The Discovery of the Long-Period, Eccentric Planet Kepler-88 d and System Characterization with Radial Velocities and Photodynamical Analysis

Weiss, Lauren M.; Fabrycky, Daniel C.; Agol, Eric; Mills, Sean M.; Howard, Andrew W.; Isaacson, Howard; Petigura, Erik A.; Fulton, Benjamin J.; Hirsch, Lea A.; Sinukoff, Evan

doi:10.3847/1538-3881/ab88ca

Cited by 12 publications

(6 citation statements)

References 61 publications

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“…The Kepler mission [6], and its extension Kepler/K2 [23], demonstrated the potentiality of this technique, able to characterise planets also for stars too faint for a spectroscopy analysis and radial velocity measurement. Some examples of the application of the TTV technique on multiple planet systems are: Kepler-9 [4,5,22], Kepler-11 [30,31], Kepler-88 [39,57], K2-24 [42,43], and WASP-47 [54,56].…”

Section: Introductionmentioning

confidence: 99%

Exploiting the transit timing capabilities of Ariel

et al. 2021

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The Transit Timing Variation (TTV) technique is a powerful dynamical tool to measure exoplanetary masses by analysing transit light curves. We assessed the transit timing performances of the Ariel Fine Guidance Sensors (FGS1/2) based on the simulated light curve of a bright, 55 Cnc, and faint, K2-24, planet-hosting star. We estimated through a Markov-Chain Monte-Carlo analysis the transit time uncertainty at the nominal cadence of 1 second and, as a comparison, at a 30 and 60-s cadence. We found that at the nominal cadence Ariel will be able to measure the transit time with a precision of about 12s and 34s, for a star as bright as 55 Cnc and K2-24, respectively. We then ran dynamical simulations, also including the Ariel timing errors, and we found an improvement on the measurement of planetary masses of about 20-30% in a K2-24-like planetary system through TTVs. We also simulated the conditions that allow us to detect the TTV signal induced by an hypothetical external perturber within the mass range between Earth and Neptune using 10 transit light curves by Ariel.

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Section: Introductionmentioning

confidence: 99%

Exploiting the transit timing capabilities of Ariel

et al. 2021

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“…When data quality is high enough to resolve the synodic chopping signal (Deck & Agol 2015), the mass-eccentricity degeneracy can be broken. This is more feasible for systems with large TTV amplitudes, such as KOI-142/Kepler-88 (Weiss et al 2020). In the case of Kepler-80, where the data for the outer planet is particularly low-S/N and the baseline of the observations limited, the TTV solution could be improved with additional data over extended baseline to better identify and fit the chopping signal.…”

Section: Transit Timing Variations: Insights and Limitationsmentioning

confidence: 99%

Kepler-80 Revisited: Assessing the Participation of a Newly Discovered Planet in the Resonant Chain

Weisserman

Becker

Vanderburg

2023

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In this paper, we consider the chain of resonances in the Kepler-80 system and evaluate the impact that the additional member of the resonant chain discovered by Shallue & Vanderburg has on the dynamics of the system and the physical parameters that can be recovered by a fit to the transit timing variations (TTVs). Ultimately, we calculate the mass of Kepler-80 g to be 0.8 ± 0.3M ⊕ when assuming all planets have zero eccentricity, and 1.0 ± 0.3 M ⊕ when relaxing that assumption. We show that the outer five planets are in successive three-body mean-motion resonances (MMRs). We assess the current state of two-body MMRs in the system and find that the planets do not appear to be in two-body MMRs. We find that while the existence of the additional member of the resonant chain does not significantly alter the character of the Kepler-80 three-body MMRs, it can alter the physical parameters derived from the TTVs, suggesting caution should be applied when drawing conclusions from TTVs for potentially incomplete systems. We also compare our results to those of MacDonald et al., who perform a similar analysis on the same system with a different method. Although the results of this work and MacDonald et al. show that different fit methodologies and underlying assumptions can result in different measured orbital parameters, the most secure conclusion is that which holds true across all lines of analysis: Kepler-80 contains a chain of planets in three-body MMRs but not in two-body MMRs.

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“…Dynamical measurements of the Kepler planet-hosting stars provide an excellent means for detecting Jovian companions to small planets. Radial velocity (RV) measurements have led to the identification of Jovian and substellar companions in 16 Kepler systems, including precise characterization of their orbital periods, eccentricities, and minimmum masses in six systems (e.g., Marcy et al 2014;Gettel et al 2016;Otor et al 2016;Mills et al 2019b;Weiss et al 2020;Zhang et al 2021). Although the ESA Gaia mission has great promise for finding Jovians around nearby stars, the majority of Kepler stars are too distant (∼1000 pc) to produce sufficient single-measurement astrometric precision to characterize planetary orbits from Jovian-mass companions at 1-10 au.…”

Section: Introductionmentioning

confidence: 99%

The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory

Weiss,

Isaacson,

Howard

et al. 2023

ApJS

Self Cite

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Despite the importance of Jupiter and Saturn to Earth’s formation and habitability, there has not yet been a comprehensive observational study of how giant exoplanets correlate with the architectural properties of close-in, sub-Neptune-sized exoplanets. This is largely because transit surveys are particularly insensitive to planets at orbital separations ≳1 au, and so their census of Jupiter-like planets is incomplete, inhibiting our study of the relationship between Jupiter-like planets and the small planets that do transit. To investigate the relationship between close-in, small and distant, giant planets, we conducted the Kepler Giant Planet Survey (KGPS). Using the W. M. Keck Observatory High Resolution Echelle Spectrometer, we spent over a decade collecting 2844 radial velocities (RVs; 2167 of which are presented here for the first time) of 63 Sunlike stars that host 157 transiting planets. We had no prior knowledge of which systems would contain giant planets beyond 1 au, making this survey unbiased with respect to previously detected Jovians. We announce RV-detected companions to 20 stars from our sample. These include 13 Jovians ( 0.3 M J < M sin i < 13 M J , 1 au < a < 10 au), eight nontransiting sub-Saturns, and three stellar-mass companions. We also present updated masses and densities of 84 transiting planets. The KGPS project leverages one of the longest-running and most data-rich collections of RVs of the NASA Kepler systems yet, and it will provide a basis for addressing whether giant planets help or hinder the growth of sub-Neptune-sized and terrestrial planets. Future KGPS papers will examine the relationship between small, transiting planets and their long-period companions.

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The Discovery of the Long-Period, Eccentric Planet Kepler-88 d and System Characterization with Radial Velocities and Photodynamical Analysis

Cited by 12 publications

References 61 publications

Exploiting the transit timing capabilities of Ariel

Exploiting the transit timing capabilities of Ariel

Kepler-80 Revisited: Assessing the Participation of a Newly Discovered Planet in the Resonant Chain

The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory

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