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JWST Reveals CH$_4$, CO$_2$, and H$_2$O in a Metal-rich Miscible Atmosphere on a Two-Earth-Radius Exoplanet

Authors :
Benneke, Björn
Roy, Pierre-Alexis
Coulombe, Louis-Philippe
Radica, Michael
Piaulet, Caroline
Ahrer, Eva-Maria
Pierrehumbert, Raymond
Krissansen-Totton, Joshua
Schlichting, Hilke E.
Hu, Renyu
Yang, Jeehyun
Christie, Duncan
Thorngren, Daniel
Young, Edward D.
Pelletier, Stefan
Knutson, Heather A.
Miguel, Yamila
Evans-Soma, Thomas M.
Dorn, Caroline
Gagnebin, Anna
Fortney, Jonathan J.
Komacek, Thaddeus
MacDonald, Ryan
Raul, Eshan
Cloutier, Ryan
Acuna, Lorena
Lafrenière, David
Cadieux, Charles
Doyon, René
Welbanks, Luis
Allart, Romain
Publication Year :
2024

Abstract

Even though sub-Neptunes likely represent the most common outcome of planet formation, their natures remain poorly understood. In particular, planets near 1.5-2.5$\,R_\oplus$ often have bulk densities that can be explained equally well with widely different compositions and interior structures, resulting in grossly divergent implications for their formation. Here, we present the full 0.6-5.2$\,\mu \mathrm{m}$ JWST NIRISS/SOSS+NIRSpec/G395H transmission spectrum of the 2.2$\,R_\oplus$ TOI-270d ($4.78\,M_\oplus$, $T_\mathrm{eq}$=350-380 K), delivering unprecedented sensitivity for atmospheric characterization in the sub-Neptune regime. We detect five vibrational bands of CH$_4$ at 1.15, 1.4, 1.7, 2.3, and 3.3$\,\mu$m (9.4$\sigma$), the signature of CO$_2$ at 4.3$\,\mu$m (4.8$\sigma$), water vapor (2.5$\sigma$), and potential signatures of SO$_2$ at 4.0$\,\mu \mathrm{m}$ and CS$_2$ at 4.6$\,\mu\mathrm{m}$. Intriguingly, we find an overall highly metal-rich atmosphere, with a mean molecular weight of $5.47_{-1.14}^{+1.25}$. We infer an atmospheric metal mass fraction of $58_{-12}^{+8}\%$ and a C/O of $0.47_{-0.19}^{+0.16}$, indicating that approximately half the mass of the outer envelope is in high-molecular-weight volatiles (H$_2$O, CH$_4$, CO, CO$_2$) rather than H$_2$/He. We introduce a sub-Neptune classification scheme and identify TOI-270d as a "miscible-envelope sub-Neptune" in which H$_2$/He is well-mixed with the high-molecular-weight volatiles in a miscible supercritical metal-rich envelope. For a fully miscible envelope, we conclude that TOI-270d's interior is $90_{-4}^{+3}\,$wt$\,\%$ rock/iron, indicating that it formed as a rocky planet that accreted a few wt % of H$_2$/He, with the overall envelope metal content explained by magma-ocean/envelope reactions without the need for significant ice accretion. TOI-270d may well be an archetype of the overall population of sub-Neptunes.<br />Comment: 25 pages, 12 figures

Details

Database :
arXiv
Publication Type :
Report
Accession number :
edsarx.2403.03325
Document Type :
Working Paper