Catalog of Nearby Exoplanets

By R. P. Butler, Jason T. Wright, G. Marcy, Debra A. Fischer, S. Vogt, C. Tinney, H. R. Jones, B. Carter, J. Johnson, C. McCarthy and 2 more. 2006

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We present a catalog of nearby exoplanets. It contains the 172 known low-mass companions with orbits established through radial velocity and transit measurements around stars within 200 pc. We include five previously unpublished exoplanets orbiting the stars HD 11964, HD 66428, HD 99109, HD 107148, and HD 164922. We update orbits for 83 additional exoplanets, including many whose orbits have not been revised since their announcement, and include radial velocity time series from the Lick, Keck, and Anglo-Australian Observatory planet searches. Both these new and previously published velocities are more precise here due to improvements in our data reduction pipeline, which we applied to archival spectra. We present a brief summary of the global properties of the known exoplanets, including their distributions of orbital semimajor axis, minimum mass, and orbital eccentricity.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/f20789de7ec421ef1d2e11d935b084787b661a45

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Citations in the corpus

Hot Jupiters in Binary Star Systems (2007, background): “Statistics from radial velocity planet searches (Marcy et al. 2005; Butler et al. 2006) show that the occurrence rate of giant planets within 0.1 AU (“hot-Jupiters”) is ∼ 1%; extrapolating to 20 AU the occurrence is 12%.”
Carbon monoxide and water vapor in the atmosphere of the non-transiting exoplanet HD 179949 b (2014, methodology): “…which implies the knowledge of the planet radial velocity curve, the velocity of the observer with respect to the barycenter of the solar system (Vobs(t)) and the systemic velocity of HD 179949, that is Vsys = (−24.35±0.18) km s−1(Butler et al. 2006): VP(t) = KP sin[2πϕ(t)] + Vobs(t) + Vsys.”
GIANT PLANET MIGRATION, DISK EVOLUTION, AND THE ORIGIN OF TRANSITIONAL DISKS (2009, methodology): “The null hypoth- 4 Where possible, we have updated the data from Fischer & Valenti (2005) using the improved orbital parameters given in Butler et al.(2006). esis is again not strongly rejected by a KS test, but the KS probability of 2% is somewhat lower than before: this illustrates the typical…”
Origins of Eccentric Extrasolar Planets: Testing the Planet-Planet Scattering Model (2007, methodology): “Previous work has shown that the bootstrap-style estimates of parameter uncertainties employed by Butler et al. (2006) can differ significantly from uncertainty estimates based on the posterior probability distribution for model parameters (Ford 2005; Gregory 2005, 2006).”
The planet search programme at the ESO CES and HARPS - IV. The search for Jupiter analogues around solar-like stars (2012, methodology): “We refined the orbital parameters with our data sets and included also the AAT (Butler et al. 2006) and CORALIE data (Naef et al. 2001) as shown in Fig.”
A New Planet around an M Dwarf: Revealing a Correlation between Exoplanets and Stellar Mass (2007, methodology): “To date, there are only two nearby M dwarfs known to harbor Jupiter–mass companions: GJ 876 (Marcy et al. 1998, 2001; Rivera et al. 2005) and GJ 849 (Butler et al. 2006a).”
HAT-P-7b: An Extremely Hot Massive Planet Transiting a Bright Star in the Kepler Field (2008, background): “We note that in order to get a reduced chi-square value near unity for the radial velocity fit, it was necessary to quadratically increase the noise component with an amplitude of 3.8 m s−1, which is well within the range of stellar jitter observed for late F stars; see Butler et al. (2006).”
RETIRED A STARS AND THEIR COMPANIONS. III. COMPARING THE MASS–PERIOD DISTRIBUTIONS OF PLANETS AROUND A-TYPE STARS AND SUN-LIKE STARS (2009, background): “This is in contrast to planets around solar-type stars, which have approximately uniform eccentricity distributions between 0.0 and 0.8 for semimajor axes & 0.3 AU (Butler et al. 2006; Wright et al. 2009).”
A Planetary Companion to the Hyades Giant ϵ Tauri (2007, background): “…have mainly observed thousands of nearby, field, and solar-type dwarfs by precise Doppler techniques, revealing about 200 extrasolar planets (e.g., Butler et al. 2006).7 The planets exhibit a wide variety in their properties such as mass, semimajor axis, eccentricity, and multiplicity (e.g.,…”
Extrasolar planet population synthesis - II. Statistical comparison with observations (2009, background): “At masses much larger than one Jupiter mass (& 7 MX), and especially in the DBP domain, the number of planets is clearly lower than inferred from the dN/dM ∝ M−1.05 law, again in good agreement with Marcy et al. (2005) or Butler et al. (2006).”
UNVEILING THE STRUCTURE OF PRE-TRANSITIONAL DISKS (2010, background): “Given the detection of over one hundred Jupitermass planets (Butler et al. 2006) and about one dozen Neptune-mass planets (see references within Endl et al. (2008)), it is natural to wonder if we can see evidence for the incipient stages of planet formation and particularly if pre-transitional…”
The Keck Planet Search: Detectability and the Minimum Mass and Orbital Period Distribution of Extrasolar Planets (2008, methodology): “Our value forα agrees with thedN/dM ∝ M−1.1 found by Butler et al. (2006a) by fitting the mass function of planets detected in the combined Keck, Lick, and AAT sur- FIG.”
THE FORMATION MECHANISM OF GAS GIANTS ON WIDE ORBITS (2009, neutral): “Since the total mass in planets is already quite large compared to other known planetary systems (Butler et al. 2006), we set the mass of the putative fourth body to be 7MJup.”
A BCool magnetic snapshot survey of solar-type stars (2013, background): “Epsilon Eridani is an active K-star (K2V according to the SIMBAD data base) and a possible planet hosting star (Hatzes et al. 2000; Butler et al. 2006; Benedict et al. 2006; Anglada-Escudé & Butler 2012) and as such its magnetic field properties are of significant interest in the study of the…”
Debris Disks around Sun-like Stars (2007, background): “…both bands (D. E. Backman et al., in preparation) and a planet orbiting it (Hatzes et al. 2000). a This star has a known planet orbiting at 2.03 AU (Butler et al. 2006). b The first line for HD 69830 here shows our naive solution for this system, based on the fluxes at 24 and 70 m, and assuming…”
Debris disc stirring by secular perturbations from giant planets (2009, background): “Exoplanet data are from Butler et al. (2006) for most planets, except forǫ Eridani (Benedict et al. 2006) and HD 69830 (Lovis et al. 2006).”
TIDALLY HEATED TERRESTRIAL EXOPLANETS: VISCOELASTIC RESPONSE MODELS (2009, background): “Study of tidal exoplanets is important partly because eccentricities in the overall exoplanet population are higher than expected (Butler et al. 2006; Tremaine & Zakamska 2004; Namouni 2005), e.g. GJ436b at e=0.15 (Deming et al. 2007), suggesting the importance and prevalence of multiple planet…”
TERRESTRIAL PLANET OCCURRENCE RATES FOR THE KEPLER GK DWARF SAMPLE (2015, background): “However, radial velocity studies have revealed that eccentric orbits are common for Porb>10 days (Butler et al. 2006).”