Chen, G.; Pallé, E.; Parviainen, H.; Wang, H.; van Boekel, R.; Murgas, F.; Yan, F.; Béjar, V. J. S.; Casasayas-Barris, N.; Crouzet, N.; Esparza-Borges, E.; Fukui, A.; Garai, Z.; Kawauchi, K.; Kurita, S.; Kusakabe, N.; de Leon, J. P.; Livingston, J.; Luque, R.; Madrigal-Aguado, A.; Mori, M.; Narita, N.; Nishiumi, T.; Oshagh, M.; Sánchez-Benavente, M.; Tamura, M.; Terada, Y.; Watanabe, N.
Bibliographical reference
Monthly Notices of the Royal Astronomical Society
Description
We present the optical transmission spectrum of the hot Jupiter WASP-104b based on one transit observed by the blue and red channels of the Double Spectrograph (DBSP) at the Palomar 200-inch telescope and 14 transits observed by the MuSCAT2 four-channel imager at the 1.52-m Telescopio Carlos Sánchez. We also analyse 45 additional K2 transits, after correcting for the flux contamination from a companion star. Together with the transit light curves acquired by DBSP and MuSCAT2, we are able to revise the system parameters and orbital ephemeris, confirming that no transit timing variations exist. Our DBSP and MuSCAT2 combined transmission spectrum reveals an enhanced slope at wavelengths shorter than 630 nm and suggests the presence of a cloud deck at longer wavelengths. While the Bayesian spectral retrieval analyses favour a hazy atmosphere, stellar spot contamination cannot be completely ruled out. Further evidence, from transmission spectroscopy and detailed characterization of the host star's activity, is required to distinguish the physical origin of the enhanced slope.
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