Published September 1, 2023
| Version v1
Journal article
Open
ACCESS, LRG-BEASTS, \& MOPSS: Featureless Optical Transmission Spectra of WASP-25b and WASP-124b
Creators
- 1. Center for Astrophysics | Harvard | Smithsonian
- 2. Department of Physics, Imperial College London
- 3. Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology
- 4. Bloomberg Center for Physics and Astronomy
- 5. Centre for Exoplanets and Habitability, University of Warwick
- 6. Department of Astronomy, University of Michigan
- 7. Carnegie Earth | Planets Laboratory
- 8. Department of Physics and Astronomy, Johns Hopkins
- 9. Space Telescope Science Institute (STScI)
- 10. Astrophysics Group, Department of Physics \& Astronomy
- 11. Facultad de Ingeniera y Ciencias, Universidad Adolfo
- 12. University of Michigan, Astronomy
- 13. University of Michigan, Astronomy Department
- 14. Las Campanas Observatory, Carnegie Institution of Washington
Description
We present new optical transmission spectra for two hot Jupiters: WASP-25b (M~=~0.56~M$_J$; R~=~1.23~R$_J$; P~=~3.76~days) and WASP-124b (M~=~0.58~M$_J$; R~=~1.34~R$_J$; P~=~3.37~days), with wavelength coverage of 4200 -- 9100\AA~and 4570 -- 9940\AA, respectively. These spectra are from EFOSC2 mounted on the New Technology Telescope (NTT) and IMACS on Magellan Baade. No strong spectral features were found at 4 and 6 scale heights, respectively. \texttt{Exoretrievals} and \texttt{PLATON} retrievals moderately favor ($\sim 3 \sigma$) stellar activity for WASP-25b, while a completely featureless spectrum is slightly favored ( < 2 $\sigma$) for WASP-124b. For both planets the retrievals found a wide range in the depth where the atmosphere is optically thick ($\sim$0.4 $\mu$bars -- 6 bars), and recover a temperature that is consistent with the planets' equilibrium temperatures, but with wide uncertainties (up to $\pm$400K). For WASP-25b, the models also favor stellar spots that are $\sim$1400--1800K cooler than the surrounding photosphere. The fairly weak constraints on parameters owe to the relatively low precision of the data, with an average precision of 840 and 1300~ppm per bin for WASP-25 and WASP-124b, respectively. The average width of each bin is $\sim$ 150{\AA} and 160 {\AA}, respectively. However, some contribution might still be due to an inherent absence of absorption or scattering in the planets' upper atmospheres, possibly because of aerosols. We attempt to fit the strength of the sodium signals to the aerosol--metallicity trend proposed by \cite{McGruder:2023}, and find WASP-25b is consistent with the prediction, while WASP-124b has too large uncertainties to better constrain the predicted trend.
Notes
The binned light curves for each transit (Figures 6 - 11). Including the unused partial transit of WASP-124 on UT190615. The individual transmission spectra of each night, including the unused partial transit of WASP-124. In addition, the combined transmission spectra (Table 6).
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W124_ut180915_PCA_B1p58.png
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