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

被引：115

作者：

Ahrer, Eva-Maria ^{[1
,2
]}

Stevenson, Kevin B. ^{[3
]}

Mansfield, Megan ^{[4
]}

Moran, Sarah E. ^{[5
]}

Brande, Jonathan ^{[6
]}

Morello, Giuseppe ^{[7
,8
,9
]}

Murray, Catriona A. ^{[10
]}

Nikolov, Nikolay K. ^{[11
]}

de la Roche, Dominique J. M. Petit Dit ^{[12
]}

Schlawin, Everett ^{[4
]}

Wheatley, Peter J. ^{[1
,2
]}

Zieba, Sebastian ^{[13
,14
]}

Batalha, Natasha E. ^{[15
]}

Damiano, Mario ^{[16
]}

Goyal, Jayesh M. ^{[17
]}

Lendl, Monika ^{[12
]}

Lothringer, Joshua D. ^{[18
]}

Mukherjee, Sagnick ^{[19
]}

Ohno, Kazumasa ^{[19
]}

Batalha, Natalie M. ^{[19
,20
]}

Battley, Matthew P. ^{[1
,2
]}

Bean, Jacob L. ^{[21
]}

Beatty, Thomas G. ^{[22
]}

Benneke, Bjorn ^{[23
,24
]}

Berta-Thompson, Zachory K. ^{[10
]}

Carter, Aarynn L.

Cubillos, Patricio E. ^{[25
,26
]}

Daylan, Tansu ^{[27
]}

Espinoza, Nestor ^{[28
]}

Gao, Peter ^{[29
]}

Gibson, Neale P. ^{[30
]}

Gill, Samuel ^{[2
]}

Harrington, Joseph ^{[31
,32
]}

Hu, Renyu ^{[33
,34
]}

Kreidberg, Laura ^{[13
]}

Lewis, Nikole K. ^{[35
,36
]}

Line, Michael R. ^{[37
]}

Lopez-Morales, Mercedes ^{[38
]}

Parmentier, Vivien ^{[39
,40
]}

Powell, Diana K. ^{[38
]}

Sing, David K. ^{[28
,41
]}

Tsai, Shang-Min ^{[39
]}

Wakeford, Hannah R. ^{[42
]}

Welbanks, Luis ^{[37
]}

Alam, Munazza K. ^{[29
]}

Alderson, Lili ^{[42
]}

Allen, Natalie H. ^{[28
]}

Anderson, David R. ^{[1
,2
]}

Barstow, Joanna K. ^{[43
]}

Bayliss, Daniel ^{[2
]}

机构：

[1] Univ Warwick, Ctr Exoplanets & Habitabil, Coventry, England

[2] Univ Warwick, Dept Phys, Coventry, England

[3] Johns Hopkins APL, Laurel, MD 20723 USA

[4] Univ Arizona, Steward Observ, Tucson, AZ USA

[5] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ USA

[6] Univ Kansas, Dept Phys & Astron, Lawrence, KS USA

[7] Inst Astrofis Canarias IAC, Tenerife, Spain

[8] Univ La Laguna ULL, Dept Astrofis, Tenerife, Spain

[9] INAF, Palermo Astron Observ, Piazza Parlamento, Palermo, Italy

[10] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO USA

[11] Space Telescope Sci Inst, Baltimore, MD USA

[12] Univ Geneva, Dept Astron, Sauverny, Switzerland

[13] Max Planck Inst Astron, Heidelberg, Germany

[14] Leiden Univ, Leiden Observ, Leiden, Netherlands

[15] NASA, Ames Res Ctr, Moffett Field, CA USA

[16] Jet Prop Lab, Pasadena, CA USA

[17] HBNI, Natl Inst Sci Educ & Res NISER, Sch Earth & Planetary Sci SEPS, Jatani, India

[18] Utah Valley Univ, Dept Phys, Orem, UT USA

[19] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA USA

[20] Univ Calif Santa Cruz, Astrobiol Program, Santa Cruz, CA USA

[21] Univ Chicago, Dept Astron & Astrophys, Chicago, IL USA

[22] Univ Wisconsin Madison, Dept Astron, Madison, WI USA

[23] Univ Montreal, Dept Phys, Montreal, PQ, Canada

[24] Univ Montreal, Inst Res Exoplanets, Montreal, PQ, Canada

[25] Austrian Acad Sci, Space Res Inst, Graz, Austria

[26] INAF Osservatorio Astrofisico Torino, Pino Torinese, Italy

[27] Princeton Univ, Dept Astrophys Sci, Princeton, NJ USA

[28] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD USA

[29] Carnegie Inst Sci, Earth & Planets Lab, Washington, DC USA

[30] Trinity Coll Dublin, Sch Phys, Dublin, Ireland

[31] Univ Cent Florida, Dept Phys, Planetary Sci Grp, Orlando, FL USA

[32] Univ Cent Florida, Florida Space Inst, Orlando, FL USA

[33] CALTECH, Astrophys Sect, Jet Prop Lab, Pasadena, CA USA

[34] CALTECH, Div Geol & Planetary Sci, Pasadena, CA USA

[35] Cornell Univ, Dept Astron, Ithaca, NY USA

[36] Cornell Univ, Carl Sagan Inst, Ithaca, NY USA

[37] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA

[38] Ctr Astrophys Harvard & Smithsonian, Cambridge, MA USA

[39] Univ Oxford, Dept Phys, Atmospher Ocean & Planetary Phys, Oxford, England

[40] Univ Cote Azur, Observ Cote Azur, CNRS, Lab Lagrange, Nice, France

[41] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD USA

[42] Univ Bristol, Sch Phys, Bristol, England

[43] Open Univ, Sch Phys Sci, Milton Keynes, England

[44] NASA, BAER Inst, Ames Res Ctr, Moffett Field, CA USA

[45] New York Univ Abu Dhabi, Dept Phys, Abu Dhabi, U Arab Emirates

[46] New York Univ Abu Dhabi, Ctr Astro Particle & Planetary Phys CAP3, Abu Dhabi, U Arab Emirates

[47] Univ Coll London, Mullard Space Sci Lab, Dorking, England

[48] Univ Leicester, Sch Phys & Astron, Leicester, England

[49] European Space Agcy, Space Telescope Sci Inst, Baltimore, MD USA

[50] UCL, Dept Phys & Astron, London, England

来源：

NATURE | 2023年 / 614卷 / 7949期

基金：

英国科研创新办公室; 英国科学技术设施理事会;

关键词：

LINE LISTS; ATMOSPHERE; SPECTRUM; METHANE; CLOUDS; CARBON; ISOTOPOLOGUES; CHEMISTRY; NITROGEN; SURFACE;

D O I：

10.1038/s41586-022-05590-4

中图分类号：

O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];

学科分类号：

07 ; 0710 ; 09 ;

摘要：

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 (for example, refs. (1,2)) 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, which, 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 micrometres, exhibit minimal systematics and reveal well defined molecular absorption features in the planet's spectrum. Specifically, we detect gaseous water in the atmosphere and place an upper limit on the abundance of methane. The otherwise prominent carbon dioxide feature at 2.8 micrometres is largely masked by water. The best-fit chemical equilibrium models favour an atmospheric metallicity of 1-100-times solar (that is, an enrichment of elements heavier than helium relative to the Sun) and a substellar C/O ratio. The inferred high metallicity and low C/O ratio may indicate significant accretion of solid materials during planet formation (for example, refs. (3,4)(,)) or disequilibrium processes in the upper atmosphere (for example, refs. (5,6)).

引用

页码：653 / +

页数：23

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