1. GEMS JWST: Transmission spectroscopy of TOI-5205b reveals significant stellar contamination and a metal-poor atmosphere
- Author
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Cañas, Caleb I., Lustig-Yaeger, Jacob, Tsai, Shang-Min, Müller, Simon, Helled, Ravit, Louie, Dana R., Caloca, Giannina Guzmán, Kanodia, Shubham, Gao, Peter, Libby-Roberts, Jessica, Hardegree-Ullman, Kevin K., Colón, Knicole D., Czekala, Ian, Delamer, Megan, Han, Te, Lin, Andrea S. J., Mahadevan, Suvrath, May, Erin M., Ninan, Joe P., Piette, Anjali A. A., Stefánsson, Guðmundur, Stevenson, Kevin B., Teske, Johanna, and Wallack, Nicole L.
- Subjects
Astrophysics - Earth and Planetary Astrophysics - Abstract
Recent discoveries of transiting giant exoplanets around M dwarfs (GEMS) present an opportunity to investigate their atmospheric compositions and explore how such massive planets can form around low-mass stars contrary to canonical formation models. Here, we present the first transmission spectra of TOI-5205b, a short-period ($P=1.63~\mathrm{days}$) Jupiter-like planet ($M_p=1.08~\mathrm{M_J}$ and $R_p=0.94~\mathrm{R_J}$) orbiting an M4 dwarf. We obtained three transits using the PRISM mode of the JWST Near Infrared Spectrograph (NIRSpec) spanning $0.6-5.3$ um. Our data reveal significant stellar contamination that is evident in the light curves as spot-crossing events and in the transmission spectra as a larger transit depth at bluer wavelengths. Atmospheric retrievals demonstrate that stellar contamination from unocculted star spots is the dominant component of the transmission spectrum at wavelengths $\lambda\lesssim3.0$ um, which reduced the sensitivity to the presence of clouds or hazes in our models. The degree of stellar contamination also prevented the definitive detection of any $\mathrm{H_2O}$, which has primary absorption features at these shorter wavelengths. The broad wavelength coverage of NIRSpec PRISM enabled a robust detection of $\mathrm{CH_4}$ and $\mathrm{H_2S}$, which have detectable molecular features between $3.0-5.0$ um. Our gridded and Bayesian retrievals consistently favored an atmosphere with both sub-solar metallicity ($\log\mathrm{[M/H]}\sim-2$ for a clear atmosphere) and super-solar C/O ratio ($\log\mathrm{[C/O]}\sim3$ for a clear or cloudy atmosphere). This contrasts with estimates from planetary interior models that predict a bulk metallicity of 10--20%, which is $\sim100\times$ the atmospheric metallicity, and suggests that the planetary interior for TOI-5205b is decoupled from its atmosphere and not well mixed., Comment: 27 pages + appendix, includes figure sets that will appear in journal, submitted to AAS. Comments welcome
- Published
- 2025