using JWST's Near InfraRed Camera (NIRCam). The long-wavelength spectroscopic and short-wavelength photometric light curves span 2.0 - 4.0 \(\mu\)m, exhibit minimal systematics, and reveal well-defined molecular absorption features in the planet's spectrum. Specifically, we detect gaseous H\(_2\)O in the atmosphere and place an upper limit on the abundance of CH\(_4\). The otherwise prominent CO\(_2\) feature at 2.8 \(\mu\)m is largely masked by H\(_2\)O. The best-fit chemical equilibrium models favour an atmospheric metallicity of 1-100\(\times\) solar (i.e., an enrichment of elements heavier than helium relative to the Sun) and a sub-stellar carbon-to-oxygen (C/O) ratio. The inferred high metallicity and low C/O ratio may indicate significant accretion of solid materials during planet formation or disequilibrium processes in the upper atmosphere.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.2211.10489</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Abundance ; Astrochemistry ; Atmospheric models ; Carbon ; Chemical reactions ; Constraining ; Deposition ; Extrasolar planets ; Infrared cameras ; Infrared photometry ; Light curve ; Metallicity ; Molecular absorption ; Observatories ; Oxygen ; Physics - Earth and Planetary Astrophysics ; Physics - Instrumentation and Methods for Astrophysics ; Physics - Solar and Stellar Astrophysics ; Planet formation ; Planetary atmospheres ; Spectral resolution ; Transit ; Upper atmosphere</subject><ispartof>arXiv.org, 2022-11</ispartof><rights>2022. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><rights>http://creativecommons.org/licenses/by/4.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,782,786,887,27932</link.rule.ids><backlink>$$Uhttps://doi.org/10.1038/s41586-022-05590-4$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.48550/arXiv.2211.10489$$DView paper in arXiv$$Hfree_for_read</backlink></links><search><creatorcontrib>Eva-Maria Ahrer</creatorcontrib><creatorcontrib>Stevenson, Kevin B</creatorcontrib><creatorcontrib>Mansfield, Megan</creatorcontrib><creatorcontrib>Moran, Sarah E</creatorcontrib><creatorcontrib>Brande, 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Luis</creatorcontrib><creatorcontrib>Alam, Munazza K</creatorcontrib><creatorcontrib>Alderson, Lili</creatorcontrib><creatorcontrib>Allen, Natalie H</creatorcontrib><creatorcontrib>Anderson, David R</creatorcontrib><creatorcontrib>Barstow, Joanna K</creatorcontrib><creatorcontrib>Bayliss, Daniel</creatorcontrib><creatorcontrib>Bell, Taylor J</creatorcontrib><creatorcontrib>Blecic, Jasmina</creatorcontrib><creatorcontrib>Bryant, Edward M</creatorcontrib><creatorcontrib>Burleigh, Matthew R</creatorcontrib><creatorcontrib>Carone, Ludmila</creatorcontrib><creatorcontrib>Casewell, S L</creatorcontrib><creatorcontrib>Changeat, Quentin</creatorcontrib><creatorcontrib>Chubb, Katy L</creatorcontrib><creatorcontrib>Crossfield, Ian J M</creatorcontrib><creatorcontrib>Crouzet, Nicolas</creatorcontrib><creatorcontrib>Decin, Leen</creatorcontrib><creatorcontrib>Jean-Michel Désert</creatorcontrib><creatorcontrib>Feinstein, Adina D</creatorcontrib><creatorcontrib>Flagg, Laura</creatorcontrib><creatorcontrib>tney, Jonathan J</creatorcontrib><creatorcontrib>Gizis, John E</creatorcontrib><creatorcontrib>Heng, Kevin</creatorcontrib><creatorcontrib>Iro, Nicolas</creatorcontrib><creatorcontrib>Kempton, Eliza M -R</creatorcontrib><creatorcontrib>Kendrew, Sarah</creatorcontrib><creatorcontrib>Kirk, James</creatorcontrib><creatorcontrib>Knutson, Heather A</creatorcontrib><creatorcontrib>Komacek, Thaddeus D</creatorcontrib><creatorcontrib>Pierre-Olivier Lagage</creatorcontrib><creatorcontrib>Leconte, Jérémy</creatorcontrib><creatorcontrib>Lustig-Yaeger, Jacob</creatorcontrib><creatorcontrib>MacDonald, Ryan J</creatorcontrib><creatorcontrib>Mancini, Luigi</creatorcontrib><creatorcontrib>May, E M</creatorcontrib><creatorcontrib>Mayne, N J</creatorcontrib><creatorcontrib>Yamila Miguel</creatorcontrib><creatorcontrib>Mikal-Evans, Thomas</creatorcontrib><creatorcontrib>Molaverdikhani, Karan</creatorcontrib><creatorcontrib>Palle, Enric</creatorcontrib><creatorcontrib>Piaulet, Caroline</creatorcontrib><creatorcontrib>Rackham, Benjamin V</creatorcontrib><creatorcontrib>Redfield, Seth</creatorcontrib><creatorcontrib>Rogers, Laura K</creatorcontrib><creatorcontrib>Pierre-Alexis, Roy</creatorcontrib><creatorcontrib>Rustamkulov, Zafar</creatorcontrib><creatorcontrib>Shkolnik, Evgenya L</creatorcontrib><creatorcontrib>Sotzen, Kristin S</creatorcontrib><creatorcontrib>Taylor, Jake</creatorcontrib><creatorcontrib>Tremblin, P</creatorcontrib><creatorcontrib>Tucker, Gregory S</creatorcontrib><creatorcontrib>Turner, Jake D</creatorcontrib><creatorcontrib>Miguel de Val-Borro</creatorcontrib><creatorcontrib>Venot, Olivia</creatorcontrib><creatorcontrib>Zhang, Xi</creatorcontrib><title>Early Release Science of the exoplanet WASP-39b with JWST NIRCam</title><title>arXiv.org</title><description>Measuring the metallicity and carbon-to-oxygen (C/O) ratio in exoplanet atmospheres is a fundamental step towards constraining the dominant chemical processes at work and, if in equilibrium, revealing planet formation histories. Transmission spectroscopy provides the necessary means by constraining the abundances of oxygen- and carbon-bearing species; however, this requires broad wavelength coverage, moderate spectral resolution, and high precision that, together, are not achievable with previous observatories. Now that JWST has commenced science operations, we are able to observe exoplanets at previously uncharted wavelengths and spectral resolutions. Here we report time-series observations of the transiting exoplanet WASP-39b using JWST's Near InfraRed Camera (NIRCam). The long-wavelength spectroscopic and short-wavelength photometric light curves span 2.0 - 4.0 \(\mu\)m, exhibit minimal systematics, and reveal well-defined molecular absorption features in the planet's spectrum. Specifically, we detect gaseous H\(_2\)O in the atmosphere and place an upper limit on the abundance of CH\(_4\). The otherwise prominent CO\(_2\) feature at 2.8 \(\mu\)m is largely masked by H\(_2\)O. The best-fit chemical equilibrium models favour an atmospheric metallicity of 1-100\(\times\) solar (i.e., an enrichment of elements heavier than helium relative to the Sun) and a sub-stellar carbon-to-oxygen (C/O) ratio. The inferred high metallicity and low C/O ratio may indicate significant accretion of solid materials during planet formation or disequilibrium processes in the upper atmosphere.</description><subject>Abundance</subject><subject>Astrochemistry</subject><subject>Atmospheric models</subject><subject>Carbon</subject><subject>Chemical reactions</subject><subject>Constraining</subject><subject>Deposition</subject><subject>Extrasolar planets</subject><subject>Infrared cameras</subject><subject>Infrared photometry</subject><subject>Light curve</subject><subject>Metallicity</subject><subject>Molecular absorption</subject><subject>Observatories</subject><subject>Oxygen</subject><subject>Physics - Earth and Planetary Astrophysics</subject><subject>Physics - Instrumentation and Methods for Astrophysics</subject><subject>Physics - Solar and Stellar Astrophysics</subject><subject>Planet formation</subject><subject>Planetary atmospheres</subject><subject>Spectral resolution</subject><subject>Transit</subject><subject>Upper atmosphere</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2022</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GOX</sourceid><recordid>eNotj81OwkAURicmJhLkAVw5ievizJ3O305CUDFEDW3CsplO74SSQrEtCm9vBVff5uTLOYTccTaOjZTs0TXH8nsMwPmYs9jYKzIAIXhkYoAbMmrbDWMMlAYpxYA8zVxTnegSK3Qt0sSXuPNI60C7NVI81vvK7bCjq0nyGQmb05-yW9O3VZLS9_ly6ra35Dq4qsXR_w5J-jxLp6_R4uNlPp0sImeljQoOhdRKMWckOs9t0SsFlgtUymru46AsQxtyCVIhB53HwRfax8Kr4I0XQ3J_uT3nZfum3LrmlP1lZufMnni4EPum_jpg22Wb-tDseqcMtDCaAQcjfgEw5lKY</recordid><startdate>20221118</startdate><enddate>20221118</enddate><creator>Eva-Maria Ahrer</creator><creator>Stevenson, Kevin B</creator><creator>Mansfield, Megan</creator><creator>Moran, Sarah E</creator><creator>Brande, 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Roy</creator><creator>Rustamkulov, Zafar</creator><creator>Shkolnik, Evgenya L</creator><creator>Sotzen, Kristin S</creator><creator>Taylor, Jake</creator><creator>Tremblin, P</creator><creator>Tucker, Gregory S</creator><creator>Turner, Jake D</creator><creator>Miguel de Val-Borro</creator><creator>Venot, Olivia</creator><creator>Zhang, Xi</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope><scope>GOX</scope></search><sort><creationdate>20221118</creationdate><title>Early Release Science of the exoplanet WASP-39b with JWST NIRCam</title><author>Eva-Maria Ahrer ; Stevenson, Kevin B ; Mansfield, Megan ; Moran, Sarah E ; Brande, Jonathan ; Morello, Giuseppe ; Murray, Catriona A ; Nikolov, Nikolay K ; Dominique J M Petit dit de la Roche ; Everett Schlawin ; Wheatley, Peter J ; Zieba, Sebastian ; Batalha, Natasha E ; Damiano, Mario ; Goyal, Jayesh M ; Lendl, Monika ; Lothringer, Joshua D ; Mukherjee, Sagnick ; Ohno, Kazumasa ; Batalha, Natalie M ; Battley, Matthew P ; Bean, Jacob L ; Beatty, Thomas G ; Benneke, Björn ; Berta-Thompson, Zachory K ; Carter, Aarynn L ; Cubillos, Patricio E ; Daylan, Tansu ; Espinoza, Néstor ; Gao, Peter ; Gibson, Neale P ; Gill, Samuel ; Harrington, Joseph ; Hu, Renyu ; Kreidberg, Laura ; Lewis, Nikole K ; Line, Michael R ; López-Morales, Mercedes ; Parmentier, Vivien ; Powell, Diana K ; Sing, David K ; Shang-Min Tsai ; Wakeford, Hannah R ; Welbanks, Luis ; Alam, Munazza K ; Alderson, Lili ; Allen, Natalie H ; Anderson, David R ; Barstow, Joanna K ; Bayliss, Daniel ; Bell, Taylor J ; Blecic, Jasmina ; Bryant, Edward M ; Burleigh, Matthew R ; Carone, Ludmila ; Casewell, S L ; Changeat, Quentin ; Chubb, Katy L ; Crossfield, Ian J M ; Crouzet, Nicolas ; Decin, Leen ; Jean-Michel Désert ; Feinstein, Adina D ; Flagg, Laura ; tney, Jonathan J ; Gizis, John E ; Heng, Kevin ; Iro, Nicolas ; Kempton, Eliza M -R ; Kendrew, Sarah ; Kirk, James ; Knutson, Heather A ; Komacek, Thaddeus D ; Pierre-Olivier Lagage ; Leconte, Jérémy ; Lustig-Yaeger, Jacob ; MacDonald, Ryan J ; Mancini, Luigi ; May, E M ; Mayne, N J ; Yamila Miguel ; Mikal-Evans, Thomas ; Molaverdikhani, Karan ; Palle, Enric ; Piaulet, Caroline ; Rackham, Benjamin V ; Redfield, Seth ; Rogers, Laura K ; Pierre-Alexis, Roy ; Rustamkulov, Zafar ; Shkolnik, Evgenya L ; Sotzen, Kristin S ; Taylor, Jake ; Tremblin, P ; Tucker, Gregory S ; Turner, Jake D ; Miguel de Val-Borro ; Venot, Olivia ; Zhang, Xi</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a959-d12d57660a85eac19d331f0b3e66971c4f690e9fb5256e127b4fcd7c43c6fc8c3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2022</creationdate><topic>Abundance</topic><topic>Astrochemistry</topic><topic>Atmospheric models</topic><topic>Carbon</topic><topic>Chemical reactions</topic><topic>Constraining</topic><topic>Deposition</topic><topic>Extrasolar planets</topic><topic>Infrared cameras</topic><topic>Infrared photometry</topic><topic>Light curve</topic><topic>Metallicity</topic><topic>Molecular absorption</topic><topic>Observatories</topic><topic>Oxygen</topic><topic>Physics - Earth and Planetary Astrophysics</topic><topic>Physics - Instrumentation and Methods for Astrophysics</topic><topic>Physics - Solar and Stellar Astrophysics</topic><topic>Planet formation</topic><topic>Planetary atmospheres</topic><topic>Spectral resolution</topic><topic>Transit</topic><topic>Upper atmosphere</topic><toplevel>online_resources</toplevel><creatorcontrib>Eva-Maria Ahrer</creatorcontrib><creatorcontrib>Stevenson, Kevin B</creatorcontrib><creatorcontrib>Mansfield, Megan</creatorcontrib><creatorcontrib>Moran, Sarah E</creatorcontrib><creatorcontrib>Brande, Jonathan</creatorcontrib><creatorcontrib>Morello, Giuseppe</creatorcontrib><creatorcontrib>Murray, Catriona A</creatorcontrib><creatorcontrib>Nikolov, Nikolay K</creatorcontrib><creatorcontrib>Dominique J M Petit dit de la Roche</creatorcontrib><creatorcontrib>Everett Schlawin</creatorcontrib><creatorcontrib>Wheatley, Peter J</creatorcontrib><creatorcontrib>Zieba, Sebastian</creatorcontrib><creatorcontrib>Batalha, Natasha E</creatorcontrib><creatorcontrib>Damiano, Mario</creatorcontrib><creatorcontrib>Goyal, Jayesh M</creatorcontrib><creatorcontrib>Lendl, Monika</creatorcontrib><creatorcontrib>Lothringer, Joshua D</creatorcontrib><creatorcontrib>Mukherjee, 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E</au><au>Daylan, Tansu</au><au>Espinoza, Néstor</au><au>Gao, Peter</au><au>Gibson, Neale P</au><au>Gill, Samuel</au><au>Harrington, Joseph</au><au>Hu, Renyu</au><au>Kreidberg, Laura</au><au>Lewis, Nikole K</au><au>Line, Michael R</au><au>López-Morales, Mercedes</au><au>Parmentier, Vivien</au><au>Powell, Diana K</au><au>Sing, David K</au><au>Shang-Min Tsai</au><au>Wakeford, Hannah R</au><au>Welbanks, Luis</au><au>Alam, Munazza K</au><au>Alderson, Lili</au><au>Allen, Natalie H</au><au>Anderson, David R</au><au>Barstow, Joanna K</au><au>Bayliss, Daniel</au><au>Bell, Taylor J</au><au>Blecic, Jasmina</au><au>Bryant, Edward M</au><au>Burleigh, Matthew R</au><au>Carone, Ludmila</au><au>Casewell, S L</au><au>Changeat, Quentin</au><au>Chubb, Katy L</au><au>Crossfield, Ian J M</au><au>Crouzet, Nicolas</au><au>Decin, Leen</au><au>Jean-Michel Désert</au><au>Feinstein, Adina D</au><au>Flagg, Laura</au><au>tney, Jonathan J</au><au>Gizis, John E</au><au>Heng, Kevin</au><au>Iro, Nicolas</au><au>Kempton, Eliza M -R</au><au>Kendrew, Sarah</au><au>Kirk, James</au><au>Knutson, Heather A</au><au>Komacek, Thaddeus D</au><au>Pierre-Olivier Lagage</au><au>Leconte, Jérémy</au><au>Lustig-Yaeger, Jacob</au><au>MacDonald, Ryan J</au><au>Mancini, Luigi</au><au>May, E M</au><au>Mayne, N J</au><au>Yamila Miguel</au><au>Mikal-Evans, Thomas</au><au>Molaverdikhani, Karan</au><au>Palle, Enric</au><au>Piaulet, Caroline</au><au>Rackham, Benjamin V</au><au>Redfield, Seth</au><au>Rogers, Laura K</au><au>Pierre-Alexis, Roy</au><au>Rustamkulov, Zafar</au><au>Shkolnik, Evgenya L</au><au>Sotzen, Kristin S</au><au>Taylor, Jake</au><au>Tremblin, P</au><au>Tucker, Gregory S</au><au>Turner, Jake D</au><au>Miguel de Val-Borro</au><au>Venot, Olivia</au><au>Zhang, Xi</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Early Release Science of the exoplanet WASP-39b with JWST NIRCam</atitle><jtitle>arXiv.org</jtitle><date>2022-11-18</date><risdate>2022</risdate><eissn>2331-8422</eissn><abstract>Measuring the metallicity and carbon-to-oxygen (C/O) ratio in exoplanet atmospheres is a fundamental step towards constraining the dominant chemical processes at work and, if in equilibrium, revealing planet formation histories. Transmission spectroscopy provides the necessary means by constraining the abundances of oxygen- and carbon-bearing species; however, this requires broad wavelength coverage, moderate spectral resolution, and high precision that, together, are not achievable with previous observatories. Now that JWST has commenced science operations, we are able to observe exoplanets at previously uncharted wavelengths and spectral resolutions. Here we report time-series observations of the transiting exoplanet WASP-39b using JWST's Near InfraRed Camera (NIRCam). The long-wavelength spectroscopic and short-wavelength photometric light curves span 2.0 - 4.0 \(\mu\)m, exhibit minimal systematics, and reveal well-defined molecular absorption features in the planet's spectrum. Specifically, we detect gaseous H\(_2\)O in the atmosphere and place an upper limit on the abundance of CH\(_4\). The otherwise prominent CO\(_2\) feature at 2.8 \(\mu\)m is largely masked by H\(_2\)O. The best-fit chemical equilibrium models favour an atmospheric metallicity of 1-100\(\times\) solar (i.e., an enrichment of elements heavier than helium relative to the Sun) and a sub-stellar carbon-to-oxygen (C/O) ratio. The inferred high metallicity and low C/O ratio may indicate significant accretion of solid materials during planet formation or disequilibrium processes in the upper atmosphere.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.2211.10489</doi><oa>free_for_read</oa></addata></record>
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subjects Abundance
Astrochemistry
Atmospheric models
Carbon
Chemical reactions
Constraining
Deposition
Extrasolar planets
Infrared cameras
Infrared photometry
Light curve
Metallicity
Molecular absorption
Observatories
Oxygen
Physics - Earth and Planetary Astrophysics
Physics - Instrumentation and Methods for Astrophysics
Physics - Solar and Stellar Astrophysics
Planet formation
Planetary atmospheres
Spectral resolution
Transit
Upper atmosphere
title Early Release Science of the exoplanet WASP-39b with JWST NIRCam
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