Early Release Science of the exoplanet WASP-39b with JWST NIRSpec G395H
dc.contributor.author | Alderson, L | |
dc.contributor.author | Wakeford, HR | |
dc.contributor.author | Alam, MK | |
dc.contributor.author | Batalha, NE | |
dc.contributor.author | Lothringer, JD | |
dc.contributor.author | Redai, JA | |
dc.contributor.author | Barat, S | |
dc.contributor.author | Brande, J | |
dc.contributor.author | Damiano, M | |
dc.contributor.author | Daylan, T | |
dc.contributor.author | Espinoza, N | |
dc.contributor.author | Flagg, L | |
dc.contributor.author | Goyal, JM | |
dc.contributor.author | Grant, D | |
dc.contributor.author | Hu, R | |
dc.contributor.author | Inglis, J | |
dc.contributor.author | Lee, EKH | |
dc.contributor.author | Mikal-Evans, T | |
dc.contributor.author | Ramos-Rosado, L | |
dc.contributor.author | Roy, P-A | |
dc.contributor.author | Wallack, NL | |
dc.contributor.author | Batalha, NM | |
dc.contributor.author | Bean, JL | |
dc.contributor.author | Benneke, B | |
dc.contributor.author | Berta-Thompson, ZK | |
dc.contributor.author | Carter, AL | |
dc.contributor.author | Changeat, Q | |
dc.contributor.author | Colón, KD | |
dc.contributor.author | Crossfield, IJM | |
dc.contributor.author | Désert, J-M | |
dc.contributor.author | Foreman-Mackey, D | |
dc.contributor.author | Gibson, NP | |
dc.contributor.author | Kreidberg, L | |
dc.contributor.author | Line, MR | |
dc.contributor.author | López-Morales, M | |
dc.contributor.author | Molaverdikhani, K | |
dc.contributor.author | Moran, SE | |
dc.contributor.author | Morello, G | |
dc.contributor.author | Moses, JI | |
dc.contributor.author | Mukherjee, S | |
dc.contributor.author | Schlawin, E | |
dc.contributor.author | Sing, DK | |
dc.contributor.author | Stevenson, KB | |
dc.contributor.author | Taylor, J | |
dc.contributor.author | Aggarwal, K | |
dc.contributor.author | Ahrer, E-M | |
dc.contributor.author | Allen, NH | |
dc.contributor.author | Barstow, JK | |
dc.contributor.author | Bell, TJ | |
dc.contributor.author | Blecic, J | |
dc.contributor.author | Casewell, SL | |
dc.contributor.author | Chubb, KL | |
dc.contributor.author | Crouzet, N | |
dc.contributor.author | Cubillos, PE | |
dc.contributor.author | Decin, L | |
dc.contributor.author | Feinstein, AD | |
dc.contributor.author | Fortney, JJ | |
dc.contributor.author | Harrington, J | |
dc.contributor.author | Heng, K | |
dc.contributor.author | Iro, N | |
dc.contributor.author | Kempton, EM-R | |
dc.contributor.author | Kirk, J | |
dc.contributor.author | Knutson, HA | |
dc.contributor.author | Krick, J | |
dc.contributor.author | Leconte, J | |
dc.contributor.author | Lendl, M | |
dc.contributor.author | MacDonald, RJ | |
dc.contributor.author | Mancini, L | |
dc.contributor.author | Mansfield, M | |
dc.contributor.author | May, EM | |
dc.contributor.author | Mayne, NJ | |
dc.contributor.author | Miguel, Y | |
dc.contributor.author | Nikolov, NK | |
dc.contributor.author | Ohno, K | |
dc.contributor.author | Palle, E | |
dc.contributor.author | Parmentier, V | |
dc.contributor.author | Petit dit de la Roche, DJM | |
dc.contributor.author | Piaulet, C | |
dc.contributor.author | Powell, D | |
dc.contributor.author | Rackham, BV | |
dc.contributor.author | Redfield, S | |
dc.contributor.author | Rogers, LK | |
dc.contributor.author | Rustamkulov, Z | |
dc.contributor.author | Tan, X | |
dc.contributor.author | Tremblin, P | |
dc.contributor.author | Tsai, S-M | |
dc.contributor.author | Turner, JD | |
dc.contributor.author | de Val-Borro, M | |
dc.contributor.author | Venot, O | |
dc.contributor.author | Welbanks, L | |
dc.contributor.author | Wheatley, PJ | |
dc.contributor.author | Zhang, X | |
dc.date.accessioned | 2023-01-19T11:47:59Z | |
dc.date.issued | 2023-01-09 | |
dc.date.updated | 2023-01-18T20:23:11Z | |
dc.description.abstract | Measuring the abundances of carbon and oxygen in exoplanet atmospheres is considered a crucial avenue for unlocking the formation and evolution of exoplanetary systems. Access to an exoplanet’s chemical inventory requires high precision observations, often inferred from individual molecular detections with low-resolution space-based and high-resolution ground-based facilities. Here we report the medium-resolution (R≈600) transmission spectrum of an exoplanet atmosphere between 3–5 μm covering multiple absorption features for the Saturn-mass exoplanet WASP-39b, obtained with JWST NIRSpec G395H. Our observations achieve 1.46× photon precision, providing an average transit depth uncertainty of 221 ppm per spectroscopic bin, and present minimal impacts from systematic effects. We detect significant absorption from CO2 (28.5σ ) and H2O (21.5σ ), and identify SO2 as the source of absorption at 4.1 μ m (4.8σ ). Best-fit atmospheric models range between 3× and 10× solar metallicity, with sub-solar to solar C/O ratios. These results, including the detection of SO2, underscore the importance of characterising the chemistry in exoplanet atmospheres, and showcase NIRSpec G395H as an excellent mode for time series observations over this critical wavelength range. | en_GB |
dc.description.sponsorship | Science and Technology Facilities Council (STFC) | en_GB |
dc.description.sponsorship | UKRI | |
dc.identifier.citation | Published online 9 January 2023 | en_GB |
dc.identifier.doi | 10.1038/s41586-022-05591-3 | |
dc.identifier.grantnumber | ST/W507337/1 | en_GB |
dc.identifier.grantnumber | MR/T040866/1 | |
dc.identifier.uri | http://hdl.handle.net/10871/132275 | |
dc.identifier | ORCID: 0000-0001-6707-4563 (Mayne, Nathan) | |
dc.language.iso | en | en_GB |
dc.publisher | Nature Research | en_GB |
dc.rights | © 2023. This version is made available under the CC-BY 4.0 license: https://creativecommons.org/licenses/by/4.0/ | en_GB |
dc.title | Early Release Science of the exoplanet WASP-39b with JWST NIRSpec G395H | en_GB |
dc.type | Article | en_GB |
dc.date.available | 2023-01-19T11:47:59Z | |
dc.description | This is the author accepted manuscript. The final version is available from Nature Research via the DOI in this record | en_GB |
dc.description | Data Availability: The data used in this paper are associated with JWST program ERS 1366 (observation #4) and are available from the Mikulski Archive for Space Telescopes (https://mast.stsci.edu). Science data processing version (SDP_VER) 2022_2a generated the uncalibrated data that we downloaded from MAST. We used JWST Calibration Pipeline software version (CAL_VER) 1.5.3 with modifications described in the text. We used calibration reference data from context (CRDS_CTX) 0916, except as noted in the text. All the data and models presented in this publication can be found at 10.5281/zenodo.7185300. | en_GB |
dc.description | Code Availability: The codes used in this publication to extract, reduce and analyze the data are as follows; STScI JWST Calibration pipeline45 (https://github.com/spacetelescope/jwst), Eureka!53 (https://eurekadocs.readthedocs.io/en/latest/), ExoTiC-JEDI47 (https://github.com/ExoTiC/ExoTiC-JEDI), juliet71 (https://juliet.readthedocs.io/en/latest/), Tiberius15,49,50, transitspectroscopy51 (https://github.com/nespinoza/transitspectroscopy). In addition, these made use of batman65 (http://lkreidberg.github.io/batman/docs/html/index.html), celerite86 (https://celerite.readthedocs.io/en/stable/), chromatic (https://zkbt.github.io/chromatic/), Dynesty72 (https://dynesty.readthedocs.io/en/stable/index.html), emcee69 (https://emcee.readthedocs.io/en/stable/), exoplanet83 (https://docs.exoplanet.codes/en/latest/), ExoTEP75–77, ExoTHETyS79 (https://github.com/ucl-exoplanets/ExoTETHyS), ExoTiCISM57 (https://github.com/Exo-TiC/ExoTiC-ISM), ExoTiC-LD58 (https://exoticld.readthedocs.io/en/latest/), george68 (https://george.readthedocs.io/en/latest/) JAX82 (https://jax.readthedocs.io/en/latest/), LMFIT70 (https://lmfit.github.io/lmfit-py/), Pylightcurve78 (https://github.com/ucl-exoplanets/pylightcurve), Pymc3138 (https://docs.pymc.io/en/v3/index.html) and Starry84 (https://starry.readthedocs.io/en/latest/), each of which use the standard python libraries astropy139,140, matplotlib141, numpy142, pandas143, scipy64 and xarray144. The atmospheric models used to fit the data can be found at ATMO[Tremblin2015,Drummond2016,Goyal2018,Goyal2020]88–91, PHOENIX92–94, PICASO98,99 (https://natashabatalha.github.io/picaso/), Virga98,107 (https://natashabatalha.github.io/virga/), and gCMCRT115 (https://github.com/ELeeAstro/gCMCRT). | en_GB |
dc.identifier.eissn | 1476-4687 | |
dc.identifier.journal | Nature | en_GB |
dc.relation.ispartof | Nature | |
dc.rights.uri | https://creativecommons.org/licenses/by/4.0/ | en_GB |
dcterms.dateAccepted | 2022-11-24 | |
dcterms.dateSubmitted | 2022-10-13 | |
rioxxterms.version | AM | en_GB |
rioxxterms.licenseref.startdate | 2023-01-09 | |
rioxxterms.type | Journal Article/Review | en_GB |
refterms.dateFCD | 2023-01-18T20:23:22Z | |
refterms.versionFCD | AM | |
refterms.dateFOA | 2023-01-19T11:48:03Z | |
refterms.panel | B | en_GB |
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