Detection of the tidal deformation of WASP-103b at 3 <i>σ</i> with CHEOPS <i>(Corrigendum)</i>

Barros, S. C. C.; Akinsanmi, Babatunde; Boué, G.; Smith, A. M. S.; Laskar, Jacques; Ulmer-Moll, S.; Lillo-Box, J.; Queloz, D.; Cameron, A. Collier; Sousa, S. G.; Ehrenreich, D.; Hooton, Matthew J.; Bruno, G.; Demory, B. O.; Correia, A. C. M.; Wilson, T. G.; Bonfanti, A.; Hoyer, S.; Alibert, Yann; Alonso, R.; Anglada-Escudé, G.; Barbato, D.; Bárczy, T.; Barrado, D.; Baumjohann, W.; Beck, M.; Beck, T.; Benz, W.; Bergomi, Maria; Billot, N.; Bonfils, X.; Bouchy, F.; Brandeker, Alexis; Broeg, C.; Cabrera, J.; Cessa, Virginie; Charnoz, S.; Damme, C. Corral Van; Davies, Melvyn B.; Deleuil, M.; Deline, A.; Delrez, Laetitia; Erikson, A.; Fortier, A.; Fossati, L.; Fridlund, M.; Muñoz, A. García; Gillon, M.; Güdel, M.; Isaak, K. G.; Heng, Kevin; Kiss, L. L.; Étangs, A. Lecavelier des; Lendl, M.; Magrin, Demetrio; Nascimbeni, V.; Maxted, P. F. L.; Olofsson, G.; Ottensamer, R.; Pagano, I.; Πάλλη, Ε.; Parviainen, H.; Peter, G.; Piotto, G.; Pollacco, D.; Ragazzoni, Roberto; Rando, N.; Rauer, H.; Ribas, I.; Salmon, Sébastien; Santos, N. C.; Scandariato, G.; Ségransan, D.; Simon, A. E.; Steller, M.; Szabó, Gy. M.; Thomas, N.; Udry, S.; Ulmer, B.; Grootel, V. Van; Walton, N. A.

doi:10.1051/0004-6361/202142196e

Cited by 4 publications

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“…In such cases, addition of new precise data can change the situation dramatically as we experienced in the TTV analysis of WASP-103 b. Before the inclusion of 10 precise light curves from Kirk et al (2021), our results were in agreement with the finding of Maciejewski et al (2018), Patra et al (2020), and most recently Barros et al (2022), which also lacks these data points, of an increase in the orbital period against the expectation of an orbital decay from this ultra short-period hot-Jupiter (P orb " 0.926 days). When the recent data were added, a negative quadratic coefficient was found.…”

Section: Discussion On Transit Timing Variationssupporting

confidence: 91%

“…They constrained the reduced tidal quality factor to be Q 1 ą p1.1 ˘0.1q ˆ10 5 with 95% confidence as a result, contradicting the previous findings and potential mass-loss expected from the nature of the planet. Most recently Barros et al (2022) also found an increase in the orbital period based on their data set extended by their own observations with CHEOPS as well as re-reduced HST and Spitzer data. However, their quadratic model is not statistically superior to the linear model.…”

Section: Wasp-103 Systemmentioning

confidence: 71%

“…The linear model turned out to be superior to the linear + quadratic model, the quadratic term of which is found to be negative. However, until the time of the recent publication of very precise transit observations of WASP-103 b by Kirk et al (2021), the trend that was observed in the TTV was an upward parabola as found by Patra et al (2020) and Barros et al (2022), which lack the data from Kirk et al (2021) in their analysis, in contrast of the expectation of an orbital decay from the ultra-short period. These observations seem to have changed the picture and showed the need for further precise observations of the target to reveal its orbital period behaviour.…”

Section: Wasp-103 Systemmentioning

confidence: 91%

“…We observed the transits of the planet in high precision with 1 m T100 three times, and 1.23 m telescope of CAHA twice in addition to an observation with T35 with inferior quality. We collected 55 precise light curves from the literature, including 14 from Southworth et al (2015), the TRAPPIST light curve from (Gillon et al 2014), three from Lendl et al (2017), one light curve from (Turner et al 2017), two from (Delrez et al 2018), eight in total from Maciejewski et al (2018), four from Patra et al (2020), 10 very precise light curves obtained with different instruments to form a transmission spectrum of WASP-103 b from Kirk et al (2021), and most recently twelve light curves from Barros et al (2022), four of which we had to eliminate due to insufficient sampling for timing analyis. We found 22 complete light curves in the ETD, five of which were eliminated by our selection criteria.…”

Section: Wasp-103 Systemmentioning

confidence: 99%

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Homogeneous transit timing analyses of 10 exoplanet systems

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Esmer

Yalçınkaya

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We study the transit timings of 10 exoplanets in order to investigate potential Transit Timing Variations (TTVs) in them. We model their available ground-based light curves, some presented here and others taken from the literature, and homogeneously measure the mid-transit times. We statistically compare our results with published values and find that the measurement errors agree. However, in terms of recovering the possible frequencies, homogeneous sets can be found to be more useful, of which no statistically relevant example has been found for the planets in our study. We corrected the ephemeris information of all ten planets we studied and provide these most precise light elements as references for future transit observations with space-borne and ground-based instruments. We found no evidence for secular or periodic changes in the orbital periods of the planets in our sample, including the ultra-short period WASP-103 b, whose orbit is expected to decay on an observable timescale. Therefore, we derive the lower limits for the reduced tidal quality factors (Q$^{\prime }_{\star }$) for the host stars based on best fitting quadratic functions to their timing data. We also present a global model of all available data for WASP-74 b, which has a Gaia parallax-based distance value ∼25 per cent larger than the published value.

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Section: Discussion On Transit Timing Variationssupporting

confidence: 91%

Section: Wasp-103 Systemmentioning

confidence: 71%

Section: Wasp-103 Systemmentioning

confidence: 91%

Section: Wasp-103 Systemmentioning

confidence: 99%

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Homogeneous transit timing analyses of 10 exoplanet systems

Baştürk

Esmer

Yalçınkaya

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Signature of the atmospheric asymmetries of hot and ultra-hot Jupiters in light curves

Falco,

Leconte,

Mechineau

et al. 2024

A&A

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With the new generation of space telescopes such as the James Webb Space Telescope (JWST), it is possible to better characterize the atmospheres of exoplanets. The atmospheres of Hot and are highly heterogeneous and asymmetrical. The difference between the temperatures on the day and night sides is especially extreme in the case of We introduce a new tool to compute synthetic light curves from 3D general circulation model (GCM) simulations, developed in the framework. We show how rotation induces a variation in the flux during the transit that is a source of information on the chemical and thermal distribution of the atmosphere. We find that the day-night gradient linked to has an effect close to stellar limb darkening, but opposite to tidal deformation. We confirm the impact of the atmospheric and chemical distribution on variations in the central transit time, though the variations found are smaller than those in available observational data, which could indicate that the east-west asymmetries are underestimated, due to the chemistry or clouds.

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The phase curve of the ultra-hot Jupiter WASP-167b as seen by TESS

Kálmán,

Derekas,

Csizmadia

et al. 2024

A&A

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Ultra-hot Jupiters (UHJs) orbiting pulsating A/F stars represent an important subset of the exoplanetary demographic. They are excellent candidates for the study of exoplanetary atmospheres, and are astrophysical laboratories for the investigation of planet-to-star interactions. We analysed the TESS light curve of the WASP-167 system, consisting of an F1V star and a substellar companion on a $ 2.02$ day orbit. We modelled the combination of the ellipsoidal variability and the Doppler beaming to measure the mass of WASP-167b, and the reflection effect to obtain constraints on the geometric albedo, while placing a special emphasis on noise separation. We implemented a basic model to determine the dayside ($T_ Day $), nightside ($T_ Night $), and intrinsic ($T_ Internal $) temperatures of WASP-167b, and put a constraint on its Bond albedo. We confirm the transit parameters of the planet seen in the literature. We find that a resonant $ $ stellar signal (which may originate from planet-to-star interactions) interferes with the phase curve analysis. After careful and thought-out treatment of this signal, we find $M_p = 0.34 0.22$ $M_J$. We measure a dayside temperature of $2790 100$ K, classifying WASP-167b as an UHJ. We find a $2 upper limit of $0.51$ on its Bond albedo, and determine the geometric albedo at $0.34 uncertainty). With an occultation depth of $106.8 27.3$ ppm in the TESS passband, the UHJ WASP-167b is an excellent target for atmospheric studies, especially those at thermal wavelength ranges, where the stellar pulsations are expected to be less influential.

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Detection of the tidal deformation of WASP-103b at 3 σ with CHEOPS (Corrigendum)

Cited by 4 publications

References 0 publications

Homogeneous transit timing analyses of 10 exoplanet systems

Homogeneous transit timing analyses of 10 exoplanet systems

Signature of the atmospheric asymmetries of hot and ultra-hot Jupiters in light curves

The phase curve of the ultra-hot Jupiter WASP-167b as seen by TESS

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