The California Legacy Survey. I. A Catalog of 178 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades

Rosenthal, Lee J.; Fulton, Benjamin J.; Hirsch, Lea A.; Isaacson, Howard; Howard, Andrew W.; Dedrick, Cayla M.; Sherstyuk, Ilya A.; Blunt, Sarah; Petigura, Erik A.; Knutson, Heather A.; Behmard, Aida; Chontos, Ashley; Crepp, Justin R.; Crossfield, Ian J. M.; Dalba, Paul A.; Fischer, Debra A.; Henry, Gregory W.; Kane, Stephen R.; Kosiarek, Molly R.; Marcy, Geoffrey W.; Rubenzahl, Ryan A.; Weiss, Lauren M.; Wright, Jason T.

doi:10.3847/1538-4365/abe23c

Cited by 190 publications

(161 citation statements)

References 135 publications

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“…The CLS sample contains 178 RV planet detections around 719 stars (Rosenthal et al 2021a;Fulton et al 2021). The CLS stars cover a broad range of stellar properties, including FGKM-type dwarf and giant stars.…”

Section: Sample Descriptionmentioning

confidence: 99%

“…In this work, we make use of the recently released planet sample from the radial velocity (RV) survey-the California Legacy Survey (CLS; Rosenthal et al 2021a)-and derive the intrinsic multiplicity distribution of planets around Sun-like stars. We describe the general method to model the multiplicity distribution in any RV survey in Section 2.…”

Section: Introductionmentioning

confidence: 99%

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The Intrinsic Multiplicity Distribution of Exoplanets Revealed from the Radial Velocity Method

Zhu

2022

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Planet multiplicities are useful in constraining the formation and evolution of planetary systems, but they are usually difficult to constrain observationally. Here, we develop a general method that can properly take into account the survey incompleteness and recover the intrinsic planet multiplicity distribution. We then apply it to the radial velocity (RV) planet sample from the California Legacy Survey (CLS). Within the 1 au (10 au) region, we find 21% ± 4% (19.2% ± 2.8%) of Sun-like stars host planets with masses above 10 M ⊕ (0.3 M J), about 30% (40%) of which are multiplanet systems; in terms of the RV semi-amplitude K, 33% ± 7% (25% ± 3%) of Sun-like stars contain planets of K > 1 m s−1 (3 m s−1), and each system hosts on average 1.8 ± 0.4 (1.63 ± 0.16) planets. We note that the hot Jupiter rate in the CLS Sun-like sample is higher than the consensus value of ∼1% by a factor of about three. We also confirm previous studies on the correlation between inner ( <1 au) and outer ( >1 au) planets.

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Section: Sample Descriptionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The Intrinsic Multiplicity Distribution of Exoplanets Revealed from the Radial Velocity Method

Zhu

2022

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“…Using a stellar mass of 1.35 ± 0.03 M (Takeda et al 2007) and a radial velocity of 468.42 ± 2.09 m s −1 (Justesen & Albrecht 2019), we derive a planetary mass of 𝑀 P = 6.24 +0.17 −0.18 M J . Furthermore, we are able to derive an inclination of 𝑖 = 41.6 +1.0 −0.9 degrees determined from a planet separation of 0.04869 +0.00039 −0.00040 AU (Rosenthal et al 2021), which is consistent with those determined in Lockwood et al (2014) and Pelletier et al (2021). Despite having ∼ 3× weaker constraints on 𝐾 P , we are able to match the constraints on the inclination and the mass of the planet due to the recent improvement on the constraints on the measured semimajor axis (Rosenthal et al 2021) than what was used in Pelletier et al (2021).…”

Section: Discussionmentioning

confidence: 93%

“…Furthermore, we are able to derive an inclination of 𝑖 = 41.6 +1.0 −0.9 degrees determined from a planet separation of 0.04869 +0.00039 −0.00040 AU (Rosenthal et al 2021), which is consistent with those determined in Lockwood et al (2014) and Pelletier et al (2021). Despite having ∼ 3× weaker constraints on 𝐾 P , we are able to match the constraints on the inclination and the mass of the planet due to the recent improvement on the constraints on the measured semimajor axis (Rosenthal et al 2021) than what was used in Pelletier et al (2021). This highlights the importance of regular improvements to the system parameters on planets with large monitoring radial velocity surveys such as in Rosenthal et al (2021) which are essential for retrieving precise orbital parameters in high resolution atmospheric studies.…”

Section: Discussionmentioning

confidence: 93%

Water observed in the atmosphere of τ Bootis Ab with CARMENES/CAHA

Webb,

Gandhi,

Brogi

et al. 2022

Preprint

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Characterising the atmospheres of hot Jupiters is important in understanding the formation and migration of these exotic planets. However, there are still many open questions about the chemical and physical properties of these atmospheres. Here, we confirm the detection of water vapour in thermal emission from the non-transiting hot Jupiter 𝜏 Boötis Ab with the high resolution NIR CARMENES spectrograph. Combining over 17 h of observations (560 spectra) and using a Bayesian cross-correlation to log-likelihood approach, we measure a systemic velocity of 𝑉 sys = −11.51 +0.59 −0.60 km s −1 and a radial velocity semi-amplitude of 𝐾 P = 106.21 +1.76 −1.71 km s −1 for the planet, which results in an absolute mass of 𝑀 P = 6.24 +0.17 −0.18 M J and an orbital inclination of 41.6 +1.0 −0.9 degrees. Our retrieved 𝑉 sys shows a significant shift (+5 km s −1 ) from the literature value, which could be caused by an inaccurate time of periastron. Within the explored model grid, we measure a preference for solar water abundance (VMR = 10 −3 ) and no evidence for additional minor species in the atmosphere. Given the extensive orbital coverage of the data, we searched for a phase dependency in the water signal but found no strong evidence of variation with orbital phase. This detection is at odds with recent observations from SPIRou/CFHT and their tight upper limit on water abundance. We recommend further observations of the atmosphere 𝜏 Boötis Ab to try and resolve these discrepancies.

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“…We conducted a periodogram search for an outer planet in our RV data using RVSearch, an algorithm that iteratively searches for periodic signals in RV time series data (Rosenthal et al 2021). We finely sampled a grid of outer planet periods (P c ) with 31 < P c < 10,000 days.…”

Section: Periodogrammentioning

confidence: 99%

Kepler-1656b’s Extreme Eccentricity: Signature of a Gentle Giant

Angelo¹,

Naoz²,

Petigura³

et al. 2022

Self Cite

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Highly eccentric orbits are one of the major surprises of exoplanets relative to the solar system and indicate rich and tumultuous dynamical histories. One system of particular interest is Kepler-1656, which hosts a sub-Jovian planet with an eccentricity of 0.8. Sufficiently eccentric orbits will shrink in the semimajor axis due to tidal dissipation of orbital energy during periastron passage. Here our goal was to assess whether Kepler-1656b is currently undergoing such high-eccentricity migration, and to further understand the system’s origins and architecture. We confirm a second planet in the system with M c = 0.40 ± 0.09 M jup and Pc = 1919 ± 27 days. We simulated the dynamical evolution of planet b in the presence of planet c and find a variety of possible outcomes for the system, such as tidal migration and engulfment. The system is consistent with an in situ dynamical origin of planet b followed by subsequent eccentric Kozai–Lidov perturbations that excite Kepler-1656b’s eccentricity gently, i.e., without initiating tidal migration. Thus, despite its high eccentricity, we find no evidence that planet b is or has migrated through the high-eccentricity channel. Finally, we predict the outer orbit to be mutually inclined in a nearly perpendicular configuration with respect to the inner planet orbit based on the outcomes of our simulations and make observable predictions for the inner planet’s spin–orbit angle. Our methodology can be applied to other eccentric or tidally locked planets to constrain their origins, orbital configurations, and properties of a potential companion.

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The California Legacy Survey. I. A Catalog of 178 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades

Cited by 190 publications

References 135 publications

The Intrinsic Multiplicity Distribution of Exoplanets Revealed from the Radial Velocity Method

The Intrinsic Multiplicity Distribution of Exoplanets Revealed from the Radial Velocity Method

Water observed in the atmosphere of τ Bootis Ab with CARMENES/CAHA

Kepler-1656b’s Extreme Eccentricity: Signature of a Gentle Giant

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