The atmospheric composition of the ultra-hot Jupiter WASP-178 b observed with ESPRESSO
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arXiv
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2024
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| author | Damasceno, Y. C. Seidel, J. V. Prinoth, B. Psaridi, A. Esparza-Borges, E. Stangret, M. Santos, N. C. Zapatero-Osorio, M. R. Alibert, Y. Allart, R. Silva, T. Azevedo Cointepas, M. Silva, A. R. Costa Cristo, E. Di Marcantonio, P. Ehrenreich, D. Hernández, J. I. González Herrero-Cisneros, E. Lendl, M. Lillo-Box, J. Martins, C. J. A. P. Micela, G. Pallé, E. Sousa, S. G. Steiner, M. Vaulato, V. Zhao, Y. Pepe, F. |
| author_facet | Damasceno, Y. C. Seidel, J. V. Prinoth, B. Psaridi, A. Esparza-Borges, E. Stangret, M. Santos, N. C. Zapatero-Osorio, M. R. Alibert, Y. Allart, R. Silva, T. Azevedo Cointepas, M. Silva, A. R. Costa Cristo, E. Di Marcantonio, P. Ehrenreich, D. Hernández, J. I. González Herrero-Cisneros, E. Lendl, M. Lillo-Box, J. Martins, C. J. A. P. Micela, G. Pallé, E. Sousa, S. G. Steiner, M. Vaulato, V. Zhao, Y. Pepe, F. |
| contents | We search for atmospheric constituents for the UHJ WASP-178 b with two ESPRESSO transits using the narrow-band and cross-correlation techniques, focusing on the detections of NaI, H$α$, H$β$, H$γ$, MgI, FeI and FeII. Additionally, we show parallel photometry used to obtain updated and precise stellar, planetary and orbital parameters. We report the resolved line detections of NaI (5.5 and 5.4 $σ$), H$α$ (13 $σ$), H$β$ (7.1 $σ$), and tentatively MgI (4.6 $σ$). In cross-correlation, we confirm the MgI detection (7.8 and 5.8 $σ$) and additionally report the detections of FeI (12 and 10 $σ$) and FeII (11 and 8.4 $σ$), on both nights separately. The detection of MgI remains tentative, however, due to the differing results between both nights, as well as compared with the narrow-band derived properties. None of our resolved spectral lines probing the mid- to upper atmosphere show significant shifts relative to the planetary rest frame, however H$α$ and H$β$ exhibit line broadenings of 39.6 $\pm$ 2.1 km/s and 27.6 $\pm$ 4.6 km/s, respectively, indicating the onset of possible escape. WASP-178 b differs from similar UHJ with its lack of strong atmospheric dynamics in the upper atmosphere, however the broadening seen for FeI (15.66 $\pm$ 0.58 km/s) and FeII (11.32 $\pm$ 0.52 km/s) could indicate the presence of winds in the mid-atmosphere. Future studies on the impact of the flux variability caused by the host star activity might shed more light on the subject. Previous work indicated the presence of SiO cloud-precursors in the atmosphere of WASP-178 b and a lack of MgI and FeII. However, our results suggest that a scenario where the planetary atmosphere is dominated by MgI and FeII is more likely. In light of our results, we encourage future observations to further elucidate these atmospheric properties. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2406_08348 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The atmospheric composition of the ultra-hot Jupiter WASP-178 b observed with ESPRESSO Damasceno, Y. C. Seidel, J. V. Prinoth, B. Psaridi, A. Esparza-Borges, E. Stangret, M. Santos, N. C. Zapatero-Osorio, M. R. Alibert, Y. Allart, R. Silva, T. Azevedo Cointepas, M. Silva, A. R. Costa Cristo, E. Di Marcantonio, P. Ehrenreich, D. Hernández, J. I. González Herrero-Cisneros, E. Lendl, M. Lillo-Box, J. Martins, C. J. A. P. Micela, G. Pallé, E. Sousa, S. G. Steiner, M. Vaulato, V. Zhao, Y. Pepe, F. Earth and Planetary Astrophysics We search for atmospheric constituents for the UHJ WASP-178 b with two ESPRESSO transits using the narrow-band and cross-correlation techniques, focusing on the detections of NaI, H$α$, H$β$, H$γ$, MgI, FeI and FeII. Additionally, we show parallel photometry used to obtain updated and precise stellar, planetary and orbital parameters. We report the resolved line detections of NaI (5.5 and 5.4 $σ$), H$α$ (13 $σ$), H$β$ (7.1 $σ$), and tentatively MgI (4.6 $σ$). In cross-correlation, we confirm the MgI detection (7.8 and 5.8 $σ$) and additionally report the detections of FeI (12 and 10 $σ$) and FeII (11 and 8.4 $σ$), on both nights separately. The detection of MgI remains tentative, however, due to the differing results between both nights, as well as compared with the narrow-band derived properties. None of our resolved spectral lines probing the mid- to upper atmosphere show significant shifts relative to the planetary rest frame, however H$α$ and H$β$ exhibit line broadenings of 39.6 $\pm$ 2.1 km/s and 27.6 $\pm$ 4.6 km/s, respectively, indicating the onset of possible escape. WASP-178 b differs from similar UHJ with its lack of strong atmospheric dynamics in the upper atmosphere, however the broadening seen for FeI (15.66 $\pm$ 0.58 km/s) and FeII (11.32 $\pm$ 0.52 km/s) could indicate the presence of winds in the mid-atmosphere. Future studies on the impact of the flux variability caused by the host star activity might shed more light on the subject. Previous work indicated the presence of SiO cloud-precursors in the atmosphere of WASP-178 b and a lack of MgI and FeII. However, our results suggest that a scenario where the planetary atmosphere is dominated by MgI and FeII is more likely. In light of our results, we encourage future observations to further elucidate these atmospheric properties. |
| title | The atmospheric composition of the ultra-hot Jupiter WASP-178 b observed with ESPRESSO |
| topic | Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2406.08348 |