![]() ![]() The detected perturbation of TrES-5b may be caused by a second exoplanet in the TrES-5 system. We carried out the N-body modeling based on the three-body problem. We have detected timing variations with a semi-amplitude of A ≈ 0.0016 days and a period of P ≈ 99 days. To obtain the necessary amount of photometric data for this exoplanet, we have organized an international campaign to search for exoplanets based on the Transit Timing Variation method (TTV) and as a result of this we collected 30 new light curves, 15 light curves from the Exoplanet Transit Database (ETD) and 8 light curves from the literature for the timing analysis of the exoplanet TrES-5b. In this work, we present transit timing variations detected for the exoplanet TrES-5b. Benni, Paul Shadick, Stan Hentunen, Veli-Pekka Salisbury, Mark Esseiva, Nicolas Garlitz, Joe Bretton, Marc Ogmen, Yenal Karavaev, Yuri Ayiomamitis, Anthony Mazurenko, Oleg Alonso, David Molina Velichko, Sergey F. Possible existence of the exoplanet TrES-5 c Transit timing analysis of the exoplanet TrES-5 b. We calculated possible masses and resonances of the objects: M Ëœ 0.24 Mjup on the 1:2 Resonance and M Ëœ 3.15 Mjup on the 1:3 Resonance. We detected a perturbation of TrES-5b which can be caused by a second exoplanet in the TrES-5 system. ![]() We carried out the N-body modelling by means of the three-body problem. On the basis of the obtained data, we detected timing variations with the period P ≠100 days. We managed to collect N light curves for TrEs-5b. To obtain necessary photometric data for this exoplanet, we have organized an international campaign for exoplanet searching based on the Transit Timing Variation (TTV) method. In this paper, we present timing variations detected for the TrES-5b exoplanet. Photometric data for TrES-1 and TrES-2 are only available in electronic form at the CDS via anonymous ftp to (130.79.128.5) or via ĭetected Timing for Exoplanet TrES-5b. We also conclude that any sinusoidal variations that might be indicative of exomoons need to be confirmed with higher statistical significance by further observations, noting that TrES-2 is in the field-of-view of the Kepler Space Telescope. In both cases, TrES-1 and TrES-2, we are able to put upper constraints on the presence of additional perturbers masses. As for TrES-2, we find a better ephemeris of Tc = 2 453 957.63512(28) + 2.4706101(18) Ã- Epoch and a good fit for a sine function with a period of 0.2 days, compatible with a moon around TrES-2 and an amplitude of 57 s, but it is not a uniquely low χ2 value that would indicate a clear signal. Likewise, a light time effect caused, e.g., by a 0.09 M_⊙ mass star at a distance of 7.8 AU is possible. ) in the 3:2 and 2:1 MMRs having high FAPs based on our transit observations from the ground.Results: For TrES-1, we can exclude planetary companions (>1 M⊠For each model we calculated the χ2 residuals and the false alarm probability (FAP). To model possible transit timing variations, we used polynomials of different orders, simulated O-C diagrams corresponding to a perturbing third mass, and we used sinusoidal fits. Based on these new data and previously published work, we studied the observed light curves and searched for variations in the difference between observed and calculated (based on a fixed ephemeris) transit times. Methods: Using the IAC 80 cm telescope, we observed transits of TrES-1 and TrES-2 over several years. The aim of this work is a detailed analysis of transit light curves from TrES-1 and TrES-2, obtained over a period of three to four years, in order to search for variabilities in observed mid-transit times and to set constraints on the presence of additional third bodies. Transit timing analysis of the exoplanets TrES-1 and TrES-2 ![]()
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