FRIENDS OF HOT JUPITERS. I. A RADIAL VELOCITY SEARCH FOR MASSIVE, LONG-PERIOD COMPANIONS TO CLOSE-IN GAS GIANT PLANETS

By H. Knutson, B. Fulton, B. Montet, M. Kao, H. Ngo, Andrew W. Howard, J. Crepp, S. Hinkley, Gáspár Á. Bakos, K. Batygin and 3 more. 2013

198 citations recorded by the source corpus.

In this paper we search for distant massive companions to known transiting gas giant planets that may have influenced the dynamical evolution of these systems. We present new radial velocity observations for a sample of 51 planets obtained using the Keck HIRES instrument, and find statistically significant accelerations in fifteen systems. Six of these systems have no previously reported accelerations in the published literature: HAT-P-10, HAT-P-22, HAT-P-29, HAT-P-32, WASP-10, and XO-2. We combine our radial velocity fits with Keck NIRC2 adaptive optics (AO) imaging data to place constraints on the allowed masses and orbital periods of the companions responsible for the detected accelerations. The estimated masses of the companions range between 1–500 MJup, with orbital semi-major axes typically between 1–75 AU. A significant majority of the companions detected by our survey are constrained to have minimum masses comparable to or larger than those of the transiting planets in these systems, making them candidates for influencing the orbital evolution of the inner gas giant. We estimate a total occurrence rate of 51% ± 10% for companions with masses between 1–13 MJup and orbital semi-major axes between 1–20 AU in our sample. We find no statistically significant difference between the frequency of companions to transiting planets with misaligned or eccentric orbits and those with well-aligned, circular orbits. We combine our expanded sample of radial velocity measurements with constraints from transit and secondary eclipse observations to provide improved measurements of the physical and orbital characteristics of all of the planets included in our survey.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/ed8f11d5279066145a6083e7d16c834a539fade0

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Citations in the corpus

The Apparently Decaying Orbit of WASP-12b (2017, background): “One possibility is gravitational forcing by another planet, although no other nearby planets are known in the WASP-12 system (Knutson et al. 2014).”
The GAPS Programme with HARPS-N at TNG - XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets (2017, unknown): “Long-term RV monitoring is also essential in order to discover long-period companions, derive their orbital parameters, and thus investigate their possible inﬂuence on the eccentricity and obliquity of the orbits of the close-in giant planets (e.g. Matsumura et al. 2010; Knutson et al. 2014).”
WASP-47: A HOT JUPITER SYSTEM WITH TWO ADDITIONAL PLANETS DISCOVERED BY K2 (2015, background): “…of Technology, Cambridge, MA 02139, USA 6 Planet Hunter While systems exist with a known hot Jupiter and a distant (& 200-day period) companion (Knutson et al. 2014; Endl et al. 2014) or a warm Jupiter (orbital period 6.3 - 15.8 days) and a close-in planet (for example, KOI 191: Steffen et al.…”
Unresolved stellar companions with Gaia DR2 astrometry (2020, methodology): “…13 hosts with known companions within 1.1 arcsec, namely: HAT-P-14, HAT-P8, HD 68988, HD 86081, WASP-36, WASP-3, XO-5, HAT-P-24, HAT-P-30, HAT-P-33, HD 109749, WASP-48, and WASP-76 (see Knutson et al. 2014; Ngo et al. 2015; Piskorz et al. 2015; Bryan et al. 2016; Evans, Southworth & Smalley 2016b).”
SPITZER SECONDARY ECLIPSES OF THE DENSE, MODESTLY-IRRADIATED, GIANT EXOPLANET HAT-P- 20 b ?> USING PIXEL-LEVEL DECORRELATION (2014, methodology): “To close the loop on this system, we have derived new orbital parameters using a joint MCMC fit of the RV and secondary eclipse timings, as described by Knutson et al. (2014).”
SOAR TESS Survey. I. Sculpting of TESS Planetary Systems by Stellar Companions (2019, background): “…similar to the majority of planets detected by Kepler, and many large planets, 12 The Astronomical Journal, 159:19 (24pp), 2020 January Ziegler et al. similar to the extensively studied population of hot Jupiters (e.g., Wu et al. 2007; Knutson et al. 2014; Evans et al. 2016; Ngo et al. 2016).”
The Eccentric Kozai-Lidov Effect and Its Applications (2016, background): “The observational studies that showed that Hot Jupiters are likely to have far away companion (e.g., Knutson et al. 2014; Ngo et al. 2015; Wang et al. 2015) promoted further investigations of two planet systems.”
Limits on Planetary Companions from Doppler Surveys of Nearby Stars (2016, methodology): “…analyses of the long-period accelerations in the Keck RV time series have been used to estimate the fraction of stars with wide-orbit planets (Knutson et al. 2014; Montet et al. 2014) For this Doppler planet search completeness study, we analyzed RVs from four instruments with independent RV…”
CHARACTERIZING THE COOL KOIs. VII. REFINED PHYSICAL PROPERTIES OF THE TRANSITING BROWN DWARF LHS 6343 C (2014, methodology): “Following Torres (1999) and Knutson et al. (2014), the maximum RV acceleration is defined such that |v̇| < 68.8m s−1 yr−1 ( Mcomp MJup )( d pc ρ arcsec )−2 , (1) for a system at a distance d, with a companion with mass Mcomp at an angular separation ρ.”
EXTRACTING RADIAL VELOCITIES OF A- AND B-TYPE STARS FROM ECHELLE SPECTROGRAPH CALIBRATION SPECTRA (2015, background): “…is separation in arcseconds between the primary and companion, d(RV )dt is the radial velocity trend, and Φ is a function of the inclination angle, eccentricity, longitude of periastron, and phase in orbit, which assumes a minimum value of √ 27/2 (Torres 1999; Liu et al. 2002; Knutson et al. 2014).”
ASTROMETRIC EXOPLANET DETECTION WITH GAIA (2014, background): “Gaia astrometry may nonetheless clarify the existence of massive outer companions of hot Jupiters, which have been invoked to explain their inward migration (e.g. Bakos et al. 2009; Neveu et al. 2013; Knutson et al. 2014).”