JWST COMPASS: A NIRSpec/G395H Transmission Spectrum of the Sub-Neptune TOI-836c

Planets between the sizes of Earth and Neptune are the most common in the Galaxy, bridging the gap between the terrestrial and giant planets in our solar system. Now that we are firmly in the era of JWST, we can begin to measure, in more detail, the atmospheres of these ubiquitous planets to better...

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Bibliographic Details
Published in:The Astronomical journal 2024-08, Vol.168 (2), p.77
Main Authors: Wallack, Nicole L., Batalha, Natasha E., Alderson, Lili, Scarsdale, Nicholas, Adams Redai, Jea I., Aguichine, Artyom, Alam, Munazza K., Gao, Peter, Wolfgang, Angie, Batalha, Natalie M., Kirk, James, López-Morales, Mercedes, Moran, Sarah E., Teske, Johanna, Wakeford, Hannah R., Wogan, Nicholas F.
Format: Article
Language:English
Subjects:
Aerosols
Atmosphere
Atmospheric correction
Atmospheric pressure
Exoplanet atmospheres
Exoplanet atmospheric composition
Exoplanets
Extrasolar planets
Galaxies
Infrared spectroscopy
James Webb Space Telescope
Neptune
Planet formation
Planetary atmospheres
Planetary composition
Planetary evolution
Planets
Solar system
Stellar planets
Trajectory measurement
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Summary:Planets between the sizes of Earth and Neptune are the most common in the Galaxy, bridging the gap between the terrestrial and giant planets in our solar system. Now that we are firmly in the era of JWST, we can begin to measure, in more detail, the atmospheres of these ubiquitous planets to better understand their evolutionary trajectories. The two planets in the TOI-836 system are ideal candidates for such a study, as they fall on either side of the radius valley, allowing for direct comparisons of the present-day atmospheres of planets that formed in the same environment but had different ultimate end states. We present results from the JWST NIRSpec G395H transit observation of the larger and outer of the planets in this system, TOI-836c (2.587 R ⊕ , 9.6 M ⊕ , T eq ∼ 665 K). While we measure average 30-pixel binned precisions of ∼24 ppm for NRS1 and ∼43 ppm for NRS2 per spectral bin, we do find residual correlated noise in the data, which we attempt to correct using the JWST Engineering Database. We find a featureless transmission spectrum for this sub-Neptune planet and are able to rule out atmospheric metallicities
ISSN:0004-6256
1538-3881
DOI:10.3847/1538-3881/ad3917