Exploiting the transit timing capabilities of Ariel

Borsato, L.; Nascimbeni, V.; Piotto, G.; Szabó, Gy. M.

doi:10.1007/s10686-021-09737-5

Cited by 8 publications

(11 citation statements)

References 55 publications

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“…For comparison, in Table 5 we also show the mean error of the transit times, σT C , for CHEOPS and TESS transits. The improvement on our estimations of the transit times from CHEOPS light curves in comparison to those from TESS transits is consistent with the results of previous works (e.g., Borsato et al 2021;Bonfanti et al 2021). The final O−C diagram of each planet is shown in Fig.…”

Section: Timing Analysissupporting

confidence: 91%

Characterization of the HD 108236 system with CHEOPS and TESS Confirmation of a fifth transiting planet

Hoyer

Bonfanti

Leleu

et al. 2022

A&A

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Context. The HD 108236 system was first announced with the detection of four small planets based on TESS data. Shortly after, the transit of an additional planet with a period of 29.54 d was serendipitously detected by CHEOPS. In this way, HD 108236 (V=9.2) became one of the brightest stars known to host five small transiting planets (R p <3 R ⊕ ). Aims. We characterize the planetary system by using all the data available from CHEOPS and TESS space missions. We use the flexible pointing capabilities of CHEOPS to follow up the transits of all the planets in the system, including the fifth transiting body. Methods. After updating the host star parameters by using the results from Gaia eDR3, we analyzed 16 and 43 transits observed by CHEOPS and TESS, respectively, to derive the planets' physical and orbital parameters. We carried out a timing analysis of the transits of each of the planets of HD 108236 to search for the presence of transit timing variations. Results. We derived improved values for the radius and mass of the host star (R ⋆ = 0.876 ± 0.007 R ⊙ and M ⋆ = 0.867 +0.047 −0.046 M ⊙ ). We confirm the presence of the fifth transiting planet f in a 29.54 d orbit. Thus, the HD 108236 system consists of five planets of R b =1.587±0.028, R c =2.122±0.025, R d =2.629±0.031, R e =3.008±0.032, and R f =1.89±0.04 [R ⊕ ]. We refine the transit ephemeris for each planet and find no significant transit timing variations for planets c, d, and e. For planets b and f , instead, we measure significant deviations on their transit times (up to 22 and 28 min, respectively) with a non-negligible dispersion of 9.6 and 12.6 min in their time residuals. Conclusions. We confirm the presence of planet f and find no significant evidence for a potential transiting planet in a 10.9 d orbital period, as previously suggested. Further monitoring of the transits, particularly for planets b and f , would confirm the presence of the observed transit time variations. HD 108236 thus becomes a key multi-planetary system for the study of formation and evolution processes. The reported precise results on the planetary radii -together with a profuse RV monitoring -will allow for an accurate characterization of the internal structure of these planets.

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Section: Timing Analysissupporting

confidence: 91%

Characterization of the HD 108236 system with CHEOPS and TESS Confirmation of a fifth transiting planet

Hoyer

Bonfanti

Leleu

et al. 2022

A&A

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“…This paper extends the work of Szabó et al [46], Borsato et al [7], and Garai [18] and focusses on some straightforward applications to stellar astrophysics along with some more speculative potential applications. Section 2 focusses on advances that can be made through the application of Ariel's Core Survey data to stellar astrophysics.…”

Section: Introductionmentioning

confidence: 56%

“…Exomoons can cause both transit timing and transit duration variations through their gravitational interactions with the transiting planet they orbit [26]. As discussed in Borsato et al [7], Ariel will make precise measurements of both. The exomoon itself can also be directly detected through its transit.…”

Section: Exomoons and Exoringsmentioning

confidence: 99%

“…This short paper outlines a variety of science which might be executed with the ground-breaking data included in Ariel's Core Survey. A very short summary of some of these potential extended use applications of the Ariel Core Survey data is included in Tinetti et al [49]; further examples and more detailed discussions can also be found in Szabó et al [46], Borsato et al [7], and Garai (2020).…”

Section: Introductionmentioning

confidence: 99%

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Extended use of the Ariel Core Survey Data

Haswell

2021

Exp Astron

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“…Combining observations from wide field transit surveys, e.g., Kepler, TESS (Borucki et al, 2010;Ricker et al, 2015) and follow-up observations using focused telescopes e.g., CHEOPS (Benz et al, 2021), has been proved to be feasible in TTV detecting and related researches (Borsato et al, 2021). Sariya et al (2021) report TTVs of HAT-P-12b in the baseline of ten years, using light curves from small ground-based telescopes.…”

Section: Introductionmentioning

confidence: 99%

Detecting and Monitoring Tidal Dissipation of Hot Jupiters in the Era of SiTian

Yang,

Wang,

Wei

et al. 2022

Preprint

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Transit Timing Variation (TTV) of hot Jupiters provides direct observational evidence of planet tidal dissipation. Detecting tidal dissipation through TTV needs high precision transit timings and long timing baselines. In this work, we predict and discuss the potential scientific contribution of SiTian Survey in detecting and analyzing exoplanet TTV. We develop a tidal dissipation detection pipeline for SiTian Survey that aims at time-domain astronomy with 72 1-meter optical telescopes. The pipeline includes the modules of light curve deblending, transit timing obtaining, and TTV modeling. SiTian is capable to detect more than 25,000 exoplanets among which we expect ∼50 sources showing evidence of tidal dissipation. We present detection and analysis of tidal dissipating targets, based on simulated SiTian light curves of XO-3b and WASP-161b. The transit light curve modeling gives consistent results within 1σ to input values of simulated light curves. Also, the parameter uncertainties predicted by Monte-Carlo Markov Chain are consistent with the distribution obtained from simulating and modeling the light curve 1000 times. The timing precision of SiTian observations is ∼ 0.5 minutes with one transit visit. We show that differences between TTV origins, e.g., tidal dissipation, apsidal precession, multiple planets, would be significant, considering the timing precision and baseline. The detection rate of tidal dissipating hot Jupiters would answer a crucial question of whether the planet migrates at an early formation stage or random stages due to perturbations, e.g., planet scattering, secular interaction. SiTian identified targets would be constructive given that the sample would extend tenfold.

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Exploiting the transit timing capabilities of Ariel

Cited by 8 publications

References 55 publications

Characterization of the HD 108236 system with CHEOPS and TESS Confirmation of a fifth transiting planet

Characterization of the HD 108236 system with CHEOPS and TESS Confirmation of a fifth transiting planet

Extended use of the Ariel Core Survey Data

Detecting and Monitoring Tidal Dissipation of Hot Jupiters in the Era of SiTian

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