Transit timing variations and linear ephemerides of confirmed <i>Kepler</i> transiting exoplanets

Gajdoš, Pavol; Vaňko, M.; Parimucha, Š.

doi:10.1088/1674-4527/19/3/41

Cited by 24 publications

(37 citation statements)

References 18 publications

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“…The timing accuracy of our three measurements is very satisfying. Figure 4 shows that all measurements agree within 1 σ with themselves and with the prediction of Gajdoš et al (2019). Similarly to our case of Kepler-94b, our timing precision from 4 to 10 minutes does not allow us to refine the ephemeris.…”

Section: Kepler-63bsupporting

confidence: 50%

“…We obtained photometric data for three transit events from Kepler-63b, but all observations covered the event only partially and lack either ingress or egress (Figure 3). Our observations correspond to epochs 421, 430, and 439 with respect to the recent ephemeris of Gajdoš et al (2019). The associated uncertainty of this ephemeris amounts to only 0.2 minutes.…”

Section: Kepler-63bmentioning

confidence: 58%

“…The planet orbits almost over the poles of its host star, revealing signatures of the repeated crossing of a long-lived polar spot (Sanchis-Ojeda et al 2013). The most current ephemeris employing all available Kepler data is drawn from Gajdoš et al (2019).…”

Section: Kepler-63bmentioning

confidence: 99%

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Detection capability of ground-based meter-sized telescopes for shallow exoplanet transits

Mallonn,

Poppenhaeger,

Granzer

et al. 2021

Preprint

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Meter-sized ground-based telescopes are frequently used today for the follow-up of extrasolar planet candidates. While the transit signal of a Jupiter-sized object can typically be detected to a high level of confidence with small telescope apertures as well, the shallow transit dips of planets with the size of Neptune and smaller are more challenging to reveal. We employ new observational data to illustrate the photometric follow-up capabilities of meter-sized telescopes for shallow exoplanet transits. We describe in detail the capability of distinguishing the photometric signal of an exoplanet transit from an underlying trend in the light curve. The transit depths of the six targets we observed, Kepler-94b, Kepler-63b, K2-100b, K2-138b, K2-138c, and K2-138e, range from 3.9 ppt down to 0.3 ppt. For five targets of this sample, we provide the first ground-based photometric follow-up. The timing of three targets is precisely known from previous observations, and the timing of the other three targets is uncertain and we aim to constrain it. We detect or rule out the transit features significantly in single observations for the targets that show transits of 1.3 ppt or deeper. The shallower transit depths of two targets of 0.6 and 0.8 ppt were detected tentatively in single light curves, and were detected significantly by repeated observations. Only for the target of the shallowest transit depth of 0.3 ppt were we unable to draw a significant conclusion despite combining five individual light curves. An injection-recovery test on our real data shows that we detect transits of 1.3 ppt depth significantly in single light curves if the transit is fully covered, including out-of-transit data toward both sides, in some cases down to 0.7 ppt depth. For Kepler-94b, Kepler-63b, and K2-100b, we were able to verify the ephemeris. In the case of K2-138c with a 0.6 ppt deep transit, we were able to refine it, and in the case of K2-138e, we ruled out the transit in the time interval of more than ± 1.5 σ of its current literature ephemeris.

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Section: Kepler-63bsupporting

confidence: 50%

Section: Kepler-63bmentioning

confidence: 58%

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Detection capability of ground-based meter-sized telescopes for shallow exoplanet transits

Mallonn,

Poppenhaeger,

Granzer

et al. 2021

Preprint

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“…Kepler-108 was discovered by Rowe et al (2014) and since then, has been studied by Van Eylen & Albrecht (2015), Morton et al (2016), Holczer et al (2016), Mustill et al (2017), andGajdoš et al (2019). The latest data for our study (see Table 1) were taken by Mills & Fabrycky (2017), who performed photodynamic TTV and transit duration variation (TDV) analyses.…”

Section: Kepler-108mentioning

confidence: 93%

Exploiting periodic orbits as dynamical clues for Kepler and K2 systems

Antoniadou

Libert

2020

A&A

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Many extrasolar systems possessing planets in mean-motion resonance or resonant chain have been discovered to date. The transit method coupled with transit timing variation analysis provides an insight into the physical and orbital parameters of the systems, but suffers from observational limitations. When a (near-)resonant planetary system resides in the dynamical neighbourhood of a stable periodic orbit, its long-term stability, and thus survival, can be guaranteed. We use the intrinsic property of the periodic orbits, namely their linear horizontal and vertical stability, to validate or further constrain the orbital elements of detected two-planet systems. We computed the families of periodic orbits in the general three-body problem for several two-planet Kepler and K2 systems. The dynamical neighbourhood of the systems is unveiled with maps of dynamical stability. Additional validations or constraints on the orbital elements of K2-21, K2-24, Kepler-9, and (non-coplanar) Kepler-108 near-resonant systems were achieved. While a mean-motion resonance locking protects the long-term evolution of the systems K2-21 and K2-24, such a resonant evolution is not possible for the Kepler-9 system, whose stability is maintained through an apsidal anti-alignment. For the Kepler-108 system, we find that the stability of its mutually inclined planets could be justified either solely by a mean-motion resonance, or in tandem with an inclination-type resonance. Going forward, dynamical analyses based on periodic orbits could yield better constrained orbital elements of nearresonant extrasolar systems when performed in parallel to the fitting of the observational data. keywordscelestial mechanics -planets and satellites: dynamical evolution and stability -planetary systems -methods: analytical -methods: numerical -chaos 1 See e.g. exoplanet.eu (Schneider et al. 2011) or NASA Exoplanet Archive (Akeson et al. 2013).

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“…5). Among the Kepler planets, only two that exhibit TTVs have shorter orbital periods than AU Mic b (Kepler-25 b and Kepler-1530 c, see Gajdoš et al 2019). AU Mic b has a TTV semi-amplitude of A ≥ 11.5 min, which is large in comparison to other planets with known TTVs.…”

Section: Large-amplitude Ttvsmentioning

confidence: 98%

Transit timing variations of AU Microscopii b and c

Szabó

Garai

Brandeker

et al. 2022

A&A

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Here we report large-amplitude transit timing variations (TTVs) for AU Microcopii b and c as detected in combined TESS (2018, 2020) and CHEOPS (2020, 2021) transit observations. AU Mic is a young planetary system with a debris disk and two transiting warm Neptunes. A TTV on the order of several minutes was previously reported for AU Mic b, which was suggested to be an outcome of mutual perturbations between the planets in the system. In 2021, we observed AU Mic b (five transits) and c (three transits) with the CHEOPS space telescope to follow-up the TTV of AU Mic b and possibly detect a TTV for AU Mic c. When analyzing TESS and CHEOPS 2020-2021 measurements together, we find that a prominent TTV emerges with a full span of ≥ 23 minutes between the two TTV extrema. Assuming that the period change results from a periodic process -such as mutual perturbations-we demonstrate that the times of transits in the summer of 2022 are expected to be 30-85 minutes later than predicted by the available linear ephemeris.

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Transit timing variations and linear ephemerides of confirmed Kepler transiting exoplanets

Cited by 24 publications

References 18 publications

Detection capability of ground-based meter-sized telescopes for shallow exoplanet transits

Detection capability of ground-based meter-sized telescopes for shallow exoplanet transits

Exploiting periodic orbits as dynamical clues for Kepler and K2 systems

Transit timing variations of AU Microscopii b and c

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