Probing Transit Timing Variation and Its Possible Origin with 12 New Transits of TrES-3b

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dc.authoridJoshi, Yogesh C./0000-0001-8657-1573
dc.authoridJiang, Ing-Guey/0000-0001-7359-3300
dc.authoridMANNADAY, VINEET/0000-0002-0638-950X
dc.authoridPuskullu, Caglar/0000-0001-9213-0969
dc.contributor.authorMannaday, Vineet Kumar
dc.contributor.authorThakur, Parijat
dc.contributor.authorJiang, Ing-Guey
dc.contributor.authorSahu, D. K.
dc.contributor.authorJoshi, Y. C.
dc.contributor.authorPandey, A. K.
dc.contributor.authorJoshi, Santosh
dc.date.accessioned2025-01-27T21:00:06Z
dc.date.available2025-01-27T21:00:06Z
dc.date.issued2020
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractWe present 12 new transit light curves of the hot-Jupiter TrES-3b observed during 2012-2018 to probe the transit timing variation (TTV). By combining the midtransit times determined from these 12 transit data with those reestimated through uniform procedure from 71 transit data available in the literature, we derive new linear ephemeris and obtain the timing residuals that suggest the possibility of TTV in the TrES-3 system. However, the frequency analysis shows that the possible TTV is unlikely to be periodic, indicating the absence of an additional body in this system. To explore the other possible origins of TTV, the orbital decay and apsidal precession ephemeris models are fitted to the transit time data. We find the decay rate of TrES-3b to be (P) overt dot(q) = -4.1 +/- 3.1 ms( )yr(-1), and the corresponding estimated modified stellar tidal quality factor of Q(*)' similar to 1.11 x 10(5) is consistent with the theoretically predicted values for the stars hosting the hot-Jupiters. The shift in the transit arrival time of TrES-3b after 11 years is expected to be T-s(hift) similar to 69.55 s, which is consistent with the rms of the timing residuals. Besides, we find that the apsidal precession ephemeris model is statistically less probable than the other considered ephemeris models. It is also discussed that despite the fact that the linear ephemeris model appears to be the most plausible model to represent the transit time data, the possibility of the orbital decay cannot be completely ruled out in the TrES-3 system. To confirm this, further high-precision and high-cadence follow-up observation of transits of TrES-3b would be important.
dc.description.sponsorshipUniversity Grants Commission (UGC), New Delhi [UGC-MRP 43-521/2014(SR)]; IUCAA, Pune through IUCAA Associateship Programme; Ministry of Science and Technology, Taiwan [MOST 106-2112-M-007-006-MY3]; Department of Science and Technology (DST), India through the Indo-Austria project on transiting exoplanets [INT/AUSTRIA/BMWF/P-14]; TUBITAK (Scientific and Technological Research Council of Turkey) [113F353]; National Planning Agency (DPT) of Turkey [DPT-2007K120660]; Scientific Research Projects Coordination Unit of Istanbul University [3685]; TUBITAK [13CT100-523, 13CT100537]; Canakkale Onsekiz Mart University Astrophysics Research Center; Ulupinar Observatory; Istanbul University Observatory Research and Application Center; [VEGA 2/0031/18]; [APVV-15-0458]
dc.description.sponsorshipWe thank the anonymous referee for useful comments that improved the quality of the paper. We also thank J.Z. Gazak, D. Foreman-Mackey, and D. Ragozzine for their valuable suggestions and discussions, which have been very helpful in improving the paper. We thank the staff at IAO, Hanle and CREST (IIA), Hosakote, as well as at DFOT (ARIES), Nainital, for providing support during the observations. The time allocation committees of the HCT, DFOT, and AZT-11 are gratefully acknowledged for providing the observation times. P.T. and V.K.M. acknowledge the University Grants Commission (UGC), New Delhi, for providing the financial support through Major Research Project no. UGC-MRP 43-521/2014(SR). P.T. expresses his sincere thanks to IUCAA, Pune, for providing the supports through IUCAA Associateship Programme. I.G.J. acknowledges funding from the Ministry of Science and Technology, Taiwan, through the grant No. MOST 106-2112-M-007-006-MY3. Y.C.J. acknowledges the Department of Science and Technology (DST), India, for their support through the Indo-Austria project on transiting exoplanets, INT/AUSTRIA/BMWF/P-14. M.V. would like to thank the project VEGA 2/0031/18 and APVV-15-0458. C.P. acknowledges the funding from TUBITAK (Scientific and Technological Research Council of Turkey) under grant No. 113F353. C.P. also thanks Canakkale Onsekiz Mart University Astrophysics Research Center, Ulupinar Observatory, and Istanbul University Observatory Research and Application Center for their support and allowing use of T122 and T60, which were supported partly by the National Planning Agency (DPT) of Turkey (project DPT-2007K120660 carried out Canakkale Onsekiz Mart University) and the Scientific Research Projects Coordination Unit of Istanbul University (project no. 3685). C. P. thanks TUBITAK for a partial support in using the T100 telescope with project numbers 13CT100-523 and 13CT100537. We thank N.P. Gibson, J.W. Lee, and D. Ricci for sharing the transit light curves of TrES-3b with us. We are also thankful to A. Sozzetti, K.D. Colon, P. Kundurthy, and J.D. Turner for making their transit light curves publicly available.
dc.identifier.doi10.3847/1538-3881/ab9818
dc.identifier.issn0004-6256
dc.identifier.issn1538-3881
dc.identifier.issue1
dc.identifier.scopus2-s2.0-85089507584
dc.identifier.scopusqualityQ1
dc.identifier.urihttps://doi.org/10.3847/1538-3881/ab9818
dc.identifier.urihttps://hdl.handle.net/20.500.12428/26936
dc.identifier.volume160
dc.identifier.wosWOS:000546811700001
dc.identifier.wosqualityQ1
dc.indekslendigikaynakWeb of Science
dc.indekslendigikaynakScopus
dc.language.isoen
dc.publisherIop Publishing Ltd
dc.relation.ispartofAstronomical Journal
dc.relation.publicationcategoryinfo:eu-repo/semantics/openAccess
dc.rightsinfo:eu-repo/semantics/openAccess
dc.snmzKA_WoS_20250125
dc.subjectStellar Atmosphere Models
dc.subjectHigh-Precision Photometry
dc.subjectLimb-Darkening Law
dc.subjectOrbital Decay
dc.subjectHot-Jupiter
dc.subjectPhysical-Properties
dc.subjectLight Curves
dc.subjectPlanets
dc.subjectI.
dc.titleProbing Transit Timing Variation and Its Possible Origin with 12 New Transits of TrES-3b
dc.typeArticle

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