Transiting Exoplanet Monitoring Project (TEMP). III. On the Relocation of the Kepler-9 b Transit

Wang, Songhu; Wu, Dong-Hong; Addison, Brett C.; Laughlin, Gregory; Liu, Hui-Gen; Wang, Yong-Hao; Yang, Tao-Zhi; Yang, Ming; Yisikandeer, Abudusaimaitijiang; Hong, R. Q.; Li, Bin; Liu, Jinzhong; Zhao, Haibin; Wu, Zhenyu; Hu, Shaoming; Zhou, Xu; Zhou, Ji-Lin; Zhang, Hui; Zheng, Jie; Wang, Wei; Zhang, Fan; Niu, Hubiao; Chen, Yuanyuan; Lu, H.; Peng, Xiyan; Li, Kai; Guo, Dadong

doi:10.3847/1538-3881/aaa253

Cited by 39 publications

(21 citation statements)

References 33 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Figure 8 shows these nine system in the context of all multi-planet transiting systems. Spectroscopic transits and analyses of spot crossing events have been performed on a number of Jovian-sized planets in the multi-planet systems, including KOI-94 (Hirano et al 2012;Albrecht et al 2013), Kepler-30 (Sanchis-Ojeda et al 2012), WASP-47 (Sanchis-Ojeda et al 2015), and Kepler-9 (Wang et al 2018), finding these to be well aligned systems. The warm Neptune systems Kepler-25 (Albrecht et al 2013;Benomar et al 2014;Campante et al 2016), Kepler-50, Kepler-60 (Chaplin et al 2013, and HD 106315 all inhabit low obliquity orbits too.…”

Section: The Obliquities Of Warm Neptune Systemsmentioning

confidence: 99%

The Warm Neptunes around HD 106315 Have Low Stellar Obliquities

Zhou

Rodriguez

Vanderburg

et al. 2018

View full text Add to dashboard Cite

We present the obliquity of the warm Neptune HD 106315c measured via a series of spectroscopic transit observations. HD 106315c is a 4.4 R Earth warm Neptune orbiting a moderately rotating late F-star with a period of 21.05 days. HD 106315 also hosts a 2.5 R Earth super-Earth on a 9.55 day orbit. Our Doppler tomographic analyses of four transits observed by the Magellan/MIKE, HARPS, and TRES facilities find HD 106315c to be in a low stellar obliquity orbit, consistent with being well aligned with the spin axis of the host star at λ = −10.9 +3.6 −3.8• . We suggest, via dynamical N-body simulations, that the two planets in the system must be co-planar, and thus are both well aligned with the host star. HD 106315 is only the fourth warm Neptune system with obliquities measured. All warm Neptune systems have been found in well aligned geometries, consistent with the interpretation that these systems are formed in-situ in the inner protoplanetary disk, and also consistent with the majority of Kepler multi-planet systems that are in low obliquity orbits. With a transit depth of 1.02 mmag, HD 106315c is among the smallest planets to have been detected in transit spectroscopy, and we discuss its detection in the context of TESS and the next generations of spectrographs. Subject headings: planets and satellites: individual (HD106315c), planets and satellites: dynamical evolution and stability

show abstract

Section: The Obliquities Of Warm Neptune Systemsmentioning

confidence: 99%

The Warm Neptunes around HD 106315 Have Low Stellar Obliquities

Zhou

Rodriguez

Vanderburg

et al. 2018

View full text Add to dashboard Cite

show abstract

“…Ground-based observatories can in principle recover transits for faint Kepler stars with long period planets, and coordinated multi-observatory campaigns have shown promise in achieving the requisite phase coverage (Freudenthal et al 2018;von Essen et al 2018;Wang et al 2018). However, their photometric precisions are typically limited by low observing efficiencies and the presence of time-correlated noise due to imperfect guiding and point-spread function (PSF) variations (Zhao et al 2014;Croll et al 2015;Stefansson et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Diffuser-assisted Infrared Transit Photometry for Four Dynamically Interacting Kepler Systems

Vissapragada

Jontof-Hutter

Shporer

et al. 2020

View full text Add to dashboard Cite

We present ground-based infrared transit observations for four dynamically interacting Kepler planets, including Kepler-29b, Kepler-36c, KOI-1783.01, and Kepler-177c, obtained using the Wide-field Infrared Camera on the Hale 200" telescope at Palomar Observatory. By utilizing an engineered diffuser and custom guiding software, we mitigate time-correlated telluric and instrumental noise sources in these observations. We achieve an infrared photometric precision comparable to or better than that of space-based observatories such as the Spitzer Space Telescope, and detect transits with greater than 5σ significance for all planets aside from Kepler-36c. For Kepler-177c (J = 13.9) our measurement uncertainties are only 1.2× the photon noise limit and 1.9 times better than the predicted photometric precision for Spitzer IRAC photometry of this same target. We find that a single transit observation obtained 4 − 5 years after the end of the original Kepler mission can reduce dynamical mass uncertainties by as much as a factor of three for these systems. Additionally, we combine our new observations of KOI-1783.01 with information from the literature to confirm the planetary nature of this system. We discuss the implications of our new mass and radius constraints in the context of known exoplanets with low incident fluxes, and we note that Kepler-177c may be a more massive analog to the currently known super-puffs given its core mass (4.2±0.8M ⊕ ) and large gas-to-core ratio (2.5±0.2). Our demonstrated infrared photometric performance opens up new avenues for ground-based observations of transiting exoplanets previously thought to be restricted to space-based investigation.

show abstract

“…Families of periodic orbits in 2/1 MMR for planetary mass ratio ρ = 0.69 of Kepler-9bc, along with the evolutions initiated by the orbital elements given byHolman et al (2010),Wang et al (2018b), andBorsato et al (2019), which locate the pair close to the family of unstable (red) periodic orbits.…”

mentioning

confidence: 76%

Exploiting periodic orbits as dynamical clues for Kepler and K2 systems

Antoniadou

Libert

2020

A&A

View full text Add to dashboard Cite

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).

show abstract

Transiting Exoplanet Monitoring Project (TEMP). III. On the Relocation of the Kepler-9 b Transit

Cited by 39 publications

References 33 publications

The Warm Neptunes around HD 106315 Have Low Stellar Obliquities

The Warm Neptunes around HD 106315 Have Low Stellar Obliquities

Diffuser-assisted Infrared Transit Photometry for Four Dynamically Interacting Kepler Systems

Exploiting periodic orbits as dynamical clues for Kepler and K2 systems

Contact Info

Product

Resources

About