An Excess of Jupiter Analogs in Super-Earth Systems

  title={An Excess of Jupiter Analogs in Super-Earth Systems},
  author={Marta L. Bryan and Heather A. Knutson and Eve J. Lee and Benjamin J. Fulton and Konstantin Batygin and Henry Ngo and Tiffany Meshkat},
  journal={The Astronomical Journal},
We use radial velocity (RV) observations to search for long-period gas giant companions in systems hosting inner super-Earth (1–4 R⊕, 1–10 M⊕) planets to constrain formation and migration scenarios for this population. We consistently refit published RV data sets for 65 stars and find nine systems with statistically significant trends indicating the presence of an outer companion. We combine these RV data with AO images to constrain the masses and semi-major axes of these companions. We… 

Kepler-167e as a Probe of the Formation Histories of Cold Giants with Inner Super-Earths

The observed correlation between outer giant planets and inner super-Earths is emerging as an important constraint on planet formation theories. In this study, we focus on Kepler-167, which is

Mutual Orbital Inclinations between Cold Jupiters and Inner Super-Earths

Previous analyses of Doppler and Kepler data have found that Sun-like stars hosting “cold Jupiters” (giant planets with a ≳ 1 au) almost always host “inner super-Earths” (1–4 R⊕, a ≲ 1 au). Here we

Revisiting the Long-period Transiting Planets from Kepler

Currently, we have only limited means to probe the presence of planets at large orbital separations. Foreman-Mackey et al. searched for long-period transiting planets in the Kepler light curves using

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

  • Wei Zhu
  • Geology, Physics
    The Astronomical Journal
  • 2022
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

Occurrence rates of small planets from HARPS

Context. The stars in the Milky Way thin and thick disks can be distinguished by several properties such as metallicity and kinematics. It is not clear whether the two populations also differ in the

The Magellan-TESS Survey. I. Survey Description and Midsurvey Results

Kepler revealed that roughly one-third of Sunlike stars host planets orbiting within 100 days and between the size of Earth and Neptune. How do these planets form, what are they made of, and do they

TESS-Keck Survey. IX. Masses of Three Sub-Neptunes Orbiting HD 191939 and the Discovery of a Warm Jovian plus a Distant Substellar Companion

Exoplanet systems with multiple transiting planets are natural laboratories for testing planetary astrophysics. One such system is HD 191939 (TOI 1339), a bright (V = 9) and Sun-like (G9V) star,

Formation of planetary systems by pebble accretion and migration

At least 30% of main sequence stars host planets with sizes of between 1 and 4 Earth radii and orbital periods of less than 100 days. We use N-body simulations including a model for gas-assisted

Transiting Planets Near the Snow Line from Kepler. I. Catalog

We present a comprehensive catalog of cool (period P ≳ 2 yr) transiting planet candidates in the 4 yr light curves from the prime Kepler mission. Most of the candidates show only one or two transits

The Pan-Pacific Planet Search – VIII. Complete results and the occurrence rate of planets around low-luminosity giants

Our knowledge of the populations and occurrence rates of planets orbiting evolved intermediate-mass stars lags behind that for solar-type stars by at least a decade. Some radial velocity surveys



Statistics of Long Period Gas Giant Planets in Known Planetary Systems

We conducted a Doppler survey at Keck combined with NIRC2 K-band adaptive optics (AO) imaging to search for massive, long-period companions to 123 known exoplanet systems with one or two planets


We report the discovery of two super-Earth-mass planets orbiting the nearby K0.5 dwarf HD 7924, which was previously known to host one small planet. The new companions have masses of 7.9 and 6.4 M ⨁

Transiting Planet Candidates Beyond the Snow Line Detected by Visual Inspection of 7557 Kepler Objects of Interest

We visually inspected the light curves of 7557 Kepler Objects of Interest (KOIs) to search for single transit events (STEs) that were possibly due to long-period giant planets. We identified 28 STEs

The Planet-Metallicity Correlation

We have recently carried out spectral synthesis modeling to determine Teff, log g, v sin i, and [Fe/H] for 1040 FGK-type stars on the Keck, Lick, and Anglo-Australian Telescope planet search


We present precision radial velocity data that reveal a multiple exoplanet system orbiting the bright nearby G5V star 61 Virginis. Our 4.6 years of combined Keck/HIRES and Anglo-Australian Telescope

The California-Kepler Survey. IV. Metal-rich Stars Host a Greater Diversity of Planets

Probing the connection between a star’s metallicity and the presence and properties of any associated planets offers an observational link between conditions during the epoch of planet formation and

A super-Earth orbiting the nearby M-dwarf GJ 536

We report the discovery of a super-Earth orbiting the star GJ 536 based on the analysis of the radial-velocity time series from the HARPS and HARPS-N spectrographs. GJ 536 b is a planet with a

The Impact of Stellar Multiplicity on Planetary Systems, I.: The Ruinous Influence of Close Binary Companions

The dynamical influence of binary companions is expected to profoundly influence planetary systems. However, the difficulty of identifying planets in binary systems has left the magnitude of this

Dynamically Hot Super-Earths from Outer Giant Planet Scattering

The hundreds of multiple planetary systems discovered by the Kepler mission are typically observed to reside in close-in ( AU), low-eccentricity, low-inclination orbits. We run N-body experiments to


A search of the time-series photometry from NASA's Kepler spacecraft reveals a transiting planet candidate orbiting the 11th magnitude G5 dwarf KIC 10593626 with a period of 290 days. The