Kepler-90: Giant Transit-timing Variations Reveal a Super-puff

Liang, Yan; Robnik, Jakob; Seljak, Uroš

doi:10.3847/1538-3881/abe6a7

Cited by 8 publications

(3 citation statements)

References 36 publications

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“…This 11 yr baseline was necessary to sample the orbit of Kepler-90 h, which is nearly 1 yr (P h = 331 days), resulting in significant aliasing during the seasonal Kepler field RV follow-up. The RVs place upper limits on all of the small planets (Kepler-90 b, c, d, e, f, i) and yield masses for the two Saturn-sized planets: M g = 49 ± 29 M ⊕ and M h = 0.63M J ± 0.15M J , consistent with the results of Liang et al (2021). The residual RVs have significant scatter (rms = 13.7 m s −1 ), which is atypical for a slowly rotating, magnetically quiet Sunlike star (T eff = 6000 K, v i sin = 3.6 km s −1 , log ¢ = -R 5.2 HK , expected jitter = 9.3 m s −1 ).…”

Section: A11 Koi-104 (Kepler-94)supporting

confidence: 83%

“…The eighth planet (Kepler-90 i) was detected with candidate status at the time owing to its small size (Aviv Ofir, private communication) and was later confirmed with an independent photometric search (Shallue & Vanderburg 2018). Liang et al (2021) found that Kepler-90 g is much lower in mass than Kepler-90 h (15 ± 1 M ⊕ for planet g vs. 203 ± 5 M ⊕ for planet h) by fitting their transit timing and depth variations determined from the Kepler photometry.…”

Section: A11 Koi-104 (Kepler-94)mentioning

confidence: 96%

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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

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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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Section: A11 Koi-104 (Kepler-94)supporting

confidence: 83%

Section: A11 Koi-104 (Kepler-94)mentioning

confidence: 96%

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

View full text Add to dashboard Cite

show abstract

“…As for transits, all but one of the compact multis in our sample are devoid of a transiting giant planet with a period in the range of P = 100-500 days confirmed by the Kepler search pipeline. One exception is the Kepler-90 (KOI-351) system, which contains a Sun-like star and eight confirmed transiting planets, the outermost of which has a period of P = 332 days and mass 203 ± 5 M ⊕ (Liang et al 2021). This outer planet may be partially sculpting the edge of the inner seven planets.…”

Section: Implications For the Edge-of-the-multismentioning

confidence: 99%

Can Cold Jupiters Sculpt the Edge-of-the-multis?

Sobski,

Millholland

2023

ApJ

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Compact systems of multiple close-in super-Earths/sub-Neptunes (compact multis) are a ubiquitous outcome of planet formation. It was recently discovered that the outer edges of compact multis are located at smaller orbital periods than expected from geometric and detection biases alone, suggesting some truncation or transition in the outer architectures. Here we test whether this edge-of-the-multis might be explained in any part by distant giant planets in the outer regions (≳1 au) of the systems. We investigate the dynamical stability of observed compact multis in the presence of hypothetical giant (≳0.5 M Jup) perturbing planets. We identify what parameters would be required for hypothetical perturbing planets if they were responsible for dynamically sculpting the outer edges of compact multis. Edge-sculpting perturbers are generally in the range of P ∼ 100–500 days for the average compact multi, with most between P ∼ 200 and 300 days. Given the relatively close separation, we explore the detectability of the hypothetical edge-sculpting perturbing planets, finding that they would be readily detectable in transit and radial velocity data. We compare to observational constraints and find it unlikely that dynamical sculpting from distant giant planets contributes significantly to the edge-of-the-multis. However, this conclusion could be strengthened in future work by a more thorough analysis of the detection yields of the perturbing planets.

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HD 191939 revisited: New and refined planet mass determinations, and a new planet in the habitable zone

Orell-Miquel¹,

Nowak²,

Murgas³

et al. 2023

A&A

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HD 191939 (TOI-1339) is a nearby (d = 54 pc), bright (V = 9 mag), and inactive Sun-like star (G9 V) known to host a multi-planet transiting system. Ground-based spectroscopic observations confirmed the planetary nature of the three transiting sub-Neptunes (HD 191939 b, c, and d) originally detected by TESS and were used to measure the masses for planets b and c with 3σ precision. These previous observations also reported the discovery of an additional Saturn-mass planet (HD 191939 e) and evidence for a further, very long-period companion (HD 191939 f). Here, we report the discovery of a new non-transiting planet in the system and a refined mass determination of HD 191939 d. The new planet, HD 191939 g, has a minimum mass of 13.5±2.0 M⊕ and a period of about 280 days. This period places the planet within the conservative habitable zone of the host star, and near a 1:3 resonance with HD 191939 e. The compilation of 362 radial velocity measurements with a baseline of 677 days from four different high-resolution spectrographs also allowed us to refine the properties of the previously known planets, including a 4.6σ mass determination for planet d, for which only a 2σ upper limit had been set until now. We confirm the previously suspected low density of HD 191939 d, which makes it an attractive target for attempting atmospheric characterisation. Overall, the planetary system consists of three sub-Neptunes interior to a Saturn-mass and a Uranus-mass planet plus a high-mass long-period companion. This particular configuration has no counterpart in the literature and makes HD 191939 an exceptional multi-planet transiting system with an unusual planet demographic worthy of future observation.

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Kepler-90: Giant Transit-timing Variations Reveal a Super-puff

Cited by 8 publications

References 36 publications

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

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

Can Cold Jupiters Sculpt the Edge-of-the-multis?

HD 191939 revisited: New and refined planet mass determinations, and a new planet in the habitable zone

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