High-resolution Transmission Spectroscopy of Ultrahot Jupiter WASP–33b with NEID

We report an attempt to detect molecular and atomic species in the atmosphere of the ultrahot Jupiter WASP-33b using the high-resolution echelle spectrograph NEID with a wavelength coverage of 380–930 nm. By analyzing the transmission spectrum of WASP-33b using the line-by-line technique and the cro...

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Bibliographic Details
Published in:The Astronomical journal 2024-01, Vol.167 (1), p.36
Main Authors: Yang, Yuanheng, Chen, Guo, Wang, Songhu, Yan, Fei
Format: Article
Language:English
Subjects:
Astrochemistry
Atmosphere
Chemical composition
Cross correlation
Exoplanet atmospheres
Exoplanet atmospheric composition
Exoplanets
Extrasolar gaseous giant planets
Gaussian process
High resolution
High resolution spectroscopy
Hot Jupiters
Jupiter
Jupiter atmosphere
Spectroscopy
Spectrum analysis
Transmission spectroscopy
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Summary:We report an attempt to detect molecular and atomic species in the atmosphere of the ultrahot Jupiter WASP-33b using the high-resolution echelle spectrograph NEID with a wavelength coverage of 380–930 nm. By analyzing the transmission spectrum of WASP-33b using the line-by-line technique and the cross-correlation technique, we confirm previous detection of H α , H β , H γ , and Ca ii infrared triplets. We find no evidence for a significant day-to-night wind in WASP-33b, taking into account the effects of stellar pulsations using a relatively novel Gaussian process method and poorly constrained systemic velocity measurements. We also detect the previously reported pretransit absorption signal, which may be a pulsation mode induced by the planet. Combined with previous CARMENES and HARPS-N observations, we report the nondetection of TiO, Ti i , and V i in the transmission spectrum, while they were already detected in the dayside atmosphere of WASP-33b. This implies a difference in the chemical compositions and abundances between the dayside and terminator atmospheres of WASP-33b and certainly requires further improvements in the sensitivity of the detection methods.
ISSN:0004-6256
1538-3881
DOI:10.3847/1538-3881/ad10a3